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Cover Caption
Using the Okayama 188 cm telescope and multi-band camera MuSCAT (bottom of the back cover),researchers succeeded in observing the extrasolar planet K2-3d (top of the back cover, artistic
visualization), which is about the same size and temperature as the Earth, pass in front of its host star
(top of the cover, artistic visualization) blocking some of the stellar light (bottom of the cover).
Credit: NAOJ

Postscript
Editor Publications Committee
HANAOKA, Yoichiro
UEDA, Akitoshi
OE, Masafumi
SÔMA, Mitsuru
NISHIKAWA, Jun
HIROTA, Tomoya
YOSHIDA, Haruo
Publisher

PrinterNational Institutes of Natural Sciences

National Astronomical Observatory of Japan
2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan
TEL: +81-422-34-3600
FAX: +81-422-34-3960
http://www.nao.ac.jp/
Kyodo Telecom System Information Co., Ltd.
4-34-17 Nakahara, Mitaka-shi, Tokyo 181-0005, Japan
TEX: +81-422-46-2525
FAX: +81-422-46-2528

Annual Report of the
National Astronomical Observatory of Japan

Volume 19, Fiscal 2016

T A

B

L

Preface

E

O F

C

O N T

E

N

Masahiko HAYASHI
Director General
National Astronomical Observatory of JapanI Scientific Highlights April 2016 – March 2017001

II Status Reports of Research Activities
01. Subaru Telescope
02. Okayama Astrophysical Observatory
03. Nobeyama Radio Observatory
04. Mizusawa VLBI Observatory
05. Solar Observatory
06. NAOJ Chile Observatory
07. Center for Computational Astrophysics
08. Hinode Science Center
09. Gravitational Wave Project Office
10. TMT-J Project Office
11. JASMINE Project Office
12. Extra-Solar Planet Detection Project Office
13. RISE Project Office
14. Solar-C Project Office
15. Astronomy Data Center
16. Advanced Technology Center
17. Public Relations Center
18. Division of Optical and Infrared Astronomy
19. Division of Radio Astronomy
20. Division of Solar and Plasma Astrophysics
21. Division of Theoretical Astronomy
22. Office of International Relations

067
071
075
078
082
084
087
090
092
095
098
100
102
103
104
106
113
120
122
125
126
130

T

S

III Organization132

IV Finance

153

V KAKENHI (Grants-in-Aid for Scientific Research)

154

VI Research Collaboration

155

VII Graduate Course Education

157

VIII Public Access to Facilities

162

IX Overseas Travel

166

X Award Winners

167

XI Library, Publications168

XII Important Dates

169

XIII Publications, Presentations
1. Refereed Publications

172

2. Publications of the National Astronomical Observatory of Japan

187

3. Report of the National Astronomical Observatory of Japan188

4. Conference Proceedings

188

5. Publications in English

193

6. Conference Presentations

194

Annual Report of the
National Astronomical Observatory of Japan
Volume 19, Fiscal 2016

P R E FA C E

Masahiko HAYASHI
Director General of NAOJ

It is my pleasure to present the Annual Report of the
National Astronomical Observatory of Japan.

and the main interferometer, which creates laser lightinterference patters with orthogonal 3 km arms. With KAGRAIn February of 2016, it was announced that LIGO had

added to the LIGO and VIRGO gravitational wave detector

directly detected gravitational waves. Currently in Japan, thenetwork, the locations of gravitational wave sources will be

Large-scale Cryogenic Gravitational Wave Telescope KAGRA

able to be determined with a precision of a couple of degrees.

is being constructed in Kamioka, led by the University of

Follow-up observations by electromagnetic telescopes will

Tokyo Institute for Cosmic Ray Research (ICRR) together

further advance this research, giving us detailed insight intowith the National Astronomical Observatory of Japan (NAOJ)

the nature of black holes and neutron stars. Multi-messenger

and the High Energy Accelerator Research Organization

astronomy has already begun.

(KEK). Attempts in Japan to directly detect gravitational

ALMA started Cycle 4 observations from October 2016.

waves began in the 1970’s with the creation of a resonant-

The number of observational proposals submitted frommass detector by Dr. Hiromasa Hirakawa at the University ofaround the world reached 1600, surpassing the Hubble SpaceTokyo. Laser interferometer type detectors started at NAOJ

Telescope. In June of every year, 150 leading astronomers

from the 1980’s; and in the 1990’s TAMA300 with 300 m

from the various countries assemble and spend days cooped

arm-lengths was completed and succeeded in continuous

up in a hotel, holding meetings to examine these proposals

operation. At NAOJ, making the best use of experiences likeand adopt about 400 of them. In Japan, more than half of thethese, the Advanced Technology Center has been developing

proposals were written by young researchers such as graduate

key components for KAGRA such as the end mirror vibration

students and post-docs.

isolation systems, utilizing 14 m high multistage pendulums,

Almost 1/4 of ALMA’s observations are occupied withplanetary system formation observations. When I was an

we will be able to pursue the evolution of the large-scale

undergraduate student, more than 35 years ago, I read astructure of the Universe and get closer to understanding thereview paper of the “Kyoto Model.” I remember thinking, “Ittrue nature of dark matter and dark energy.

is a beautiful model. But to actually observe planets forming

Regarding the open question of TMT, in FY 2016 thein the Universe, high resolution better than 1 arcsecond

Hawai`i State Board of Land and Natural Resources held

would be needed. I don’t think I’ll see planetary systempublic hearings with area residents about reissuing theformation observations within my lifetime.” Now, multiple

Maunakea Science Reserve Use Permit, resulting in a newring structures, like those seen in the HL Tauri protoplanetarypermit being issued in September 2017. Thanks to continuing

disk, are being discovered around one young star after

dialog between TMT International Observatory and the local

another. I expect that by observing the disks of many young

residents, in Hilo Hawai`i the number of people supportingstars, we will be able to see the structural evolution of thethe construction of TMT is now higher than ever.

protoplanetary disks generated as a result of planetary systemformation.

From the experience with the Subaru Telescope, theresistance in the Japanese astronomy community to building

Thanks to ALMA’s extremely high sensitivity, it detected

telescopes overseas disappeared. For ALMA it was a natural

the redshifted 88 μm wavelength emission line of ionizedassumption that the telescopes would be arrayed overseas; theoxygen coming from a galaxy more than 13.1 billion light-

construction and operation also proceeded as an international

years away discovered by the Subaru Telescope. This emission

project. For NAOJ, that was a new challenge. Fortunately,line is a good indicator of star formation activity. But becausewith the incorporation of NAOJ in 2004 the personnel system

it is in the far infrared, it can’t be observed from the ground,

for academic faculty was reconsidered and the project system

so previously it had only been observed by using flying

was established, changing the organizational structure to give

instruments. But when the redshift exceeds 3 (i.e. the distanceit the flexibility needed for large international projects. It also

exceeds 12 billion light-years) the observed wavelength of

became possible to have people with exceptional, specialized

this emission line shifts to submillimeter waves, making it

skills participate in large international projects as contract

visible to ALMA. This is an excellent observational method to

employees. Moreover by representing Japan in this kind ofunderstand the details of star formation in the early Universe

large international project, NAOJ’s duty as an inter-university

and the history of element production.

research institute became better defined; this role has

At the Subaru Telescope, the strategic program using the

become making great contributions to strengthening researchultra-wide-field prime-focus camera (Hyper Suprime-Cam) isthroughout all of Japan in the field of astronomy. Based onproceeding smoothly. This camera’s survey speed (= limiting

considerations like these, from here forward we would likemagnitude x field of view area) is more than 10 times thatto continue efforts towards realizing large-scale internationalof previous surveys. Equipped with this camera, the Subaru

collaboration projects.

Telescope will without a doubt be on the world’s leading edgeof observations until the U.S.A.’s Large Synoptic Survey
Telescope starts operation in the mid-2020’s.
In February 2017, roughly 60 nights of data taken as partof this strategic program were made available in Public Data
Release 1. The largest data set covers 108 square degrees
on the sky. The data was taken in 9 colors. The limiting
magnitude is 26.4 mag with the red filter. The stellar image
size is 0.6 to 0.8 arcsecond. There is no comparable data set in
the world. By the way the volume of the data set is equivalent
to 10 million pictures taken with a normal digital camera.
Ultimately, the survey will be 10 times this size, acquiring
data across 1400 square degrees on the sky. Observations with
Hyper Suprime-Cam will elucidate the distribution of dark
matter across wide regions (and in terms of distance, about
90 % of the way out to the edge of the Universe). Hopefully

Masahiko HAYASHI
Director General of NAOJ

I Scientific Highlights(April 2016 – March 2017)
01 Oxygen Abundance Determination of B-type Stars with O I 7771-5 Å Lines

Takeda, Y., Honda, S.

003

IRIS, Hinode, SDO, and RHESSI Observations of a White Light are Produced Directly by
Non-thermal Electrons

Lee, K.-S., et al.

004

03 Impact of New Gamow-Teller Strengths on Explosive Type Ia Supernova Nucleosynthesis

Mori, K., et al.

005

Imanishi, M., et al.

006

02

04 Compact Dense Molecular Gas Emission at the Putative AGN Location in NGC 1068
05

ALMA Molecular Line Observations of Luminous Infrared Galaxies as a Tool to Detect
Extremely Deeply Buried AGNs

Imanishi, M., et al.

007

06

Dense Molecular Gas Emission and Infrared Radiative Pumping in the Ultraluminous
Infrared Galaxy IRAS 20551−4250

Imanishi, M., et al.

008

Zenitani, S., Nagai, T.

009

Tanaka, M.

010

Hirai, Y., et al.

011

10 Magnetic Properties of Solar Active Regions That Govern Large Solar Flares and Eruptions

Toriumi, S., et al.

012

11 Various Local Heating Events in the Earliest Phase of Flux Emergence

Toriumi, S., et al.

013

Wong, K. C., et al.

014

Terai, T., et al.

015

Onodera, M., et al.

016

15 Imaging of Diffuse H I Absorption Structure in the SSA22 Protocluster Region at z = 3.1

Mawatari, K., et al.

017

16

Properties of Interstellar Dust Responsible for Steep Extinction Curves toward Type Ia
Supernovae

Nozawa, T.

018

17

Formation of Overheated Regions and Truncated Disks around Black Holes;
Three-dimensional General Relativistic Radiation-magnetohydrodynamics Simulations

Takahashi, H., et al.

019

Wakita, S., et al.

020

07 New Electron Orbits in Collisionless Magnetic Reconnection
08 Kilonova Emission from Compact Binary Mergers
09 Chemodynamical Evolution of Dwarf Galaxies Deduced from r-process Elements

12

H0LiCOW - Lens Mass Model of HE 0435-1223 and Blind Measurement of Its Time-delay
Distance for Cosmology

13 Photometric Measurements of H2O Ice Crystallinity on TNOs
14 ISM Excitation and Metallicity of Star-forming Galaxies at z  3.3 from Near-IR Spectroscopy

18 Chondrule Formation by Planetesimal Collisions
19

Revisiting the Completeness and Luminosity Function in High-redshift Low-luminosity
Quasar Surveys

Niida, M., et al.

021

20

Near-infrared Spectroscopy of Nearby Seyfert Galaxies for Examinig the Ionization
Mechanism of Narrow-line Regions

Terao, K., et al.

022

Tagawa, H., et al.

023

21 Mergers of Accreting Stellar-mass Black Holes22

The Validation of Made-to-measure Method for Reconstruction of Phase Space Distribution
FunctionsTagawa, H., et al.

024

23

Nitrogen Isotopic Ratio of Cometary Ammonia from High-resolution Optical Spectroscopic
Observations of C/2014 Q2 (Lovejoy)

Shinnaka, Y., Kawakita, H.

025

24

Ortho-to-Para Abundance Ratios of NH2 in 26 Comets: Implications for the Real Meaning of
OPRs

Shinnaka, Y., et al.

026

25

Nitrogen Isotopic Ratios of NH2 in Comets: Implication for 15N-Fractionation in Cometary
Ammonia

Shinnaka, Y., et al.

027

26

Imaging Observations of Entire Hydrogen Coma of Comet 67P/Churyumov-Gerasimenko in2015 September

Shinnaka, Y., et al.

028

27 Record-breaking Faint Satellite Galaxy of the Milky Way Discovered

Homma, D., et al.

029

28 Large Scale Environment of the Most Massive SMBHs

Shirasaki, Y., et al.

030

Takekoshi, T., et al.

031

29

The 1.1 mm Continuum Survey of the Small Magellanic Cloud: Physical Properties andEvolution of the Dust-selected Clouds001

30 Circumstellar and Explosion Properties of Type Ibn Supernovae

Moriya, T., Maeda, K.

032

Moriya, T.

033

32 Supernovae Powered by Magnetars That Transform into Black Holes

Moriya, T., et al.

034

33

Moriya, T., et al.

035

Yagi, M., et al.

036

Furusawa, H., et al.

037

31 Radio Transients Associated with Accretion-induced Collapse of White Dwarfs
Properties of Magnetars Mimicking 56Ni

34 Catalog of Ultra Diffuse Galaxies in the Coma Cluster
35 Lyα Rate of UV-bright Star-forming Galaxies at Redshift 7
36

A Spectroscopically Confirmed Double Source Plane Lens System in the Hyper SuprimeCam Subaru Strategic Program

Tanaka, M., et al.

038

37

Thermo‑optical Simulation and Experiment for the Assessment of Single, Hollow, and Large
Aperture Retroreflector for LLR

Araki, H., et al.

039

38 The Far Distance to G7.47+0.06 from Proper Motion Measurement of H2O Masers

Yamauchi, A., et al.

040

39 Enhanced Star Formation of Less Massive Galaxies in a Proto-Cluster at z = 2.5

Hayashi, M., et al.

041

Fukui, A., et al.

042

41 Astrometry of H2O Masers in Massive Star-forming Region S255IR-SMA1

Burns, R. A., et al.

043

42 Developments of Millimeter-wave MKID Camera

Sekimoto, Y., et al.

044

43 Formation of Spiral Arm in Galaxies by Swing Amplification

Michikoshi, S., Kokubo, E.

045

44 Planetesimal Formation by Gravitational Instability of Porous-Dust AggregatesMichikoshi, S., Kokubo, E.

046

45 N-Body Simulation of Chariklo’s Ring

Michikoshi, S., Kokubo, E.

047

Kawakita, H., et al.

048

Noda, H., et al.

049

48 Spiral Structure and Differential Dust Size Distribution in the LkHα 330 Disk

Akiyama, E., et al.

050

49 Seasonal Variation of the Radial Brightness Contrast of Saturn’s Rings Viewed in Mid-infrared

Fujiwara, H., et al.

051

Discovery of Ubiquitous Fast-propagating Intensity Disturbances by the Chromospheric
Lyman Alpha Spectropolarimeter (CLASP)

Kubo, M., et al.

052

51 High-contrast Imaging of Intermediate-mass Giants with Long-term Radial Velocity Trends

Ryu, T., et al.

053

Shin, J. W., et al.

054

53 Heavy Element Synthesis in Type II Supernovae: Sensitivity to Nuclear Equation of States

Famiano, M. A., et al.

055

54 Relativistic Screening Effects on Big Bang Nucleosynthesis and Low-lying Resonances

Famiano, M. A., et al.

056

55 Detectability of Cosmic Dark Flow in the Type Ia Supernova Redshift-Distance Relation

Mathews, G. J., et al.

057

56 Impact of Sterile Neutrino Dark Matter on Core-collapse Supernova Explosion

Warren, M. L., et al.

058

40 Transit Observation of Potentially Habitable Super-Earth K2-3d with Okayama188 cm/MuSCAT

46

Mid-Infrared Spectroscopic Observations of the Classical Nova V2676 Oph with Subaru/
COMICS

47 Success of a Laser Link Experiment with the Hayabusa2 Laser Altimeter

50

52

New Neutrino Source for the Study of Solar Neutrino Physics in the Vacuum-matter
Oscillation Transition Region

57

Neutrino Antineutrino Pair Emissions in Strongly Magnetized Neutron-Star-Matter in
Relativistic Quantum Approach

Maruyama, T., et al.

059

58

Possible Measurements of Reaction Cross Sections for Explosive Nucleosynthesis using
Laser -Driven γ-ray Pulses

Hayakawa, T., et al.

060

59

Isomer Producution Ratio of 113Cd following Neutron-Capture Reactions to Investigate theOrigin of 115Sn

Hayakawa, T., et al.

061

60

Solving the Red Supergiant and Supernova Rate Problems via Relic Supernova Neutrino
SpectrumHidaka, J., et al.

062

He, J., et al.

063

Inoue, A. K., et al.

064

63 Terahertz and Far-Infrared Windows Opened at Dome A in Antarctica

Shi, S.-C., et al.

065

64 Development of Terahertz Photon Counting Detectors

Matsuo, H., et al.

066

61 Non-Extensive Statistics Solution to the Cosmological Lithium Problem
62002

Detection of an Ionized Oxygen Emission Line from a High Redshift Galaxy in theReionization Era

Oxygen Abundance Determination of B-type Stars
with O I 7771–5 Å Lines
TAKEDA, Yoichi(NAOJ)		

It is known that anomalous abundances are observedin specific light elements (e.g., C or N) in B-type mainsequence stars, which are interpreted as due to mixing
caused by rotation-induced meridional circulation.
However, the appreciable He enrichment in B-type stars
once reported by [1] can not be explained within theframework of the canonical theory of stellar evolution.
If this is real, it would require a special non-canonicaldeep mixing extending to the core where transformationof H→He takes place. Yet, given that He abundance
determination from strong He lines is difficult (which
critically depends on a choice of microturbulent velocity)and the conclusion of [1] may not necessarily be reliable.
In this context, oxygen abundances play a key role,since an appreciable He-enrichment should accompany
a significant O-deficit due to dredge-up of ON-cycle
product from the deep core region. So, the necessity/
existence of non-canonical mixing may be judged byexamining the surface oxygen abundances of B stars,
where the standard calculation predicts negligibly small
O-anomaly ([2]).
Motivated by this consideration, we decided to
conduct an O-abundance analysis for a well-definedsample of B-type stars, while employing the O I 7771–5 Åtriplet lines. The observations for selected 34 targets(where Be stars and B supergiants are not included)
in a wide range of ve sin i (~ 0–250 km s−1) as well as
T eff (~ 10000–28000 K) were carried out mostly in2015 September by using the MALLS spectrographattached to the 2 m NAYUTA telescope at Nishi-Harima
Astronomical Observatory of Hyogo University. The
resolving power and typical signal-to-noise ratio of thespectra are R ~ 12000 and S/N ~ 200–300, respectively.
By using the atmospheric parameters determined fromuvbyβ colors, we derived the oxygen abundances byapplying the spectrum-fitting technique to the O I triplet
lines while taking into account the non-LTE effect. The
following conclusions were obtained:— The strength of O I 7771–5 Å lines decreases with anincrease in Teff, while the non-LTE effect is considerablylarge for both late-B as well as early-B stars (non-LTE
abundance correcton is on the order of ~ −1 dex) and thus
has to be taken into account by all means.
— The resulting oxygen abundances of our sample stars
distribute around the solar abundance and do not show
any systematic dependence upon ve sin i as well as Teff,
which means that any meaningful oxygen abundance
anomaly is not observed.
— Since this doe not contradict the prediction fromHONDA, Satoshi(University of Hyogo)

the standard stellar evolution calculations (e.g., [2]),the appreciable enrichment of surface He abundancesuggested by [1] may be questionable and worth
reinvestigation.
See [3] for more details of this study.
HR 7437
HR 7106
HR 0708
HR 6779
HR 7739
HR 7121
HR 8634
HR 7236
HR 7528
HR 8418
HR 8781
HR 7906
HR 7963
HR 7306
HR 8522
HR 8301
HR 7178
HR 7447
HR 8579
HR 7592
HR 7372
HR 0718
HR 7852
HR 8335
HR 6787
HR 7298
HR 7039
HR 7613
HR 7710
HR 8797
HR 8238
HR 7426
HR 7773
HR 0779

0.2

7700

7750

Wavelength (Å)

7800

7850

Figure 1: Spectra of our 34 target stars in the 7700–7850 Å region,
which are arranged in the descending order of ve sin i.

circles: Teff < 15000 K
triangles: Teff > 15000 K

solar abundance

9
AN

				

8
0

100
200 10000-1ve sin i (km s )20000
Teff (K)

30000

Figure 2: The resulting AN (non-LTE oxygen abundance) plottedagainst ve sin i as well as Teff.
References[1] Lyubimkov, J. S., et al.: 2004, MNRAS, 351, 745.
[2] Georgy, C., et al.: 2013, A&A, 553, 24.
[3] Takeda, Y., Honda, S.: 2016, PASJ, 68, 32.

I Scientific Highlights

003

IRIS, Hinode, SDO, and RHESSI Observations of a White Light
are Produced Directly by Non-thermal Electrons
LEE, Kyoung-Sun1, IMADA, Shisuke2, WATANABE, Kyoko3, BAMBA, Yumi4, BROOKS, David H.5
1: NAOJ, 2: Nagoya University, 3: National Defense Academy of Japan, 4: Institute of Space and Astronautical Science, 5: George Mason
University

Sometimes strong solar flares produce continuum
enhancements as a photospheric response, which istermed a white light flare (WLF). Previous observations
showed that the continuum enhancement in WLFs is wellcorrelated with hard X-ray emission both spatially andtemporally [1,2]. From the correlation, it has been thoughtthat WLFs are produced by the transported energy fromaccelerated particles such as non-thermal electrons [3].
With recent high spatial resolution observations, WL
emission has been reported even in weak flares [4]. The
electron flux from these low energy events is not enoughto penetrate and heat the photosphere directly. Therefore,
other heating mechanisms have also been considered. For
example, WL emission is produced by electrons that heat
the chromosphere directly and the photosphere indirectly[5]. However, the true heating mechanism in the lower
atmosphere remains unclear.
(a)

(b)

(c)

(d)
HMI Continuum

(e)

(f)

(g)

(h)
HMI Continuum
running diff(i)

IRIS SJI CII 1330
Hinode EIS Fe XII 195

(j)

(k)

(l) 22-Oct-2014 14:06:43.179 UT

IRIS SJI CII 1330
Polarity Inversion Line

-300

-250
X (arcsecs)

-200

-150

Figure 1: Context images for the X1.6 class flare. (a-c): AIA
211 Å, (e-g): AIA 1700 Å, (i-k): IRIS C II 1330 Å slit
jaw images with EIS 195 Å intensity contours (grayline) before the flare, at the first HXR peak, and at theflare peak. (d, h): SDO/HMI continuum and a running
difference image at HXR peak, respectively. (l): thepolarity inversion line from the HMI magnetogram. The
bright kernel we analyzed is marked with an arrow.

We have investigated An X1.6 flare occurred in
AR 12192 on 2014 October 22 at 14:02 UT which wasobserved by several spectrometer in multi-wavelengths,
Hinode, IRIS, SDO, and RHESSI (Figure 1). We analyzea bright kernel which produces a WLF with continuum004

I Scientific Highlights

enhancement and a HXR peak. Taking advantage of thespectroscopic observations of IRIS and Hinode/EIS, we
measure the temporal variation of the plasma propertiesand dynamics in the bright kernel through chromosphereand corona. We found that explosive evaporation wasobserved when the WL emission occurred, even though
the intensity enhancement in hotter lines is quite weak.
The temporal correlation of the WL emission, HXR peak,and evaporation flows indicate that the WL emission was
produced by accelerated electrons.
To understand the WL emission process, we calculated
the energy flux deposited by non-thermal electronsobserved by RHESSI and compared it to the dissipatedenergy estimated from a chromospheric line (Mg II triplet)
observed by IRIS. The deposited energy flux from thenon-thermal electrons is about 3 ~ 7.7 × 1010 erg cm−2 s−1
for a given low energy cut-off of 30 ~ 40 keV, assuming
the thick target model. The energy flux estimated fromthe temperature changes in the chromosphere measured
using the Mg II subordinate line is about 4.6–6.7 ×
109 erg cm−2 s−1: ~ 6–22 % of the deposited energy. This
comparison of estimated energy fluxes implies that thecontinuum enhancement was directly produced by the
non-thermal electrons.
This research has been published to the AstrophysicalJournal in 2017 [6].

References[1] Neidig, D. F.: 1989, Sol. Phys., 121, 261.
[2] Watanabe, K., et al.: 2010, ApJ, 715, 651.
[3] Brown, J. C.: 1971, Sol. Phys., 18, 489.
[4] Hudson, H. S.,Wolfson, C. J., Metcalf, T. R.: 2006, Sol. Phys.,234, 79.
[5] Machado, M. E., Emslie, A. G., Avrett, E. H.: 1989, Sol. Phys.,
124, 303.
[6] Lee, K.-S., et al.: 2017, ApJ, 836, 150.

Impact of New Gamow-Teller Strengths
on Explosive Type Ia Supernova Nucleosynthesis
FAMIANO, Michael(NAOJ/Western Michigan University)

		

IWAMOTO, Koichi

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

HIDAKA, Jun

HONMA, Michio(Meisei University)		

(Aizu University)

NOMOTO, Ken’ichi, OTSUKA, Takaharu(Nihon University)			

Type Ia supernovae (SNe Ia) are thought to be athermonuclear explosion on accreting white dwarfs. SNe
Ia produce a large amount of iron group elements andplay an important role on galactic chemical evolution.
However, it is known that some of neutron-excess nuclei
are overproduced compared with solar abundance inconventional network calculations [1].
Electron capture heavily affects nucleosynthesis
because density at the center of SNe Ia reaches higher
than 10 9 g/cm 3 . Recently the Gamow-Teller (GT)transition strength of an unstable nucleus 56 Ni wasmeasured [2] and it was shown that a conventional theory
did not reproduce the experimental data qualitatively.
In this study, we used a new shell model GXPF1J [3],which reproduces the experimental value better, in orderto calculate electron capture rates of unstable nuclei
and calculated nucleosynthesis. Then we calculated
nucleosynthesis using the conventional shell model
KBF [4] and compared the results. In addition to that,
we compared a deflagration model W7 and a delayeddetonation model WDD2 bacause the explosion dynamics
of SNe Ia is not understood well.
As a result, it is shown that the difference inabundances of each nucleus is a few percent between
the two shell models. This is because the density andthe chemical potential of electrons decrease so rapidlythat the difference between GT strengths becomes
small. The upper figure in Figure 1 shows the result of
nucleosynthesis with W7 and GXPF1J. It can be seenthat 54Fe and 58Ni are still overproduced. On the other
hand, the lower figure shows the result with WDD2 and
GXPF1J. This figure shows that the overproduction of theneutron-excess nuclei is improved. Moreover, we pointout that the production of 54Cr depends on the burning
regime and observations of that nuclei can distinguish the
explosion dynamics [5].

(University of Tokyo)
102(Yi /Yi,Sun )/(YFe /YFe,Sun )SUZUKI, Toshio(NAOJ/Nihon University)

1

10

Fe
Mn

0

10

S
Si

10

-1
O

10

Ar

Ne

Ni

Ca
Ti

K

Co
Cr

P

V
Cl

Al
Mg

-2

Zn

Sc

Cu

Na

10-310

20

30

40

50

60

Mass Number

70

102

(Yi /Yi,Sun )/(YFe /YFe,Sun )MORI, Kanji(University of Tokyo)

101
S

-3

Co

P
Mg

10 10

Ti
K

-1

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Ca

Ar

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-2

Ni

Cr

0

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70

Figure 1: (Upper) Comparison to solar for the deflagration
model W7. The abundance is normalized by the solar
abundance and the 56Fe abundance. (Lower) Comparison
to solar for the delayed-detonation model WDD2.

References[1] Iwamoto, K., et al.: 1999, ApJS, 125, 439.
[2] Sasano, M., et al.: 2011, Phys. Rev. Lett., 107, 202501.
[3] Suzuki, T., et al.: 2011, Phys. Rev. C, 83, 044619.
[4] Caurier, E., et al.: 1999, Nucl. Phys. A, 653, 439.
[5] Mori, K., et al.: 2016, ApJ, 833, 179.

I Scientific Highlights

005

Compact Dense Molecular Gas Emission at the Putative AGN
Location in NGC 1068
IMANISHI, Masatoshi, NAKANISHI, KouichiroIZUMI, Takuma					(NAOJ)		 		(University of Tokyo)

According to the widely accepted unified modelof active galactic nucleus (AGN), a mass accretingsupermassive blackhole is surrounded by a toroidallydistributed dust and gas, the so-called torus. Various
observational properties of AGNs can naturally be
explained by different viewing angle toward the torus.
However, since the torus is very compact in size ( < 10 pc
or < 0.15″ at distance ~15 Mpc), its observational
understanding is still highly incomplete. ALMA is
expected to play an important role for its observational
understanding, thanks to its very high angular resolution.
We have observed the nearby well-studied AGN,
NGC 1068 (z=0.0037, distance is ~14 Mpc) using ALMAat the HCN J = 3–2 (265.89 GHz) and HCO + J = 3–2(267.56 GHz) lines. The achieved angular resolution is0.1″ × 0.2″. Molecular gas observations of NGC 1068
have previously been conducted with > 0.5″ angularresolution, but molecular gas emission at the location of
the putative AGN torus has not been clearly revealed,because it is overwhelmed by the nearby, very brightmolecular gas emission at the eastern side of the hostgalaxy. Thanks to our new very high angular resolution
ALMA data, we successfully detected molecular gas
emission at the putative AGN torus location (C-peak in
Figure 1), by clearly separating from the nearby brightmolecular gas emission in the host galaxy [1]. The
estimated dense molecular gas mass and size are several
× 105 M and ~10 pc, respectively, both of which areroughly comparable to theoretically predicted values.
We have also detected the possible sign of molecular
gas emission which bridges between the eastern brightmolecular gas emission knot and the AGN position(Figure 1). We may be witnessing the theoretically argued
molecular gas supply from the host galaxy to the torus.
Additionally, we found that the HCN-to-HCO + flux
ratios at J = 3–2 in the central several arcsec regions of
NGC 1068 are high, as seen in AGN-important regions(Figure 2). This supports the previously argued scenariothat physical conditions at the NGC 1068 nuclear regions
are dominated by AGN activity. However, thanks to thevery high sensitivity of ALMA, we have also detected
continuum emission at several off-nuclear regions,suggesting the presence of weak (~10 % of AGN
luminosity), but a detactable amount of star-formation
activity in the central several arcsec of NGC 1068.
Reference[1] Imanishi, M., et al.: 2016, ApJL, 822, L10.

006

I Scientific Highlights

Figure 1: Integrated intensity maps and velocity profiles, atselected positions, of HCN J = 3–2 (Upper) and HCO+
J = 3–2 (Lower) in the NGC 1068 nucleus.

Figure 2: Spectra at the representative positions (shown in Figure1) in NGC 1068.

ALMA Molecular Line Observations of Luminous Infrared Galaxies
as a Tool to Detect Extremely Deeply Buried AGNs
IMANISHI, Masatoshi, NAKANISHI, KouichiroIZUMI, Takuma					(NAOJ)		 		(University of Tokyo)

W h e n g a s - r i c h g a l a x i e s c o l l i d e a n d m e rg e ,star-formation and AGN (= mass accretion onto asupermassive blackhole) are activated and generateenergy at dust-obscured regions, and become luminous
infrared galaxies (LIRGs). Since these energy sources are
obscured by dust, observations at the wavelengths of low
dust extinction effects are necessary. An AGN has two
distinguished properties, when compared to a starburst(= active star-formation). First, an AGN can produce alarger amount of hot ( > 100 K) dust, originating in thehigh radiative energy generation efficiency (6–42 % ofMc2) by a mass-accreting supermassive blackhole, thana starburst. Second, the X-ray to UV luminosity ratio ismuch higher in an AGN than a starburst. Due to thesedifferent properties, an AGN and a starburst can input
different physical/chemical effects to the surrounding
molecular gas, and so can produce different molecularline flux ratios. Since there are rotational J-transition linesof many molecules at the almost dust-extinction-free (sub)millimeter wavelength, these molecular line flux ratios
can be a powerful tool to scrutinize dust-obscured energy
sources in LIRGs. High dipole moment molecules, suchas HCN and HCO+, can be particularly effective to probe
how dense molecular gas at LIRG’s nuclei are affected by
dust-obscured energy sources.
Using ALMA, we have conducted HCN and HCO+
J = 3–2 observations, at the submillimeter 250 GHz range,of starbursts, optically-identified AGNs, and LIRGs
whose energy sources were diagnosed based on previous
infrared spectroscopy. We have confirmed that AGNimportant galaxies identified through previous optical/
infrared/X-ray spectroscopy tend to display higher HCNto-HCO+ flux ratios at J = 3–2 than starburst-dominatedregions (Figure 1) [1]. More importantly, our ALMA
observations have discovered extremely deeply buried
AGN candidates which do not show AGN signaturesin the optical/infrared/X-rays, but do show in the (sub)millimeter. These LIRGs display elevated HCN-toHCO+ J = 3–2 flux ratios and signatures of vibrationallyexcited (v 2 = 1f ) HCN emission lines. Detection of
the vibrationally excited (v2 = 1f ) HCN emission lines( T > 1000 K) requires the presence of strong infrared 14
μm continuum emission, most likely originating in AGNheated hot dust. We argue that (sub)millimeter molecularline observations can be the most powerful way toelucidate deeply buried AGNs in LIRGs, thanks to much
lower dust extinction effects than other methods (infraredor hard X-rays). Further systematic ALMA molecularline observations are important to better understand theenergetic role of elusive deeply buried AGNs in LIRGs.

Figure 1: The observed HCN-to-HCO + flux ratios at J = 3–2(modified from [1]). “SB”, “Sy1”, “Sy2”, “LIRG (IRAGN)”, and “IR elusive AGN(?)” mean starburstdominated regions, optically identified Seyfert 1 type
AGNs, optically identified Seyfert 2 type AGNs,
luminous infrared galaxies with optically-elusive,
but infrared-detectable buried AGN signatures, andcandidates of infrared-elusive, but (sub)millimeterdetectable extremely deeply buried AGNs, respectively.
Sources with AGN signatures tend to show elevated
HCN-to-HCO+ J= 3–2 flux ratios, compared to starbursts[1].

Figure 2: Zoom-in spectra of two LIRGs which show thesignatures of vibrationally excited (v 2 = 1f ) HCN
emission lines. The extended tails at the lower frequency
side of the bright HCO+ J = 3–2 emission lines at thevibrational ground level (v =0) are usually interpreted as
the contribution from the HCN v2 = 1f J = 3–2 emission
lines. Both of these sources show high HCN-to-HCO+
J = 3–2 flux ratios (second and third objects from theright in Figure 1).

Reference[1] Imanishi, M., et al.: 2016, AJ, 152, 218.

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Dense Molecular Gas Emission and Infrared Radiative Pumping
in the Ultraluminous Infrared Galaxy IRAS 20551−4250
IMANISHI, Masatoshi, NAKANISHI, KouichiroIZUMI, Takuma					(NAOJ)		 		(University of Tokyo)

Ultraluminous infrared galaxies (ULIRGs) which emithuge infrared luminosity with LIR > 1012 L are usually
produced by gas-rich galaxy mergers and are shining
brightly due to dust thermal radiation heated by starburst
and/or AGN activity hidden behind dust. Distinguishing
the hidden energy sources of the ULIRG population isclosely related to understand how stars are formed andsupermassive blackholes grow in mass during gas-richgalaxy mergers in the universe. Since the compact AGN
can easily be embedded in dust, we need to observe at the
wavelengths where dust extinction effects are small. (Sub)millimeter is one such wavelength and molecular line
flux ratios in this wavelength can be a good tool to probe
the highly embedded energy sources in ULIRGs, because
the ratios are expected to be different between AGNs andstarbursts, due to different physical/chemical effects tothe surrounding molecular gas, coming from different
amount of hot dust and X-ray radiation. Molecular gas
observations, such as HCN, HCO + , and HNC havebeen conducted for nearby ULIRGs, and it has beenargued that elevated HCN emission can be a good AGN
indicator.
Possible explanations for the enhanced HCN emissionin AGNs include (1) higher HCN abundance in molecular
gas largely influenced by AGN radiation, and (2) higher
HCN excitation in AGNs. Additionally, it was proposedthat an infrared radiative pumping can contribute. Namely,
HCN is vibrationally excited by absorbing infrared 14 μm
photons, and through the decay back to the vibrational
ground level, HCN rotational J-transition line fluxes canbe higher. Since an AGN can emit the infrared 14 μm
photons more strongly than a starburst, due to AGNheated hot dust emission, this mechanism is expected
to work more efficiently in an AGN. However, HCO+
and HNC can also be vibrationally excited by absorbing
infrared 12 μm and 22 μm photons, respectively. We
need to investigate the strengths of vibrationally excitedemission lines for all of HCN, HCO+, and HNC, if weare to confirm if this mechanism is indeed responsible forelevated HCN emission in AGNs.
We have observed the ULIRG, IRAS 20551–4250,
using ALMA (Figure 1), and detected vibrationallyexcited (v 2 =1f ) J = 3–2 emission lines for HCN and
HNC, but did not for HCO+ (Figure 2). We calculated
an infrared radiative pumping rate for HCN, HCO +,and HNC, by using the available Spitzer IRS 5–35 μm
infrared spectrum, and found that observational results
can be explained if HCN abundance is higher than008

I Scientific Highlights

HCO+ and HNC by a factor of at least a few. Based on
the vibrational excitation temperature and Einstein A
coefficients for vibrational and rotational transitions, weestimated that the infrared radiative pumping plays arole for rotational level population at least for HCN and
HNC [1]. It is demonstrated that including the infrared
radiative pumping, in addition to the widely assumed
collisional excitation, is needed to understand molecular
gas emission in AGNs.

Figure 1: Spectrum of IRAS 20551–4250 obtained with ALMA
[1]. Although the HCN-to-HCO + J = 3–2 flux ratio isslightly less than unity, it is still higher than starburst
galaxies.

Figure 2: Spectra and integrated intensity maps of vibrationallyexcited (v2=1f) J = 3–2 emission lines of HCN (Left),
HCO+ (Middle), and HNC (Right) [1].

Reference[1] Imanishi, M., et al.: 2016, ApJ, 825, 44.

New Electron Orbits in Collisionless Magnetic Reconnection
ZENITANI, Seiji

				

NAGAI, Tsugunobu(NAOJ)			(Tokyo Tech)

Magnetic reconnection, an explosive energy-releaseprocess in space plasmas, is mediated by complex particle
motion of plasmas. The electron motion is one of thesmallest elements in reconnection systems, and has long
been studied by using particle-in-cell (PIC) simulations.
However, as PIC data have become larger and larger insize, it has become more and more difficult to diagnose
particle orbits in simulations. The theories on particle
orbits in the reconnection system were established in
1980’s.
In this work, we extensively analyzed electron
dynamics in magnetic reconnection by using a 2D PIC
simulation. We surveyed twenty million trajectories, so as
not to overlook any interesting trajectories. As a result, wediscovered various electron orbits that have never been
discussed before. Figure 1 show example electron orbits.
One can see that the red and blue orbits do not cross the
midplane (the horizontal dotted line), while the traditional
theories assume that all orbits cross the midplane. We
examined and classified various electron orbits, as
schematically illustrated in Figure 2. The new orbits areindicated by the double frames. Surprisingly, it was foundthat a majority of electrons follow the new orbits. These
results raise a serious question to previous discussions
for the kinetic physics of magnetic reconnection. Since
the particle orbits are fundamental elements, our findings
could lead to the revision of theoretical models.
Our results were published in the Physics of Plasmas
journal [1]. Owning to fundamental results in thisresearch field, our paper was highlighted by American
Institute of Physics (AIP) [2] and by Physics of Plasmas.
We note that NASA’s Magnetospheric Multiscale(MMS) spacecraft will start detail observation in
the nightside reconnection regions in the Earthmagnetosphere in May, 2017. Our findings will provide
a clue to interpret MMS data and to understand thefundamental physics of magnetic reconnection.
References[1] Zenitani, S., Nagai, T.: 2016, Phys. Plasmas, 23, 102102.
[2] https://publishing.aip.org/publishing/journal-highlights/
japanese-researchers-find-new-classes-electron-orbits

Figure 1: Typical electron orbits in our PIC simulation. Magnetic field lines are
overplotted.

Figure 2: Summary of electron orbits in magnetic reconnection (Ref. [1]). The
new orbits are indicated by the double frames.

I Scientific Highlights

009

Kilonova Emission from Compact Binary Mergers
TANAKA, Masaomi(NAOJ)

010

I Scientific Highlights-20

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Figure 1: Expected observed magnitudes of kilonova models at
200 Mpc distance. The red, blue, and green lines show
the models of NS-NS merger, BH-NS merger, and awind model, respectively.

16

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Mergers of compact stars, i.e., neutron star (NS)and black hole (BH), are promising candidates for
direct detection of gravitational waves (GWs). On 2015
September 14, Advanced LIGO has detected the first everdirect GW signals from a BH-BH merger (GW150914)[1]. This discovery marked the dawn of GW astronomy.
NS-NS mergers and BH-NS mergers are also importantand leading candidates for the GW detection. Whenthe designed sensitivity is realized, Advanced LIGO,Advanced Virgo, and KAGRA can detect the GWs fromthese events up to ~200 Mpc (for NS-NS mergers) and~800 Mpc (for BH-NS mergers). Although the event rates
are still uncertain, more than one GW events per year are
expected.
Since localization only by the GW detectors is notaccurate, e.g., more than a few 10 deg2, identification ofelectromagnetic counterparts is essentially important tostudy the astrophysical nature of the GW sources. NS-NS
mergers and BH-NS mergers are expected to emit EM
emission in various forms. Among variety of emission
mechanisms, optical and infrared emission powered byradioactive decay of r-process nuclei is of great interest.
This emission is called “kilonova”. Observations ofkilonova will also have important implications for theorigin of r-process elements in the Universe.
In this paper, we reviewed the current understandingof kilonova emission by performing radiative transfer
simulations of the dynamical ejecta from NS-NS mergers
and BH-NS mergers [2]. Kilonova emission from the
dynamical ejecta of 0.01 M has a typical luminosity
is an order of 1040–1041 erg s−1 with the characteristic
timescale of about 1 week (Figure 1). Because of thehigh opacity and the low temperature, the spectral peakis located at red optical or near-IR wavelengths (Figure2). In addition to the emission from the dynamical ejecta,
a subsequent disk wind can cause an additional emission
which may peak earlier with a bluer color if the emission
is not absorbed by the precedent ejecta.
At 200 Mpc distance, a typical peak brightness ofkilonova emission is about 22 mag in the red optical
wavelengths (i or z bands, Figure 1). The emission quickly
fades to > 24 mag within ~10 days. To distinguish GW
sources from SNe, observations with multiple visits in atimescale of < 10 days are important to select the objects
with rapid temporal evolution. The use of multiple filters
are also helpful to select red objects. Since the extremely
high expansion velocities (v ~ 0.1–0.2c) are uniquefeatures of dynamical mass ejection from compact binary
mergers, detection of extremely smooth spectrum will be
the smoking gun to conclusively identify the GW sources.

-10
10000

Wavelength (A)Figure 2: Expected observed spectra of the NS-NS merger modelcompared with the spectra of normal Type Ia SN 2005cf
and broad-line Type Ic SN 1998bw.

References[1] Abbott, B. P., et al.: 2016, Phys. Rev. Lett., 116, 061102.
[2] Tanaka, M.: 2016, Advances in Astronomy, 2016, 634197.

Chemodynamical Evolution of Dwarf Galaxies Deduced
from r-process Elements
HIRAI, Yutaka(University of Tokyo/NAOJ)

FUJII, Michiko S.

(University of Tokyo)		

SAITOH, Takayuki R.

(Tokyo Institute of Technology)

HIDAKA, Jun(Meisei University/NAOJ)

Abundances of r-process elements (such as Eu andBa) could help us clarify early evolutionary histories ofgalaxies. The r-process abundances in the Local Groupgalaxies tend to be lower than those of the Milky Way
halo. The r-process abundances would reflect the starformation rates and mixing of metals in the early stagesof galaxy formation.
One of the most promising astrophysical sites ofr-process elements are neutron star mergers. Previous
studies show that it is possible to explain the observed
abundances of r-process elements by neutron star mergers[1]. However, the relation among r-process abundances,
star formation rates, and efficiency of metal mixing is not
yet understood.
In this study, we perform a series of chemodynamical
simulations of dwarf galaxies with different starformation rates and efficiencies of metal mixing toclarify how the star formation rates and efficiency ofmetal mixing affect the r-process abundances. We use
the N-body/hydrodynamic simulation code, asura [4]. In
this study, we implement the r-process element ejection
models by neutron star mergers [1] and metal mixing
model [5] to asura. We adopt the isolated dwarf galaxy
models with different central densities and total massesof halos.
Figure 1 shows r-process abundance ratios in dwarf
galaxy models with different star formation histories[2]. According to Figure 1, stars with r-process elements
appear at higher metallicity in higher star formation
rates due to their faster chemical evolution. This result
suggests that early star formation rates should be lessthan 10−3 M yr−1 to explain the abundances of r-processelements in extremely metal-poor stars.
Figure 2 shows r-process abundance ratios withdifferent efficiencies of metal mixing [3]. Figure 2 (a)and (b) do not have stars with high r-process abundance
ratios ([Ba/Fe] > 1). On the other hand, Figure 2 (c), (d),and (e) have these stars. We assume an efficiency ofmetal mixing estimated from turbulence theory in Figure
2 (a) and (b). This result suggests that it is possible toexplain observed abundances of r-process elements in
dwarf galaxies if the metals are mixed with the efficiency
consistent with estimation from turbulence theory. We
find that the timescale of metal mixing is less than 40 Myr
in Figure 2 (a) and (b). This timescale is significantly
shorter than the dynamical times (~100 Myr) of dwarf

ISHIMARU, Yuhri(International Christian University)

KAJINO, Toshitaka(NAOJ/Beihang University/University of Tokyo)

galaxies. Our results demonstrate that future observations
will be able to more precisely estimate star formation
rates and efficiency of metal mixing through r-process
abundances.

Figure 1: r-process abundance ratios in galaxies with different starformation rates. Grey scales show model prediction. Smalland large dots represent observational results with theMilky Way and the Local Group dwarfs (SAGA database[6]). Star formation rates increase from (A) to (D).

Figure 2: r-process abundances in galaxies with different
efficiencies of metal mixing. Color contours show themodel prediction. Small, large, and red dots represent
observational results of the Milky Way, the Local Groupdwarfs, and the Reticulum II ultrafaint dwarf (SAGA
database [6]). Efficiencies of metal mixing decrease from(a) to (d). (e) represents the model without metal mixing.
(f) shows observations. The red shaded region showsthat the area with no stars in dwarfs. We correct the Baabundances to only reflect contributions from r-process.
References[1] Hirai, Y., et al.: 2015, ApJ, 814, 41.
[2] Hirai, Y., et al.: 2017, MNRAS, 466, 2474.
[3] Hirai, Y., Saitoh, T. R.: 2017, ApJL, 838, L23.
[4] Saitoh, T. R., et al.: 2008, PASJ, 60, 667.
[5] Saitoh, T. R.: 2017, AJ, 153, 85.
[6] Suda, T., et al.: 2008, PASJ, 60, 1159.

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Magnetic Properties of Solar Active Regions
That Govern Large Solar Flares and Eruptions
TORIUMI, ShinSCHRIJVER, Carolus J.

HUDSON, HughI Scientific Highlights(MSSL)NAGASHIMA, Kaori(University of Glasgow)		

It is known that solar flares and coronal massejections (CMEs), especially the larger ones, emanatefrom active regions (ARs) holding sunspots. In order tounderstand the statistical properties of ARs that produce
such strong flare events, we surveyed all flare events with
GOES levels ≥ M5 within 45° from the Sun’s disk centerfor 6 years from May 2010 [1]. Figure 1 shows a sample
flare event that occurred in NOAA AR 12192, which
exhibited the largest sunspots in about 24 years. Fromthese observational data, we measured various parameterssuch as sunspot area, magnetic flux, field strength, area offlare ribbons (elongated intensity enhancements observedin the chromosphere), and flare duration, and conductedstatistical analysis.
As a result, we found that more than 80 % of the
29 ARs that produced a total of 51 flare events exhibit“δ-sunspots,” the most complex magnetic configuration in
the sunspot classification. It is suggested that the δ-spots,
in which positive and negative magnetic polarities areclosely packed, store a high magnetic energy, which
could be released in the form of solar flares. The above
trend is consistent with previous observations [2].
We also found that the flare duration is linearly relatedwith the size scales of flare ribbons (ribbon distance,
ribbon area, and total flux inside the ribbon). These
relations can be explained by the standard flare model
based on the magnetic reconnection theory [3].
It has been known that some flares do not accompany
any CME eruptions. Our statistical results show that theratio of the ribbon area to the sunspot area is significantly
smaller for the CME-less events compared to the CMEeruptive ones. This result may indicate that in the noneruptive ARs, large over-lying arcade fields may inhibit
the CME eruptions, which is well in line with preceding
event studies [4].
Figure 2 displays the observation of perhaps thelargest-ever-imaged sunspot-related flare ribbons. This
great sunspot appeared in July 1946 and ranks 4th insize since the late 19th century. Comparison with the
SDO statistics suggests that this AR might contain a totalmagnetic flux of 1.5 × 1023 Mx and that the magnetic
energy contributing to the flare eruption (not the released
energy) could amount to 8 × 1033 erg. If we suppose thatthe largest sunspot group in history (April 1947: total
flux ~ 2 × 1023 Mx) causes a strong flare eruption, theestimated magnetic energy reaches 1034 erg, which isalready in the category of “superflares.”012

HARRA, Louise K.

(LMATC)		
(MPS)

500
400
y [arcsec]

			(NAOJ)			

(a) Intensitygram

300
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300
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200

400

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Figure 1: Sample flare data. (a) Continuum image showing theentire AR. (b) Magnetogram showing the magnetic
fields (white: positive, black: negative), on which theflare ribbons observed by near UV band image are
overplotted.

1946-07-25 Great flare RGO 14585
(a)

(b)

Figure 2: Great flare event in July 25, 1946, in RGO 14585.
(Left) Sunspots observed in Ca II K1v. (Right) flareribbons observed in H-alpha. Images courtesy of Paris
Observatory.

References[1] Toriumi, S., et al.: 2017, ApJ, 834, 56.
[2] Sammis, I., et al.: 2000, ApJ, 540, 583.
[3] Shibata, K., Magara, T.: 2011, Living Reviews in Solar Physics,
8, 6.
[4] Sun, X., et al.: 2015, ApJL, 804, L28.

Various Local Heating Eventsin the Earliest Phase of Flux Emergence
TORIUMI, Shin, KATSUKAWA, Yukio(NAOJ)				

CHEUNG, Mark C. M.
(LMSAL)

Emerging flux region (2015-08-19 10:47 UT)-255

SOT/SP CP

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-260

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Solar active regions (ARs) are formed through the
emergence of magnetic flux from the convection zone,
and when it emerges to the surface, various sporadic local
heating events are observed in the lower atmosphere(chromosphere and transition region). With the aim ofunderstanding the mechanisms of such heating events,
we analyzed the coordinated observation data of flux
emergence by Hinode and IRIS. As the emergence ishard to predict, there are not many observations of thiskind so far, and thus the data set we show here, which iscomposed of optical and near-UV observations by thetwo instruments, is particularly rare.
The target emerging region appeared within NOAAAR 12401 on August 19, 2015 (Fig. 1). We first analyzed
the Hinode Ca II H images and picked up 151 heating
events. Out of the 29 events that are also covered by the
Hinode’s photospheric magnetic measurement, we foundthat 7 events occur in the locations where positive andnegative polarities are closely nearby (mixed-polarity
events), while another 10 are located in unipolar regions(unipolar events).
IRIS UV spectra of the mixed-polarity events showenhanced and broadened profiles with tails reaching ±150 km s−1, which are suggestive of the strong heatingsand bi-directional jets. Each event leaves flare-like light
curves with fast rise and extended decay. Moreover,Hinode revealed that most of this group have U-shaped
photospheric magnetic fields. From these observational
results, we concluded that the mixed-polarity events arecaused by magnetic reconnection [2,3].
For the unipolar events, we did not find strong intensity
enhancements in the IRIS UV spectra, but they showedsystematic red shifts. The Doppler velocities measured
from the peaks of the spectra were up to 40 km s−1, whichindicates the strong downflow that exceeds the local
sound speed. These results suggest that the unipolar
heating events are due to shocks or strong compressions
caused by fast downflows along the overlying arch
filament system [4].
As shown above, the combination of the photosphericvector magnetogram by Hinode and the UV spectroscopic
data by IRIS allows us to discuss the mechanisms ofa variety of local heating events in the emerging flux
regions. Future missions that provide the the detailed field
information not only in the photosphere but also in theupper atmosphere may further reveal the relation between
the dynamics of magnetic fields and the chromosphericand coronal heating.

Intensity [DN]

				

−0.2
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1335
Wavelength [Å]

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6302
Wavelength [Å]6303

Figure 1: Flux emergence event in NOAA AR 12401. Top row
shows Hinode/SOT photospheric magnetogram (left)
and Ca II H intensity (right: also red contours in theleft image). Sample heating event with yellow arrow isshown in the rows below: The second row shows thenear UV and Ca II H intensity images and photosphericmagnetogram (yellow and turquoise dots represent
where the fields have U- and Ω-shaped configurations,
respectively). Bottom two rows are the IRIS UV spectra
and photospheric circular polarization (colors correspondto the + signs in the second row).

References[1] Toriumi, S., et al.: 2017, ApJ, 836, 63.
[2] Ellerman, F.: 1917, ApJ, 46, 298.
[3] Rutten, R. J., et al.: 2013, J. Phys.: Conf. Ser., 440, 012007.
[4] Shibata, K., et al.: 1989, ApJ, 345, 584.

I Scientific Highlights013

H0LiCOW - Lens Mass Model of HE 0435-1223
and Blind Measurement of Its Time-delay Distance for Cosmology
WONG, Kenneth C.1/2, SUYU, Sherry H.3/4/2, AUGER, Matthew W.5, BONVIN, Vivien6, COURBIN, Frederic6
FASSNACHT, Christopher D.7, HALKOLA, Aleksi7, RUSU, Cristian E.7, SLUSE, Dominique8
SONNENFELD, Alessandro9, TREU, Tommaso10, COLLETT, Thomas E.11, HILBERT, Stefan12
KOOPMANS, Leon V. E.13, MARSHALL, Philip J.14, RUMBAUGH, Nicholas7
1: NAOJ, 2: Academia Sinica Institute of Astronomy and Astrophysics, 3: Max Planck Institute for Astrophysics, 4: Technische Universität
München, 5: University of Cambridge, 6: École polytechnique fédérale de Lausanne, 7: University of California, Davis, 8: Université de Liège,
9: Kavli Institute for the Physics and Mathematics of the Universe, 10: University of California, Los Angeles, 11: University of Portsmouth, 12:Loyola Marymount University, 13: Kapteyn Astronomical Institute, 14: Kavli Institute for Particle Astrophysics and Cosmology

Gravitational lens time delays provide a one-stepmethod to determine the Hubble Constant, H 0. Thismethod is independent of the cosmic distance ladder [1]and serves as a test of systematic effects in individual
H0 probes. This method rests on the fact that light raysfrom the source take different paths through space-time
to each of the image positions. These paths have different
lengths and traverse different gravitational potentials
before reaching the observer, leading to an offset inarrival times. If the source is variable, the delays can bemeasured by monitoring the images. The measured timedelays can be used to calculate the time-delay distance,
DΔ t, a combination of angular diameter distances among
the observer, lens and source. DΔ t is primarily sensitive to
H0 with weaker dependence on other parameters.
The H 0 Lenses in COSMOGRAIL’s Wellspring(H0LiCOW) [2] project is modeling five lensed quasars
with measured time delays to obtain a robust constraint
on H0 to < 3.5 % precision. The first two lenses have been
analyzed [3,4], and analysis of the third lens, HE 04351223 (hereafter HE0435), has now been completed [5].
HE0435 is a quad-image lens for which accurate
time delays have been measured [6]. We have widefield imaging and spectroscopy to characterize mass
projected along the line of sight [7,8], which can bias
the inferred DΔ t if unaccounted for. We have deep HST/
WFC3 observations in the F160W filter, along witharchival HST/ACS imaging in F555W and F814W, formodeling the lens system. This deep, high-resolution
imaging is crucial in order to use the full surface
brightness distribution of the extended quasar host galaxy
as constraints. We have also measured the lens galaxy’s
velocity dispersion with Keck/LRIS, which helps to breakdegeneracies in the mass model. We try a range of models
with different assumptions such as the parameterizationof the mass profile, the region over which the lensed
images are fit, etc. to test for systematic effects. Our final
result combines the distributions from all of these models.
Throughout our analysis, we blind the DΔ t and H0values by subtracting the median from the distributions.
This allows us to evaluate the precision and relative
offsets of these distributions and their correlations withother parameters without seeing the absolute value. This014

I Scientific Highlights

is done to remove confirmation bias and the tendencyof experimenters to stop investigating systematic errors
when they obtain an answer consistent with the “expected”
result. After finalizing our analysis and coming to aconsensus among the coauthors, we unblind the results
and do not make any further changes to the models.
From our analysis, we determine the time-delay
distance to be DΔ t = 2612 +208
−191 Mpc. For a flat ΛCDM
cosmology, we constrain the Hubble constant to be H0 =−1 Mpc−1. We combine this result with the first
73.1+5.7−6.0 km s
two H0LiCOW lenses to obtain a 3.8 % constraint of H0−1 Mpc−1 for flat ΛCDM, in good agreement= 71.9+2.4−3.0 km s
with the latest distance ladder results [1] and in tension
with Planck (Planck Collaboration 2016).

Figure 1: Multicolor HST image of HE0435.

References[1] Riess, A. G., et al.: 2016, ApJ, 826, 56.
[2] Suyu, S. H., et al.: 2017, MNRAS, 468, 2590.
[3] Suyu, S. H., et al.: 2010, ApJ, 711, 201.
[4] Suyu, S. H., et al.: 2013, ApJ, 766, 70.
[5] Wong, K. C., et al.: 2017, MNRAS, 465, 4895.
[6] Bonvin, V., et al.: 2017, MNRAS, 465, 4914.
[7] Sluse, D., et al.: 2017, MNRAS, submitted (arXiv:1607.00382)[8] Rusu, C. E., et al.: 2017, MNRAS, 467, 4220.
[9] Planck Collaboration: 2016, A&A, 594, A13.

Photometric Measurements of H2O Ice Crystallinity on TNOs
TERAI, Tsuyoshi(NAOJ)

ITOH, Yoichi(University of Hyogo)

OASA, Yumiko

FURUSHO, Reiko, WATANABE, Junichi(Saitama University)			

Trans-neptunian objects (TNOs), a small body
population beyond Neptune's orbit, were formed at low
temperature of a few 10 K in the distant region fromthe Sun. H2O ice is the most abundant volatile materialof these bodies and should originally have been in theamorphous phase. However, crystalline H 2O ice has
been detected from almost all TNOs of which the nearinfrared spectra were obtained in high quality, such as(50000) Quaoar [1]. The transition from amorphous to
crystalline ice requires heating up to ~100 K. Althoughseveral hypotheses for H 2 O ice crystallization on
the surface of TNOs have been suggested, including
radiogenic heating [2], cryovolcanism [3], andmicrometeorite impact annealing [4], the mechanism
remains unclear. It is important to investigate
homogeneity/diversity of the surface abundance of
crystalline H2O ice among TNOs and its relationships
with the orbital elements and body size for revealing the
crystallization processes.
Crystallinity of H2O ice can be determined by strengthof the diagnostic absorption at 1.65 μm. However, most
TNOs are too faint to acquire the near-infrared spectrawith sufficiently high S/N ratio even by large-aperture
telescopes. Therefore, we introduced a photometricmethod using Subaru/MOIRCS and the narrow band
NB1657 with the center wavelength of 1.657 μm,
allowing us to measure the fraction of crystalline H2O
ice on TNOs precisely and efficiently [5]. We obtained
the imaging data with H and NB1657 filters for six TNOs
which were known to contain H2O ice on the surface.
As a result of comparison between the measured H –NB1657 indexes and those estimated from the model
spectra, all of the target TNOs except for (38682) Huya
showed more than 50 % crystallinity (see Figure 1).
It is interesting that crystalline H 2 O ice has
been detected from not only the large-size TNOs
including (136108) Haumea, (50000) Quaoar, and(90482) Orcus, but also from the relatively small objects,(315530) 2008 AP129 and (42355) Typhon. It is difficult
to explain the surface crystallization of such small-size
objects by cryovolcanism or radiogenic heating withlong-lived isotopes (e.g., 40K), but, the decay of shortlived isotopes (e.g., 26Al) could induce sufficient heating[2].
We also found that while H2O ice on Haumea andQuaoar is highly dominated by the crystalline state,
Orcus has only ~50 % crystallinity. The low bulk densityof Orcus (~1.5 g cm−3) could cause suppression of thesurface heating and stagnation in crystallization.

(NAOJ)

Figure 1: The solid and dotted horizontal lines show the reflective
colors in H – NB1657 (Δ(H – NB1657)) of the observed
TNOs and their uncertainties, respectively. The curves
represent the relation between the Δ(H– NB1657) indexand H 2O ice crystallinity estimated from the model
spectra.

References[1] Jewitt, D. C., Luu, J.: 2004, Nature, 432, 731.
[2] Guilbert-Lepoutre, A., et al.: 2011, A&A, 529, A71.
[3] Cook, J. C., et al.: 2007, ApJ, 663, 1406.
[4] Porter, S. B., et al.: 2010, Icarus, 208, 492.
[5] Terai, T., et al.: 2016, ApJ, 827, 65.

I Scientific Highlights

015

ISM Excitation and Metallicity of Star-forming Galaxies at z  3.3
from Near-IR Spectroscopy
ONODERA, Masato, ARIMOTO, Nobuo

CAROLLO, C. Marcella, LILLY, Simon, TACCHELLA, Sandro

		 (NAOJ)							 (ETH Zurich)				

RENZINI, Alvio

CAPAK, Peter

DADDI, Emanuele

SCOVILLE, Nick

TATEHORA, S.

ZAMORANI, G.

(INAF-Padova)		
(Caltech)			

(IPAC)			

(SOKENDAI)		

We study the relationship between stellar mass, starformation rate (SFR), ionization state, and gas-phasemetallicity for a sample of 41 normal star-forming
galaxies at 3 <~ z <~ 3.7 [1]. The gas-phase oxygen
abundance, ionization parameter, and electron densityof ionized gas are derived from rest-frame opticalstrong emission lines measured on near-infrared spectra
obtained with Keck/Multi-Object Spectrograph for InfraRed Exploration (MOSFIRE). We remove the effect ofthese strong emission lines in the broadband fluxes tocompute stellar masses via spectral energy distribution
fitting, while the SFR is derived from the dust-corrected
ultraviolet luminosity. The ionization parameter is weakly
correlated with the specific SFR, but otherwise theionization parameter and electron density do not correlatewith other global galaxy properties such as stellar mass,
SFR, and metallicity. The mass-metallicity relation (MZR)
at z  3.3 shows lower metallicity by  0.7 dex than thatat z = 0 [2,3] at the same stellar mass (Figure 1). Our
sample shows an offset by  0.3 dex from the locallydefined mass-metallicity-SFR relation [4], indicating that
simply extrapolating such a relation to higher redshift
may predict an incorrect evolution of MZR. Furthermore,
within the uncertainties we find no SFR-metallicity
correlation, suggesting a less important role of SFR incontrolling the metallicity at high redshift. We finallyinvestigate the redshift evolution of the MZR by using
the model by Lilly et al. [5], finding that the observed
evolution from z = 0 to z  3.3 can be accounted for by
the model assuming a weak redshift evolution of the starformation efficiency.

016

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Figure 1: Mass–metallicity relation of our sample, shown withcircles [1]. The filled and open circles are those with andwithout Hβ detection, respectively. Squares represent themeasurements on the stacked spectra in bins of stellar
mass and SFR. The bins above and below the best-fit
main-sequence are shown with filled and open symbols,
respectively. The best-fit linear relation for our sample
is shown with a dashed line. The solid line is the z = 0
relation [4].

References[1] Onodera, M., et al.: 2016, ApJ, 822, 42.
[2] Maiolino, R., et al.: 2008, A&A, 488, 463.
[3] Tremonti, C. A., et al.: 2004, ApJ, 613, 898.
[4] Mannucci, F., et al.: 2010, MNRAS, 408, 2115.
[5] Lilly, S. J., et al.: 2013, ApJ, 772, 119.

Imaging of Diffuse H I Absorption Structurein the SSA22 Protocluster Region at z = 3.1
MAWATARI, Ken, INOUE, Akio
(Osaka Sangyo University)		

		

MATSUDA, Yuichi(NAOJ)			

YAMADA, Toru

(JAXA)			

UMEHATA, Hideki(Open University)			

When and how galaxies formed and evolved are
big questions in the modern astronomy. It is generally
considered that gas composed of hydrogen, helium,
and so on fell into dark matter overdensity region,
the gas was compressed to form stars, and stars wereassembled to form galaxies. Unlike the dark matterand stellar component of galaxies whose behaviors
are easily predicted theoretically or easily investigatedobservationally, behaviors of gaseous matter is still
mysterious. Comparing spatial distribution of galaxies
and gas is important, especially in distant porto-cluster
region because galaxy formation at high-redshift isconsidered to preferentially occur in such a high density
environment.
So far, gas in the distant Universe has been
investigated through absorption lines (e.g., H I Lyα, Lyβ,
C IV, O I) imprinted in the background QSO spectra. In
this work, we used galaxies, not QSOs, as backgroundlight sources to map gas structure traced by the absorption
systems with high spatial resolution. Furthermore, wedeveloped a new scheme to characterize strength of
H I Lyα absorption by the foreground gas using multiband photometry including narrow-band data (we call
ΔNB method) [1]. Continuum flux of background lightsources and absorption flux by the foreground H I gas,
which are spectroscopically measured in other work[2], are estimated from the broad-band and narrow-band
photometry, respectively (Figure 1). This ΔNB method
enables us to investigate the absorption systems in wider
area with shorter observing time than spectroscopy,
while we can investigate only H I gas at a given redshiftcorresponding to a used narrow-band filter.
We applied the new scheme to imaging data of z = 3.1
SSA22 proto-supercluster region, which were taken with
the Subaru/S-Cam. We obtained a very wide (~ 50 Mpc)
map of H I gas structure with ~ 3 Mpc spatial resolution(Figure 1). The H I gas absorption is significantly strong
over the entire SSA22 field, compared with those in thetwo control fields (SXDS and GOODS-N fields). On
the other hand, it is also revealed that gas distribution
in the proto-supercluster region does not align with thegalaxies’ distribution perfectly in relatively small scale(~ 3 Mpc). These suggest that the H I gas not only is
associated with the individual galaxies but also spreadsout diffusely across intergalactic space only within the
proto-supercluster. Such a diffuse gas component may be

HAYASHINO, Tomoki, OTSUKA, Takuya(Tohoku University)

OUCHI Masami, MUKAE, Shirou(Tokyo University)an ancestor of Warm Hot Intracluster Medium (WHIM[3])which is associated with nearby superclusters andoccupies roughly half of baryons in the Universe.
We also investigated the H I absorption strength asa function of distance from the nearest z = 3.1 galaxy.
We confirmed that the absorption becomes stronger atthe distance less than 100 kpc, which may be due to the
H I gas associated with the individual galaxies. AntiCorrelation between strengths of absorption by thecircumgalactic H I gas and of Lyα emission from thegalaxies themselves is also found, which suggests thatobserved properties of distant galaxies are affected by thecircumgalactic gas distribution and neutrality.

Figure 1: Schematic picture of H I gas mapping by our ΔNB
method. We conduct imaging observations of galaxies
with multiple filters. Absorption flux by z = 3.1 H I gas isevaluated from an offset between the observed narrowband flux and continuum flux (ΔNB), where the latter isestimated from the broad-band fluxes. Right panel shows
spatial distribution of ΔNB values estimated in the
SSA22 porto-supercluster region. Redder color meansstronger H I Lyα absorption. Contours shows number
density of Lyα emitters.

References[1] Mawatari, K., et al.: 2017, MNRAS, 467, 3951.
[2] Lee, K.-G., et al.: 2014, ApJ, 795, L12.
[3] Zappacosta, L., et al.: 2005, MNRAS, 357, 929.

I Scientific Highlights

017

Properties of Interstellar Dust Responsible
for Steep Extinction Curves toward Type Ia Supernovae
NOZAWA, Takaya(NAOJ)

Type Ia supernovae (SNe Ia) show remarkablehomogenity in terms of their absolute magnitude andspectral energy distribution. As such, they are ideal
objects not only for measuring the cosmic expansion as
standard candles but also for extracting the extinction
properties caused by interstellar dust in their hostgalaxies. It has been known, however, that the extinction
curves observed for SNe Ia are very steep with unusually
low total-to-selective extinction ratios of RV = 1.0–2.5[1], compared to the average value of R V = 3.1 in the
Milky Way (MW) [2]. The origin of such highly low RVvalues casts challenging problems in modelling the natureand evolution of interstellar dust in external galaxies,
which has been invoked as one of the critical issues
for improving the current precision of cosmologicalparameters [3].
In order to reveal the properties of interstellar dustthat causes steep extinction laws toward SNe Ia, wesearch for physical dust models that lead to good fits tothe extinction curves obtained from the empirical formula(called the CCM formula) by Cardelli et al. (1989) [2]with RV = 2.0, 1.5, and 1.0 [4]. In the fitting calculations,
we apply a two-component dust model composed ofgraphite and silicate, and consider the power-law grain
size distribution. For simplicity, we assume that graphiteand silicate grains have the same size distribution, in
which the important quantities to be assigned are thepower-law index q, the maximum cut-off radius amax, andthe graphite-to-silicate mass ratio fgs.
We find that the steep extinction curves with RV =2.0, 1.5, and 1.0 can be reasonably explained even by
the simple power-law grain size distribution with a fixedindex of q = −3.5 by taking the maximum cut-off radiiof amax = 0.13 μm, 0.094 μm, and 0.057 μm, respectively(Fig. 1). These maximum cut-off radii are smaller thanamax  0.25 μm considered valid in the MW [5,6], clearly
demonstrating that the interstellar dust responsible
for steep extinction curves is biased to smaller sizes.
The mass ratios of graphite to silicate grains are in anarrow range of f gs = 0.45–0.60, indicating that thechemical composition of interstellar dust is not changed
dramatically for different RV. This is the first study toquantitatively reveal the properties of interstellar dust thatarises the steep extinction curves.

018

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Figure 1: Extinction curves calculated from the best-fit values ofamax and fgs for a two-component dust model following
the power-law size distribution with an index of q =−3.5. The filled circles are the data of extinction at
wavelengths of representative photometric bands fromultraviolet to near-infrared, derived from the CCM
formula [2] for each RV value. For reference, the average
MW extinction curve (RV = 3.1) is drawn by the blackline, and the gray thin lines plot the extinction curves
measured along a variety of lines of sight in our Galaxy[7]. The steep extinction curves with RV = 1.0 (green),
1.5 (red), and 2.0 (blue) as suggested for SNe Ia can benicely fitted by power-law grain size distributions withthe maximum cut-off radii of amax = 0.057 μm, 0.094 μm,
and 0.13 μm, respectively, which indicates that the
maximum cut-off radius is an important quantity todescribe the variety of extinction curves.

References[1] Howell, D. A.; 2011, Natur. Commun., 2, 350.
[2] Cardelli, J. A., Clayton, G. C., Mathis, J. S.; 1989, ApJ, 345,
245.
[3] Conley, A., et al.; 2007, ApJL, 664, L13.
[4] Nozawa, T.; 2016, Planet. Space Sci., 133, 36.
[5] Mathis, J. S., Rumple, W., Nordsieck, K. H.; 1977, ApJ, 217,425.
[6] Nozawa, T., Fukugita, M.; 2013, ApJ, 770, 27.
[7] Fitzpatrick, E. L., Massa, D.; 2007, ApJ, 663, 320.

Formation of Overheated Regions and Truncated Disks around Black Holes;
Three-dimensional General Relativistic
Radiation-magnetohydrodynamics Simulations
TAKAHASHI, Hiroyuki, OHSUGA, Ken, KAWASHIMA, Tomohisa

				(NAOJ)					It is believed that the black hole accretion flows are
the central engine of the luminous compact objects likeactive galactic nuclei and black hole binaries (BHBs).
The X-ray spectra of such objects are mainly composedof the soft component and the power-low component.
The soft component is dominant over the power-low
component in the high-soft state as well as in the slim
disk state. In contrast, the power-low component is quite
prominent in the low-hard state and in the very high state.
The soft component is explained to be multi-color
disk blackbody model, which is emitted from therelatively cold, optically thick accretion disk. On theother hand, the power-low component is thought to be
produced due to the Compton upscattering in the hot andless-dense regions (so-called disk corona). These features
are motivated from observations, but both the structure
and the formation mechanism of the hot, rarefied plasmaaround the cold disk are not understood yet.
In this paper, we perform the three-dimensional
General Relativistic Radiation Magnetohydrodynamic
simulations to study the formation of the hot, rarefied
corona. Figure 1 shows global structure of accretion
disk. The radiation pressure dominated accretion flow isformed around the black holes. Due to the strong radiation
generated in the accretion disks, strong bipolar jets areformed, which are accelerated by the radiation force. We
found that far from the black hole, the gas temperatureof the disk gas is about a few 10 7 K. The radiation
temperature coincides with the gas temperature due to thestrong coupling between the gas and radiation throughthe absorption and emission processes. Close to the blackhole, however, the gas temperature deviates from theradiation temperature and it increases with approaching
to the black hole. The maximum gas temperature reaches
1011 K close to the black hole. This indicates the fact thatthe high temperature gas cloud is formed near the black
hole. Then we investigate the reason why such a hightemperature cloud is formed. We compare the coolingtimescale and dynamical timescale that gas falls onto theblack hole. Far from the black hole, the cooling time ismuch shorter than the dynamical time, so that the gas andradiation are in local thermodynamic equilibrium. Thissituation is violated close to the black hole since the infall
timescale becomes shorter as approaching to black holedue to the strong gravity. As a result, high temperaturecorona is formed around the black hole. This feature ismore manifest for the low accretion rate case since the

SEKIGUCHI, Yuichiro(Toho University)

cooling time is reciprocal to the square of the density.
Also we find that the coronal temperature is higher forthe case of rapidly rotating black hole. We do not have a
confidence, but this result would indicate that the blackhole rotation energy is transported to the accretion disk
and it would be responsible for disk heating.

Figure 1: Global structure of radiation dominated accretion disksnear the black hole at t = 0.3 s. The Figure shows thedensity (blue-white-red volume rendering), the outflow
velocity (white-red volume data), and the magnetic Fieldlines (gray lines).

Reference[1] Takahashi, H. R., et al.: 2016, ApJ, 826, 23.

I Scientific Highlights

019

Chondrule Formation by Planetesimal Collisions
WAKITA, Shigeru, MATSUMOTO, Yuji, OSHINO, Shoichi(NAOJ)HASEGAWA, Yasuhiro(Jet Propulsion Laboratory, California Institute of Technology)

Chondrules are sub-mm sized spherical materials
found in primitive meteorites, chondrites. Chondrules
had once heated and melted in the solar nebula. Several
theories are proposed for the formation process ofchondrules. Planetesimal collisions are one of candidatesof chondrule formation: impact jetting, which can be
induced by planetesimal-protoplanet collisions, could
produce chondrules, when the impact velocity of thecollisions exceeds 2.5 km/s [1].
We investigate the abundance of chondrules formedby impact jetting and their formation timing [2]: both ofthem are derived from semi-analytical calculations ofplanetesimal-protoplanet collisions and the subsequent
formation of protoplanets. We find that the planetesimalprotoplanet collisions with the impact velocity higher than
2.5 km/s would occur around 2 au in the protoplanetary
disk at 3 million years. This timing is consistent with theisotopic studies of chondrules [3]. We also constraint on
the mass of the disk and planetesimals to trigger impact
jetting [4], using the strength of magnetic fields in thesolar nebula based on the measurements of chondrules [5].
It is need to consider undifferentiated planetesimalplanetesimal collisions, not potentially differentiatedprotoplanet-planetesimal ones. This is because chondrules
is not differentiated, and their precursors also would be
undifferentiated. Thus, we examine whether planetesimalplanetesimal collisions can produce chondrules or not[6]. We perform various kind of collisions with theparameters of the impact velocity and the size of target
planetesimal using iSALE-2D shock physics code
[7,8,9]. Our numerical results show that planetesimalplanetesimal collisions with 2.5 km/s can also producechondrules [Figure 1(a)]. The mass of chondrule would
increase as the impact velocity increases and it would
vary with the size of target planetesimals. We also findthat the original position of chondrules is in a region ofa few hundreds depth from the surface [Figure 1(b)] andthe progenitor of chondrules originates from the impactor
planetesimals than the larger target planetesimals.
We also check the fate of produced chondrules semianalytically and find that the half of produced chondrules
accrete on the protoplanet, and the other half would doon the planetesimals [10]. Those results indicate thattarget planetesimals or protoplanet are very important toconsider chondrule formation via impact jetting.

020

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Figure 1: Results of 10 km sized planetesimals colliding eachother with a impact velocity of 2.5 km/s. Right side ofpanels show temperature and left ones show velocity. (a)2.0 seconds after collision. (b) Tracing back to original
position of materials.

References[1] Johnson, B. C.: 2015, Nature, 517, 339.
[2] Hasegawa, Y., et al.: 2016, ApJ, 816, 8.
[3] Connelly, J. N., et al.: 2012, Science, 338, 651.
[4] Hasegawa, Y., et al.: 2016, ApJL, 820, L12.
[5] Fu, R. R. et al.: 2014, Science, 346, 1089.
[6] Wakita, S., et al.: 2017, ApJ, 834, 125.
[7] Amsden, A., et al.: 1980, Los Alamos National Laboratories
Report, LA-8095, 101.
[8] Collins, G. S., et al.: 2004, Meteorit. Planet. Sci., 39, 217.
[9] Wünnemann, K., et al.: 2006, Icarus, 180, 514.
[10] Matsumoto, Y., et al.: 2017, ApJ, 837, 103.

Revisiting the Completeness and Luminosity Functionin High-redshift Low-luminosity Quasar Surveys
				

NIIDA, Mana, NAGAO, Tohru(Ehime University)			

KOBAYASHI, Masakazu(NIT, Kure College)		

IKEDA, Hiroyuki(NAOJ)		

TOBA, Yoshiki

At the center of most galaxies, there is a supermassive
blackhole (SMBH) whose mass is 106 – 109 M. It is
now recognized that SMBHs already existed at z ~ 7 [1].
However it is totally unclear how those SMBHs haveformed and evolved. To investigate the evolution of
SMBHs, quasars who release the huge radiative energy
powered by the gravitational energy of SMBHs areuseful. The luminosity of quasars correlates with the massof SMBHs. Therefore, to examine the mass evolution of
SMBHs, it is important to measure the evolution of thequasars number densities as a function of the redshift
and luminosity (quasar luminosity functions; QLFs).
However, the number densities of the low-luminosity
quasars at the high redshift derived by the previous
studies have large uncertainty [2,3]. This is due to thelarge systematic error in the quasar selection method
based on the imaging data.
To derive the accurate number density of the lowluminosity quasars at the high redshift, we improve themethod of the quasar selection. We specifically focus
on the luminosity dependence of quasar spectra (theBaldwin effect [4]) whose effect on the quasar selection
was ignored in the previous studies. We quantify thisluminosity dependence using the Baryon Oscillation
Spectroscopic Survey (BOSS) quasar catalog. Basedon these obtained results and using the latest model ofthe inter-galactic medium (IGM) attenuation [5], we
establish the new method for deriving the quasar number
densities. By this method, we calculate the completenessof quasar survey at z ~ 4–5, using the COSMOS deep
images observed with Subaru/Suprime-Cam. Based on
this result, we revisit the low-luminosity quasar number
densities. In the results, the revisited number densitiesare ~24 % lower and ~43 % higher than that estimatedby the conventional method at z ~ 4 and 5, respectively(Fig. 1). Recent surveys of high-luminosity quasars
have reported that the quasar number densities increase
from the early univers to z ~ 2 and then decrease to now.
Furthermore the higher-luminosity quasars show the peakof their number densities at higher redshifts than lowerluminosity quasars. This indicates that more massive
SMBHs grew earlier (i.e., down-sizing). The results ofour study suggest that the low-luminosity quasar number
density decrease from z ~ 2 to z ~ 5. This indicates thateven at high-redshift the evolution of quasar number
densities is consistent with the down-sizing evolutionary(ASIAA)		

MATSUOKA, Kenta(University of Florence)

TANIGUCHI, Yoshiaki(Open University)

picture. See [6] for more details.

Figure 1: Redshift evolution of the quasar number density for eachluminosity. Filled squares and open squares show theresults of this study and those of conventional method,respectively. We also show the results of the previous
studies for high-luminosity or low redshift quasars
as each symbols. The filled squares at z ~ 4 and 5 areslightly shifted to the right direction to avoid the overlap
with other symbols. Our study makes it possible tomeasure the low-luminosity quasar number densities atz ~ 4, 5 more accurately.

References[1] Mortlock, D. J., et al.: 2011, Nature, 474, 616.
[2] Ikeda, H., et al.: 2011, ApJL, 728, L25.
[3] Ikeda, H., et al.: 2012, ApJ, 756, 160.
[4] Baldwin, J. A.: 1977, ApJ, 214, 679.
[5] Inoue, A., et al.: 2014, MNRAS, 442, 1805.
[6] Niida, M., et al.: 2016, ApJ, 832, 208.

I Scientific Highlights

021

Near-infrared Spectroscopy of Nearby Seyfert Galaxies
for Examinig the Ionization Mechanism of Narrow-line Regions
TERAO, Koki, NAGAO, Tohru

		(Ehime University)		

MATSUOKA, Kenta(The University of Florence)

HASHIMOTO, Tetsuya(National Tsing Hua University)		

TOBA, Yoshiki(ASIAA)		

The active galactic nucleus (AGN) feedback, which
is a negative/positive feedback effect on star formation
activity, has been paid a lot more attention recently. A
massive galaxy has a supermassive black hole (SMBH)
at its center, and the inflow of interstellar medium (ISM)
to SMBH invokes its AGN activity, which releases
vast gravitational potential energy to the ISM in the
suppression of star-formation activity in its host galaxy.
However, how the AGN activity transmits its energy
to the ISM remains a serious mystery. We here focus
on a shock ionization of the ISM in narrow-line regions(NLRs) as another possible physical mechanism of the
AGN feedback, i.e., the AGN activity inputs its energy
to the ISM through a shock heating induced by a jet or
AGN wind. Therefore it is interesting to explore whether
and how the fast shock contributes the NLR ionization in
AGNs.
Although it is widely accepted that NLRs in AGNs aremostly photoionized by photons from a central engine,
the possibility of shock ionization induced by a jet or
AGN wind at off-nucleus regions. The discrimination
between the shock-ionization and photoionization of
NLRs in AGNs was extremely difficult. As a reason
for that in previous studies of NLRs, optical line-ratio
diagnostics have failed to discriminate between the two
mechanisms, because optical NLR spectra predicted by
the photoionization and shock ionization models are very
similar in each other [1].
The near-infrared emission-line flux ratio of[Fe II]1.257 μm/[P II]1.188 μm is a very powerful indicator
to discriminate the photoionization and shock ionization[2,3]. The [Fe II ]/[P II ] ratio in fast shock-excited
regions is expected to be high (~ 20) while that in purely
photoionized regions is low (~ 2).
We carried out the near-infrared spectroscopic
observations of 26 nearby Seyfert galaxies with a nearinfrared spectrograph (ISLE) boarded on the 188 cm
telescope at Okayama Astrophysical Observatory. As aresult, we measured the [Fe II]/[P II] flux ratio or its lower
limit for 19 objects and 22 Seyfert galaxies from theliterature. Based on the collected data, we found that theionization mechanism of the NLR is the photoionizationin most cases ([Fe II ]/[P II ] < 5) but the fast shock
contributes in some Seyfert galaxies ([Fe II]/[P II] > 10).
We found that these is no significant correlation between
the [Fe II]/[P II] and the radio-loudness (Figure 1). We

022

I Scientific Highlights

IKEDA, Hiroyuki(NAOJ)YANAGISAWA, Kenshi(NAOJ)TANIGUCHI, Yoshiaki(The Open University of Japan)

checked the effect of the shocks from star-formation
activities using some starburst indicators (far-infrared
luminosity and the mid-infrared PAH emission), andconfirmed that the [Fe II]/[P II] ratio is independent the
starburst activities. These results suggest that the NLR insome Seyfert galaxies is affected by fast shocks whose
origin is the radio jet and other mechanisms such as thepowerful AGN wind [4].

Figure 1: Relation between the [Fe II]/[P II] ratio and the radioloudness of nearby Seyfert galaxies. Perpendicular
dashed line shows the threshold dividing the radio-loudand radio-quiet populations.

References[1] Allen, M. G., et al.: 2008, ApJS, 178, 20.
[2] Oliva, E., et al.: 2001, A&A, 369, L5.
[3] Hashimoto, T., et al.: 2011, PASJ, 63, L7.
[4] Terao, K., et al.: 2016, ApJ, 833, 190.

Mergers of Accreting Stellar-mass Black HolesTAGAWA, Hiromichi(NAOJ)		

UMEMURA, Masayuki

GOUDA, Naoteru(University of Tsukuba)

Recent observations have revealed the existenceof supermassive black holes (SMBHs) with masses9>~ 10 M at redshifts higher than 6 [1]. However, theformation history of these SMBHs is not still revealed.
There are two major competitive scenarios for the growthof SMBHs: one is the mass accretion, and the other is themerger of BHs (or stars). As for the mass accretion, theconstraints from observed SMBHs at high redshifts havebeen argued. Possible building blocks of SMBHs are theremnants of first stars. First stars of several tens M canleave black holes (BHs) of few tens M after supernova
explosion. If recently discovered high-redshift SMBHs
grow via mass accretion from such stellar-mass BHs, theaccretion rate is required to be higher than the Eddington
accretion rate. However, the continuous accretion isunlikely to be sustained due to feedback, and thus theaverage mass accretion rates should be lower thanthe Eddington rate [2]. Then, if the BHs grow via BH
mergers by a few orders of magnitude, the high-redshift
SMBHs can be formed from stellar-mass BHs.
Then we focus on the promotion of BH mergers inabundant gas at high-redshift epochs. Recent radiationhydrodynamic simulations on the formation of first stars
show that multiple massive stars form in a primordial
gas cloud of ~ 104–105 M with the density of around107 cm−3 and the extension of ~0.01 pc, where the gas
fraction is 99 %. According to the mass function of firststars, multiple BHs of several tens M may be born asremnants of supernovae, in such a primordial could [3].
In this circumstance, high mass-accretion rates onto
BHs are expected. On the other hand, plenty of gas canexert dynamical friction on moving BHs. Recently, we
have explored the early merger of BHs through the gas
dynamical friction, and have shown that the merger timeof multiple BHs merger in the gas number density of ngas
6
−3
7>
~ 10 cm is ~10 yr, which is shorter than the Eddington
timescale [4]. However, this study [4] did not consider
the effect of the mass accretion onto BHs. Thus, in thecompetition between the mass accretion and the merger,
which mechanism dominates the growth of massive BHs
is not clear. Then, we present post-Newtonian N-bodysimulations on mergers of accreting stellar-mass black
holes (BHs), where such general relativistic effects as the
pericenter shift and gravitational wave (GW) emission
are taken into consideration. The attention is concentrated
on the effects of the dynamical friction and the HoyleLyttleton mass accretion by ambient gas. As a result,
we show that mergers of accreting stellar-mass BHs areclassified into four types: a gas drag-driven, an interplaydriven, a three body-driven, or an accretion-driven(University of Tokyo/NAOJ)

merger. Using the simulation results for a wide range ofparameters, we derive a critical accretion rate (ṁc), below
which the BH growth is promoted faster by mergers(Figure 1). We find that BH mergers proceed before
significant mass accretion, even if the accretion rate is~10 Eddington accretion rate, and then all BHs can merge
into one heavy BH [5].
10-2
-3

10

p = -0.86

p = -1.19

10-4

ε

		

-5

10

10-6

rtyp = 0.1 pc
rtyp = 0.04 pc
rtyp = 0.02 pc
rtyp = 0.01 pc

p = -0.96

p = -1.02

low n gasm·E (η = 0.1)

-7

10

104

105

106

107

108

-3

109

1010

1011

1012

n gas [cm ]Figure 1: The critical accretion efficiency (ϵ c = ṁc / ṁHL) as afunction of ambient gas density n gas . Red, orange,
blue, and brown plots represent the critical conditionin high-density regions for rtyp = 0.1, 0.04, 0.02, and0.01 pc, respectively. Red, orange, blue, and brown lines
represent the curves fitted by ngas,c = aϵ p for rtyp = 0.1,
0.04, 0.02, and 0.01 pc. Pink line represents the criticalcondition in low-density regions. The green dashed line
represents the Eddington accretion rate ṁE (η = 0.1),
where η is the radiative energy conversion efficiency.

References
1] Fan, X., et al., 2001, AJ, 122, 2833.
[2] Milosavljevic, M., Couch, S. M., Bromm V.: 2009, ApJ, 696,
146.
[3] Susa, H., Hasegawa, K., Tominaga, N.: 2014, ApJ, 792, 32.
[4] Tagawa, H., et al.: 2015, MNRAS, 451, 2174.
[5] Tagawa, H., Umemura, M., Gouda, N.: 2016, MNRAS, 462,
3812.

I Scientific Highlights

023

The Validation of Made-to-measure Method
for Reconstruction of Phase Space Distribution Functions
GOUDA, Naoteru(University of Tokyo / NAOJ)

Investigating the dynamical structures of galaxies
is important to infer their formations and evolutions
especially in the era of highly precise Galactic survey
mission, Gaia [1] and JASMINE [2]. To infer the realphase-space distribution function (DF) of the total ofmatters in a galaxy by the comparison of the theoreticallyconstructed stellar DFs with precise observational data,
accurate theoretical construction of the stellar DFs is very
important.
For that purpose, we investigate how accurately
phase-space DFs in galactic models can be reconstructedby a made-to-measure (M2M, [3]) method, whichconstructs N-particle models of stellar systems fromvarious observational data, such as photometric andvarious kinematic data. The advantage of the M2M
method is that this method can be applied to various
galactic models without assumption of the spatial
symmetries of gravitational potentials adopted in galactic
models, and furthermore, numerical calculations of theorbits of the stars cannot be severely constrained by thecapacities of computer memories. Therefore, when weconstruct DFs using immense data such as Gaia data, theM2M method is best suitable method among crrently
proposed methods.
Although the M2M method has been applied tovarious galactic models, the degree of accuracy for therecovery of DFs derived by the M2M method in galactic
models has never been investigated carefully. Then
we investigate the degree of accuracy for the recoveryof the DFs for the anisotropic Plummer model andthe axisymmetric Stäckel model, which have analytic
solutions of the DFs. Furthermore, this study provides thedependence of the degree of accuracy for the recovery of
the DFs on various parameters and procedures adopted inthis paper. The parameters which we investigate are thetotal number of particles used in the M2M modelling run,the number of constraints such as the mass or kinematic
observables, the initial phase space distribution of theparticles, configurations of the kinematic observables,
higher order velocity moments, and a temporalsmoothing.
As a result, we derive the dependence on the particle
number and the data number (Figure 1). We find that thedegree of accuracy for the recovery of the DFs derived by
the M2M method using Nd observational data is 6.5 × 102
N −1.6% for the spherical target model, and 24.3 N −0.075%dd
for the axisymmetric target model. Therefore, by using
the Gaia data of Nd ~ 109, the DFs can be constructed024

I Scientific Highlights

YANO, Taihei(NAOJ)

HARA, Takuji(University of Tokyo)

with the uncertainty of about 5 % [4].
2422

fdif [%](NAOJ)		

20
18
16
6

7

10

8

10

10

N
24
22

fdif,min [%]TAGAWA, Hiromichi

		

20
18
16
10

30

100

300

Nm
Figure 1: The upper panel shows the degree of accuracy for therecovery of the DFs f dif for the axisymmetric three
integral target model as a function of the particle number
N. Red circle, black square, orange triangle, blue
inverted triangle, green diamond, and magenta plus plots
represent the results for the kinematic data number Nk= 16 and the mass data number as Nm = 8, 16, 32, 64,
128, and 256, respectively. Cyan cross plot represents
the results for N k = 64 and N m = 128. Each line
represents the curve fitted by fdif = a × N −0.5 + fdif,minfor concolorous plots. The lower panel shows f dif,min
as a function of Nm for Nk = 16. The line represents theb.
curve fitted by fdif = a × N m
References[1] Perryman, M. A. C., et al.: 2001, A&A, 369, 339.
[2] Gouda, N.: 2012, in Astronomical Society of the PacificConference Series, Vol. 458, Galactic Archaeology: Near-Field
Cosmology and the Formation of the Milky Way, ed. W. Aoki,
M. Ishigaki, T. Suda, T. Tsujimoto, N. Arimoto, 417.
[3] Syer, D., Tremaine, S.: 1996, MNRAS, 282, 223.
[4] Tagawa, H., et al.: 2016, MNRAS, 463, 927.

Nitrogen Isotopic Ratio of Cometary Ammonia
from High-resolution Optical Spectroscopic Observationsof C/2014 Q2 (Lovejoy)
SHINNAKA, Yoshiharu

KAWAKITA, Hideyo(NAOJ/JSPS Research Fellow/University of Liège)(Kyoto Sangyo University)
20

12

A)

8

12
8
4

6
4
2

0

0

-4

-2
570.32 570.34 570.36 570.38 570.4
Wavelength (nm)571.06 571.08 571.1 571.12 571.14
Wavelength (nm)

10
8

24

C)

Relative flux

4
2

12
8
4

0

10

D)

20
16

6

-2

B)

10

Relative flux

Relative flux

16

Relative flux

Icy materials present in comets provide clues forhelping us to understand the origin and evolution of ourSolar system and planetary systems. In particular, isotopic
ratios in cometary molecules provide a diagnostic of
the physicochemical conditions, which the molecules
formed and were processed during the evolutionary
stages from the interstellar medium to the solar nebula.
The temperatures at which molecules form control thefractionation of the heavier isotopes (e.g., in the case of
deuterium-fractionation in water).
We performed high-resolution optical spectroscopic
observations of comet C/2014 Q2 (Lovejoy) on 2015
January 11 (at 1.321 au from the Sun, pre-perihelion) byusing the High Dispersion Spectrograph (HDS) mounted
on the Subaru Telescope on Maunakea, Hawaii. We
derived the 14N/15N ratio of NH2 (126 ± 25), the orthoto-para abundance ratios (OPRs) of the H2O+ ion (2.77 ±0.24) and NH2 (1.19 ± 0.04), which correspond to nuclear
spin temperatures of >24 K (3σ lower limit) and 27 ± 2
K, respectively, and the intensity ratio of the green to reddoublet of forbidden oxygen lines (0.107 ± 0.007) [1].
Ammonia in the comet have to have formed under
low-temperature conditions at ~10 K or less to reproduce
the derived 14N/15N ratio of ammonia if it is assumed thatthe 15N-fractionation of ammonia occurred through ionmolecule chemical reactions. However, this temperature
is inconsistent with the nuclear spin temperatures ofwater and ammonia estimated from the OPRs. Therefore,
the interpretation of the nuclear spin temperature as thetemperature at molecular formation might be incorrect.
An isotope-selective photodissociation of molecular
nitrogen by protosolar ultraviolet radiation may play
an important role in the 15N-fractionation observed incometary volatiles.

Relative flux

		

0
-4
572.34 572.36 572.38 572.4 572.42
Wavelength (nm)E)

574.12 574.14 574.16 574.18 574.2
Wavelength (nm)8

A. 100-100 F1 (570.3582 nm)

6

B. 111-101 F2 (571.0959 nm)
111-101 F1 (571.1275 nm)

4

C. 110-202 F1 (572.3810 nm)

2

D. 110-220 F1 (574.1556 nm)

0E. 312-422 F1 (576.2995 nm)
312-422 F2 (576.3076 nm)-2576.26 576.28 576.3 576.32 576.34
Wavelength (nm)Figure 1: Measurements of seven 15NH2 lines (denoted by blue
solid lines and black arrows). The red dotted lines is theresults of ad hoc fitting. Gray dashed lines indicate the±1σ error of the continuum levels.

Reference[1] Shinnaka, Y., Kawakita, H.: 2016, AJ, 152, 145.

I Scientific Highlights

025Ortho-to-Para Abundance Ratios of NH2 in 26 Comets:
Implications for the Real Meaning of OPRs		SHINNAKA, Yoshiharu

KAWAKITA, Hideyo(NAOJ/JSPS Research Fellow/University of Liège)(Kyoto Sangyo University)

JEHIN, Emmanuël, DECOCK, Alice, HUTSEMÉKERS, Damien, MANFROID, Jean
(University of Liège)

1.35
1.3

OPR of NH3

1.25
1.2
1.15
1.1
1.05
1
0.95
0.9

Jupiter-family
comets (JFCs)

Oort Cloud comets (OCCs)

JFCs (2< TJ < 3)

OCCs (TJ < 2)
8P/Tuttle
153P/H-Z
C/1995 O1
C/1999 S4
C/2000 WM1
C/2001 A2
C/2001 Q4

9P/Tempel 1
73P-B/SW 3
73P-C/SW 3
81P/Wild 2
88P/Howell103P/Hartley 2

C/2002 T7
C/2002 V1
C/2002 X5
C/2002 Y1
C/2003 K4
C/2009 K5
C/2009 P1

C/2012 S1
C/2012 X1
C/2013 R1
C/2013 US10
C/2014 E2
C/2014 Q2

Figure 1: OPR of NH3 estimated from those of NH2 in 26 comets.
No clear difference in the OPRs for different dynamicalclasses can be seen. The nuclear-spin statistical weights
ratio of NH3 (1.0) is indicated by the horizontal dashed
line.
1.35

JFCs (2 < TJ < 3)
73P-B/SW 3
73P-C/SW 3
103P/Hartley 2

1.3
1.25
OPR of NH3Abundance ratios of nuclear-spin isomers forcometary molecules having identical protons, such as
water and ammonia, have been measured and discussed
from the viewpoint of primordial characters in comet. In
the case of ammonia, its ortho-to-para abundance ratio(OPR) is usually estimated from OPRs of NH2 because ofdifficulty in measuring OPR of ammonia directly.
To derive an OPR of NH 2 in a comet, we use thefluorescence excitation model of NH 2 in the optical
wavelength region. The OPR of NH 2 is a unique freeparameter in the model and is determined from a χ 2
fitting between the observed high-resolution andsynthesized spectra based on the assumption that NH2 isthe fluorescence equilibrium condition in the coma. An
OPR of NH2 determined from high-resolution spectra of
NH2 was converted to that of NH3 by assuming NH3 as asole-parent of NH2 and also by assuming the conservationof total nuclear-spin for the photodissociation reaction of
NH3 to NH2. We also assume that photodissociation rates
are the same for both ortho- and para-NH3.
We report our survey for OPRs of NH2 in 26 comets(Fig. 1) [1]. The data were mainly acquired by 8-m
telescopes with high-resolution optical spectrographs,
the Ultraviolet, Visual Echelle Spectrograph (UVES)
mounted on the Very Large Telescope (VLT) and theHigh Dispersion Spectrograph (HDS) mounted on the
Subaru Telescope. A weighted mean of ammonia OPRs
for the comets is 1.12 ± 0.01 and no significant difference
is found between the Oort Cloud comets and the Jupiterfamily comets. These values correspond to ~30 K as
nuclear-spin temperatures.
Moreover, based on comparison of OPRs (andnuclear-spin temperatures) of NH3 with those of water,
14N/15N ratios in NH , and D/H ratios in water (Fig. 2),
3
The OPRs of NH3 in comets probably reflect the physicochemical conditions in cometary coma, rather than theconditions for the molecular formation or condensationin the pre-solar molecular cloud and the solar nebula.
Relationship between the OPRs of NH3 and water is aclue to understanding the real meaning of the OPRs.

OCCs (TJ < 2)
C/1995 O1
C/1999 S4
C/2000 WM1
C/2001 A2
C/2001 Q4
C/2002 T7
C/2003 K4
C/2012 S1
C/2013 R1
C/2014 Q2

1.2
1.15
1.1
1.05
1
0.95

1

1.5

2

2.5
3
OPR of H2O

3.5

4

Figure 2: Correlation between OPRs of NH 3 and water. The
horizontal and vertical dashed lines show the nuclearspin statistical weight ratio of NH3 (1.0) and water (3.0).

Reference[1] Shinnaka, Y., et al.: 2016, MNRAS, 426, S195.

026

I Scientific Highlights

Nitrogen Isotopic Ratios of NH2 in Comets:
Implication for 15N-Fractionation in Cometary Ammonia
		

SHINNAKA, Yoshiharu(NAOJ/JSPS Research Fellow/University of Liège)

KAWAKITA, Hideyo(Kyoto Sangyo University)

JEHIN, Emmanuël, DECOCK, Alice, HUTSEMÉKERS, Damien, MANFROID, Jean
(University of Liège)				

240

ARAI, Akira(Kyoto Sangyo University)

NH3

220
200
180
160
140

80
60
40

CN [3]

100

NH3 [4]120
HCN [1,2]

Comets are remnants of icy planetesimals formedin the solar nebula 4.6 Gyr ago. In general, the icymaterials in comets are definitely one of the keys for us tounderstand the origin and evolution of our Solar system.
The isotopic ratios are diagnostics for the physicochemical conditions governing molecular formation. In
comets, 14N/15N ratios have been measured from HCN
in three comets and from CN in more than 20 comets[1,2,3]. Those ratios are enriched in 15N compared tothe elemental abundances of the Sun by a factor of~3, have a small diversity and do not depend on the
dynamical types of the comets. The origin of this high
15N-fractionation is still in debate because CN probably
comes not only from HCN, but also from other materials
in the coma. Consequently, an interpretation of theisotopic ratios in cometary CN is quite complicated dueto the multiple possible parents of CN. In contrast with
CN, the isotopic ratios of nitrogen in NH3 give us a muchclearer interpretation than in CN because NH3 is directly
incorporated in the nuclear ices.
To estimate the 14N/15N ratios in NH3, 14N/15N ratios
have been determined from high-resolution spectra of
NH2 in the optical wavelength region. NH2 is indeed
a dominant photodissociation product of NH 3. These
high-S/N ratio high-resolution spectra were taken by theHigh Dispersion Spectrograph (HDS) mounted on the
Subaru Telescope summit of Mauna Kea, Hawaii, USA
and the Ultraviolet and Visible Echelle Spectrograph(UVES) mounted on the UT2 of the Very Large
Telescopes (VLT) at European Southern Observatory(ESO)’s Paranal Obsrvatory, Chile.
Those ratios were also found to be enriched in 15N
compared to the Sun by a factor of ~3 [4]. In this paper,
we present 14N/15N ratios in NH2 for 20 comets as total.
Our sample includes short-period comets as well as
long-period comets. We found that the 14N/15N ratios incometary NH2 also show a small dispersion and do notdepend on the dynamical origin of the comets (Fig. 1).
Interpretation of 14N/15N ratio in cometary volatiles
is still in debate. In order to reduce the measurement
uncertainty for each comet, we should develop theemission model of 15 NH 2 considering the Swings
effect as well as need more high-S/N spectra by
next-generation large telescopes such as the TMT
and E-ELT. We can truly discuss the variation of
14N/15N ratios in comets if 14N/15N ratios with smaller

Nitrogen isotopic ratio				

Oort cloud comets

Short-period comets

1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20
comets
1. C/2000 WM1
2. C/2001 Q4
3. C/2002 T7
4. C/2002 V1
5. C/2002 X5

6. C/2002 Y1
7. C/2003 K4
8. C/2009 P1
9. C/2012 F6
10. C/2012 S1

11. C/2013 R1
12. C/2013 US10
13. C/2014 E2
14. C/2014 Q2
15. 8P/Tuttle

16. 9P/Tempel 1
17. 73P-B/SW3
18. 73P-C/SW3
19. 88P/Howell20. 103P/Hartley 2

Figure 1: 14N/15N ratio in comets. Three black bars indicate therange of 14N/15N ratios in HCN and the weighted meansof 14N/15N ratios in CN and NH3.

uncertainties will be obtained for each comet.

References[1] Bockelée-Morvan, D., et al.: 2008, ApJ, 679, L49.
[2] Biver, N., et al.: 2016, A&A, 589, A78.
[3] Manfroid, J., et al.: 2009, A&A, 503, 613.
[4] Shinnaka, Y., et al.: 2016, MNRAS, 426, S195.

I Scientific Highlights

027

Imaging Observations of Entire Hydrogen Comaof Comet 67P/Churyumov-Gerasimenko in 2015 September
SHINNAKA, Yoshiharu1/2/3, FOUGERE, Nicolas4, KAWAKITA, Hideyo5, KAMEDA, Shingo6
COMBI, Michael R.4, IKEZAWA, Shota6, SEKI, Ayana6, KUWABARA, Masaki7, SATO, Masaki6
TAGUCHI, Makoto6, YOSHIKAWA, Ichiro7
1: NAOJ, 2: JSPS Research Fellow, 3: University of Liège, 4: University of Michigan, 5: Kyoto Sangyo University, 6: Rikkyo University, 7:
University of Tokyo

028

I Scientific Highlights

low-cost mission support precise observations by a large
mission. We hope this will become one of model cases
for micro spacecraft missions.
200
180
140
120
100

Rayleigh

160

80
60
40
20
0
200
180
160
140
120
100

Rayleigh

The water production rate, QH2O of a comet is oneof the fundamental parameters to understand cometaryactivity when a comet approaches the Sun within 2.5 au
because water is the most abundant icy material in the
cometary nucleus (~70 % of icy materials). For instance,
the slopes of the water production rate with respect toheliocentric distance, r H, of comets seem to depend on
dynamical ages of the comets [1].
Comet 67P/Churyumov-Gerasimenko (hereafter
67P) is a Jupiter-family comet with an orbital period of~6.5 years. During the 2015 apparition of the comet, thecomet was the target of ESA’s Rosetta mission. QH2Oof the comet have been derived by various instruments
on board the Rosetta spacecraft throughout the 2015
apparition. However, measurement of an absolute QH2O
is difficult because the Rosetta spacecraft was located in
the cometary coma. Note that an obtained QH2O strongly
depends on the coma models [2,3].
To derive gas production rates based on in situ
measurements by the Rosetta instruments at the close
distances from the comet 67P, entire coma observations
from the ground-based and space observatories canrealize the critical calibration for the gas production rates.
We performed wide-field imaging observations of Lyαemission in comet 67P by the LAICA telescope on board
the micro spacecraft for deep space exploration, the
PROCYON, on UT 2015 September 7, 12, and 13 [4].
To estimate a QH2O from a single Lyα image, we use
the two-dimensional axi-symmetric Direct Simulation
Monte-Carlo (DSMC) model of atomic hydrogen coma
using the Adaptive Mesh Particle Simulator code [5](Fig. 1). Because there were bad observing conditions
during the time the comet could be observed from
Earth, our observations were important to test the comamodels for the comet. Combined with Rosetta’s results,
such as water production rates at different r H andchemical composition, we could accurately estimate thetotal ejected mass of the comet in the 2015 apparition.
Moreover, 67P shows that the activity in the 2015
apparition was comparable to those in the past fourthapparitions at least, and has much icy materials in the
nucleus.
This result is the first scientific achievement by amicro spacecraft for deep space exploration. Moreover,this provides an ideal example where observations by a

80
60
40
6

1.57x10 km

200Figure 1: Trimmed reduce Lyα (upper) and reproduced (lower)
images of hydrogen coma of comet 67P by 2D axisymmetric model in Rayleigh units on UT 2015 Sept 13.
Yellow allow is solar direction.

References[1] A'Hearn, M. F., et al.: 1995, Icarus, 118, 223.
[2] Fougere, N., et al.: 2016, MNRAS, 462, S156.
[3] Hansen, K. C., et al.: 2016, MNRAS, 462, S491.
[4] Shinnaka, Y., et al.: 2017, AJ, 154, 76.
[5] Crismani. M. M. J., et al.: 2015, Geophys. Res. Lett., 42, 8803.

Record-breaking Faint Satellite Galaxy of the Milky Way Discovered
HOMMA, Daisuke1, CHIBA, Masashi1, OKAMOTO, Sakurako2, KOMIYAMA, Yutaka3, TANAKA, Masayuki3
TANAKA, Mikito1, ISHIGAKI, Miho N.4, AKIYAMA, Masayuki1, ARIMOTO, Nobuo3, GARMILLA, Jose A.5
LUPTON, Robert H.5, STRAUSS, Michael A.5, FURUSAWA, Hisanori3, MIYAZAKI, Satoshi3
MURAYAMA, Hitoshi4, NISHIZAWA, Atsushi J.6, TAKADA, Masahiro4
USUDA, Tomonori3, WANG, Shiang-Yu7
1: Tohoku University, 2: Shanghai Astronomical Observatory, 3: NAOJ, 4: Kavli IPMU, WPI, 5: Princeton University, 6: Nagoya University, 7:
ASIAA

Currently, some 50 satellite galaxies to the Milky
Way have been identified. About 40 of them are faint anddiffuse and belong to the category of so-called “dwarf
spheroidal galaxies”. Many recently discovered dwarf
galaxies, especially those seen in systematic photometricsurveys such as the Sloan Digital Sky Survey (SDSS)and the Dark Energy Survey (DES) are very faint withabsolute luminosity in the optical waveband below -8
magnitude. However, previous searches made use oftelescopes with a diameter of 2.5 to 4 meters, so only
satellites relatively close to the Sun or those with higher
magnitudes were identified. Those that are more distantor faint ones in the halo of the Milky Way are yet to be
detected. We therefore carefully examined the early dataof the Subaru Strategic Survey with HSC and searchedfor very faint dwarf satellites which were overlooked byprevious surveys.
By identifying an over density of stars in the sky withcharacteristic distribution to the old stellar populationin the color-magnitude diagram (Fig. 1 and 2), we
discovered an extremely faint dwarf satellite galaxy of
the Milky Way and named it as Virgo I – the first faintdwarf satellite galaxy located in the direction of theconstellation Virgo [1]. Though the absolute magnitudeof Virgo I is as faint as −0.8 in the optical waveband, it isidentified as a galaxy because it is spatially extended witha radius of 124 light years – systematically larger than aglobular cluster with comparable luminosity. The faintest
dwarf satellites identified so far was Segue I, discoveredby SDSS (−1.5 mag) and Cetus II in DES (0.0 mag).
Cetus II is yet to be confirmed, as it is too compact as agalaxy. Virgo I may ultimately turn out to be the faintest
one ever discovered. It lies at a distance of 280,000 lightyears from the Sun, and such a remote galaxy with faintbrightness has not been identified in previous surveys.
The Subaru Strategic Survey using HSC will continue
to explore much wider areas of the sky and is expected tofind more satellites like Virgo I.

Figure 1: The position of Virgo I in the constellation of Virgo (left)
and a density map of Virgo I’s member stars in a 0.1 deg
x 0.1 deg area (right).

Figure 2: Stars in the color-magnitude diagram. Old stellar
populations show a characteristic distribution along the
curve seen in the diagram. From left to right: Bootes I,
Segue I, Virgo I, and a general field outside Virgo I. The
spatial distribution of the stars, which are located inside
the green band for Virgo I, is shown in the right panel of
Figure 1. Note that stars in a general field outside Virgo
I (right panel) show no characteristic feature.

Reference[1] Homma, D., et al.: 2016, ApJ, 832, 21.

I Scientific Highlights029

Large Scale Environment of the Most Massive SMBHs
SHIRASAKI, Yuji

(NAOJ/SOKENDAI)		

KOMIYA, Yutaka

It has been recognized that most of the galaxies havea supermassive black hole (SMBH) with mass in therange of 105–1010 M at their center. The mechanism toevolve the BHs up to 1010 M is still an open question.
In order to deliver a large amount of matter to acompact region inside the BH, it is required to remove
angular momentum efficiently from the matter. Several
mechanisms have been proposed to explain the evolutionof the BHs, such as the internal mechanism which relieson the secular evolution due to disk and/or bar instability,
the external mechanism which includes the galaxy
merger and the interaction with nearby galaxies, and the
hot halo model in which quiescent gas accretion from the
hot halo and/or recycled gas from evolving stars feeds
the BHs. According to the numerical simulation, thesecular evolution has a difficulty to evolve the BHs up
to the most highest mass ranges ( > 109 M), thus large
scale environmental effect may mainly contribute to thefeeding to the most massive BHs. If this is the case, it
could be observed that there is a relation between the BH
mass and the properties of galaxies around them.
To investigate the existence of such a relation, we
explored the dependence of galaxy clustering around
AGNs on the BH mass, and found that there is a tendency
that galaxies are more clustered around the most massive
BHs than those around the lower mass BHs [1]. The
aim of this work [2] is to reveal what kind of galaxies
contributes to the increase of clustering, which can be aclue to the understanding the evolutionary history of themost massive BHs and also the surrounding galaxies. To
measure the color of galaxies with good precision, weused two catalogs derived from UKIRT Infrared DeepSky Survey (UKIDSS) Large Area Survey (LAS) andfrom SDSS DR8 for deriving galaxy samples. The AGN
samples for which BH masses are measured are derived
from two AGN catalogs [3,4].
By using the nature of galaxy clustering, it is possible
to measure in a statistical way the color distributionof galaxies associated with AGNs without knowing
the redshift of galaxies if redshifts of the AGNs are
known. That is, by measuring the color distributions athigh density region around AGN ( < 1 Mpc; on region)
and at lower density region (3–5 Mpc; off region),and subtracting latter from former, we can obtain thecolor distribution of the clustering galaxies. The color
was measured by fitting the galaxy’s spectral energy
distribution (SED) to the synthesis model of SED
calculated assuming its redshift to be the same as the
AGN redshift.
The color distributions obtained in this way are030

I Scientific Highlights

OHISHI, Masatoshi, MIZUMOTO, Yoshihiko(University of Tokyo)			

(NAOJ/SOKENDAI)

shown in Figure 1. The larger color index (D opt-IR )corresponds to redder color. The top panel is for lower
mass BHs (log (M BH/M ) = 7.5–9.0) and the bottom
panel is for the most massive BHs (log (M BH/M ) =9.0–10.0). The redshift range is 0.3–0.6 and the numberof AGNs used to derive them is 289 for both. The color
distribution is approximated by a double Gaussian
distribution, and each Gaussian component is related toa red or blue galaxy. The vertical axis is proportional tothe clustering strength, so the relative clustering strengthof each component can be inferred from the area of the
distribution. By measuring the mixing ratio of the twocomponents, we have obtained the red galaxy fraction of~60±10 % for lower mass sample and > 90 % for the most
massive sample. From this result, we revealed that theenvironment of the most massive BHs is enriched with
red galaxies in which star formation is terminated, whichindicates that there is a link between the termination ofstar formation and the growth of the most massive BHs.

Figure 1: Color distributions of galaxies around AGNs.

References[1] Komiya, Y., et al.: 2013, ApJ, 775, 43.
[2] Shirasaki, Y., et al.: 2016, PASJ, 68, 23.
[3] Greene, J. E., Ho, L. C.: 2007, ApJ, 667, 131.
[4] Shen, Y., et al.: 2011, ApJS, 194, 45.

The 1.1 mm Continuum Survey of the Small Magellanic Cloud:Physical Properties and Evolution of the Dust-selected Clouds
TAKEKOSHI, Tatsuya1/2, MINAMIDANI, Tetsuhiro1/2/3/4, KOMUGI, Shinya4/5, KOHNO, Kotaro4
TOSAKI, Tomoka6, SORAI, Kazuo1, MULLER, Erik2, Mizuno, Norikazu2/3/7, Kawamura, Akiko2
ONISHI, Toshikazu8, FUKUI, Yasuo9, EZAWA, Hajime2/3, OSHIMA, Tai2/3, SCOTT, Kimberly S.10/11
AUSTERMANN, Jason E.10/12, MATSUO, Hiroshi2/3, ARETXAGA, Itziar13, HUGHES, David H.13
KAWABE, Ryohei2/3/7, WILSON, Grant W.10, Yun, Min S.10
1: Hokkaido University, 2: NAOJ, 3: SOKENDAI, 4: University of Tokyo, 5: Kogakuin University, 6: Joetsu University of Education, 7: Joint
ALMA Observatory, 8: Osaka Prefecture University, 9: Nagoya University, 10: University of Massachusetts, 11: National Radio Astronomy
Observatory, 12: National Institute of Standards and Technology, 13: INAOEThe Small Magellanic Cloud (SMC) is a dwarf
galaxy that provides a unique opportunity to study thephysics of the interstellar medium (ISM) because of
its proximity (~60 kpc) and low metallicity (~1/5 Z).
These peculiarities make the SMC an ideal laboratory
to investigate the physics of the ISM under the extreme
conditions such as galaxies forming in the early Universe.
Previously, observations of giant molecular clouds(GMCs) in the SMC has been conducted by CO lines(e.g., [1]). On the other hand, recent study suggests that,in a low-metallicity environment, the fraction of “COdark” gas in the GMCs can be a dominant component[2]. Therefore, it is essential to investigate GMCs in lowmetallicity environments by means other than CO line
observations, and dust continuum observations using asubmillimeter imager can provide an alternative method
to investigate the GMC.
In this study, we conducted a 1.1 mm continuum
survey using the AzTEC instrument on the ASTE
telescope to investigate the physical properties of the
GMCs in the SMC. The observations covered a total of a
4.5 deg2 field of the SMC, and noise levels of 5–12 mJybeam−1 are achieved with a effective resolution of 40″,
which corresponds to 12 pc.
Figure 1 shows the obtained 1.1 mm continuum map.
Most of the representative star-forming regions in the
SMC, such as N27, N66, N81, N83, N84, and N88, weredetected with sufficient S/N ratios of > 10 at the peak
positions. We identified a total of 44 objects, and thephysical properties were derived by the SED analysis
under the assumption of single-temperature thermal dust
emission using 1.1 mm and Herschel bands. As the result,the 1.1 mm objects displayed masses of 4×103–3×105 M,and dust temperatures of 17–45 K.
We found three important facts from the detailinvestigation of the 1.1 mm objects. First, the dust
temperature of the 1.1 mm objects show good correlation
with the Spitzer 24 μm, and this supports that the heating
source of the cold dust is mainly local star-formation
activity. Second, the 1.1 mm objects in the SMC should
trace dense gas objects corresponding to the GMC in
our galaxy or nearby galaxies, because the mass, size,

density, and mass function are very similar to those of
GMCs in our galaxy and the Large Magellanic Cloud.
In addition, the 1.1 mm objects displayed good spatial
correlation with the 24 μm and CO emission. Third, theclassification of the 1.1 mm objects in terms of starformation activity revealed that the starless objects harborlower dust temperatures and smaller gas masses and radii
compared to those of the star-forming objects, suggestingthat starless objects are younger evolution phase of the
GMC.
These results were published in the AstrophysicalJournal [3].

N78

N66
N27

N88

N81
N83/84

Figure 1: The 1.1 mm continuum map of the SMC.

References[1] Mizuno, N., et al.: 2001, PASJ, 53, L45.
[2] Glover, S. C. O., Clark, P. C.: 2012, MNRAS, 426, 377.
[3] Takekoshi, T., et al.: 2017, ApJ, 835, 55.

I Scientific Highlights

031

Circumstellar and Explosion Properties of Type Ibn Supernovae
MORIYA, Takashi

I Scientific Highlights(Kyoto University)

are different even though both SNe are characterized by
the narrow emission lines.
1044

-1

bolometric luminosity (erg s )Type Ibn supernovae (SNe) are SNe with narrow
helium emission lines and they are a subtype of Type Ib
SNe. The narrow emission lines typically have thevelocity of about 1000 km/s and the velocity is too small
to originate from SN ejecta. Therefore, the narrow lines
are considered to originate from dense circumstellar
media (CSM) around the progenitors and Type Ibn SNe
appear when the progenitors of Type Ib SNe (Wolf-Rayetstars) somehow experience huge mass loss shortly before
their explosions. Studying Type Ibn SNe are important tounderstand the mass loss from massive stars that are notunderstood well. There are many studies of Type IIn SNethat show narrow hydrogen emission lines but few studies
are performed for Type Ibn SNe.
So far, individual Type Ibn SNe have been studied
in details but no studies are performed to have a general
picture of Type Ibn SNe. Therefore, we gathered all theavailable Type Ibn SNe in the literature and investigatedtheir general properties. We got the following findings [1].
Figs. 1 and 2 summarize the light curves (LCs).
First, the peak luminosities of Type Ibn SNe arehigher than normal Type Ib SNe on average. This canbe explained by the existence of dense CSM. If the SN
ejecta collide to the dense CSM, kinetic energy of the SN
ejecta can be efficiently converted to radiation. Therefore,
Type Ibn SNe have a different luminosity source thanType Ib SNe that are powered by the nuclear decay of
56Ni.
Secondly, the amount of 56 Ni produced by the
explosions is found to be less in Type Ibn SNe thanType Ib SNe. The amount of 56Ni can be constrainedby the late-phase LCs. Type Ibn SNe are brighter thanType Ib SNe at around the peak but Type Ibn SNe become
fainter than Type Ib SNe at the late phase. Therefore, theamount of 56Ni produced in Type Ibn SNe are smaller
than that in Type~Ib SNe. This may be due to the smaller
56Ni production at the explosions or large fallback.
Finally, we found Type Ibn SNe are bright for much
shorter periods than Type IIn SNe. Both Type Ibn andType IIn SNe are considered to be powered by theinteraction between SN ejecta and dense CSM. Because
Type IIn SNe are bright for more than 100 days due tothe long-lasting interaction, their progenitors somehow
need to have high mass-loss rates at least for 100 years
before their explosions. However, Type Ibn SNe shine
only for several tens of days and their CSM do not extend
as in Type IIn SNe. Type Ibn SNe and Type IIn SNeare estimated to have similar CSM densities but theirprogenitors’ enhanced mass-loss periods may significantly
differ, which may indicate their mass-loss mechanisms

032

MAEDA, Keiichi(NAOJ)		

Type IIn
IIb
Ib
Ic
Ic-BL

a

43

10

1042
SN 2011hw
LSQ12btw
LSQ13ccw
ASASSN-15ed
SN 2006jc
SN 2010al
OGLE-2012-SN-006
SN 2014av

1041

1040
-50

56

Ni decay
0

50

100

150

200

days from the peakFigure 1: LCs of Type Ibn SNe and other SNe.

1

relative luminosity

				

b

0.1

0.01

0.001
-50

Type IIn
IIb
Ib
Ic
Ic-BL
0

SN 2011hw
LSQ12btw
LSQ13ccw
ASASSN-15ed
SN 2006jc
SN 2010al
OGLE-2012-SN-006
SN 2014av
50
100
days from the peak

150

Figure 2: The same as Fig. 1 but scaled at the peak luminosity.

Reference[1] Moriya, T. J., Maeda, K.: 2016, ApJ, 824, 100.

200

Radio Transients Associated with Accretion-induced Collapseof White Dwarfs
MORIYA, Takashi(NAOJ)-1-1

radio luminosity (erg s Hz )A* = 10
1
0.1
0.01
0.001

ejecta model B
1 GHz

1029

1028

27

10

1026
1

10

100

1000

10000

days after AIC

1029

A* = 10
1
0.1
0.01
0.001

ejecta model B
10 GHz-1-1

radio luminosity (erg s Hz )Accretion-induced collapse (AIC) is a theoretically
predicted fate of white dwarfs (WDs). If a WD composedof oxygen, neon, and magnesium has a companion star
which accretes matter onto the WD, the WD’s mass caneventually become close to the Chandrasekhar mass
limit. At this moment, the electron-capture reactions ofmagnesium can be triggered at the WD center and the
WD collapses to be a neutron star (NS). (When a WD
composed of carbon and oxygen becomes closer to the
Chandrasekhar mass limit, the explosive burning ofcarbon leads to Type Ia supernovae). Merger of two WDs
can also lead to the formation of a NS if a WD is left
after the merger. For example, if a WD heavier than the
Chandrasekhar mass limit that is composed of carbon andoxygen is formed after the merger and a carbon burning
flame propagates from the surface to the center of the new
massive WD, the WD is eventually composed of oxygen,neon, and magnesium. When the temperature becomes
sufficiently low and the central density becomes highenough, the electron-capture reactions of magnesium canbe triggered to transform the WD to a NS.
It is known that AIC ejects less than 0.1 M  .
However, little amount of radio active elements like 56Ni
are contained in the ejecta and AIC is considered not
to be accompanied by a bright transient. However, thevelocity of the ejecta from AIC is more than a few times
faster than that in typical supernovae. The fast shock canaccelerate electrons and the shock can be bright in radio
thanks to the synchrotron emission from the accelerated
electrons. In this study, radio light curves (LCs) of AIC
that has fast shock waves are investigated.
Fig. 1 is an example of radio LCs obtained in thisstudy [1]. The maximum peak luminosities in radio fromSNe are about 1028 erg s−1 Hz−1. Therefore, AIC can be as
bright as or even brighter than SNe in radio wavelengths.
AIC does not become bright in optical so transients very
faint in optical but very bright in radio are promising
candidates of AIC.
Because AIC is bright in radio, AIC can be discoveredby performing transient surveys in radio. However, theexpected event rate of AIC is small and a deep and wide
radio transient survey is required to find it. We investigate
expected numbers of AIC detections in the future planned
radio transient surveys. As a result, we found that aplanned transient survey with Square Kilometer Arraycan find a few AIC in a year. If we are able to perform
a radio transient survey with a optical transient survey,
we can efficiently discover radio-bright but optical-fainttransients that are promising candidates of AIC.

1028

1027

1026
0.1

1

10
days after AIC

100

1000

Figure 1: Examples of radio LCs of AIC at 1 and 10 GHz. A=1
corresponds to AIC that explodes with in a circumstellar
medium made by the mass-loss rate of 10−5 M yr−1 andthe wind velocity of 1000 km/s. A is proportional to the
mass-loss rate and is inversely proportional to the windvelocity.

Reference[1] Moriya, T. J.: 2016, ApJL, 830, L38.

I Scientific Highlights

033

Supernovae Powered by Magnetars That Transform into Black HolesMETZGER, Brian D.

I Scientific Highlights(Institute for Theoretical and Experimental Physics)

no BH formationt BH= 7.5 days
5 days
2.5 days
1 day
0.5 days
0.25 days

46-1

New kinds of supernovae (SNe) are starting to bediscovered thanks to the recent large transient surveys.
One of them is so-called superluminous SNe that are
more than about 10 times brighter than normal SNe. The
mechanism to make superluminous SNe so bright is not
yet revealed. The most popular model is to make SNesuperluminous with rapidly-rotating strongly-magnetizedneutron stars (magnetars) that are formed during the SN
explosions. If a magnetar that has a rotation period of lessthan a few ms and a dipole magnetic field of about 1014 G
is formed during a SN explosion, the rotation energyof the magnetar (about 1052 erg) is released as a dipole
radiation in a timescale of several days. It is known thatobservational properties of superluminous SNe can be
explained if the magnetar can release its rotational energy
and the released energy is efficiently thermalized.
Neutron stars have the maximum mass to support
themselves and the neutron stars whose mass exceeds the
maximum mass transform into black holes. The maximum
mass depends on the rotation velocity of neutron stars.
The maximum mass of non-rotating neutron stars is about
2.2 M and that of rapidly-rotating neutron stars is about
2.7 M, depending on the equation of state. If a magnetar
whose mass is between about 2.2 M and about 2.7 Mis formed during a SN explosion, it can heat up the SN
at first when it rotates rapidly. However, when it loses a
lot of rotational energy and its rotational energy becomesless than that required to support itself, the magnetartransforms into a black hole and the SN suddenly loses
its central heating source. In this study, we investigate
observational properties of such SNe that are poweredby magnetars that need rotational energy to support
themselves and suddenly lose their central heating source
due to the black-hole formation [1].
Fig. 1 presents how SN light curves (LCs) are affectedby the transformation of magnetars into black holes.
Because the black-hole formation leads to the sudden lossof the central heating sources, LCs become fainter when
the black-hole formation occurs. In addition, if the black
holes are formed shortly after the SN explosion, the shock
breakout signals caused by the shock wave launched by
the magnetar energy input can be clearly seen in the LCs.
Fig. 2 shows comparisons between LCs of the SNepowered by magnetars transforming into black holes andthose of some observed SNe. SNe powered by magnetars
that transform into black holes do not become as brightas superluminous SNe but their LCs are consistent withthose of recently-found rapidly-evolving transients thathave the peak luminosities between superluminous SNeand normal SNe.

034

BLINNIKOV, Sergei I.

(Columbia University)

log bolometric luminosity (erg s )(NAOJ)			

45

44

43

42

41

Mej = 5 M , Eej = 1051 erg
Em = 5 x 1052erg, tm = 5 days
0

10

20

30

40

50

60

days

Figure 1: SN LCs in which magnetars powering the SNe transform
into black holes. t BH is the time when magnetarstransform into black holes.
-22

absolute R band magnitude

MORIYA, Takashi

SN 2002bj
SN 2010gx
PTF10iam
SNLS04D4ec
SNLS05D2bk
SNLS06D1hc
NS2p4m2
NS2p4m4
NS2p4m5
NS2p4m6

-21

-20

-19

-18

-17

0

10

20

30

40

50

60

70

days

Figure 2: Comparison between model SN LCs in which magnetars
powering the SNe transform into black holes and someobserved SN LCs.

Reference[1] Moriya, T. J., Metzger, B. D., Blinnikov, S. I.: 2016, ApJ, 833,
64.

Properties of Magnetars Mimicking 56Ni
CHEN, Ting-Wan(University of Bonn)the black region may actually be powered by magnetars
even if they look as if they are powered by 56Ni. The
dots in Fig. 2 are LC properties of superluminous SNeand they locate in the region where magnetars can mimic
56Ni.

G)

100

10

14

Recent large-scale transient surveys revealed theexistence of extremely luminous supernovae (SNe)that are called superluminous SNe. The luminosities ofcanonical SNe can be explained by the energy provided
by the nuclear decay of 56Ni that is synthesized during
the SN explosions. However, while the required amountof 56Ni to explain the luminosities of canonical SNe is of
the order of 0.1 M at most, superluminous SNe require
more than 5 M of 56Ni to account for their luminosities.
It is difficult to synthesize this amount of 56Ni during
the SN explosions. Thus, to replace the 56Ni heating
mechanism, an alternative scenario to explain the huge
luminosities of superluminous SNe, i.e., the formationof the rapidly-rotating strongly-magnetized neutron stars(magnetars) that can release their huge rotational energy
through the radiation caused by the strong magnetic fields
and efficiently thermalize the radiation is suggested. On
the other hand, if we look into the light curves (LCs) of
superluminous SNe, it is known that the decline rates of
their LCs are often consistent with that is expected fromthe nuclear decay of 56Co made by the nuclear decay of
56Ni. Thus, if magnetars are actually the major heating
source to make superluminous SNe bright, magnetars
should be able to reproduce the LC decline rates thatare consistent with those of 56 Co. In this study, weinvestigated the conditions for magnetars to reproduce
SN LCs that look as if they are powered by 56Ni [1].
As a result, it is found that magnetars need to emit theirradiation almost by the pure dipole radiation to mimic
56 Ni. In addition, it is found that, for magnetars that
release their rotational energy through dipole radiation
to mimic a LC powered by a certain amount of 56Ni,
only their dipole magnetic fields need to be in a certain
range and the condition does not depend on their initialrotational periods. In Fig. 1, we present the require
magnetic field strength to mimic a given amount of 56Ni.
For example, a typical amount of 56Ni required to explain
the peak luminosities of superluminous SNe are about
10 M and it can be found that about 1014 G is required
for magnetars to mimic LCs powered by this amount of
56Ni. Interestingly, the required magnetic field strengths
for magnetars to explain the early LCs of superluminous
SNe are also about 1014 G. Fig. 2 shows rise times andpeak luminosities of SN LCs that can be powered bymagnetars as if 56Ni is powering them. The gray region
indicates all the LC properties that magnetars can mimic
56Ni. However, if a LC requires more 56Ni than ejecta, forexample, we can clearly say that the LC is not poweredby 56Ni. If we exclude this kind of region, the black
region remains. In other words, the SN LCs that fall into

LANGER, Norbert(MPE)		B (10(NAOJ)			

30

1

20
MNi1B142 = 10

l=2
0.01

0.1

1
MNi (M )10

100

Figure 1: Dipole magnetic fields that magnetars require to mimic
given amounts of 56Ni.

fast decliner
slow decliner46

κ = 0.2 cm2 g-1-1

MORIYA, Takashi

log peak luminosity (erg s )		

45
M56Ni /Mej = 1

44

0.3
0.1

43

0.03
0.01

42
0

20

40

60

80

100 120 140
rise time (days)

160

180

200

220

Figure 2: SN LC properties for which magnetars can power like
56Ni.

Reference[1] Moriya, T. J., Chen, T.-W., Langer, N.: 2017, ApJ, 835, 177.

I Scientific Highlights

035

Catalog of Ultra Diffuse Galaxies in the Coma Cluster
YAGI, Masafumi, KOMIYAMA, Yutaka, YAMANOI, Hitomi

				(NAOJ)					Ultra Diffuse Galaxy(UDG) is a new category ofgalaxy population proposed by [1]. They are low surface
brightness galaxies (LSBs) with a large spatial extents.
[1] adopted the selection criteria that the central surface
brightness in g-band is fainter than 24 mag/arcsec2 andthe effective radius (half-light radius) is larger than 1.5
kpc. They reported 48 UDGs in the Coma cluster. If weassume a typical mass-to-luminosity ratio of galaxies,
UDGs in cluster environment cannot maintain their large
extensions by their self-gravity alone. Thus, they are
expected to have a lot of dark matter. The nature of UDGs
(e.g., their formation mechanism) is still full of mysteries.
We analyzed wide survey data of the Coma cluster
in R-band obtained with the Subaru Prime Focus
Camera(Suprime-Cam) in the public archive data of
SMOKA [2]. UDGs were detected with high S/N in
the Suprime-Cam data [2]. As the spatial resolution ismuch higher in data used in [2] than that of [1], we canresolve UDGs near brighter neighbors. We also detected
the region near the cluster center where backgroundlights and the bright tails of galaxies affect. Though
the observed band is different, [2] detected 854 UDGs
in the Coma cluster. We also revisited the other data of
our own (e.g., [3]) that overlap the survey region. Our
previous studies didn't pay special attention to this galaxy
population, as their foci were on the statistical natureof the galaxies in the cluster (e.g., luminosity function)
not on individual galaxy types. We obtained color
information of a subset of the UDGs from the previous
studies.
After [2], we continued the study and reported the
UDG catalog as [4] with several new results. The radial
density profile of UDGs is comparable to that of highsurface-brightness members in general, but a sign ofexcess of UDGs exists at 1.0–1.7 Mpc from the center(Figure 1). We also found that the major axes of UDGs
tend to align to the radial direction toward the galaxy
center, which is statistically significant. The Comacluster is elongated along the large-scale filament toward
the southwest, and the radial alignment of UDGs are
significantly high around the direction (Figure 2).

References[1] van Dokkum, P., et al.: 2015, ApJL, 798, L45.
[2] Koda, J., et al.: 2015, ApJL, 807, L2.
[3] Yamanoi, H., et al.: 2012, AJ, 144, 40.
[4] Yagi, M., et al.: 2016, ApJS, 225, 11.

036

I Scientific Highlights

KODA, Jin

(Stony Brook University)

Figure 1: The radial profile of the galaxy number density of
UDGs (black dots), and member galaxies from SDSS
DR7 (red Xs; shifted by +0.5 dex for comparison.) The
overdensity of UDGs around 0.6–1.0 degree (1.0–1.7
Mpc) is recognized.

Figure 2: Histograms of the azimuthal angle of UDG positions
from the cluster center. UDGs elongated along the radial
direction toward the cluster center are shown in black,and and others are in red. The number of the elongatedUDGs are significantly large around −150(southwest)
direction.

Lyα Rate of UV-bright Star-forming Galaxies at Redshift 7
FURUSAWA, Hisanori1, KASHIKAWA, Nobunari2/1, KOBAYASHI, Masakazu R. A.3, DUNLOP, James S.4
SHIMASAKU, Kazuhiro5, TAKATA, Tadafumi2/1, SEKIGUCHI, Kazuhiro2/1, NAITO, Yoshiaki5
FURUSAWA, Junko1, OUCHI, Masami5, NAKATA, Fumiaki1, YASUDA, Naoki5, OKURA, Yuki6
TANIGUCHI, Yoshiaki7, YAMADA, Toru8, KAJISAWA, Masaru9, FYNBO, Johan P. U.10, Le FÈVRE, Olivier11
1: NAOJ, 2: Graduate University for Advanced Studies, 3: National Institute of Technology, Kure College, 4: Edinburgh University, 5:
University of Tokyo, 6: Riken, 7: The Open University of Japan, 8: ISAS, 9: Ehime University, 10: Copenhagen University, 11: LAM

We perform a survey of star-formaing galaxies thatare very bright in UV luminosities at redshift 7. Followup spectroscopy on these high-z galaxies is conducted,
determining rest-frame equivalent widths (EW0s) of the
Lyα emissions, and the Lyα rate, which is a franction ofstar-formation galaxies showing strong Lyα emissionof these galaxies [1]. Recent observational studies haverevealed that the number density of bright star-formation
galaxies may be larger than expected in previous
observations. Also, the very bright galaxies may include
metal-poor galaxies comprising a primordial stellar
population [2]. It is crucial to increase the sample volume
of such bright galaxies to discuss galaxy formation at thisepoch.
We select star-forming galaxies (LBGs) using
the public near-infrared (NIR) data set by UKIRTUKIDSS and VISTA-UltraVISTA(J = 25.5; 5σ) covering
1.65 square degrees. In order to apply z-dropout
search, we conduct very deep z'-band imaging (z ~26.5; 5σ) with Subaru/Suprime-Cam. This data set
enables us to investigate the very-bright LBGs at
z = 7 with quite a low number density. We find 18
candidates of very bright galaxies (MUV < −21.75). An
optical follow-up spectroscopy was performed with
Subaru/FOCAS on 9 candidates, in which a galaxy
shows possible Lyα emission at z = 7.168 at S/N= 5.5 with EW0 = 3.7 Å (Fig. 1). The other candidates
show no significant emission lines (EW0 < 10 Å).
Previous studies have suggested that the Lyα rateincreases from z = 4 to z = 6. The Lyα rate is higher
and more rapidly increases towards high redshifts for
fainter star-forming galaxies. For galaxies with MUV >−21.75, the Lyα rate may stop increasing and possibly
decrease from z = 6 to z ~ 7 [3]. Our study for the firsttime discusses the Lyα rate (EW0 > 50 or 55) for the very
bright galaxies (−23 < MUV < −21.75) (Fig. 2), deriving
the following results: (1) An increase of the Lyα rate of
the very-bright galaxies may level off at z = 7 and may beclose to or lower than that at z = 4–6. (2) The Lyα rate of
the very-bright galaxies at z = 7 may be at the same levelor higher than that for fainter galaxies (MUV > −21.75) atthe same redshifts.
The very-bright galaxies are also importantcomponents to discuss cosmic reionization. The EW 0
distribution of our very-bright galaxy sample implies

high neutral hydrogen rate at z = 7. An increase of asample volume of the very-bright galaxies at this epoch
is desiable to statistaically understand formation andevolution history and roles of this very bright populationin the reionization.

Figure 1: Spectrum of a Lyα emitter at z = 7.168.

Figure 2: Evolution of Lyα rate in different magnitude ranges.

References[1] Furusawa, H., et al.: 2016, ApJ, 822, 46.
[2] Sobral, D., et al.: 2015, ApJ, 808, 139.
[3] Ono, Y., et al.: 2012, ApJ, 744, 83.

I Scientific Highlights

037

A Spectroscopically Confirmed Double Source Plane Lens Systemin the Hyper Suprime-Cam Subaru Strategic Program
TANAKA, Masayuki1, WONG, Kenneth C.1, MORE, Anupreeta2, DEZUKA, Arsha3, EGAMI, Eiichi4
OGURI Masamune2/5/6, SUYU, Sherry H.7/8, SONNENFELD, Alessandro2, HIGUCHI, Ryo9
KOMIYAMA, Yutaka1, MIYAZAKI, Satoshi1/10, ONOUE, Masafusa1/10
OYAMADA, Shuri11, UTSUMI, Yousuke12
1: NAOJ, 2: Kavli Institute for the Physics and Mathematics of the universe (Kavli IPMU, WPI), 3: University of Kyoto, 4: Steward
Observatory, University of Arizona, 5: University of Tokyo, 6: Research Center for the Early universe, University of Tokyo, 7: Max Planck
Institute for Astrophysics, 8: Institute of Astronomy and Astrophysics, Academia Sinica, 9: Institute for Cosmic Ray Research, The Universityof Tokyo, 10: SOKENDAI (The Graduate University for Advanced Studies), 11: Japan Women’s University, 12: Hiroshima AstrophysicalScience Center, Hiroshima University

Strong gravitational lensing of distant objects provides
us with powerful constrains on the matter distributionof the lens galaxy. The vast majority of the known
strong lensing systems have a single background source,
but in very rare cases, two background sources can be
simultaneously lensed by the same foreground galaxy.
Such double source-plane lens systems are extremely
rare, but they are a very valuable probe of cosmology as
they are sensitive to the cosmic expansion.
Currently, there are only a few known double sourceplane lens systems. We have discovered another one inHyper Suprime-Cam Subaru Strategic Program (HSCSSP) as reported in Tanaka et al. [1]. Fig. 1 shows thesystem. The lens galaxy at the center is a very massive
galaxy at z = 0.79 likely at the center of a cluster. On thebottom-right of the lens, there is a red arc (S1) with acounter image just on the left of the lens galaxy (H). The
second source is the blue Einstein ring (S2) with several
knots (A-G). The system is dubbed ‘Eye of Horus’ due to
its resemblance to the symbol of ancient Egyptian god.
We have made a follow-up spectroscopic observationof the background sources with FIRE on Magellan. We
confirm that the red inner arc is a galaxy at z = 1.3 andthe blue ring at z = 2.0 using several emission lines fromthe galaxies. In all of the previously known systems, thesecond galaxy is too faint to confirm spectroscopically.
Our system is the first double source-plane lens systemwith spectroscopic redshifts of both sources. This isimportant because the spectroscopic redshifts are essential
to derive cosmological constraints from the system.
We have modeled the system with two independent
methods. Both models successfully reproduce the overall
configuration of the system. However, any smoothmodels do not reproduce the A+C split, implying theexistence of a subhalo or foreground structure. We do
not observe a clear hint of a satellite galaxy in the HSC
images, but we have been awarded further follow-up
observations with ALMA and LGSAO-assisted near-IR
imaging observations. These observations may be able
to detect the satellite galaxy responsible for the split,
allowing us to model the system more precisely.

038

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We expect to find 10 more such double sourceplane lens systems in HSC-SSP. Combining all ofthem together, we expect to place a very strong, highly
complementary constraints to other probes on thecosmological parameters.

Figure 1: Pseudo-color image of the lens system. The prominent
knots in inner arc (green) and outer ring (white) arelabeled and the measured spectroscopic redshifts areindicated. The inset shows the image without symbols.
The horizontal bar shows a scale of 10 arcsec.

Reference[1] Tanaka, M., et al.: 2016, ApJL, 826, L19.

Thermo‑optical Simulation and Experiment for the Assessmentof Single, Hollow, and Large Aperture Retroreflector for LLRARAKI, Hiroshi1, KASHIMA, Shingo1, NODA, Hirotomo1, KUNIMORI, Hiroo2, CHIBA, Kouta3,
MASHIKO, Hitomi3, KATO, Hiromasa3, OTSUBO, Toshimichi4, MATSUMOTO, Yoshiaki5, TSURUTA, Seiitsu1
ASARI, Kazuyoshi1, HANADA, Hideo1, YASUDA, Susumu6, UTSUNOMIYA, Shin1, TAKINO, Hideo7
1: NAOJ, 2: NICT, 3: Iwate University, 4: Hitotsubashi University, 5: PTI Co., Ltd., 6: JAXA, 7: Chiba Institute of Technology

Lunar laser ranging (LLR) has made a significant
contribution especially to Selenodesy and General
Relativity. The accuracy of LLR is less than 2 cm dueto the improvement of the ground station. However, thelunar retroreflector has room for improvement on theranging accuracy [1].
The single element retroreflector (SERR) has anadvantage on the accuracy over the arrayed corner cubeon the Moon because it has no internal optical path
difference. SERR whose aperture is 20 cm can yield
two times reflection performance compared with the
A15 retroreflector [2]. Thus we investigated the thermal
deformation and optical degradation of the hollow type
SERR (hereafter CCM; Corner Cube Mirror) with 20 cm
aperture through the thermo-optical simulation, because
the prism type SERR with the same aperture made ofsynthetic quarts shows severe optical degradation due tothe inhomogeneity of the refractive index as well as theweight problem.
Mathematical model of CCM (Figure 1) is preparedon the lunar surface with its optical axis aligned to the
Earth at −43.3 degrees in the lunar latitude (the same
latitude as Tycho crater) to simulate the equilibrium
temperature and thermal deformation of the CCM. Single
crystal silicon (Si) and the CLEARCERAM™-Z EX(OHARA Inc.; hereafter CCZ-EX®) are selected as CCM
material for higher thermal diffusivity, lower thermal
expansion, and higher specific stiffness. Other parts are
made of carbon fiber reinforced plastics (CFRP). Thermal
Desktop®, ANSYS®12, and CodeV10.6SR1 are used forthe temperature, deformation, and optical evaluation,
respectively.
The deformation of CCM is 40–50 µm (Si) or 1 µm
(CCZ-EX ® ) at the lunar noon if the CCM is fixed
perfectly to the structure on multi-points, while thedeformation is less than 0.25 µm at most if the perfectly
fixed point of the CCM is limited to one. The optical
performance of the former CCM is quite poor (Strehl ratio< 0.1; Figure 2), while it is excellent for the latter case(Strehl ratio > 0.9; Figure 2). Through this simulation, it
has turned out for the first time that 20-cm aperture CCM
made of single-crystal Si or “ultra-low expansion glass–ceramics” such as CCZ-EX® can be used for CCM withno thermal control if the perfectly fixed point of CCM islimited to one.
In addition, high temperature annealing from 100 to1000 °C is confirmed effective experimentally to enhance
the adhesive strength between optically contacted Si
surfaces, which is an important knowledge for the
fabrication process of CCM.

Figure 1: [left] General view of the CCM system. [right]
Mathematical model of the CCM system for Thermal
Desktop®. CCM aperture is 20 cm.

Figure 2: Strehl ratios of the aberrated focus image by CCM.
[Upper left] CCM made of Si fixed on 3 points perfectly.
[Lower left] CCM made of Si fixed on 3 points and oneof them is perfectly. [Upper right] CCM made of CCZEX® fixed on 3 points perfectly. [Lower right] CCM
made of CCZ-EX® fixed on 3 points and one of them isperfectly.
References[1] Araki, H., et al.: 2016, Earth Planets Space, 68, 101.
[2] Otsubo, T., et al.: 2011, Earth Planets Space, 63, e13-16.

I Scientific Highlights

039

The Far Distance to G7.47+0.06
from Proper Motion Measurement of H2O Masers
YAMAUCHI, Aya1/2, YAMASHITA, Kazuyoshi2, HONMA, Mareki2, SUNADA, Kazuyoshi2
NAKAGAWA, Akiharu3, UENO, Yuji2
1: JSPS, 2: NAOJ, 3: Kagoshima University

We report a distance measurement of an ultra-compact
HII region G7.47+0.06 associated with IRAS 17591-2228.
The kinematic distances obtained from its radial velocity
suggest that G7.47+0.06 may be farther away than the
distance between the Galactic center and the Sun, ≈ 8 kpc(e.g., 25.1 +10.8−4.2 kpc, Wink et al. 1982 [1]).
We applied a new method to determine a source
distance based on absolute proper motions proposed by
Sofue (2011) [2]. Given a rotation curve, and assuming
circular motion of an object, a distance to the object isobtained from not only the radial velocity but also theproper motion kinematically. The distance of an object
with its galactic longitude l ≈ 0° located farther from the
Galactic center than seen from the Sun is more accurately
obtained by using the proper motion rather than using theradial velocity.

The proper motion is μ = −5.03 ± 0.07 mas yr−1 and isapproaching the Galactic center (Figure 1).
Considering uncertainties of the Galactic rotation
curve and the solar peculiar motion, the detected propermotion leads to a source distance of D = 20 ± 2 kpc(Figure 2), demonstrating that astrometric observation can
provide an accurate distance measurement at 10 % leveleven for sources too far to measure the annual parallax.
Garay et al. (1993) estimated the physical parametersof the HII region using the near kinematic distance of D
= 6.3 kpc [4]. Scaling their parameters from D = 6.3 kpc
to 20 kpc, the H2O maser features are associated with amassive star-forming region corresponding to the spectral
type of O5.5.

10

Decl. offset [mas]

5

(b)

0

-5

-10

-15

60

55

50

45

R.A. offset [mas]40

35

Figure 1: Yamauchi et al. (2016) [3]. Distribution of maser
features (vLSR =−17 – −15 km s−1) throughout all epochs.
Thin dashed arrows indicate proper motions per year ofindividual maser features. A thick arrow is parallel to the
Galactic plane, and its head points to the Galactic center.

Observations of the 22-GHz H 2 O maser line
associated with G7.47+0.06 were conducted with VERA(VLBI Exploration of Radio Astrometry) from 2009
March to 2011 December. As a result of analysis, it turned
out to be difficult to derive the distance from annual
parallax measurement. Meanwhile, we clearly detected
the source’s proper motion parallel to the Galactic plane.

040

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Figure 2: Yamauchi et al. (2016) [3]. Proper motion as a functionof distance. Color scale indicates line-of-sight velocity.
Dashed curves indicate the distances from the LSR
in the cases of flat rotation. Solid curves indicate thedistance from the Sun in the case of Θ = Θ0 (R/R0)α and
α = 0.05. The intersections of the curves and a white
rectangle corresponding to μ = −5.03 ± 0.07 mas yr−1
give a source distance.

References[1] Wink, J. E., Altenhoff, W. J., Mezger, P. G.: 1982, A&A, 108,
227.
[2] Sofue, Y.: 2011, PASJ, 63, 81.
[3] Yamauchi, A., et al.: 2016, PASJ, 68, 60.
[4] Garay, G., et al.: 1993, ApJ, 413, 368.

Enhanced Star Formation of Less Massive Galaxies
in a Proto-Cluster at z = 2.5
HAYASHI, Masao(NAOJ)		

KODAMA, Tadayuki1(Tohoku University)		

TANAKA, Ichi
(NAOJ)		

KOYAMA, Yusei, TADAKI, Ken-ichi3, SUZUKI, L. Tomoko2

SHIMAKAWA, Rhythm2(UCO/Lick Observatory)

YAMAMOTO, Moegi				(NAOJ)					 (Graduate University for Advanced Studies)

We investigate a correlation between star-formation
rate (SFR) and stellar mass for Hα emission line galaxies(HAEs) in one of the richest proto-clusters ever known
at z ~ 2.5, USS 1558-003 proto-cluster. A positive
correlation between SFR and stellar mass in star-forming
galaxies is called the main sequence of star-forming
galaxies. The well-known tight correlation provides us
with perspectives of how the star-forming galaxies evolve
over cosmic time. We find that while the star-forming
galaxies with > 10 9.3 M  are located on the universal
SFR-mass main sequence irrespective of the environment,
less massive star-forming galaxies with < 109.3 M show
a significant upward scatter from the main sequence inthis proto-cluster (see Figure 1). We here summarize theresults. Please refer to [1] for more details.
This study is based on a 9.7-hour narrow-band
imaging data with MOIRCS on the Subaru telescope.
Thanks to the very deep narrow-band data, we are able
to construct a sample, in combination with additional
H-band data taken with WFC3 on Hubble Space
Telescope (HST), of 100 HAEs reaching the dustcorrected SFRs down to 3 M yr−1 and the stellar masses
down to 108.0 M, allowing us to access less massive
galaxies in the proto-cluster. Our results suggest thatwhile the majority of massive galaxies are already settled
in a secular evolution phase and are thus found on themain sequence, some less massive galaxies are in a
starburst phase and they are significantly up-scatteredfrom the main sequence. This may be consistent withthe down-sizing scenario of mass-dependent galaxy
evolution, or since they are located in a dense protocluster, they may be experiencing some influences fromthe surrounding environment such as galaxy-galaxy
interactions.
The existence of the less massive HAEs with< 109.3 M up-scattered above the main sequence may
imply that a scatter around the main sequence increases atlower stellar masses. Diversity of star-formation history
in early phase of galaxy evolution and/or sensitivity to
the fluctuation of starburst activity at short time scales inindividual HII regions could cause the increased scatter.

1
2
3

Figure 1: Main sequence of HAEs in the USS1558-003 protocluster at z = 2.53. The blue-filled circles represent theprobable member HAEs at z ≈ 2.53, while blue-filled
diamonds represent the possible HAEs. The HAEs
spectroscopically confirmed are marked with magenta
open circles. The error bars are derived from the 1σ
photometric error. The uncertainties of stellar masses
derived from the SED fitting are estimated from astandard deviation of 100 iterations. Pentagons show themedian SFRs in each mass bin. The gray region shows
the SFRs under the limit reachable. The curves aremain sequences from the literature [2,3,4,5]. A gray line
shows a constant specific SFR of 10−8 yr−1, and an arrowroughly shows the stellar mass limit which is estimatedwith the 3σ limiting magnitude in Ks and J–Ks color of
0.36.

References[1] Hayashi, M., et al.: 2016, ApJL, 826, L28.
[2] Koyama, Y., et al.: 2013, MNRAS, 434, 423.
[3] Speagle, J. S., et al.: 2014, ApJS, 214, 15.
[4] Whitaker, K. E., et al.: 2014, ApJ, 795, 104.
[5] Shivaei, I., et al.: 2015, ApJ, 815, 98.

(NAOJ) as of the publication date
(Graduate University for Advanced Studies) as of the publication date(Max-Planck-Institut für Extraterrestrische Physik) as of the publication date

I Scientific Highlights

041

Transit Observation of Potentially Habitable Super-Earth K2-3d
with Okayama188 cm/MuSCATFUKUI, Akihiko(NAOJ)			

LIVINGSTON, John, NARITA, Norio(University of Tokyo)		

ONITSUKA, Masahiro, RYU, Tsuguru

				References[1] Crosseld, I. J. M., et al.: 2015, ApJ, 804, 10.
[2] Beichman, C., et al.: 2016, ApJ, 822, 39.
[3] Fukui, A., et al.: 2016, AJ, 152, 171.

042

I Scientific Highlights

KUSAKABE, Nobuhiko(GUAS)			

A transiting exoplanet, which has an orbit crossing
in front of its host star, allows us to probe the planetaryatmosphere by means of measuring the wavelength
dependence of the transit depths. The Kepler space craft,which had continuously monitored a specific sky region
from 2009 for four years, discovered about 30 smalltransiting planets within habitable zones. However, all of
their host stars are too far from us (> 300 pc) and thus too
faint to observe the atmospheres of the planets. On theother hand, the extended Kepler mission, K2, which has
surveyed different sky regions along the ecliptic planesince 2014, has an advantage on discovering nearby
transiting planets.
K2-3d is a transiting super-Earth (1.5 Earth radii)
orbiting a nearby (45 pc) M dwarf with a period of 45days, discovered by the K2 mission in 2015 [1]. The
planet is thought to be within the habitable zone of thehost star. The host star is bright enough (Ks = 8.6) thatnext-generation telescopes can search for molecules
related to life in the planetary atmosphere. However, K2
observed only two transits of K2-3d because the survey
period of K2 per field is only 80 days. As a result, theorbital period of the planet was only poorly measured,preventing us from predicting future transit times withhigh enough precisions for followup observations. Afterthe discovery, two additional transits were observed by
Spitzer space telescope [2], which, however, sufferedfrom instrumental systematics, leaving large room for
improvement.
We observed a transit of K2-3d with the Okayama
188cm telescope equipped with the three-band
simultaneous imager MuSCAT [3]. The transit depthof this planet is just 0.06 %, which is close to thedetection limit from the ground. However, by utilizing
the multiband simultaneity of MuSCAT to reduce thesystematics of Earth's atmospheric origin, we successfully
detected the tiny transit signal. We also reanalyzed theK2 and Spitzer data, which, combined with the MuSCAT
data, drastically improved the transit ephemeris. With thisnew ephemeris, we will be able to observe future transits
at the best timings by e.g., JWST and TMT, which
opens the way for biomarker searches in the potentially
habitable planet.

HIRANO, Teruyuki(Tokyo Institute of Technology)(Astrobiology Center)

Figure 1:

The transit light curves of K2-3d observed by the
Okayama 188 cm telescope with MuSCAT. The top,
middle, and bottom light curves are in g, r, and z-band,
respectively. The circle points and solid lines show
10-minutes binning data and best-fit theoretical lines,
respectively.

Figure 2: Residuals of the mid-transit times from the refined
linear ephemeris. The square, triangle, and circle
points represents the observed data of K2, Spitzer, and
MuSCAT, respectively. The gray and black points arefor the values in literature ([1,2]) and those refinedin this work, respectively. The purple and orange
dashed lines show the ephemerides provided by [1]and [2], respectively. The red shaded area shows 1-σuncertainties of our new ephemeris.

Astrometry of H2O Masersin Massive Star-forming Region S255IR-SMA1
NAGAYAMA, T., SUNADA, K.

We report the astrometric results of H2O masers in
S255IR-SMA1 with VERA (VLBI Exploration of Radio
Astrometry). The anuual parallax was measured to be
0.563 ± 0.036 mas, corresponding to the source distanceof D = 1.78 +0.12−0.11 kpc. Maser morphology and its propermotion appear to trace a U-shaped bow shock propagating
away from MYSO. These results are reported in Burns etal. (2016) [1], in detail.
Whether or not the outflows of low- and high-massstars are produced in the same way is not well known.
S255IR-SMA1 is the brightest source of molecular line
emission in the S255IR star-forming region and its stellar
mass is estimated to be ~ 20 M. S255IR-SMA1 is an
ideal target to study the relationship between outflows
and jets in an MYSO. We pursue VLBI observations
aimed at measuring the annual parallax, distribution andproper motions of H2O masers in S255IR-SMA1.
The observations were carried out using VERA
from 23 Nov. 2008 to 11 Aug. 2010. S255IR-SMA1 andthe positional reference source J0613+1708 with theseparation of 0.87° were simultaneosly observed with thedual beam. The correlation processing was done using
Mitaka FX correlator.
Figure 1 shows the anuual parallax of S255IR-SMA1.
Th parallax was obtained to be π = 0.563 ± 0.036 mas,corresponding to a source distance of D = 1.78 +0.12−0.11 kpc.
Figure 2 shows the ditributios and internal proper motionsof H2O masers. The elongated NE-SW morphology andbipolar outward motions of masers suggest that they areassociated with an ejection event from an MYSO. The
3D velocity of each jet lobe is estimated to be 19 km s−1
with respect to the MYSO, with a position angle of 49°.
The maser group in SW appear to trace a U-shaped bow
shock structure. Ths structure is well reproduced by thejet-driven outflow model with a jet radius of about 6 AU.

(NAOJ)			

OMODAKA, T.

(Kagoshima University)

Figure 1: Anuual parallax of S255IR-SMA1.
400
12
300

10

200

8

100

6
4

0
−100

Reference[1] Burns, R. A., et al.: 2016, MNRAS, 460, 283.

2

1 mas/yr
400

300

LSR velocity (km/s)(Kagoshima University)			

Decl. offset (mas)

BURNS, R. A., HANDA, T.

200
100
0
R.A. offset (mas)

−100

0

Figure 2: Distributions and internal proper motions of H2O masersin S255IR-SMA1. The color indicates the LSR velocity.
The black cross indicates the position of the centimetre
continuum source. 1 mas yr−1 corresponds to 8.4 km s−1
at 1.78 kpc.

I Scientific Highlights043

Developments of Millimeter-wave MKID Camera
SEKIMOTO, Y., DOMINJON, A., HASEBE, T., NOGUCHI, T., MATSUO, H., SHAN, W. L., KIUCHI, H.
(NAOJ)SEKIGUCHI, S., SHU, S., SHIMIZU, T.

NITTA, T., NAGAI, M., MURAYAMA, Y., HATTORI, S.

(University of Tokyo/NAOJ)				

MKID (Microwave Kinetic Inductance Detector)
group of Advanced Technology Center is developing
superconductive camera in millimeter and terahertz
wavelengths for Antarctica terahertz telescope/Nobeyama
45 m telescope which observes distant galaxies withwide field-of-view and for CMB B-mode polarizationin collaboration with University of Tsukuba, Saitama
University, ISAS/JAXA, KEK, and Riken. Four papers
related to millimeter/submillimeter MKID instruments
were published in 2016 fiscal year.
1. Broadband corrugated horn array [1]We are developing a broadband corrugated horn
array to observe millimeter-wave polarization with highsensitivity and high accuracy. An 80–180 GHz horn arrayexceeding the octave band has been fabricated as shownin Fig. 1 and characterized with millimeter waves. The
geometry of corrugations is so simple that the horn arraycan be directly machined from a bulk of aluminum withan end-mill.The cross-polarization and near side-lobelevels are less than -20 dB and -30 dB, respectively.The
return loss is less than -15 dB in most design frequency
bands, and the beam pattern is symmetric.The beam
pattern and the return loss are measured in the 120–
170 GHz range at room temperature.They are in good
agreement with the simulation. It is possible to reducereflection at the aperture surface and to reduce the weightby carving the unnecessary part.This design provides
an octave bandwidth of the corrugated horn array atreasonable machining time.

Figure 1: A broadband corrugated horn array [1].

2. Broadband anti-reflective structures for silicon [2]A broadband antireflective sub-wavelength structure
was developed for large diameter silicon lenses usedin the optical systems of superconducting cameras. In
this study, a broadband antireflective sub-wavelength
structure that can be easily fabricated with a dicing
blade was designed. Pyramid structure (depth 550 μm)
and straight section (depth 150 μm) have been fabricated044

I Scientific Highlights(University of Tsukuba)		

NARUSE, M.

(Saitama University)with a special V-shaped dicing blade and a normal blade,respectively (Fig. 2). The structure was fabricated on aflat surface, and transmittance at cryogenic temperatures
was measured using a Fourier transform spectrometer.
The measured average transmittance between 186 and346 GHz was approximately 95 %, and the experimental
result is in good agreement with the simulation results.

Figure 2: Broadband anti-reflective structure for Silicon [2].

3. Octave-band OMT with MKID [3]
We demonstrate a design of octave-band circular
waveguide coupled planar ortho-mode transducer (OMT)with MKIDs. In our 4-pixel prototype design, each single
pixel is sensitive to two frequency bands (90 GHz and
150 GHz) corresponding to atmospheric window. Silicon
on insulator (SOI) has been used for the OMT backshortstructure and a broadband coplanar waveguide (CPW)
180-degree hybrid is designed to cancel higher modesof a circular waveguide and add two signals from thefundamental mode together. After a microstrip bandpass
diplexer, a microstrip line to coplanar waveguidetransition structure couples signals to an MKID. MKIDs
are designed with Nb ground plane and Al/Ti bilayer
center strip line to achieve low frequency response andhigh sensitivity.
4. LiteBIRD MKID focal plane design [4]Observations of large scale B-mode polarization ofcosmic microwave background radiation (CMB) explore
the inflation theory (K. Sato 1981), which explains the
hot big-bang. This paper shows a focal plane design withcorrugated horn coupled OMT-MKID for LiteBIRD,
which observes CMB B-mode polarization from thecosmological gravitational wave.
References[1] Sekiguchi S., et al.: 2017, IEEE TST, 7, 36.
[2] Nitta, T., et al.: 2017, IEEE TST, 7, 295.
[3] Shu, S., et al.: 2016, SPIE proceedings, 99142C.
[4] Sekimoto, Y., et al.: 2016, SPIE proceedings, 99142A.

Formation of Spiral Arm in Galaxies by Swing Amplification			

MICHIKOSHI, Shugo(Kyoto Women’s University)		

λ̃ y,max

θmax [deg.]

The origin and evolution of spiral arms in disk
galaxies is a fundamental problem in astrophysics. One
theory to explain the spiral arms is swing amplification.
In a differentially rotating disk, a leading density patternrotates to a trailing one due to the shear. During therotation, the leading mode is amplified into spiral arms
due to the self-gravity if the Toomre’s Q is 1–2.

80
60
40
20
0

λ̃ x,max(NAOJ)

In our previous work, we investigated the pitch angleof spiral arms by the local linear theory and simulations[1]. The derived pitch angle formula well agrees with
N-body simulations.
We extended the our previous work and calculated
the pitch angle, the wavelengths, and amplification factorof the most amplified mode [2]. The derived formulaeof the pitch angle, the radial wavelength, the azimuthal
wavelength, and the amplification factor are

4
2
0

Dmax

KOKUBO, Eiichiro

2
1
0
15
10
5
0

1 1.2 1.4 1.6 1.8 2
κ/ Ω

Figure 1: Comparison between the theory and the simulations.
Circles and pluses denote the results of N-bodysimulations. The dotted and dashed curves show
the estimates from the linear theory with Q = 1.5
and Q = 1.8, respectively. Triangles show the lower
and upper limit of the amplification factor from thesimulations.

where κ is the epicycle frequency, Ω is the orbital
frequency, A is the Oort constant, Q is the Toomre’s Q.
Figure 1 shows the results. We confirmed that theformulae derived from the linear theory well agree with
N-body simulations.
Next, in order to understand the physics of the swing
amplification, we revisited the swing amplification
model [3]. We carefully considered its derivation andwe found that the naive treatment of the model leads tobreakdown of the model in the strong shear case such asa Keplerian rotation. Therefore we modified the model
for avoiding the breakdown. Using the modified model
we investigated the motion of stars in spiral arms. We
found that the phases of the epicycle motion of stars
are synchronized during the amplification. Based on
the phase synchronization we derived the pitch angle
formula by the order-of-magnitude discussion. The phasesynchronization may be a key process to understand theswing amplification.

References[1] Michikoshi, S., Kokubo, E.: 2014, ApJ, 787, 174.
[2] Michikoshi, S., Kokubo, E.: 2016, ApJ, 821, 35.
[3] Michikoshi, S., Kokubo, E.: 2016, ApJ, 823, 121.

I Scientific Highlights

045

Planetesimal Formation by Gravitational Instabilityof Porous-Dust Aggregates
MICHIKOSHI, Shugo

In a protoplanetary disk, small dust grains growto kilometer-sized objects called planetesimals. The
formation mechanism of planetesimals is one of today's
most important unsolved problems. Recent studies on the
dust growth showed that the icy dust aggregates formedby coagulation are not compact but significantly porous.
The internal density of dust aggregates is much smaller
than the material density. A compression mechanism isnecessary to form compact planetesimals.
It was found that the dust aggregates can becompressed by the ram pressure when the dust aggregate
mass is less than 1011 g [1]. The dust aggregates withthe mass ~> 1011 g are compressed by the self-gravity.
Due to these compression mechanisms, the compact
planetesimals may be formed.
We focused on the final stage of dust aggregate
compression. We investigated the dynamics of porous dust
aggregates by using the detailed model. We considered
the self-gravity, mutual collisions, aerodynamic drag,turbulent stirring, and scattering due to gas and calculated
the equilibrium random velocity. From the equilibrium
random velocity we calculated the Toomre’s Q to
examine the gravitational instability (GI) [2].
For the axisymmetric mode, the instability condition
is Q < 1 [3]. For 1 < Q < 2, the non-axisymmetric modecan grow due to the swing amplification mechanism[4,5]. Thus, we adopt the GI condition as Q < 2. In theminimum mass solar nebular model with α = 10−3, we
found that the GI condition is finally satisfied. In otherwords, the porous dust disk becomes gravitational
unstable to fragment to form planetesimals.
However, if the turbulent strength is sufficiently
strong, the GI would be suppressed. Thus it depends on
α whether the GI takes place. We assumed the various
parameters and checked whether GI occurs. Figure 1
shows the summary of the results. The GI is more prone
to occur for larger fg, where fg is the normalized disk
mass. Thus, the upper limit of α for the GI exists.
Using the approximations we derived the condition
for GI

where a is the distance from the central star, CD is thegas drag coefficient, M* is the central star mass, η is thegas pressure gradient parameter, Σd is the dust surface
density, Σg is the dust surface density. Figure 1 shows thisestimate, which well agrees with the numerical result.

046

I Scientific Highlights

KOKUBO, Eiichiro(Kyoto Women’s University)		

(NAOJ)

We found that if the turbulence is not strong (α−3 ), the GI takes place. The GI accelerates the<10~planetesimal formation significantly.
10−1
MMSN
10−2

α cr

α

			

10−3

10−4

GI-region crossing
Not GI-region crossing
10−1

100

101

fg

Figure 1: Parameter region for the GI on the normalized disk
mass fg and the turbulent strength α plane. The open
circle points show the cases where the GI takes place.
The filled triangles show the cases where the GI does
not take place. The solid line represents the estimate of
the critical α. The minimum mass solar nebular model(MMSN) corresponds to fg = 1.

References[1] Kataoka, A., et al.: 2013, A&A, 557, 4.
[2] Michikoshi, S., Kokubo, E.: 2016, ApJL, 825, L28.
[3] Toomre, A.: 1964, ApJ, 139, 1217
[4] Michikoshi, S., Kokubo, E.: 2016, ApJ, 821, 35.
[5] Michikoshi, S., Kokubo, E.: 2016, ApJ, 823, 121.

N-Body Simulation of Chariklo’s Ring			

MICHIKOSHI, Shugo(Kyoto Women’s University)		

Recently, two dense narrow rings around Centaur
Chariklo were discovered [1]. The existence of a ringaround Centaur Chiron was also proposed [2]. Theseobservations suggest that rings around large Centaurs
may not be rare.
Chariklo’s ring has the large optical depth which
is about 0.3–0.4. In Saturn’s ring, the gravitational
instability takes place in the region where the ring has
the large optical depth and the self-gravity wakes form.
The self-gravity wakes are small spiral structures, whichcause the efficient angular momentum transfer. Thus, inorder to investigate the detailed structure of the ring, we
performed the global N-body simulations.
We developed the simulation code using the N-bodysimulation library, FDPS [3]. We considered thegravitational interaction, and mutual collisions.
Figure 1 shows the typical result of the simulation. We
adopted the particle density ρp /ρC = 0.5 and the radius rp= 5 m, where ρp is the particle density, ρC is the Chariklo’s
density, and r p is the particle radius. The large scale
structures are not visible. For the dynamical timescales,
the ring keeps its original global shape. However, we findsmall scale structures, namely, self-gravity wakes in the
inner ring.

KOKUBO, Eiichiro(NAOJ)

We p e r f o r m e d t h e s i m u l a t i o n s w i t h v a r i o u sparameters. If ρ p /ρ C > 0.5, the rapid large aggregate
formation takes place. Thus, this case does not correspondto the real ring. For suppressing the self-gravity wakes,
the very low density particles, such as ρp /ρC < 0.1, arenecessary.
Next we examined the long term evolution of thering with the self-gravity wakes. The wakes accelerate
the viscous spreading of the ring significantly and it
typically occurs on timescales of about 100 years, whichis considerably shorter than the timescales suggested inprevious studies. Thus, the existence of these narrowrings implies the existence of shepherding satellites.

References[1] Braga-Ribas, F., et al.: 2014, Nature, 508, 72.
[2] Ortiz, J. L., et al.: 2015, A&A, 576, A18.
[3] Michikoshi, S., Kokubo, E.: 2017, ApJL, 837, L13.
[4] Iwasawa, M., et al.: 2016, PASJ, 68, 54.

Figure 1: Particle distribution of the simulated ring in the x-y plane where the particle density and radius are ρp /ρC = 0.5 and rp = 5 m,
respectively. The panel (a) shows the overall structure of the ring, while the panel (b) shows enlarged view of ring section.

I Scientific Highlights047Mid-Infrared Spectroscopic Observationsof the Classical Nova V2676 Oph with Subaru/COMICSKAWAKITA, Hideyo, ARAI, Akira, NAGASHIMA, Masayoshi(Koyama Astronomical Observatory/Kyoto Sangyo University)
			

OOTSUBO, Takafumi(The University of Tokyo)		

A classical nova is an explosive event with a sudden
increase in brightness that occurs on a white dwarf(WD) star. The explosion of the gas envelope of the
WD (accreted from the companion star) is powered bythermonuclear runaway reactions that occur at the baseof the envelope. The nature of the WD star is essential
to the chemistry of the ejected material in novae. A dustforming nova V2676 Oph (discovered in Mar 2012) was
the first nova to provide evidence of both C 2 and CN
molecules during its near-maximum phase and evidence
of CO molecules during its early decline phase [1]. The
derived carbon- and nitrogen-isotopic ratios in the nova
[2] are consistent with that the nova explosion was hosted
by a CO-rich WD rather than an ONe-rich WD. The
existence of both C2 and CN radicals in the photosphereindicates that the nova envelope was C-rich, with C/O > 1[3]. To confirm a type of the hosting WD (CO-rich or
ONe-rich), we performed the mid-infrared imaging andlow-resolution spectroscopic observations of V2676 Ophwith COMICS mounted on the Subaru telescope in June2013 and May 2014 (482 days and 782 days respectively
after its discovery) [4]. No clear [Ne II] emission line
at 12.8 μm was observed in either the 2013 or 2014
observations. Based on the absence of [Ne II] emission,
the WD hosting V2676 Oph is considered a CO-rich
WD. Both types of dust grain, carbon-rich and oxygenrich, were detected on both dates, although this nova
is considered as a Carbon-rich (C/O > 1) based on thepresence of C2 observed earlier. The 11.4 μm unidentified
infrared (UIR) emission was also detected on these dates.
The coexistence of UIR carriers and carbon-rich grains inV2676 Oph supports the formation of UIR carriers from
amorphous carbon grains. Non-equilibrium processes
are likely to be responsible for the grain formation in the
nova.

048

I Scientific Highlights

SHINNAKA, Yoshiharu(NAOJ)

Figure 1: Low-resolution N-band spectra of V2676 Oph taken on
UT 2013 June 20 and UT 2014 May 16. We assumed
the grain radii for amorphous carbon and astronomicalsilicate to be 0.1 μm to reproduce the observed spectra.
The UIR emission at 11.4 μm is clearly detected in both
spectra [4].

References[1] Nagashima, M., et al.: 2014, ApJL, 780, L26.
[2] Kawakita, H., et al.: 2015, PASJ, 67, 17.
[3] Kawakita, H., et al.: 2016, PASJ, 68, 87.
[4] Kawakita, H., et al.: 2017, AJ, 153, 74.

Success of a Laser Link Experiment with the Hayabusa2 Laser Altimeter
NODA, Hirotomo1, KUNIMORI, Hiroo2, MIZUNO, Takahide3, SENSHU, Hiroki4
OGAWA, Naoko3, TAKEUCHI, Hiroshi3, MOORE, Chris5, POLLARD Alex5
YAMAGUCHI, Tomohiro3, NAMIKI, Noriyuki1, KASE, Teiji6, SAIKI, Takanao3, TSUDA, Yuichi3
1: NAOJ, 2: NICT, 3: JAXA, 4: Chiba Inst. Tech., 5: Space Environment Research Centre, 6: NEC

References[1] Noda, H., et al.: 2017, Earth, Planets and Space, 69, 2.
[2] Smith, D., et al.: 2006, Science, 311, 53.
[3] Abshire, J., et al.: 2006, Proceedings of the conference on lasers
and electro-optics.

6

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-4

-4

-4

-2

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-2

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Figure 1: Number of signal detection with respect to the spacecraft
scan direction on December 11 (left) and 15 (right), 2015
respectively [1]. Color shows the number of detection.
The horizontal and vertical axes are the step sizes ofthe spacecraft scan, the directions of which nearlycorrespond to the right ascension and declination of thepointing direction, and the origin is the best-estimateddirection of the boresight obtained during the groundbased prelaunch test. The maximum detection number
for one tile is 17, because one data point was obtained
within 2 seconds and spacecraft stayed one attitude forabout 35 seconds.
Received intensity data on Dec. 19 in range mode

gain = 8

gain = 2

el offset = 6 asgain = 8

1000

[mV]

The Hayabusa2 spacecraft, launched on December
3, 2014, is equipped with a laser altimeter called
LIDAR. The laser altimeter is a ranging instrument
which measures time of flight of laser pulses between
spacecraft and celestial bodies with solid surface. Laserlink experiments between the LIDAR and ground-based
satellite laser ranging stations were conducted when thespacecraft was near the Earth before and after the gravity
assist operation in December 2015, and uplink laser
pulses from a ground station were successfully detected[1]. In addition to the main purpose of this experiment,
which is the demonstration of the time transfer techniquefor onboard clock calibration, it was also a unique
opportunity for the performance check of the instrument
before arrival at the asteroid, including the alignment
determination of the LIDAR field of view (FOV) axis
with respect to the spacecraft.
To determine the FOV direction, the spacecraft wasscanned spirally with 1 mrad step. Number of detectionof the laser pulses at each spacecraft attitude by LIDAR
is shown in Fig. 1. The yellow tiles correspond to thespacecraft attitudes where maximum number of laser
pulses were detected. With this information, the FOV
direction was determined with the accuracy of scanstep size. Fig. 2 shows the reception level of the laser
pulses by the LIDAR when we set the LIDAR to anotherobservational mode (range mode). Because the intensity
varied with the change of receiver gain and pointing shiftof the ground-based telescope, we confirmed that thesignals came from the ground-based laser, not from othersources such as Earth background radiation.
Hayabusa2 became the third spacecraft to establish
a laser link at a distance farther than the Moon with aground station, following the MESSENGER [2] and Mars
Global Surveyor missions [3]. The farthest distance of
successful experiment was 6.6 million km on December
19, 2015.

100

15:30

15:40

15:50

16:00
HH:MM

16:10

16:20

16:30

Figure 2: Intensity of the received pulses by LIDAR [1].
Experimental conditions of receiver gain (“high” =8, “low” = 2) and the pointing offset of the groundtelescope (el offset = 6 as) are drawn at the top. It is
obvious that the reception level changes according to thechanges of the observational conditions.

I Scientific Highlights

049

Spiral Structure and Differential Dust Size Distribution
in the LkHα 330 Disk
AKIYAMA, Eiji1, HASHIMOTO, Jun1/2, LIU, Hauyu B.3/4, LI, I-Hsiu J.4/5, BONNEFOY, Michael6/7
DONG, Ruobing8, HASEGAWA, Yasuhiro1/9, HENNING, Thomas7, SITKO, Michael L.10/11
JANSON, Markus12, FELDT, Markus7, WISNIEWSKI, John13, KUDO, Tomoyuki1, KUSAKABE, Nobuhiko2
TSUKAGOSHI, Takashi14, MOMOSE, Munetake14, MUTO, Takayuki15, TAKI, Tetsuo16
KUZUHARA, Masayuki2, MAYAMA, Satoshi17, TAKAMI, Michihiro4, OHASHI, Nagayoshi1
GRADY, Carol A.18/19, KWON, Jungmi20, THALMANN, Christian21, ABE, Lyu22, BRANDNER, Wolfgang7
BRANDT, Timothy D.23, CARSON, Joseph C.7/24, EGNER, Sebastian1, GOTO, Miwa25, GUYON, Olivier1
HAYANO, Yutaka1, HAYASHI, Masahiko1, HAYASHI, Saeko S.1, HODAPP, Klaus W.26, ISHII, Miki1
IYE, Masanori1, KNAPP, Gillian R.23, KANDORI, Ryo1, MATSUO, Taro27, MCELWAIN, Michael W.18
MIYAMA, Shoken28, MORINO, Jun-Iichi1, MORO-MARTIN, Amaya29/30, NISHIMURA, Tetsuo1
PYO, Tae-Soo1, SERABYN, Eugene18, SUENAGA, Takuya1/17, SUTO, Hiroshi1, SUZUKI, Ryuji1
TAKAHASHI, Yasuhiro H.1/20, TAKATO, Naruhisa1, TERADA, Hiroshi1, TOMONO, Daigo1, TURNER, Edwin L.20/23
WATANABE, Makoto31, YAMADA, Toru32, TAKAMI, Hideki1, USUDA, Tomonori1, TAMURA, Motohide1/2/20
1: NAOJ, 2: Astrobiology Center, 3: European Southern Observatory, 4: Academia Sinica, 5: University of Illinois at Urbana-Champaign,
6: University of Grenoble Alpes, 7: Max Planck Institute, 8: University of Arizona, 9: California Institute of Technology, 10: Space Science
Institute, 11: University of Cincinnati, 12: Stockholm University, 13: The University of Oklahoma, 14: Ibaraki University, 15: Kogakuin
University, 16: Tokyo Institute of Technology, 17: The Graduate University for Advance Studies, 18: NASA, 19: Eureka Scientific, 20: The
University of Tokyo, 21: ETH Zurich, 22: Universite de Nice, 23: Princeton University, 24: College of Charleston, 25: Universitäts-Sternwarte
München, 26: University of Hawaii, 27: Kyoto University, 28: Hiroshima University, 29: Space Telescope Science Institute, 30: Johns Hopkins
University, 31: Hokkaido University, 32: Tohoku University050

I Scientific Highlights

01(mJy arcsec-2)
2
3
4

5

12.5|
J2000 Dec.

Dust trapping accelerates the coagulation of dust
particles, and thus it represents an initial step toward theformation of planetesimals. We report H-band (1.6 µm)
linear polarimetric observations by Subaru telescopeand 0.87 mm interferometric continuum observations by
Submillimeter Array (SMA) toward a transitional disk
around LkHα 330 [1]. As results, a pair of spiral arms
were detected in the H-band emission and an asymmetric(potentially arm-like) structure was detected in the 0.87
mm continuum emission. We discuss the origin of the
spiral arm and the asymmetric structure, and suggest thata massive unseen planet is the most plausible explanation[2].
The possibility of dust trapping and grain growthcausing the asymmetric structure was also investigatedthrough the opacity index (β) by plotting the observed
SED slope between 0.87 mm from our SMA observationand 1.3 mm from literature [3,4]. The results imply thatgrains are indistinguishable from ISM-like dust in theeast side (β = 2.0 ± 0.5) [5], but much smaller in thewest side β = 0.7 +0.5
−0.4 , indicating differential dust size
distribution between the two sides of the disk. That isdust grains grow to millimeter size in the west side, while
they remain 0.1–1 micron size in the east side.
Future observations at centimeter wavelengths anddifferential polarization imaging in other bands (Y toK) with extreme AO imagers are required to understand
how large dust grains form and to further explore the dust
distribution in the disk.

12.0|
11.5|

32°
24 11|.003h45m48s.36

100 AU
48s.30 48s.26
J2000 R. A.

48s.22

48s.18Figure 1: It represents a superposed SMA 0.87 mm continuum
image on the Subaru H-band (1.6 μm) polarized intensity
image. The first contour is 8σ and increases up to 20σ
with 2σ steps.
References[1] Akiyama, E., et al.: 2016, AJ, 818, 158.
[2] Dong, R., et al.: 2015, ApJ, 809, L5.
[3] Brown, J. M., et al.: 2008, ApJL, 675, L109.
[4] Isella, A., et al.: 2013, ApJ, 775, 30.
[5] Dranie, B. T.: 2016, ApJ, 636, 1114.

Seasonal Variation of the Radial Brightness Contrastof Saturn’s Rings Viewed in Mid-infrared
FUJIWARA, Hideaki, FUJIYOSHI, Takuya, YAMASHITA, Takuya(NAOJ)MORISHIMA, Ryuji(University of California, Los Angeles/Jet Propulsion Laboratory)

Figure 1: Comparison of MIR images of Saturn’s rings in April
2005 (top) and January 2008 (bottom). 12.5 μm (left)
and 24.5 μm (right).
102

24.5
24.5

24.5
24.5

20.5
18.8
17.7

20.5
18.8
17.7

101
Surface Brightness (Jy/arcsec2)

To investigate the mid-infrared (MIR) characteristics
of Saturn’s rings, we collected and analyzed MIR highspatial resolution images of Saturn’s rings obtained in
January 2008 and April 2005 with COMICS mounted
on Subaru Telescope (Figure 1), and investigated thespatial variation in the surface brightness of the rings in
multiple bands in the MIR (Figure 2). We also composed
the spectral energy distributions (SEDs) of the C, B,
and A rings and the Cassini Division, and estimatedthe temperatures of the rings from the SEDs assuming
the optical depths measured from stellar occultation
observations by Cassini/UVIS.
We find that the C ring and the Cassini Division were
warmer than the B and A rings in 2008. This could be
accounted for by the lower albedos, lower optical depths,
and smaller self-shadowing effect in the C ring and theCassini Division than the B and A rings.
We also find that the C ring and the Cassini Divisionwere considerably brighter than the B and A rings in
the MIR in 2008, and the radial contrast of the ringbrightness is the inverse of that in 2005. This temporalvariation is probably caused by seasonal changes of theelevations of the Sun and observer above the ring plane
as varying angles will lead to differing filling factors andtemperatures of the particles in the rings.

12.5

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11.7
12.5

12.5
10.5

10.5

10-1

9.7

9.7

8.8

8.8

Reference[1] Fujiwara, H., et al.: 2017, A&A, 599, A29.
12.5µm-to-24.5µm Ratio

10-2-100000-50000-100000-500000Radius (km)50000

100000050000

100000

0.04
0.03
0.02
0.01
0

Radius (km)Figure 2: Top: profiles of surface brightness in all the bands inJanuary 2008 (red) and April 2005 (blue). Bottom:
profile of 12.5 μm-to-24.5 μm brightness ratio for
Saturn's rings in 2008. Negative and positive value ofthe radius is for the east and west side, respectively.
Region of the planetary body is shown in gray.

I Scientific Highlights

051

Discovery of Ubiquitous Fast-propagating Intensity Disturbancesby the Chromospheric Lyman Alpha Spectropolarimeter (CLASP)KUBO, Masahito1, KATSUKAWA, Yukio1, SUEMATSU, Yoshinori1, KANO, Ryouhei1, BANDO, Takamasa1
NARUKAGE, Noriyuki1, ISHIKAWA, Ryoko1, HARA, Hirohisa1, GIONO, Gabriel1/2, TSUNETA, Saku3
ISHIKAWA, Shin-nosuke3, SHIMIZU, Toshifumi3, SAKAO, Taro3, WINEBARGER, Amy R.4
KOBAYASHI, Ken4, CIRTAIN, Jonathan W.5, CHAMPEY, Patrick R.6, AUCHÈRE, Frédéric7
TRUJILLO BUENO, Javier8, ASENSIO RAMOS, Andrés8, ŠTĔPÁN, Jiří9, BELLUZZI, Luca10/11
MANSO SAINZ, Rafael12, De PONTIEU, Bart13, ICHIMOTO, Kiyoshi1/14, CARLSSON, Mats15
CASINI, Roberto16, GOTOU, Motoshi17
1: NAOJ/NINS, 2: SOKENDAI, 3: ISAS/JAXA, 4: NASA/MSFC, 5: University of Virginia, 6: UAH, 7: IAS, 8: IAC, 9: ASCR, 10: IRSOL,
11: KIS, 12: MPS, 13: LMSAL, 14: Kyoto University, 15: University of Oslo, 16: HAO, 17: NIFS/NINS[103 km]

17:04:20UT

17:04:23UT

17:04:27UT

17:04:30UT

−535

−535

−535

−535

−540

−540

−540

−540

−540

−545

−545

−545

−545

−545

−550

−550

−550

−550

−550

−555

−555

−555

−555

100

105 110[103 km]

115

100

105 110[103 km]

115

100

105 110[103 km]115

100

I Scientific Highlights−555
105 110[103 km]

115

100

105 110[103 km]

115

Figure 1: One example of the fast-propagating intensity
disturbances (sky-blue arrows). This event occurs in Box
1 of Figure 2. The background is Lyα image with the
CLASP/SJ after removal of the 30 s running temporal
average.

−400

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−700

−200

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[103 km]

1

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Figure 2: Fast propagating intensity disturbances are clearlyobserved around the centers of the green boxes. The
background image is Lyα image taken by the CLASP/
SJ.

References[1] Kano, R., et al.: 2017, ApJL, 839, L10.
[2] Kubo, M., et al.: 2016, ApJ, 832, 141.

052

17:04:34UT−535[103 km]High-cadence and high-sensitivity observations by theslit-jaw (SJ) optics system of the CLASP sounding rocket
experiment [1] reveal ubiquitous intensity disturbancesthat recurrently propagate in either the chromosphereor the transition region or both at a speed much higher
than the speed of sound [2]. The CLASP/SJ instrument
provides a time series of two-dimensional images takenwith broadband filters centered on the Lyα line (121.6 nm)
at a 0.6 s cadence. The sky-blue arrows in Figure 1
point out one example of the fast-propagating intensity
disturbances at the outer boundary of an active region. In
this case, the propagation speed is about 300 km/s, andthe similar moving patterns appear at least four times inthe same area. The multiple fast-propagating intensity
disturbances appear in the quiet Sun and in the active
region, and they are clearly detected in at least 20 areas
in a field of view of 527″ × 527″ during the 5 minute
observing time, as shown by the green boxes in Figure 2.
The apparent speeds of the intensity disturbances range
from 150 to 350 km/s. These speeds are much faster than
the speed of sound in the chromosphere or the transition
region ( < 50 km/s), and comparable to the local Alfvén
speed in the transition region. The intensity disturbances
tend to propagate along bright elongated structures
away from areas with strong photospheric magnetic
fields. This suggests that the observed fast-propagating
intensity disturbances are related to the magnetic canopy
structures. The maximum distance traveled by theintensity disturbances is about 10″, and the widths are a
few arcseconds, which are almost determined by a pixel
size of 1″. 03. The timescale of each intensity pulse isshorter than 30 s. One possible explanation for the fastpropagating intensity disturbances observed by CLASP ismagnetohydrodynamic fast-mode waves.

High-contrast Imaging of Intermediate-mass Giants
with Long-term Radial Velocity Trends
RYU, T.1/2, SATO, B.3, KUZUHARA, M.4, NARITA, N.1/4/5, TAKAHASHI, Y. H.5, UYAMA, T.5, KUDO, T.6
KUSAKABE, N.4, HASHIMOTO, J.4, OMIYA, M.2, HARAKAWA, H.2, ABE, L.7, ANDO, H.2
BRANDNER, W.8, BRANDT, T. D.9, CARSON, J. C.8/10, CURRIE, T.6, EGNER, S.6, FELDT, M.8, GOTO, M.11
GRADY, C. A.12/13/14, GUYON, O.6, HAYAHO, Y.6, HAYASHI, M.2, HAYASHI, S. S.6, HEŁMINIAK, K. G.6
HENNING, T.8, HODAPP, K W.15, IDA, S.3, ISHII, M.2, ITOH, Y.16, IYE, M.2, IZUMIURA, H.2/17
JANSON, Markus18, KAMBE, E.17, KANDORI, R.2, KNAPP, G. R.19, KOKUBO, E.1/2, KWON, J.5
MATSUO, T.20, MAYAMA, S.1, McELWAIN, M. W.21, MEDE, K.5, MIYAMA, S.22, MORINO, J.2
MORO-MARTIN, A.23/24, NISHIMURA, T.6, PYO, T.-S.6, SERABYN, E.25, SUENAGA, T.1/2, SUTO, H.2/4
SUZUKI, R.2, TAKAMI, M26, TAKATO, N.6, TAKEDA, Y.1/2, TERADA, H.2, THALMANN, C.27
TURNER, E. L.19/5, WATANABE, M.28, WISNIEWSKI, J.29, YAMADA, T.30, YOSHIDA, M.6/31
TAKAMI, H.2, USUDA, T.2, TAMURA, M.2/4/5
1: NAOJ, 2: SOKENDAI, 3: Tokyo Institute of Technology, 4: Astrobiology Center, 5: The University of Tokyo, 6: Subaru Telescope, 7:
Universite de Nice-Sophia Antipolis, 8: Max Planck Institute for Astronomy, 9: Institute for Advanced Study, 10: College of Charleston,
11: Ludwig-Maximilians-Universität, 12: Exoplanets and Stellar Astrophysics Laboratory, 13: Eureka Scientific, 14: Goddard Center for
Astrobiology, 15: University of Hawaii, 16: University of Hyogo, 17: Okayama Astrophysical Observatory, 18: Stockholm University, 19:
Princeton University, 20: Kyoto University, 21: Goddard Space Flight Center, 22: Hiroshima University, 23: Space Telescope Science Institute,
24: Johns Hopkins University, 25: Jet Propulsion Laboratory, 26: Academia Sinica, 27: ETH Zurich, 28: Hokkaido University, 29: Universityof Oklahoma, 30: ISAS/JAXA, 31: Hiroshima University

The radial velocity (RV) technique has been used as
one of the methods to search for exoplanets, discovering
more than 500 planets in last 20 years. However, thistechnique is less sensitive to wide-orbit ( > 10 au) planets
and inefficient to examine the occurrence rate of suchwide-orbit planets, even though it is crucial information
to test planet formation/evolution theories.
A long-term RV acceleration (RV trend) suggests thepresence of a possible planetary companion in a wide
orbit. However, such an RV trend could be caused not
only by a planet but also by a distant stellar or browndwarf companion. Direct-imaging technique is sensitive
to such wide-orbit companions and can help us to clarify
the cause of an RV trend through a detection or nondetection of companion.
Our RV survey conducted at Okayama AstrophysicalObservatory (OAO) has targeted intermediate-mass giants(1.5–5 M) for over a decade [1], finding the long-term
RV trends around several targets. To clarify the nature of
the RV trends observed in the OAO and another different
RV survey [2], we performed direct-imaging observations
for the six OAO targets as part of the SEEDS project [3]. (γHya, ι Dra, 18 Del, HD 5608, HD 14067, HD 109272).
We detected three stellar companions (0.61+0.12−0.14 M,
0.10 ± 0.01 M, 0.28 ± 0.06 M) in three systems (γ Hya,
HD 5608, and HD 109272) and rule out the presence ofstellar companions in the other three systems (ι Dra, 18
Del, HD 14067).
Combining the direct imaging and the RV data, wefound that the detected companions are responsible forthe observed RV trends and the causes of RV trends
for non-detection systems are low-mass stars or browndwarfs.
Gamma Hydrae

HD 109272

HD 5608

N

1”

1”

0.5”

41 AU

49.3 AU

28 AU

E

Figure 1: The detected companions are indicated by the yellow
circles. The central white areas around central the stars
were removed in analysis.

References[1] Sato, B., et al.: 2003, ApJ, 597L, 157S
[2] Kane, S. R., et al.: 2010, ApJ, 720, 1644K.
[3] Ryu, T., et al.: 2016, ApJ, 825, 127.

I Scientific Highlights

053

New Neutrino Source for the Study of Solar Neutrino Physics
in the Vacuum-matter Oscillation Transition Region [1]SHIN, Jae Won, CHEOUN, Myung-Ki(Soongsil University)		

PARK, Tae-Sun(Sungkyunkwan University)

One of open issues related to the vacuum-matter
oscillation transition region in the solar neutrino physics
is the determination of electron-neutrino survival
probability P(ν e → ν e ) in that region, which is also
closely related to the questions such as existence of sterile
neutrinos and/or non-standard neutrino interactions (NSI),
roles of CNO cycle in the Sun (metallicity problem), etc.
In this work [1], we propose a new artificial acceleratorbased electron-neutrino source for experiments of thevacuum-matter oscillation transition region. By adjusting
incident proton energy, we can produce a specificunstable isotope as an efficient electron-neutrino source.
Unstable isotope, 27Si, is our main neutrino source, which
can be produced through 27Al(p,n)27Si reaction and emits
electron-neutrinos through radioactive decay processes.
In this case, the neutrinos can have an energy range, 0 <Eν < 5 MeV, corresponding to the transition region.
Productions of 27 Si through p+ 27 Al reaction are
simulated by using GEANT4 code [2] with JENDL-4.0/
HE data [3]. Incident proton energy is chosen to be
15 MeV due to the following reasons. (1) There exist
only limited numbers of experimental data in the EXFOR
database. (2) By choosing this energy, we can suppress
productions of unnecessary unstable isotopes ( 23Mg,
25Al, 26Si, etc.) which can emit ν or ν̄ backgrounds. Aeeschematic diagram of the target geometry is drawn in
Fig. 1. For a 15 MeV proton beam with 10 mA, 3.55×1013
27Si per second (27Si/s) in the 27Al target are expected.
Reaction rates with respect to the neutrino energy
generated for the neutrino source are plotted in Fig. 2.
For both 37Cl and 71Ga, neutrinos having the continuous
energy (E th < E ν e <~ 3.79 MeV) and monoenergies(3.97 MeV and 4.813 MeV) interact with the isotopes.
Contributions of the neutrino with two mono-energies are
marginal. Consequently, we can obtain the reaction rates
or flux-averaged cross sections for both 37Cl(νe,e−)37Ar
and 71Ga(ν e,e −) 71Ge reactions in the neutrino energy
region less than ~3.79 MeV. This energy region is close
to the vacuum-matter oscillation transition region in thesolar neutrino physics. One can see that widths of energy
distributions of reaction rates for deuteron targets are
more narrow than those for both 37Cl and 71Ga becauseof the reaction thresholds. With this feature, we can also
have a chance to obtain reaction rates or energy averaged
cross sections for 2H(νe,e−pp) and 2H(νe,νenp) reactions
with narrow neutrino energy region. This is a uniquefeature in the present work because most experimental
data were obtained by using neutrino sources from pion
decay where the neutrino has broad energy region 0 ~054

I Scientific Highlights

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

55 MeV.

Graphite

Stainless steel

27Al(0.1 cm)

100 cmproton beam
(15 MeV)50 cm
Figure 1: Schematic diagram of thegeometry.

50 cm
27 Si

production target

Figure 2: Reaction rates via 37 Cl(ν e ,e − ) 37 Ar, 71 Ga(ν e ,e − ) 71 Ge,
2H(ν ,e−pp) and 2H(ν ,ν np) reactions. The neutrinos areee egenerated from decay of 27Si which are produced by the
15 MeV and 10 mA proton beam on a 27Al target.

References[1] Shin, J. W., et al.: 2016, Phys. Rev. C, 94, 045804.
[2] Agostinelli, S., et al.: 2003, Nucl. Instrum. Meth. A, 506, 250.
[3] JENDL-4.0/HE, http://wwwndc.jaea.go.jp/index.html.

Heavy Element Synthesis in Type II Supernovae:
Sensitivity to Nuclear Equation of States [1]		

FAMIANO, Michael A.

(Western Michigan University/NAOJ)		

				

AOKI, Wako

(NAOJ)		

A phenomenological model has been developedin which the enrichment of light r-process elements(relative to heavy r-process elements) in metal-poorand extremely-metal-poor stars (EMPs) is found todepend on the stiffness of the nuclear equation of state.
Here, an r-process is assumed in which an explosion
scenario is halted due to an accretion-induced collapse
and a subsequent failed or partial explosion, followedby partial ejection of r-process material. Nucleosynthsisthen results in an abundance distribution enriched in thelight r-process elements. Initial results suggest that apossible upper limit on the stiffness of the EOS may beconstrained by observations, which could complement
results of neutron star masses which place lower limits on
the EOS stiffness.
We have explored a previously-proposed model,
referred to as the tr-process [1], which assumes anr-process in a core-collapse scenario which is halted due
to an accretion-induced collapse into a BH or a stalledshock. The model attempts to explain the maximum[Sr/Ba] ejected in a single r-process event; we notethat reductions in this ratio may result from mixing
between outer and inner ejecta in the explosion or fromasymmetric explosion mechanisms. We also note thatthe observed large values of [Sr/Fe], [Ba/Fe], and [Eu/Fe] (so-called r-II stars) can be reproduced by turbulent
ejection (as suggested in [2]). The results presented
here represent one potential avenue for producing these
extremes.
The calculated [Sr/Ba] values are also shown in
Figure 1 compared to observed values in the galaxy.
The significant changes in the Ba ejection in a collapse
scenario results in a dramatic change in the [Sr/Ba] (and[Sr/Eu]) ratios. In a previous paper [2], changes in [Sr/Ba]
were suggested to be caused at least in part by turbulent
ejection of material in a collapse scenario. It is seen thatfor a softer EOS, the maximum values in [Sr/Ba] as afunction of metallicity can be achieved in a tr-process forpartial enrichment of r-process elements in a GCE model.
As noted above, the GCE results shown in these figures
represent extremes in these ratios as they are producedin collapse scenarios corresponding to the minimum
collapse time to a BH. In examining the abundance ratios
of [Sr/Ba] as they relate to the EOS, one sees that theseratios generally increase as the EOS softens. However,at some point, the EOS becomes so soft that the collapse

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

SUDA, Takuma(University of Tokyo)

time becomes early enough to prohibit Sr ejection, andthe ratios of [Sr/Ba] begin to decrease with the softnessof the EOS. This may occur for an EOS with a softness
somewhere between the Shen EOS and the LS220 EOS,
as one sees that the [Sr/Ba] ratios calculated using an
LS220 EOS drop below those calculated using a Shen
EOS at metallicities −2.5 < [Fe/H] < −2.

Figure 1: [Sr/Ba] as a function of [Fe/H] for several EOS
assumptions compared to observation.

References[1] Famiano, M. A., et al.: 2016, ApJ, 830, 61.
[2] Aoki, W., et al.: 2013, ApJ, 766, L13.

I Scientific Highlights055

Relativistic Screening Effects on Big Bang Nucleosynthesis
and Low-lying Resonances [1]		

FAMIANO, Michael A.

(Western Michigan University/NAOJ)

BALANTEKIN, A. Baha

(University of Wisconsin-Madison/NAOJ)

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

If an astrophysical environment is hot enough(greater than approximately 0.5 MeV or so), screening
in the associated nuclear reactions can be modified by
the presence of a relativistic electron-positron plasma.
For non-zero electron chemical potentials, the effectis compounded as the Debye length (which creates anadditional decrease in Coulomb energy with radiusbetween two reacting nuclei) in a plasma can drop
significantly, resulting in amplified reaction rates.
In a relativistic model, the Debye length decreases
with temperature, as shown in Figure 1. The effect ofscreening is to shift the reaction energy in the crosssection. This can result in an enhancement of nuclear
reaction rates, and the reaction rate enhancement factor
is studied in several relevant scenarios. For sub- or nearthreshold resonances, this could potentially change thereaction rates by a significant amount as the reactionenergy effectively shifts the resonance above or below
threshold.
Possible sites where relativistic plasma screening
could have a significant effect on observed results
include Big Bang Nucleosynthesis, α-rich freezeout inthe r-process, x-ray bursts, and type Ia supernovae inwhite dwarfs. Most recently, the effects of the screening
due to the relativistic electron-positron plasma during the
Big Bang Nucleosynthesis have been explored. Whilethe effects of relativistic screening were found to berelatively small in the standard Early Universe models,
further work is being done to explore the same effects inthe above-mentioned astrophysical sites. Additional work
is currently focused on possible effects on the productionof 56Ni in type Ia supernovae, effects on light curves(both frequency and duration) in X-ray bursts, and effects
on the electron fraction in the astrophysical r-process
following α-rich freezeout.
In this work we explored in detail the consequencesof the screening due to the relativistic electron-positronplasma on non-resonant and possible resonances on thesecondary reactions destroying A = 7 nuclei during the
Big Bang Nucleosynthesis. We found that effects ofscreening from the relativistic plasma are small even for
the reaction with the largest charge , namely 3He+7Be.
We note that this reaction is the least experimentally
explored one in the network of BBN reactions.
Even though the effects we find are small, it still
is worthwhile to demonstrate how robust our current

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understanding of the BBN is to effects not previously
considered. This is especially important since theinstruments scheduled to go online in the future, suchas the Thirty Meter Telescope [2], will measure theabundances of the light elements resulting from the BBN
with greater precision.

Figure 1: The Debye length for the 3He+7Be reaction as a functionof temperature (in MeV) for several electron chemical
potential assumptions.

References[1] Famiano, M. A., Balantekin, A. B., Kajino, T.: 2016, Phys. Rev.
C, 93, 045804.
[2] Skidmore, W., et al.: 2015, Research in Astron. Astrophys., 15,1945.

Detectability of Cosmic Dark Flowin the Type Ia Supernova Redshift-Distance Relation
MATHEWS, Grant J., ROSE, B. M., GARNAVICH, P. A.
(University of Notre Dame)			YAMAZAKI, D.

(Ibaraki University)

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)

We have re-analyzed [1] the detectability of large scale
dark flow (or local bulk flow) with respect to the CMB
background based upon the redshift-distance relation forType Ia supernovae (SN Ia). If a universal CMB dipole
exists it would be exceedingly interesting. Such apparent
large scale motion could provide a probe into the instants
before cosmic inflation, either as a remnant of multiple
field inflation, pre-inflation fluctuations entering thehorizon [2], or a remnant of the birth of the universe outof the mini-superspace of SUSY vacua in the M-theory
landscape. Such possibilities lead to a remnant dipole
curvature in the present expanding universe that would
appear as coherent velocity flow relative to the frame of
the cosmic microwave background . Hence, this has been
dubbed [3] “cosmic dark flow.”
We made two independent analyses: one based upon
identifying the three Cartesian velocity components;
and the other based upon the cosine dependence of thedeviation from Hubble flow on the sky. We applied theseanalyses to the Union2.1 SN Ia data [4] and to the SDSSII supernova survey [5]. For both methods, results for low
redshift, z < 0.05, are consistent with previous searches.
We find a local bulk flow of v bf ~ 300 km s −1 in the
direction of (l, b) ~ (270, 35)°. However, the search for adark flow at z > 0.05 is inconclusive. The reason that thedark flow is difficult to detect for z > 0.05 can be traced
to the large errors in the determined distance moduli of
the SN Ia data. For a fixed error in the distance modulus,
the actual error in the velocity increases with redshift.
Figure 1 from [1] illustrates the result of simulating
surveys that accumulate SNIa events at redshift bins
with Δz = z/3 centered at z = 0.05, 0.1, and 0.3. Theintersection of the horizontal dashed line with the curvesindicates the number of supernovae in Union2.1 low
redshift sample.
Based upon simulated data sets, we deduce thatthe difficulty in detecting a dark flow at high redshifts
arises mostly from the observational error in the
distance modulus. Thus, even if it exists, a dark flow is
not detectable at large redshift with current SN Ia data
sets. We estimate that a detection would require bothsignificant sky coverage of SN Ia out to z = 0.3 and areduction in the effective distance modulus error from 0.2
mag to < 0.02 mag. We estimate that a greatly expanded
data sample of ~104 SN Ia might detect a dark flow as
small as 300 km s−1 out to z = 0.3 even with a distancemodulus error of 0.2 mag. This may be achievable in anext generation large survey like LSST.

Figure 1: Illustration of the number of SN Ia required for a 3σ
detection in redshift bins centered at z = 0.05 (dotdashed line), z = 0.1 (thick dashed line), or z = 0.3 (thicksolid line). The vertical dashed line denotes a bulk flow
velocity of 326 km s−1 as inferred in our analysis of the
low redshift Union2.1 sample. The intersection of thisline with the lower z = 0.05 curve suggests that a flow
was detectable in the low redshift Union2.1 sample. Theintersection of this line with the upper curve, however,indicates that to detect a dark flow in at z = 0.3 the oneneeds N > 4582 SN Ia events.

References[1] Mathews, G. J., et al.: 2016, ApJ, 827, 60.
[2] Mathews, G. J., et al.: 2015, Phys. Rev. D, 92, 123514.
[3] Kashlinsky, A., et al.: 2008, ApJ, 686, L49.
[4] Suzuki, N., et al.: 2012, ApJ, 746, 85.
[5] Sako, M., et al.: 2008, AJ, 135, 348.

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057

Impact of Sterile Neutrino Dark Matteron Core-collapse Supernova Explosion
WARREN, M. L., MATHEWS, Grant J., MEIXNER, M.
(University of Notre Dame)HIDAKA, J., KAJINO, Toshitaka(NAOJ/University of Tokyo)

The nature of dark matter remains one of the biggest
open questions in physics. One viable dark mattercandidate is a sterile neutrino. Sterile neutrino dark matter
is an electroweak singlet that does not participate in thestrong, weak, or electromagnetic interaction.
We have re-analyzed [1] the impact of sterile neutrino
dark matter on core-collapse supernova explosions. We
considered sterile neutrino masses and mixing angles thatare consistent with sterile neutrino dark matter candidates
as indicated by recent X-ray flux measurements [2]. We
found that the interpretation of the observed 3.5 keV
X-ray excess as due to a decaying 7 keV sterile neutrino
that comprises 100 % of the dark matter would havealmost no observable effect on supernova explosions.
However, in the more realistic case in which the decaying
sterile neutrino comprises only a small fraction of thetotal dark matter density due to the presence of othersterile neutrino flavors, WIMPs, etc., a larger mixing
angle is allowed. In this case a 7 keV sterile neutrino
could have a significant impact on core-collapse
supernovae.
Figure 1 from [1] shows the electron neutrino
luminosity versus time post-bounce, both with and withouta sterile neutrino present. The neutrino luminosities of allneutrino and antineutrino flavors are enhanced from about
0.2 s to 0.4 s post-bounce. This increase in the neutrino
luminosities increases the neutrino reheating behind thestalled shock, and thus enhances the explosion energy.
The timescale of the increase of the neutrino luminosities
corresponds to the time post-bounce when the explosion
energy becomes enhanced.
A striking feature is the appearance of episodic
neutrino bursts with a period of 40–50 ms in theluminosity and flux with a 7 keV sterile neutrino. This isdue to the fact that the neutrino photospheric luminosity
is fixed by the ratio of the total internal energy to theneutrino diffusion time. When the neutrino chemical
potential falls above the resonance energy, thoseneutrinos in the energy groups corresponding to theresonance energy and width immediately have a diffusion
time scale drastically shortened by the free streamingof the sterile neutrinos to just below the neutrinosphere[3,4]. However, once a significant fraction of available
neutrinos is depleted, the process is shut off and theluminosity actually decreases until neutrinos can diffuse
back into the depleted energy and spatial groups. The

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amplitude and period of the luminosity spikes scaleroughly linearly with neutrino mass. Hence, should an
oscillation of the type shown here be detected in a next
generation neutrino detector such as Hyper-kamiokande,
its amplitude and period could be used to infer the massof the oscillating sterile neutrino.
Thus, a multi-component model is required toaccommodate a sterile neutrino mass and mixing angle
that leads to an enhanced explosion. if the decaying
sterile neutrino makes up (< 1 %) of the dark matter
density, a shorter decay lifetime is allowed corresponding
to the larger mixing angle needed to impact the explosion.

Figure 1: Neutrino luminosity versus time post-bounce. The blackline is for a simulation without a sterile neutrino, the redline is for a sterile neutrino with mass ms = 1 keV andmixing angle sin2 2θs = 10−5, and the blue line is for asterile neutrino with mass ms = 7 keV and mixing angle
sin2 2θs = 10−5.

References[1] Warren, M. L., et al.: 2016, Int. J. Mod. Phys., A31, 1650137.
[2] Boyarsky, A., et al.: 2014, Phys. Rev. Lett., 113, 251301.
[3] Hidaka, J., Fuller, G. M.: 2007, Phys. Rev. D, 76, 083516.
[4] Hidaka, J., Fuller, G. M.: 2006, Phys. Rev. D, 74, 125015.

Neutrino Antineutrino Pair Emissions in Strongly Magnetized
Neutron-Star-Matter in Relativistic Quantum Approach			

MARUYAMA, Tomoyuki

KAJINO, Toshitaka(University of Notre Dame)(NAOJ/University of Tokyo/Beihang University)

CHEOUN, Myung-Ki

MATHEWS, Grant J.

(Soongsil University)		

Magnetic fields in neutron stars play an importantrole in the interpretation of many observed phenomena.
Magnetar, which is associated with a super strong
magnetic field, show properties different than normal
neutron stars.
Many people have paid attention into coolingprocesses of neutron stars because it must giveimportant information of neutron stars structure [1].
The neutron stars are cooled by the neutrino emission,and the magnetic field is expected to affect the emission
mechanism largely because the strong magnetic field can
supply energy and momentum into the process.
In this work [2] we study the ν νˉ - pair production fromelectron and proton, which occur only under the strong
magnetic field.
We assume a uniform magnetic field along thez-direction, B = (0, 0, B), and take the electro-magnetic
vector potential Aμ to be A = (0, 0, xB, 0) at the positionr ≡ (x, y, z). The relativistic proton wave function Ψ̃ is
obtained from the following Dirac equation:[(i∂/ − e A/ ) − m ] ψ̃(t, r ) = 0 ,(1)where m is the particle mass. By solving Eq. (1), we thenobtain the energy eigenvalues as(2)
where n is the Landau level number and pz is z-componentof the proton momentum. Then, we calculate ν ˉν-pairemissions from the transition between the different
Landau levels for electrons and protons in the relativistic
quantum mechanical way [2].
In Fig. 1 we show the calculation results of ν νˉ -pairluminosity per volume, L/V at the baryon density ρB =0.2 ρ0, where ρ0 is normal nuclear matter density. The
solid circles and open squares represent the calculation
results when B = 1015 G and B = 2 × 1015 G, respectively.
Since √¯
eB = 2.4 MeV when B = 1015 G, the transitionenergy is a few MeV and much larger than the magnetar
temperature T ≈ 280–720 eV [3], and we cannot use thelow temperature expansion in the actual calculations. So,
we make the calculations at several temperatures in a few
keV temperature regions and extrapolate them up to arealistic temperature.
The solid and long-dashed lines represent result of
the fitting function L/V = cT a at B = 1015 G and B = 2(University of Notre Dame)

× 1015 G, respectively, . For comparison, we give theneutrino luminosity per volume in the modified Urca
(MU) process [4] with the dashed line.
Our results show the powers of the temperature are a= 1.6 when B = 1015 G and a = 1.2 when B = 2 × 1015 G,
while its power is a = 8 in the MU process. At the realistic
temperatures, T = 700 eV, and B = 1015 G, our results give
L/V ~ 1021 (erg/cm3·s), while the MU process gives L/V ~1011 (erg/cm3·s). Our emission process is expected to bemuch larger than the usual emission process such as the
MU process in the strong magnetic field B ~ 1015 G and
the realistic temperature region.

10−20 Lνν̄ /V (erg / cm3· s)

			

106
105
104
103
102
101
100
10−1
10−2
10−3

ρB /ρ0 = 0.2

1015 G2 x 1015 G
MU

101

102
T (KeV)

Figure 1: ν νˉ -pair emission luminosity per volume at the baryon
density ρB = 0.2 ρ0.

References[1] Yakolev, D. G., Pethick, C. J.: 2004, Ann. Rev. Astron.
Astrophys, 42, 169.
[2] Maruyama, T., et al.: 2015, Phys. Rev. D, 91, 123007.; 2016,
Phys. Lett. B, 757, 125.
[3] Kaminker, A. D., et al.: 2009, MNRAS, 395, 2257.
[4] Maxwell, O. V.: 1987, ApJ, 319, 691.; Yakolev, D. G., Levensh,
K. P.: 1995, A&A, 297, 717.

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059

Possible Measurements of Reaction Cross Sections
for Explosive Nucleosynthesis using Laser -Driven γ-ray Pulses
HAYAKAWA, Takehito, KOTAKI, Hideyuki, KANDO, Masaki(National Institutes for Quantum and Radiological Science and Technology)
		

NAKAMURA, Tatsufumi(Fukuoka Institute of Technology)

Progress in laser physics enabled us to produce
various quantum beams such as electrons, gamma-rays,
and ion beams from high field plasma generated from theinteraction between high peak power laser and materials.
The energies of these radiations become higher than
10 MeV and thus they can interact with nuclei. The
quantum beams generated by high peak power laser havea potential to be used for the study of nuclear physics.
These laser driven quantum beams have the following
features: high flux, ultra-short pulse in a range fromfemtosecond to nanosecond, and continuous energy
distribution.
A pioneering nuclear experiment with high peak
power laser for the Big-Bang nucleosynthesis was
performed at University of Texas at Austin [1]; theastrophysical cross section of the 3He(d, p)4He reactionin the plasma generated by the Texas Petawatt Laser wasmeasured. In the Extreme Light Infrastructure Nuclear
Physics (ELI-NP), it was proposed to produce extremely
neutron rich unstable isotopes using fusion reactions ofneutron rich fission products on multi-targets including
232Th with high peak power laser to study the r process[2]. It was also proposed to study the s process andphotodisintegration reactions in supernova explosions(γ process) using highly intense neutron pulse provided
from laser driven D-T nuclear fusion reactions at the
Nuclear Ignition Facility (NIF) in LLNL [3].
We have proposed nuclear experiments using
laser driven γ-ray pulses to simulate stellar nuclear
photoreactions [4]. We have proposed new conceptsof three types of experiments using laser driven γ
pulses with stellar energy distribution. First, the direct
measurement of the stellar (γ, n) reaction cross section
on the ground state of atomic nuclei using γ-ray pulse
with stellar distribution. Second, the direct measurementof the (γ, n) cross section on exited states. As shown in
Fig. 1, the main target is irradiated by the first laser andthe nuclei are exited in plasma generated by the laser;
the second laser irradiate the target to generated γ-ray
pulse with stellar energy distribution. Third, the direct
measurement of the transition probability between the
ground state and an isomer of astrophysical interest via(γ, γ’) reactions using the γ-ray pulse generated by thehigh peak power laser. An important point to consider
in these methods is the generation of γ-ray pulse withenergy distribution approximately identical with stellar

060

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KAJINO, Toshitaka(Beihang University/NAOJ/University of Tokyo)

photon distribution. We have concluded that it is possible
to generate Planckian γ-ray pulse by bremsstrahlung on
the solid gold target with electron beams with continues
energy distributions generated by the laser plasma.

Gamma pulse
generaon target

Main target
Excited nuclei

Gamma-raypulse

Neutrons

Main laser pulse
First laser pulse

Figure 1: Schematic view of experiment.

References[1] Barbui, M., et al.: 2013, Phys. Rev. Lett., 111, 082502.
[2] Habs, D., et al.: 2011, Applied Physics B, 103, 471.
[3] Berstein, L., et al.: 2014, Plasma and Fusion Research, 9,4404101.
[4] Hayakawa, T., et al.: 2017, Quantum Beam Science, 1(1), 3.

Isomer Producution Ratio of 113Cd
Following Neutron-Capture Reactions to Investigate the Origin of 115Sn
HAYAKAWA, Takehito, SHIZUMA, Toshiyuki(National Institutes for Quantum and Radiological Science and Technology)

TOH, Yosuke, HUANG, Minghui, KIMURA, Atsushi, NAKAMURA, Shoji, HARADA, Hideo, IWAMOTO, Nobuyuki					(Soongsil University)		

CHIBA, Satoshi(Tokyo Institute of Technology)

The astrophysical origin of a rare isotope 115Sn has
remained still an open question [1,2]. An isomer 113Cdm(T1/2 = 14.1 y) in 113Cd is an s-process branching pointfrom which a nucleosynthesis flow reaches to 115Sn (seeFig. 1). The s-process abundance of 115Sn depends on theisomer production ratio in the 112Cd(n, γ)113Cd reaction.
Hayakawa et al. [3] measured the 112 Cd(n, γ) 113 Cd mreaction cross section at the thermal energy with neutrons
provided from a nuclear reactor, and pointed out thatthe s-process abundance of 115Sn depends on the ratioof the 112Cd(n, γ) 113Cd m reaction cross section to the
112 Cd(n, γ) 113 Cd gs reaction cross section in typicals-process energies of 1–50 keV. However, the isomer
production ratio has not been measured in the energy
region higher than the thermal energy. Thus, we havemeasured γ rays following neutron capture reactions on
112Cd using two cluster HPGe detectors in conjunction
with a time-of-flight method at J-PARC [4].
The experiment was performed using the accurate
neutron-nucleus reaction measurement instrument(ANNRI) installed at a neutron beam line of BL04 at
the MLF in the J-PARC. Proton beams with an average
beam power of 200 kW were injected into the mercury
target at a repetition rate of 25 Hz. The proton beams
were operated with the double bunch mode. High flux
pulsed neutrons were generated by spallation reactions on
the mercury target. A 112Cd foil enriched to 98.27 % wasplaced at the center of the γ-ray detector array. The γ-rays
from the 112Cd target were measured by two cluster HPGe
detectors. In the neutron energy region higher than thethermal energy, we observed both γ rays decaying to theground state and the isomer of 113Cd. The γ rays decaying
to the ground state with energies of 299 and 316 keV wereclearly observed, whereas a γ ray with an energy of 259
keV which decays to the isomer was also observed. We
have obtained the result that the relative γ-ray intensity
ratio of the isomer except for 737 eV is almost constant in
the energy region of up to 5 keV. The isomer production
ratios calculated by a statistical model were consistented
with these ratios. The present result supports the previous
conclusion that the contribution of the s-process from the
113Cd isomer to the solar abundance of 115Sn is minor in
the previous study [3]. The astrophysical origin of 115Sn(University of Notre Dame)

KAJINO, Toshitaka(Beihang University/NAOJ/University of Tokyo)

has remained still an open question.

s-process
Sn

Sn

115

In

113

114

117

In m

116

In

116

115
113

In

115

Cd

113

Cd

112

Sn

Sn

116

m

Inm
In

Cdm

115

Cd

114

Cd

113

Cd

115

r-processFigure 1: Nuclear chart around 113Cd.

References[1] Nemeth, Zs., et al.: 1994, ApJ, 426, 357.
[2] Theis, Ch., et al.: 1998, ApJ, 500, 1039.
[3] Hayakawa, T., et al.: 2009, ApJ, 707, 859.
[4] Hayakawa, T., et al.: 2016, Phys. Rev. C, 94, 055803.

I Scientific Highlights

061

Solving the Red Supergiant and Supernova Rate Problems
via Relic Supernova Neutrino Spectrum
		

HIDAKA, Jun

KAJINO, Toshitaka(Meisei University/NAOJ)(Beihang University/NAOJ/University of Tokyo)

MATHEWS, Grant J.

(University of Notre Dame/NAOJ)

Recent observations suggested that the maximum
mass of the red supergiant progenitors of core-collapse
SNe may be as small as 16.5–18 M instead of 25 M
(RSG problem). It has been also recognized thatthe observational supernova rate is smaller than thetheoretical estimate (SNR problem). We have investigatedthese two astronomical problems via the cosmic relicsupernova neutrinos (RSNs) [1].
According to the RSG problem, we assumed thepossibility that red supergiants with M > 16.5–18 M
end their lives as failed supernovae (M fSN
min =16.5, 18 M)and analyzed their contribution to the RSN spectrum.
This change in population of different types of SNe
can be seen as the deviation in RSN spectrum. SN
explosion mechanism is sensitive to the nuclear equationof state (EoS), which affects the temperature of theneutrino sphere. Therefore it is expected that this mass
limit influences the RSN energy spectrum. Under theassumption of a initial mass function, lowering mass limitof progenitors for fSNe decreases the relative abundanceof luminous SNe and then reduces the supernova rate.
Our results showed these features.
Figure 1 shows the ratio bewteen the theoreticalObs
and observational supernova rate (R Thr
SN /R SN ). Dottedlines indicate the upper and lower limits due to theuncertainties of star formation rate. Adopted value MfSN
min =16.5–18 M clearly solves the SNR problem. The RSN
spectrum was evaluated by assuming 10 years of running
time in a Hyper-Kamiokande detector, i.e., a 106 ton
water Čerenkov detector. The result is presented in Figure
2. It shows the RSN detection rate for two cases of M fSN
min =16.5, 18 M. In addition, the figure includes the results of
MfSN
min = 25 M for comparison. The figure clearly shows
the EoS dependence of RSN spectrum in the energy rangeof Ee+ > 30 MeV, and the locations where the event rates
exceed the atmospheric background are well separated.
This finding suggests a detection of the RSN spectrum
can give insight into the SN explosion mechanism interms of the nuclear matter properties.

Thr
Obs
Figure 1: Relationship between M fSN
min and R SN /R SN at z = 0 by
−4 yr −1 Mpc −3 . Three
adopting R Obs
SN ≈ 0.6 ± 0.2 × 10
lines are shown due to the uncertainties of IMF. The
horizontal blue band indicates the range of uncertainty
caused by R Obs
SN .

Figure 2: Predicted e+ energy spectra for the cases of M fSN
min = 16.5,
18 or 25 M without neutrino oscillation. The results
for two different fSNe models based upon the stiff EoS(Shen) and the soft EoS (LS) are included. The shadedenergy range below 10 MeV indicates the region where
the background noise due to reactor ν̄e may dominate.
The shaded energy range near the horizontal axis
indicates the region where the background may be
dominated by noise from atmospheric neutrinos.

Reference[1] Hidaka, J., Kajino, T., Mathews, G. J.: 2016, ApJ, 827, 85.

062

I Scientific Highlights

Non-Extensive Statistics Solution to the Cosmological Lithium Problem
HE, Jianjun

HOU, Suqing

PARIKH, Anuj

(NAOC, Chinese Academy of Sciences) (IMP, Chinese Academy of Sciences) (Universitat Politècnica de Catalunya)

KAHL, Daid

BERTULANI, Carlos A.

(University of Tokyo)

KAJINO, Toshitaka(NAOJ/University of Tokyo/Beihang University)(Texas A&M University-Commerce)

MATHEWS, Grant J.

ZHAO, Gang

(University of Notre Dame) 		

First proposed in 1946 by George Gamow [1], thehot Big-Bang theory is now the most widely accepted
cosmological model of the universe. The theory has been
vindicated by the observation of the cosmic microwave
background, our emerging knowledge on the large-scale
structure of the universe, and the rough consistency
between calculations and observations of primordial
abundances of the lightest elements in nature. The
primordial Big-Bang Nucleosynthesis (BBN) began
when the universe was 3-minutes old and ended less thanhalf an hour later when nuclear reactions were quenchedby the low temperature and density conditions in the
expanding universe. Big Bang nucleosynthesis (BBN)
theory predicts the abundances of the light elements
D, 3He, 4He and 7Li produced in the early universe.
The primordial abundances of D and 4 He inferredfrom observational data are in good agreement withpredictions, however, the BBN theory overestimates
the primordial 7Li abundance by about a factor of three[2,3,4,5]. This is the so-called “cosmological lithiumproblem”. Solutions to this problem using conventional
astrophysics and nuclear physics have not been successful
over the past decades, probably indicating new physics
during the era of BBN [6,7].
We have investigated [8] the impact on BBN
predictions of adopting a generalized distribution todescribe the velocities of nucleons in the frameworkof Tsallis non-extensive statistics [9]. This generalized
velocity distribution is characterized by a parameter q,
and reduces to the usually assumed Maxwell-Boltzmann
distribution for q = 1. We find excellent agreement
between predicted and observed primordial abundancesof D, 4He and 7Li for 1.069 ≤ q ≤ 1.082, which is shownin Fig. 1, suggesting a new solution to the cosmologicallithium problem.
We encourage studies to examine sources for
departures from classical thermodynamics during the
BBN era so as to assess the viability of this mechanism.
Furthermore, the implications of non-extensive statistics
in other astrophysical environments should be exploredas this may offer new insight into stellar nucleosynthesis.
The Tsallis statistics has already applied to the stellar
distribution and dynamics in the galaxies, and enjoyed asuccess in the description of various phenomena inducedby plasma fluctuations.

5.0
4.0

(NAOC)-5-5

D/H: (3.02±0.23) 10

3.0
2.0
1.0

Abundance s			

4He: 0.2561±0.0108

7Li/H: (1.58±0.31) 10-10q
Figure 1: Predicted primordial abundances as a function ofparameter q (in red solid lines). The observed primordial
abundances [10,11,5] with 1σ uncertainty for D, 4He,
and 7Li are indicated as hatched horizontal bands. The
vertical (blue) band constrains the range of the parameterq to 1.069 ≤ q ≤ 1.082.

References[1] Gamow, G.: 1946, Phys. Rev., 70, 572.
[2] Cyburt, R. H., et al.: 2003, Phys. Lett. B, 567, 227.
[3] Coc, A., et al.: 2004, ApJ, 600, 544.
[4] Asplund, M., et al.: 2006, ApJ, 644, 229.
[5] Sbordone, L., et al.: 2010, A&A, 522, A26.
[6] Fields, B. D.: 2011, Ann. Rev. Nucl. Part. Sci., 61, 47.
[7] Cyburt, R. H., et al.: 2016, Rev. Mod. Phys., 88, 015004.
[8] Hou, S. Q., et al.: 2017, ApJ, 834, 165.
[9] Tsallis, C.: 1988, J. Stat. Phys., 52, 479.
[10] Olive, K. A., et al.: 2012, MNRAS, 426, 1427.
[11] Aver, E., et al.: 2010, J. Cosmol. Astro-Particle Phys., 5, 003.

I Scientific Highlights

063

Detection of an Ionized Oxygen Emission Line
from a High Redshift Galaxy in the Reionization Era
INOUE, Akio K.1, TAMURA, Yoichi2, MATSUO, Hiroshi3/4, MAWATARI, Ken1, SHIMIZU, Ikkoh5
SHIBUYA, Takatoshi6, OTA, Kazuaki7/8, YOSHIDA, Naoki9/10, ZACKRISSON, Erik11
KASHIKAWA, Nobunari3/4, KOHNO, Kotaro2, UMEHATA, Hideki2/12, HATSUKADE, Bunyo3, IYE, Masanori3
MATSUDA, Yuichi3/4, OKAMOTO, Takashi13, YAMAGUCHI, Yuki2
1: Osaka Sangyo University, 2: Institute of Astronomy, University of Tokyo, 3: National Astronomical Observatory of Japan, 4: Graduate
University for Advanced Studies, 5: Osaka University, 6: Institute for Cosmic Ray Research, University of Tokyo, 7: Kavli Institute of
Cosmology, University of Cambridge, 8: Cavendish Laboratory, University of Cambridge, 9: Department of Physics, University of Tokyo, 10:
Kavli IPMU, University of Tokyo, 11: Uppsala University, 12: European Southern Observatory, 13: Hokkaido University

The Bing Bang radiation confirmed by cosmic
microwave background (CMB) is originated fromthermal emission of ionized gas. The ionized gas is thenneutralized by atoms/electrons recombination, and ouruniverse became transparent. However, it is known that
our intergalactic space, at redshift less than 6, is filledwith low density ionized gas again. Detailed observationsof CMB suggest that our universe was reionized atredshift around 10. Our observation of an ionized oxygen[OIII]88 μm line has identified a candidate of such galaxies
in the early universe [1], as shown in figures 1 and 2.
First stars in our universe are thought to be massive
and short lived, which distributed heavy elements into
interstellar space by supernovae. A cluster of suchmassive stars could be a strong source of UV radiationand ionized emission from the heavy elements. Our
ALMA observation of a high redshift galaxy (SXDFNB1006-2, z = 7.2) is one of such galaxies discoveredby Subaru telescope having strong Lyα emission in the
middle of reionization era.
Preceding to our ALMA observation, we estimatedthe emission strengths of far-infrared atomic finestructure lines from high redshift galaxies [2]. As aresult, the ionized oxygen [OIII]88 μm line could be thebrightest emission line under strong UV radiation andlow metallicity conditions. This is also consistent with[OIII]88 μm observations by AKARI infrared satellite
towards the Tarantula Nebula in the Large Magellanic
Cloud.
The most interesting discovery from the ALMA
observation of SXDF-NB1006-2 is that ionized carbon[CII]158 μm and dust emissions were not detected [1].
This indicates that the galaxy is deficient of neutral gas
but dominated by ionized gas. Then UV radiation frommassive stars are not absorbed by the interstellar medium
and penetrate into intergalactic space, and we estimatedthat the UV radiation from the galaxy could contributeto the cosmic reionization. Our observation not only
discovered the most distant oxygen, but also proposed a
new tool to study the early history of our universe. With
coming ALMA observations, we will be observing more
on far-infrared atomic fine structure lines from the most064

I Scientific Highlights

distant objects to identify the cosmic reionization andstructure formation in the early universe.

Figure 1: (left) 3-color image from observations: green for
ALMA [OIII]88 μm, purple for Subaru Lyα and red
for UKIRT UV radiation. (right) artist’s illustration of
SXDF-NB1006-2 showing that the UV emission froma massive star cluster is penetrating into intergalactic
space and ionizing the neutral gas around.

Figure 2: (upper) [OIII]88 μm emission spectrum observed by
ALMA. (lower) Lyα emission by Subaru telescope. Peakis shifted due to absorption by neutral gas.
References[1] Inoue, A. K., et al.: 2016, Science, 352, 1559.
[2] Inoue, A. K., et al.: 2014, ApJL, 780, L18.

Terahertz and Far-Infrared Windows Opened at Dome A in Antarctica
SHI, Sheng-Cai1, PAINE, Scott2, YAO, Qi-Jun1, LIN, Zhen-Hui1, LI, Xin-Xing1, DUAN, Wen-Ying1
MATSUO, Hiroshi3, ZHANG, Qizhou2, YANG, Ji1, ASHLEY, M. C. B.4, SHANG, Zhaohui5/7, HU, Zhong-Wen6
1: Purple Mountain Observatory, CAS, 2: Smithonian Astrophysical Observatory, 3: NAOJ, 4: The University of New South Wales, 5: Tianjin
Normal University, 6: Nanjing Institute of Astronomical Optics and Technology, 7: National Astronomical Observatories, CAS

Astronomers are seeking for higher and dryer sites on
earth for better observing condition especially in infrared
to terahertz frequency region, where absorption by water
vapor dominates atmospheric transmission. Here, weshow the measurement of atmospheric transmission
from Dome A, Antarctica, using Fourier transform
spectrometer in infrared to terahertz frequency region [1].
Because of the low temperature of antarctic plateau, as
low as −80 °C in winter time, atmospheric water vapor is
scarce and the Dome A can be the best observing site on
earth.

atmospheric transmittance is small in Dome A as well
as low wind speed, the site is suitable for long baseline
terahertz interferometers.
Our atmospheric measurements were used to makedetailed comparison to existing atmospheric modeland satellite data. We have found the existing model
underestimate continuum absorption by water vapor andnew constraints on the spectral absorption lead to better
understanding of upper troposphere in relation to ourclimate on the earth.

Figure 1: Picture of Fourier transform spectrometer for Dome A
atmospheric measurement.

Figure 1 shows the Fourier transform spectrometerused for the atmospheric measurements [2]. Roomtemperature thermal detectors are used and thespectrometer was calibrated according to two temperature
blackbody sources; one at room temperature in the
spectrometer and another at outside in cold. Figure 2
shows the measured atmospheric transmittance in thesite testing campaign at Dome A during 2010–2011. The
transmittance at the supra-terahertz windows reaches ashigh as 30 %, whereas the best transmittance in ALMA
site is as high as 20 % [3]. Furthermore, we observe
numerous atmospheric windows all through the terahertz
frequencies as shown in figure 1, including 10–20 %transmittance at 2 THz, 3 THz and 5–6 THz windows
where astronomical atomic fine structure lines could
be observed from ground. The 7 THz window shows
median transmittance of about 40 % in winter, which
would be important for observing thermal emission fromprotoplanetary disks and exoplanets. Since variation of

Figure 2: Zenith atmospheric transmittance spectra measured at
Dome A. Spectra are shown for the entire year (a,c) andfor winter (April-September) only (b,d).

References[1] Shi, S.-C., et al.: 2016, Nature Astronomy, 1, 1.
[2] Li, X.-X., et al.: 2009, Proc. SPIE, 7385, 73851D.
[3] Matsushita, S., et al.: 1999, PASJ, 51, 603.

I Scientific Highlights065

Development of Terahertz Photon Counting Detectors
MATSUO, Hiroshi, EZAWA, Hajime

		(NAOJ)			

For future terahertz astronomy, we are working on a
new interferometer technology based on the HanburyBrown and Twiss intensity interferometers. The intensity
interferometers can be used with direct detectors andtheir correlation is stable against phase fluctuation. For
application to space interferometers, direct detectors canoperate under background limited performance whichsurpass the sensitivity of heterodyne receivers. Figure 1
shows the requirements on detector noise equivalent
power (NEP) to achieve the background limited
performance as a function of detector time response [1].

Figure 1: Requirements on background limited detector NEP as afunction of the detector time response [1].

When the detector response is slower than a photon
arrival rate, the required NEP is a function of input
radiation power (right hand side in Figure 1). On theother hand, when the detector response is fast enough toresolve each photon arrival, the requirement on detector
NEP is reduced in proportion to square root of the time
resolution. For example at 1 THz, 1 ns time resolution
enables the usage of detectors with NEP less than
10−17 W/√H̄z. Under lower background conditions using
grating spectrometers, the requirement on NEP do notchange, and background limited performance is realized
relatively easily.
We are developing terahertz photon counting detectors
with high time resolution using superconducting tunnel
junction detectors, similar to SIS receivers for ALMA.
When niobium tunnel junctions are cooled below 0.8 K,
they can be used as high sensitivity photon detectors[2]. Our group in NAOJ collaborating with AIST isdeveloping low leakage tunnel junctions made of Nb/
Al-AlOx/Al/Nb, and achieved 7 pA leakage current for10 μm × 10 μm junctions. With smaller junction sizes, we
expect to achieve as low as 1 pA leakage current as well
as NEP less than 10−17 W/√H̄z.

066

I Scientific Highlights

UKIBE, Masahiro, FUJII, Go, SHIKI, Shigetomo(National Institute of Advanced Industrial Science and Technology)

We have made an experiment using Nobeyama
Radioheliograph to demonstrate the capability of theintensity interferometers [3]. Figure 2 shows the crosscorrelation of signals from two 17 GHz receivers; one inamplitude and another in intensity (amplitude squared)
correlations.

Figure 2: Amplitude and intensity (amplitude squared) crosscorrelation using Nobeyama Radioheliograph 17 GHz
receivers [3].

Although in intensity there are no phase information,
delay time can be measured by the intensity crosscorrelation, which can be used to define the complex
visibilities. The same principle can be used in terahertz
intensity interferometry, where fast photon counting
detector are used to measure the intensity crosscorrelation and realize wide bandwidth and highsensitivity interferometers.
Astronomical observation using photon counting
detectors can be a new tool to study photon statistics ofastronomical sources [1]. In case of thermal source, BoseEinstein statistics is expected which can be a precision
measure of the source temperature, whereas in maser andsynchrotron sources the photon statistics could tell us thephysical condition of the sources.

References[1] Matsuo, H., Ezawa, H.: 2016, J. Low Temp. Phys., 184, 718.
[2] Ezawa, H., et al.: 2016, J. Low Temp. Phys., 184, 244.
[3] Ezawa, H., et al.: 2015, Proc. ISSTT-2015, W2-2.

II Status Reports of Research Activities
1. Subaru Telescope
1. Subaru Telescope Staff
As of the end of FY 2016, the Subaru Telescope Project
staff consisted of 19 dedicated faculty members including fivestationed at Mitaka, four engineers, one specially appointed
senior specialist and three administrative staff members.
Additional staff members include three specially appointed
research staff, three specially appointed senior specialist, fiveresearch experts, and six administration associates, all of whomare stationed at Mitaka. Moreover, 14 research/teaching staff
members, 13 of whom are stationed at Mitaka and one of whomis stationed at Pasadena, and three engineers, two of whom arestationed at Mitaka and one of whom is stationed at Nobeyama
are appointed concurrently. The project also has 73 local staff
members dispatched from the Research Corporation of the
University of Hawaii (RCUH), including scientific assistants;
engineers in charge of software and observational instruments;
technicians for facilities, machinery, vehicles, and laboratories;
telescope/instrument operators; secretaries; librarians;
administrative staff; researchers employed through Grants-inAid for Scientific Research; and graduate students. These staff
members work together in operating the telescope, observational
instruments, and observational facilities; and in conducting
open-use observations, R&D, public outreach, and educational
activities.

2. Science Highlights
In FY 2016, Subaru Telescope produced many outstanding
scientific outcomes which were published in major international
journals. Below are some examples:(1) Using the Fiber Multi-Object Spectrograph (FMOS), a 3D
map of as many as 3000 galaxies was created at the redshift of
1.2–1.5. The estimated expansion of the Universe is consistent
with the general relativity proposed by Einstein. Using Hyper
Suprime-Cam (HSC), (a) an extremely rare, double source plane
gravitational lensing system, in which two distant galaxies are
simultaneously lensed by a foreground galaxy, was discovered,
which will help us understand the history of the Universe, and (b)it was found that star-forming galaxies in the distant Universe(about 5 billion years ago) show more similarity in spatial
distribution to mysterious invisible “dark matter” than those in
the nearby Universe (about 3 billion years ago).
(2) In HSC survey data, an extremely faint dwarf galaxy was
discovered at the distance of 280 thousands light-years away,
thanks to the very high sensitivity of the Subaru Telescope.
This discovery suggests the presence of a large number of yetundetected dwarf satellites in the halo of the Milky Way andprovides important insights into galaxy formation throughhierarchical assembly of dark matter.
(3) Observations of Saturn using COMICS revealed that the
optically faint Cassini Division and the C ring were sometimes
brighter than the other rings in the mid-infrared light. The data
give important insights into the nature of Saturn’s rings.

3. Open-use
We continued to solicit proposals for observation topics foreach semester: S16A (February 1 - July 31) and S16B (August 1- January 21). Proposals were collected by the Mitaka office andadopted or rejected by the Subaru Time Allocation Committee(under the Advisory Committee for Optical and Infrared
Astronomy) based on reviews by Japanese and internationalreferees. In S16A, 41 programs (86 nights) were accepted outof 184 submitted proposals, requesting 451.7 nights in total.
In S16B, 31 proposals (49 nights) were accepted out of 142
submitted proposals, requesting 409.8 nights in total. Service
observations were made for 10 nights. In S16A and S16B, 2
and 1 accepted open-use proposals were by foreign principal
investigators, excluding University of Hawai`i observing time.
The number of applicants in submitted proposals was 2063 forJapanese researchers (Japanese astronomers at any institute andnon-Japanese astronomers belonging to Japanese institutes)
and 794 for foreign researchers. The number of researchers in
accepted proposals was 651 for Japanese astronomers and 232
for foreign astronomers.
In S16A and S16B, the number of open-use visiting observers
was 308, of which 43 were foreign astronomers. 104 astronomers
observed remotely from Mitaka. Observing proposals were
solicited and collected, the procedures for Japanese researchers
to travel for observations, and travel expense reimbursement
were handled by the Mitaka Office. Subaru Telescope
made the observing schedule and provided support for theobservers’ lodging, transportation, and observations while
in Hawai`i. In S16A and S16B, 91.9 % of the open-use time(including University of Hawai`i time) was used for actual
astronomical observations, after excluding the weather factor
and scheduled maintenance downtime. About 1.7 %, 0.3 %,and 6.1 % of observing time was lost due to instrument trouble,
communication trouble, and telescope trouble, respectively.
In S16A and S16B, remote observations from Hilo wereconducted for 2 programs with 2 nights. However, remoteobservations from Mitaka, where observers in Mitaka canparticipate in observations remotely in addition to on-site
observers at the summit, were conducted for 22 programs with 68
nights. The service observations were conducted for 11.55 nights.
The number of time exchange nights between Subaru Telescope

II Status Reports of Research Activities067

and Keck was 5.5 in S16A and 8.5 in S16B. That between
Subaru Telescope and Gemini was 5 in S16A and 2 in S16B.

4. Telescope Maintenance and Performance
Improvement
Repair plans for the optical-side mirror hatch, which broke
down in February of last year (FY 2015) were considered. Someexperiments and preparation were carried out for the repair work
during 7 days in August. The mirror hatch repair is scheduled forJune and July of next year, requiring 14 days down-time in eachmonth (total 28 days).
Primary mirror recoating work which was planned for thisyear was postponed to autumn of next year (FY 2017) due to themirror hatch incident. During the next year it will be required to
repair the mirror hatch reliably and recoat the primary mirror.
The primary mirror recoating work is scheduled for a total of 73
days down-time, with some other maintenance work.
Other general functions and capabilities of the Subaru
Telescope are continuing to be maintained the same as theprevious year.
In this year, electrical boards for the Auto Guider and ShackHartmann CEU (Central Electric Unit) Board, DPA (Driverand Power Assembly unit) for the tip and tilt secondary mirror,
bogie rubber spring for dome AZ rotation, and slip-ring fordome electrical power were replaced. Maintenance work for the
primary mirror transporter and primary mirror washing facility
were done. TWS (Telescope Work Station) user interfaces andbarcode tape for dome AZ angle detection were updated. Longterm maintenance plan were drawn up. The Hitomi satellite(ASTRO-H) which had severe incidents unfortunately wasobserved at the request of ISAS. Function tests of the primary
mirror actuator prototype, welding repair work on the dome
bogie rail were also done in the year.
In addition, while promoting the improved performance andoperational efficiency of the Subaru Telescope, renovation to thetelescope control units, which were installed more than 10 years
ago, proceeded. The local control units that were renovatedor modified in this year were the balance control unit (BLCU)
and tertiary mirror control unit (TMCU). By finishing BLCU
and TMCU replacement work this year, all renovation of thetelescope control units which has been carried out sequentiallyover 10 years was completed. It is planned to start the second
round updating the aging TSC (Telescope System Computer)
server from next year.
The major causes of the telescope trouble this year were,aging, maintenance error (human error), and defective design.
Aging on UPS2 (Uninterruptible power supply #2), maintenanceerror during PIR unit (FMOS) installation, manufacturing failure
in FRCU (PF) (Filed Rotation Control Unit for Prime Focus)
local unit, POpt (Suprime-cam) Hexa-pod trouble (random
failure?), aging of the man-basket PLC (Programmable Logic
Controller), operational error in barcode value readings, agingof the TUE (Top Unit Exchanger) gripper 2 motor encoder,
shoddy workmanship on cabling of the tip-tilt secondary
mirror, shoddy workmanship in assembling work of dome AZ

068

II Status Reports of Research Activities

slip-ring, defective design in EL cable wrapper, aging of the
AZ cable wrapper, defective design on IR-side Main Shutter,and maintenance error for operating of the safety switch #15
occurred causing observations to be canceled.
Additionally, we developed a mechanism to remotely obtainstatus logs on the local machine. We would like to continue
to utilize the telescope status log and work on preventive
maintenance for the telescope and the enclosure.

5. Instrumentation
The eight open-use facility instruments of Subaru Telescope
have been operated stably in FY 2016. Those instruments are
Hyper Suprime-Cam (HSC), Subaru Prime Focus Camera(Suprime-Cam), Faint Object Camera And Spectrograph(FOCAS), High Dispersion Spectrograph (HDS), Infrared
Camera and Spectrograph (IRCS), Cooled Mid-infrared Camera
and Spectrograph (COMICS), Multi-Object Infrared Camera andSpectrograph (MOIRCS), and 188-elements Adaptive Optics
and Laser Guide Star system (AO188/LGS).
In these years, there have been discussions on how we will
maintain or cease operation of the facility instruments, except
for HSC. As reported in last year, FMOS was decommissioned
in April, 2016. Also, it was decided to decommission SuprimeCam after the observations in May, 2017. In addition, possible
decommissioning of FOCAS was discussed because assigningdark nights to FOCAS has been almost impossible and thesituation will get worse after the commissioning of PFS. The
discussions have been held within Subaru, in SAC, and in
the Subaru users’ meeting. It was basically agreed to stop theoperation of FOCAS in early 2019 (in the earliest case), or after
the commissioning of PFS (in the latest case).
The operation of HSC has been stable, similar to the last
fiscal year. In this fiscal year, HSC observations have been madefor approximately two weeks in almost in every month except
for May and October. Although these frequent observations
did not create problems in HSC operation, there were a few
problems with the filter exchange unit (FEU) around the end of
this fiscal year which led to cancellations of the observations.
Those troubles were all recovered on the next day and further
maintenance work was made after the observing runs to remove
the cause of the troubles. We are carefully monitoring theoperation of the FEU and will work on its stabilization. For
HSC, installation of the filter transmission measurement system,
installation of the new on-axis dome-flat system, and a test of
FEU reinstallation to exchange filters during an observing run
have been made in this fiscal year.
The ongoing upgrade projects for the other facility
instruments are the fiber MOS unit for HDS; the polarimetricfunction in thermal infrared for IRCS and in mid-infrared
for COMICS; the integral field units (IFU) for FOCAS and
MOIRCS; the Transponder-Based Aircraft Detector (TBAD) for
the LGS system; and an upgrade of the real-time control system
for AO188. In addition, upgrades of the aging control computersand devices of the first generation instruments are ongoing.
In FY 2016, four carry-in (PI-type) instruments HiCIAO

(high-contrast coronagraph imager), Kyoto-3DII (optical
integral field spectrograph), SCExAO (Subaru Coronagraphic
Extreme Adaptive Optics) and CHARIS (high-contrast integralfield spectrograph) have been offered to the Subaru open-use
program. Operation of Kyoto-3DII at the Subaru telescope
ended in S17A. Among the instrument modules of SCExAO,
VAMPIRES (visible interferometric imager with differential
polarimetry) was open for public use.
A new PI-type instrument, IRD (InfraRed Doppler instrument)
was under construction, aiming to have the first-light observationin June 2017. Two other PI-type instruments proposed by the
University of Tokyo team, SWIMS (Simultaneous-color Widefield Infrared Multi-object Spectrograph) and MIMIZUKU (midinfrared multi-field imager and spectrograph), which are to be
used on the 6.5 m University of Tokyo Atacama Observatory (TAO)
telescope, were approved but only for engineering observations.
The Prime-Focus Spectrograph (PFS) is an optical/nearinfrared multi-object spectrograph at the prime focus of the
Subaru Telescope, which will be the next facility instrument
following the successful implementation of Hyper SuprimeCam (HSC). PFS is being developed through international
collaboration including seven countries, led by Tokyo IMPU.
The PFS has about 2400 optical fibers distributed over the
1.3 degree field of view of the prime focus that feed the lightof the astronomical objects to four identical spectrographs
which will be placed in the telescope dome. The spectrographmodules simultaneously cover the wavelength range from 0.38
μm to 1.26 μm. The subcomponents of PFS were developingat each partner institute aiming towards engineering firstlight in 2018. Science operation is expected to begin in 2020.
Subaru Telescope is responsible for modifying the telescope andenclosure to accept PFS; the design work and reinforcement of
the spectrograph floor have been conducted. Efforts to develop
a database that combines HSC and PFS data, so that users canaccess both instruments’ data seamlessly, has started as a USJapan collaboration. Peking University (though the Chinese
consortium) and Max-Plank Institut für Extraterrestrishe Physik(MPE) officially joined PFS collaboration and NAOJ will handle
their funds for PFS development.
We are conducting a conceptual study of “ULTIMATE-Subaru”,
Subaru Telescope’s next large facility instrument following HSC
and PFS, which will be one of the flagship instruments at theSubaru Telescope in the 2020’s. We are studying the conceptof a wide-field near-infrared imager, multi-object spectrograph,and multi-object integral field unit (IFU) spectrograph, assisted
by a ground-layer adaptive optics (GLAO) system. The GLAO
will allow us to uniformly improve the image quality over awide field of view by correcting the turbulence at the groundlayer of the Earth’s atmosphere by using an adaptive secondary
mirror. In FY 2016, we had an ULTIMATE-Subaru science
workshop at NAOJ Mitaka Campus by inviting scientists fromJapan and potential partner countries. We are also working on
the conceptual study of the GLAO system and wide-field nearinfrared instruments in collaboration with Australia and Canada.
We have now an official (short-term) agreement with Australia
to collaborate in the GLAO feasibility studies.

6. Computers and Network
One of our goals of this year was the same as a goal of theprevious year - to stably operate the fourth generation systemof computers and network called STN4. Stable operation wasachieved without serious trouble or attacks/intrusions such as
illegal access.
The observation data archive was continued from theprevious year. The archive is operational without serious
problems. The data archive system in Mitaka also showed stableperformance.
We officially rolled out remote observations from Mitaka
using the Remote Observation Monitor System for limited
instruments in 2015. An increasing number of observers areusing the Remote Observation Monitor System in Mitaka.
During the observation semesters from February 2016 throughJanuary 2017, about 40 observation programs utilized the remoteobservation monitor system for about 100 nights. The Proposal
Management System (ProMS) also worked very well.
Computers for HSC data analysis (HSC On-site Data
Analysis System) were procured in fiscal years 2010 and 2011.
We added storage to the system in FY 2016.
We purchased a test system for the HSC On-site Data
Analysis System that comprises a filesystem that surpasses NFS
in access speed. We are currently configuring the test system
toward real-time data analysis during observations in the next
fiscal year.
The online visitor forms for those who visit Subaru
Telescope in Hilo for observation and for those who visit NAOJ
in Mitaka for remote observation monitoring are operating.
Since the current rental contract for our computer andnetwork infrastructure comes to an end in February 2018, we
spent a sizable amount of time for the procurement of computersand network systems for continuous service after March 2018.
We created the specification draft for a new rental contract fromMarch 2018 to February 2023 and requested information. We
always studied ways to keep the performance and functions aswell as to reduce cost and updated the specifications.

7. Education (Under-graduate and Graduate Courses)
The number of Subaru Telescope staff members in Hilo whowere concurrently appointed by SOKENDAI (graduate school)
was eleven. The number of SOKENDAI students who had
primary supervisors affiliated with Subaru Telescope (including
those concurrently belonging to Subaru Telescope) was 16,
which constituted half of the total 32 Sokendai students hosted
in NAOJ. Of which five had supervisors who belonged primarily
to Subaru Telescope.
In FY 2016, Subaru Telescope hosted four graduate students
for long stays, of which one was a SOKENDAI student. On topof that, intensive education activities were seen also in Mitaka
in cooperation with the Division of Optical and IR Astronomy.
The numbers of graduate course students in all of Japan who
obtained master’s degrees and PhD’s based on Subaru Telescope
data were 14 and 8, respectively, of which two and four

II Status Reports of Research Activities069

belonged to the Division of Optical and IR Astronomy.
We also regularly hosted a series of educational programs
at Subaru Telescope. In December 2016, we hosted a Subaru
Winter School at National Central University in Taoyuan,
Taiwan. There were 23 participants from Japan, Taiwan, China,
and South Korea (four were from Japanese institutes). They
learned the reduction and analysis of Subaru Telescope dataand heard a series of lectures. Moreover, we hosted two Subaru
Telescope observation training courses. One was for eightundergraduate students from all over Japan held in September
2016, and the other was for six new SOKENDAI students at
NAOJ held in January 2017. In the Hilo office, we had regular
Subaru Telescope seminars in English 2–3 times per month,where open-use observers, visitors, and Subaru Telescope staff
members presented their own new research. Also in the Subaru
Telescope Mitaka office, we had many official and informal
seminars, many of which were jointly organized with otherdivisions in NAOJ and/or neighboring universities.

8. Public Information and Outreach (PIO)The Public Information and Outreach (PIO) office istasked with addressing the accountability for what the Subaru
Telescope does and is keenly aware of the importance of citizens
understanding our work, for both the short-term and long-term
success of the project. The increased importance of positiveawareness in the local community has profound meaning for the
next generation telescope project on Maunakea. Therefore PIO
pays more attention to the interaction with the local community,
in its three major areas of tasks.
Task 1: Disseminating information about the results fromthe Subaru Telescope and the work at the Subaru Telescope. The
primary tools are the postings on our own website; providingpress releases to the Japanese, local, and international media;
and holding press conferences. During Fiscal Year 2016,
there were 19 web-postings (9 in Japanese, 10 in English)
about discoveries from the Subaru Telescope. Articles about
instrument development; the work and the activities at theSubaru Telescope; and other announcement totaled 76 (46 in
Japanese, 30 in English). Some postings are also distributed
through the media as well as posting services such as theAmerican Astronomical Society’s mailing exploder. Many
articles appeared in Japanese newspapers, and some in the local
newspapers; with more prevailing in the on-line postings.
In addition, newer tools such as Twitter, Facebook, andYouTube are becoming more useful in spreading awareness in atimely manner. The PIO office is making extra effort in providing
striking visuals for such social media postings. Filming requests
from outside totaled more than 23 from Japanese media(including 1 for an English language production), in addition to
the numerous inquiries/questions from the media, educational
institutions, and museums.
Task 2: Provide escorted tours for the public and specialgroups to see the facility. The public tour program thatstarted in 2004 continues to provide opportunities to see thetelescope up-close for guests from Japan and from around

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the world. Dedicated full-time staff leads tours and provided
timely communication to those requesting tours. It is possible
to register for the general tours program on-line. Except forsummer months when the tour program was suspended due tothe inclement weather related access issues on Maunakea, a totalof 456 people visited through this program. There were 127
additional groups who visited through special tour programs
and resulted in a total head count of 1048 people who visited
the summit facility. The tours are all escorted by the assigned
staff, in either Japanese or English language. The telescope tours
include 8 tours (2 per day on 4 days) specifically targeting theresidents of the State of Hawaii, in the hope of increasing thepositive awareness of what the telescope does.
Facility tours of the Hilo Base Facility are most of thetime accompanied by other activities described in the next
major task area, namely: special lectures, hands-on sessions, orpresentations by the student group. A total of 40 groups, with
398 people, visited the base facility this year.
Task 3: Public outreach includes lectures in the local
community, special presentations in the schools, and remotepresentations for Japanese schools or museums. PIO provided/
coordinated 75 lectures at the Hilo Base Facility or in its
vicinity such as at the ‘Imiloa Astronomy Center. There were 17
lectures outside of the island, and 11 remote lectures for off-site
locations. The local lectures included 37 classroom presentations
during the Journey through the Universe program over thecourse of a week.
In place of an open house, the staff of the Subaru Telescope
participated in the annual AstroDay event at the local shopping
mall. Observatories on Maunakea, ‘Imiloa Astronomy Center,
Maunakea Visitor Information Station, and other astronomyrelated groups participated in this event. More than 2000 people
visited this family-friendly event.
Another special local event where many astronomy
observatories participate is the annual Onizuka Science Day
at the University of Hawai`i at Hilo. Six hundred selectedstudents between grades 4 and 12 (upper elementary school tohigh school) with families and teachers from all over the islandgathered for this event. PIO provided 2 hands-on workshops andan exhibit booth.
Events like these where Subaru Telescope staff meet andinteract with students and members of the local community are
effective for improving the recognition of the Subaru Telescopes
activities. Of course material about these events is distributed
via the website and social media.
A special effort was made in the following two areas:
posting articles summarizing Subaru Telescope’s achievement,
and faculty development seminars. In the summary series, there
are 22 articles published on the Subaru Telescope’s website.
The seminar speakers included prominent leaders from the local
community, so that the staff of the Subaru Telescope has better
understandings of the cultural and historical aspects of the place
where they work.

2. Okayama Astrophysical Observatory
Okayama Astrophysical Observatory, (hereafter theObservatory) serves as the observing and research base of
the optical and infrared astronomy in Japan, and it promotes
open use, primarily of the 188-cm telescope, to universities
throughout the country. It also pursues joint R&D projects with
universities, contributing toward forming stronger foundations
for astronomy research at the universities. Concurrently,
the Observatory pursues its own research activities, taking
advantage of its location and observational environment.
Every year, about 240 nights at the 188-cm telescope are
exploited for observations by researchers from across thecountry through the open use. The Observatory maintains andoperates the observing instruments and provides the observers
with support for observations, travel expenses, accommodations,
everyday needs, etc. It also engages in improving the open-use
observing instruments, developing new open-use instruments,and supporting carry-in instruments from other institutions.
Several joint projects with universities have been conducted,
including Kyoto University’s Okayama 3.8-m New Technology
Optical and Infrared Telescope Project, the Tokyo Institute ofTechnology’s Gamma-Ray Burst Optical Afterglow Followup Project, and “The Optical & Near-Infrared Astronomy InterUniversity Cooperation Program” supported by MEXT.
The Observatory’s unique research activities include a
project designed to convert the 91-cm telescope into an ultrawide-field near-infrared camera (OAO-WFC) in order toengage in a comprehensive survey of infrared-variable objects
in the Galactic plane. A new project has just begun this FY tomake the 188-cm telescope robotic and to improve the stability
and sensitivity of the high dispersion spectrograph through a
Grant-in-Aid for Scientific Research (Basic Research (A), FY
2016–2020). This project aims at establishing a large sample ofexoplanets by Doppler technique. Collaborations with foreign
researchers are also continued actively.
The personnel breakdown as of March 2017 was five fulltime staff members without term limits, including two associate
professors, one assistant professor, one engineer, and one
Chief of the Administration Office; eleven contract employees,
including one specially appointed associate professor, two
research experts, one specially appointed research staff member,
one specially appointed senior specialist, one research supporter,
three administrative supporters, and two administrative
maintenance staff members; and one temporary staff member.

1. Open Use(1) Overview
The numbers of nights allotted to open use in 2016 were
118 for the first semester (2016A, January to June) and 108.5
for the second semester (2016B, July to December). Observing
proposals submitted in response to the calls for proposals werereviewed by the Okayama program subcommittee and 1 project
observation program, 0 academic degree support program, 15

general observation proposals, and 2 miscellaneous observation
proposals were accepted for 2016A, and 1, 0, 13, and 2 were
accepted for 2016B. One and one observing proposals wereapproved for the category “Target of Opportunity (ToO)”
observations introduced since 2016A for 2016A and 2016B,
respectively. Three proposals, one from each of China, Hawai`i,
and Turkey, were accepted in 2016A, and one from Hawai`i
was accepted in 2016B. The Observatory supported theirobservations with human resources. Open-use observation
generally proceeded without incident.
(2) Observation/Research Results
The majority of objects observed through the open use in2016 were stellar sources and exoplanets. Others included Solar
System objects, the Milky Way Galaxy, galaxies outside theMilky Way, and quasi-stellar objects. The following primaryobservation themes were noted: exoplanet search and binarymass determination via precise radial velocity measurements;
exploration of the physical properties and activities of single
and binary stars via high-dispersion spectroscopy; and theobservation of exoplanet transits by precise differential
photometry. Optical low-dispersion spectroscopic observationsof stars for classification remained significant. As in previous
years, a number of observational studies were conducted byindividual groups of researchers within the open-use framework,and their respective research results were reported in meetingsand conferences or were published in peer-reviewed journals.
(3) Facility and Instrument Maintenance/Management
The 188-cm telescope and its dome had evolved into astable and high-functioning observing system by FY 2014 after
the major refurbishment in FY 2012. Efforts were made toautomate the high dispersion spectroscopic observations withthe fiber-feeding system in this FY 2016. The remote observing
environment provided to the open use with some limitations lastyear has been available for open use with no conditions since
2016A. During the maintenance period in June, the annual realuminization of the primary mirror of the 188-cm telescope andlubrication of the telescope and dome were completed. Efforts
were continued to simplify the re-aluminization process as weredone in the last year. The 1.5-m primary of KANATA Telescopeat Hiroshima University was also accepted for re-aluminizationin the maintenance period. Participants in the aluminization
work from that organization were given NAOJ-mandated safety
and hygiene training as necessary. Utmost efforts were madeto maintain high observing efficiency by conducting monthly
cleanings of the primary, secondary, and tertiary mirrors of the
188-cm telescope after September.
The dome was checked daily. The replacement of the wirerope for driving the slit door, scheduled once every 4 years,
was done successfully in November. The front sheaves for thewire were replaced just before that. Other maintenance work
was also performed, including repair of the worn-down guiding

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071

rails for the slit doors, maintenance of the dome rotation driver,and replacement of the old power lines, in order to achievesmooth open-use operation and prolonged life-time of the
facility and equipment. Safe storage of the acquired observing
data and appropriate maintenance of the computer and network
environment were carried out.
Work safety was given priority in accomplishing the
aforementioned maintenance work and observing instrument
exchanges.
(4) Conferences
The program subcommittee for the 188-cm telescope met
on May 30 and November 18 in 2016 and March 23 in 2017
to evaluate proposals for the open use of 2016B, 2017A (firstsemester of 2017) and 2017B (second semester of 2017),
respectively, and formulated an observation program for eachsemester.
The third one was held ahead of the usual schedule,
conventionally at the end of May in the next FY year, in orderto devote the activity of the Okayama program subcommittee
during FY 2017 to the Kyoto University 3.8-m telescope project.
The Okayama Users Meeting, also known as the 27th Opticaland Infrared Users Meeting, was held in the Large Seminar
Room of NAOJ Mitaka Campus on September 7 and 8. Various
reports were made: current status of the Observatory including
the telescope and dome, execution summary of the programsubcommittee, status of the open-use observing instruments
and remote observing environment, development status of thequeue observing system for the HIDES Fiber-Feeding mode, etc.
Reports on the status of and scientific results from the two newuser-led instruments for the 188-cm telescope were also made.
Reports were made on the progress of the Kyoto University 3.8m telescope project including observing instruments. Reports
were done on the research results from the open use of the 188cm telescope and on the operations of other optical and infraredobservational facilities such as the Hiroshima AstrophysicalScience Center.
A special session was arranged to discuss in more detailthan last year the practical policy and plan for the transfer of the
open-use observations from the 188-cm telescope to the Kyoto
3.8-m Telescope comprehensively. Detailed discussions were
held among interested domestic researchers including Okayama
open-use users, Kyoto University staff, NAOJ staff, and others.
The policy agreed upon at the Users Meeting was reported
later at the general meeting of the Group of Optical and Infrared
Astronomers (GOPIRA), the GOPIRA symposium and theAdvisory Committee for Optical and Infrared Astronomy at
NAOJ. Last of all, the policy that includes the following items
was reported at the Advisory Committee for Research andManagement at NAOJ on October 31, 2016. These reports
included that the operation of the open use of the 188-cm
telescope will be terminated by semester 2017B, that the openuse of the 3.8-m telescope will open in August 2018, that
the Okayama program subcommittee is given the role of thescientific committee for the operation of the open use at the 3.8m telescope, and that NAOJ continues to hold the 188-cm and072

II Status Reports of Research Activities

smaller existing telescopes and facilities for the time being, etc.
The Director General of NAOJ requested the Advisory
Committee for Optical and Infrared Astronomy make “Plans
for the transfer to and operation of the open use of the
Kyoto University 3.8-m telescope.” The Okayama programsubcommittee made the report draft upon a request from theAdvisory Committee and submitted it to the committee at theend of March 2017.

2. Developing and Maintaining Open-Use
Observing Instruments(1) HIDES (High-Dispersion Echelle Spectrograph)
The instrument HIDES is a cross-dispersed high-dispersion
echelle spectrograph, provided for open use. Development of
the fiber-link system (HIDES-F) since FY 2006 has continued
to improve its observing capabilities. Open use of the highefficiency (HE) fiber link with approximately 50-K wavelength
resolution has continued since 2011A. The HE link offers an
improvement in throughput of nearly one magnitude over theprevious value and radial velocity measurement precision of
approximately 2 m/s, which is comparable to the case of the
Coudé light path. The high-resolution (HR) link with nearly 120K wavelength resolution has been offered as a PI-type open-use
instrument since 2016A. The HR link provides a 4 times better
sensitivity at maximum than the case of the Coudé light path.
Control software was adjusted to deal with queue and automatedobservations. An astro-comb developed by researchers at
the National Institute of Advanced Industrial Science andTechnology (AIST) and their collaborators as a next generation
astronomical wavelength standard was installed into the Coudéroom of the 188-cm telescope, and the tuning and tests werecarried out. This year the total numbers of accepted proposals
to HIDES were 8 and 6 in 2016A and 2016B, including 1 and 1
project observations, respectively.
(2) ISLE (Near-Infrared Imager/Spectrograph)
ISLE is a near-infrared imager and low- or mid-dispersion
spectrograph. It has been available for open use with noconditions since 2011B. It is the only open-use instrument inEast Asia that offers near-infrared spectroscopic capability andis characterized as having the world’s best low-noise readout
capability (less than 10 electrons). Relative photometry at
the one milli-magnitude level is regularly achievable with its
imaging mode for bright sources. A carry-in YJH-band filter
from a user and the HK-band filter as standard equipment enable
it to obtain a well-connected spectrum from Y-band to K-band.
The numbers of open-use programs using ISLE conducted insemesters 2016A and 2016B were 5 and 6, respectively; which
included 1 and 1 miscellaneous category programs, respectively.
Nine of them were spectroscopy and the other two were imaging
photometry.
(3) KOOLS (Kyoto-Okayama Optical Low-dispersion
Spectrograph)
This instrument provides imaging and spectroscopic

capability in the optical. It has been available for open use as a
PI-type instrument since 2008A. It is equipped with an offsetguider and CCD charge shuffling functionality. Non-sidereal
motion objects can be tracked for long integration times. The
integral field unit using a fiber-bundle developed by a team at
Kyoto University has been made available as a PI-type openuse instrument since 2015B. When it is used, its input part isinstalled into the Cassegrain unit of the HIDES fiber link and its
output part is installed into KOOLS (KOOLS-IFU). Accepted
proposals were 4 and 1 for 2016A and 2016B including 1 and 1
ToO programs, respectively. The open use of KOOLS ended in
2016B. After that KOOLS was overhauled by the Observatory
together with researchers at Kyoto University to be a first-light
instrument for the 3.8-m telescope.
(4) Others
MuSCAT (MUlti-color Simultaneous Camera for studying
Atmospheres of Transiting exoplanets), which was previously acarry-in observing instrument, was made available to the open
use as a PI-type instrument from 2016B. It can achieve 0.05%
accuracy in relative photometry for a star of 10-th magnitude at
V-band when it performs a series of one-minute exposures. Four
programs, which included one miscellaneous category program,
were conducted with MuSCAT in 2016A and four open-use
observing programs, which included one miscellaneous one,were accepted in 2016B.

3. Joint Research with Universities(1) Kyoto University’s Okayama 3.8-m New Technology Opticaland Infrared Telescope Project
The Observatory has participated in a cooperative
implementation framework for the 3.8-m telescope project,which is spearheaded by Kyoto University, together with
Astro-Aerospace, Inc., regarding the 3.8-m telescope projectas part of the future plan of the Observatory. Discussions
were held on technological issues regarding the telescope andobserving instruments through weekly TV conferences and inperson meetings held every three months. Kyoto University
has completed the construction of the dome that houses thetelescope. The Observatory hired a specially appointed associate
professor to be in charge of transferring the open use from the
188-cm telescope to the 3.8-m telescope and strengthened thecooperative implementation framework. The Observatory also
hired a Specially Appointed Research Staff Member to prepare
open-use observing instruments and advance the conversion andrefinement of the KOOLS-IFU system, for which open use at the
188-cm telescope has been terminated, to be an initial open-use
observing instrument for the 3.8-m telescope. Kyoto University
and the Observatory jointly collected input about the observing
instruments planned for the 3.8-m telescope from the domestic
astronomical community in order to fix the specifications of theequipment around the focal planes where observing instruments
will be attached. A research program has been approved in which
one observatory staff member participates as a co-investigatoron the grant-in-aid for scientific research from the Japan Society

for the Promotion of Sciences (Basic Research A (General), FY
2016-2019) applied for by researchers at Kyoto University. The
grant allows us to develop a near-infrared fiber-fed spectrographfor the telescope.
(2) The Optical & Near-Infrared Astronomy Inter-University
Cooperation Program
The Program has entered its sixth (and final) year since
its commencement in 2011. The Observatory has contributed
the 188-cm, 91-cm, and 50-cm telescopes to the Program, andhas taken a leading role along with the Office of International
Relations. Through the cooperative observational and educational
network, OISTER, established by the Program, the Observatory
performed observations for one campaign as a PI and provided
a total of 22 nights worth of observational data on three objects
this year. As for the immediate follow-ups of gamma-ray bursts,
which are the main targets of the program, there were 12 alertsthat were observable from the Observatory, observations were
performed four times and afterglow was detected in one of them.
Three peer-reviewed papers were published utilizing OISTER.
Another 18 peer-reviewed papers that have something to dowith the Program were published. The seventh workshop on the
Program was held.
(3) Gamma Ray Burst (GRB) Optical Follow-up Project
Optical follow-up observations of GRBs using the 50cm telescope are in progress in cooperation with the Tokyo
Institute of Technology’s Kawai Laboratory. During FY 2016,
the automatic observation scheduler performed observations
on nearly every possible night; 24 GRBs were observed, with
optical afterglows successfully detected in two. Observation
results were published as 9 GRB Coordinates Network (GCN)
circulars. In addition, follow-up observations of candidate
gravitational wave sources and monitoring of 9 objects that
include dwarf novae, eclipsing binaries, asteroids, and comets
were concurrently performed, which resulted in publication offour peer-reviewed papers.
(4) Other
The Observatory welcomed four third-year undergraduate
students and their supervisor from the University of Tokyo
between August 30 and 31 and provided them with anopportunity to conduct high-dispersion spectroscopic
observations using the 188-cm telescope during the early halfnight on August 30. Test observations were conducted with
the near-infrared observing system with the 30-mm aperture
dedicated to bright star photometry (IR-TMT) having beenplaced at the Observatory during the last FY in collaboration
with researchers at Tohoku University. The observations werecarried out from the main building of the Observatory or fromTohoku University remotely by way of the internet.

4. Unique Research Projects(1) Detection of afterglow from distant GRBs and survey ofvariable stars in the Galactic plane using the ultra-wide-field

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infrared camera.
With the 91-cm reflector having been converted into an
infrared camera with an ultra-wide field of view, observations
were conducted to identify infrared counterparts for objects suchas GRBs and gravitational wave sources. Along with them, acomprehensive survey of infrared variable stars in the Galactic
plane was carried out. In FY 2016 monitoring in the Ks-band of
two regions of 20 square-degrees each centered at L=30 degrees
and 80 degrees were nearly completed. In addition, automatic
monitoring of other objects, such as the Orion star forming
region and bright blazars were carried out.
(2) Development of a far larger scale exoplanet search
Through a Grant-in-Aid for Scientific Research (Basic
Research (A), “Large scale exoplanet search with a robotic
telescope for high dispersion spectroscopy,” representative:
Hideyuki Izumiura, FY 2016–2020), a project has begun aiming
at establishing an original large scale sample of exoplanets. For
that purpose, activities have begun to develop robotic operationof spectroscopic observations with the 188-cm telescope and to
improve the sensitivity and stability of the spectrograph.
(3) East Asian Planet Search Network
The Observatory also conducts studies focusing on the
search for exoplanetary systems, involving researchers fromSouth Korea, China, Turkey, and Russia. Efforts continued in FY
2016 to secure telescope time on the Korean 1.8-m telescope,
Chinese 2.16-m telescope, Turkish 1.5-m telescope, and theObservatory’s own 188-cm telescope for continued searches for
exoplanetary systems around G-type giant stars.

5. PR/Awareness Promotion Activities
In this FY about 40 astronomy-related questions from thepublic were posed irregularly to the Observatory and wereanswered appropriately. The 4D2U screenings, co-hosted with
the Okayama Astronomical Museum, attracted 3,847 visitors.
Fifteen Observatory tours were conducted, including thosefor pupils from local elementary schools in Asakuchi City andYakage Town. The Observatory also responded to four lecture
requests made by local boards of education and community
centers. The Observatory posted four research result web
releases and 1 press release.
The yearly special open-day was suspended again following
the last FY because a serious shortage of parking space wasanticipated due to the construction of the Kyoto University 3.8m Telescope and there was some concern about being able toensure the safety of the guests.

6. Contract Staff Transfers
The following transfers of contract staff members took place
in FY 2016:
Eiji Kambe resigned as a research expert on June 30. Eiji
Kambe joined as a specially appointed associate professor on
July 1. Akihiko Fukui resigned as Specially Appointed Research074

II Status Reports of Research Activities

Staff due to the expiration of his contract on September 30.
Akihiko Fukui jointed as a Specially Appointed Senior Specialist
on October 1. Kazuya Matsubayashi joined as Specially
Appointed Research Staff on November 1.

3. Nobeyama Radio Observatory
1. Nobeyama 45-m Radio Telescope(1) Open Use Observations
The 35th open use observations period started on December
1, 2016 as scheduled. The full capabilities of the new four-pixel
receiver FOREST and limited capabilities of the Z45 receiver
are offered.
The statistics of the proposals are as follows, “General
Proposals”: 23 accepted including 5 from abroad (29 submitted),“Joint Proposals” with ASTE telescope: 4 accepted with 1
from abroad (6 submitted), “Short Programs”: 12 acceptedwith 1 from abroad (29 submitted), “Backup Programs”, which
are carried out when weather is not acceptable for the main
observations: 1 accepted (1 submitted), “DDT Programs”, which
are submitted after the deadline: 2 accepted (3 submitted).
In addition, the 45-m telescope joined the VERA open use
observations for 2 proposals. There were no applications for“Large Programs.” The S40 receiver was decommissioned.
Open use observations have been halted since March 17,
2017, when the master collimator driving system went out oforder. Most of the observations scheduled after this issue arose
will be carried over to the next observing season.
(2) Improvements and Developments
Maintenance of the 45-m telescope, the receiver systems, thecryogenics, etc. were performed.
- The replacement of the millimeter calibrator driving system
was completed. The design work for the mirror exchangesystems was done.
- The Spectral Window mode with the FOREST receiver was
implemented, and flexible setting of the spectrometer was
realized.
- Development of the new data archive system and the data
reduction procedure with the CASA pipeline started. These
will lead to automation of the observing system in the future.
- Preventive and corrective painting of the antenna mountstructure was done.
- NRO supported user instruments including the digitalspectrometer ROACH, a 90 GHz continuum camera, and thesimultaneous 22/43/86 GHz VLBI observation system.
(3) Scientific Results
We are carrying out the (a) Star Formation Legacy Project,(b) Galactic Plane Survey, and (c) Nearby Galaxy Project aslegacy projects with the 45-m telescope, and their results aredescribed below. Research results from open-use observations
are given separately in the Scientific Highlights section of thisdocument.
(a) Star Formation Legacy ProjectIn the Star Formation Legacy Project, we conducted largescale mapping observations toward three nearby star-forming
regions, Orion A, Aquila Rift, and M17 in 12CO(1–0), 13CO

(1–0), C 18O(1–0), and N 2H +(1–0). Many cores and clumps
have been identified from structure analysis of these data. In
particular, thanks to the high sensitivity a protostellar molecular
outflow was found in the Orion molecular cloud data that was
not in the data from BEARS.
(b) Galactic Plane Survey Project (FUGIN: FOREST Unbiased
Galactic plane Imaging survey with the Nobeyama 45-m
telescope)
We are conducting a simultaneous survey of the 12CO(1–0),
13CO(1–0), and C18O(1–0) emission lines in the Galactic Plane
using FOREST aboard the 45-m telescope. We plan to makemaps of the inner Galaxy and the outer Galaxy including thespiral arms and bar structure. In 2016, we covered areas with 22
and 2 square degree for a total of 24 square degree. Now, 130
square degrees have been mapped. As a result, we have revealed
a wide range of molecular clouds and their fine structures; wealso found the most distant molecular cloud, new cloud-cloud
collision systems, and an interacting region with a supernova.
(c) Nearby Galaxy Project (COMING: CO Multiline Imaging of
Nearby Galaxies)
We started COMING (CO Multiline Imaging of Nearby
Galaxies) in April 2015 to map more than 200 nearby galaxies
in 12CO(1–0), 13CO(1–0), and C18O(1–0) emission lines using
FOREST. Up to now, mapping observations of 129 galaxies
have been completed (54 % of the original plan). A paper on
the relation between molecular gas density and star formation
efficiency was published (Muraoka et al. 2016, PASJ, 68, 89)
and one on a dwarf spiral galaxy, NGC 2976, is in press. In
addition, two master theses and five undergraduate theses were
published. We also developed a data reduction pipe-line system.

2. Radio Polarimeters- Operations and maintenance were performed.
- On a monthly basis, the data are examined by solar researchgroups in Kyoto University, Ibaraki University, NICT, and
NAOJ Solar Observatory, and are archived as public data in
the NAOJ Astronomy Data Center so that researchers all over
the world can access them.
- The polar axis gears of the 1, 2, 9.4, and 17 GHz antennas were
replaced, and their pointing accuracies were improved.

3. Research Support(1) SPART (10-m telescope) (Osaka prefecture Univ.)
To better understand the influence of the activities of hoststars on the atmospheric environment of habitable planets, wehave been carrying out monitoring observations at 100 and
200 GHz bands with a 10-m telescope, the Solar Planetary
Atmosphere Research Telescope (SPART). This year we
continued the observations with SPART. To investigate short-

II Status Reports of Research Activities

075

term changes of the CO abundance in the Venusian middle
atmosphere revealed by SPART, we started simultaneous andsynergetic observations with the Atacama Large Millimeter/
Submillimeter Array, Japanese Venus Climate Orbiter
AKATSUKI (JAXA/ISAS), and the 1.6-m Pirka Telescope
employing the Near Infrared Echelle Spectrograph (Nayoro
Observatory, Faculty of science, Hokkaido University). Throughthis approach we address the links between the photochemical
reaction networks and the circulation of materials induced by the
dynamics between the Venusian upper and lower atmosphere. In
addition, the purpose-built console and display room of SPART
was completed. This room is opened to the public where visitors
can study the terrestrial planets of the Solar System, the aim of
SPART, and the history of the Nobeyama Millimeter Array.
(2) Radio Heliograph (Nagoya Univ.)
In FY 2015, an international consortium (ICCON) assumed
operation of the Nobeyama Radioheliograph (NoRH, see https://hinode.isee.nagoya-u.ac.jp/ICCON/). The remote operating
system via the internet has functioned very well. About 30
researchers from seven countries (China, Germany, Japan, South
Korea, Russia, the UK, and the USA) participated in operation,
including the system health check and data verification.
Observational data are automatically transferred to NAOJ and/or Nagoya Univ. and are stored, maintained, and made public
there. In September 2016, an international workshop, ‘Physics
with Radio Observations - Continued Operation of Nobeyama
Radioheliograph - ’, was held and 36 researchers (including 20
from overseas) attended it. In addition to science results from
NoRH, we discussed research topics during this continued
operation by ICCON, and how to collaborate with a new solar
radio telescope in China.

4. Public Outreach(1) PR activities at Nobeyama Campus
Nobeyama Campus received a cumulative total of 46,636
visitors throughout the year, including participants in special
open house events. Staff members conducted 40 guided tours,
including ones for Super Science High School (SSH) students
and the Campus Tour Week, while 4 requests for lectures and 20
requests for on-site filming and interviews were granted. These
requests, especially those by some local broadcast stations in
Nagano prefecture but also from national broadcasting media
such as NHK, increased due to efforts to strengthen cooperation
with local communities. The Campus Tour Week for educational
institutions was scheduled during the summer. Eight groups
took advantage of this opportunity, and many students in thegroups enjoyed the visit. For the workplace visits, 4 students
from 3 schools, primarily local junior-high schools, visited theobservatory. For the SSH initiative, three schools visited NRO
and participated in lectures.
In the area for permanent public access, an antenna
experience facility and some introduction movies are available
along with posters and panel displays. In this year, we tentatively
opened the Nobeyama NINS exhibition room. Also, in order to076

II Status Reports of Research Activities

familiarize the public with NRO, we renovated the website toaccommodate smartphones as well as personal computers.
A photography event for the Nobeyama starry sky was
carried out at NRO because many requests to take picturesin Nobeyama Campus at night have been received. We held
the event during the period when it does not affect radio
observations, with 31 participants who were selected fromabout 100 applicants. We used some pictures taken at the event,which were offered by the participants, for an original calendar,
displays during the Special Open House, and so on.
(2) Cooperation with Local Communities
The annual Nobeyama Special Open House was held with
contributions by Nagano Prefecture as well as Minamimaki
Village, the Minamimaki Chamber of Commerce, and its
youth division. Moreover, Jimoto Kansha Day (Thanks Day
for the Locals) was held as the Special Open House for locals(Minamimaki and Kawakami Village) at the Vegetaball Withby Shinshu University as the main host. Special sponsorshipwas made to the sora-girl event “Tebura de Hoshizora Kanshokai (Drop-by Star Gazing Event),” hosted by the Minamimaki
Tourism Association. Also, a training course and examinations
were carried out through a special partnership with ShinshuSaku Hoshizora Annai-nin, which was managed by Saku Koiki
Rengo (the union of local governments in the Saku area).
Moreover, the conference of “Nagano-ken ha Uchuu-ken(Nagano prefecture is Astro-Prefecture)” was founded with
Kiso Observatory, IoA, The Universoty of Tokyo, etc. The firstmeeting was held at Matsumoto Campus of Shinshu University
on November 23 with about 100 participants. The webpage andmailing list were set up and some activities started.
(3) The Nobeyama NINS exhibition room
After the improvement work of the building of the
Nobeyama Millimeter Array and installation of the 4D2U theaterin last year, the Nobeyama NINS exhibition room was tentatively
operated in the summer season from July to September. Fromquestionnaire results, about 8,000 guests visited the room andtheir degree of recognition of other institutes as well as NAOJ
was improved.
(4) NRO Conference Workshops- July 20-21, 2016
NRO-ALMA Joint Science/Development Workshop 2016
(representatives: Masao Saito (NRO), Daisuke Iono (Chile
Observatory))- October 20-22, 2016
ALMA/45m/ASTE Users Meeting 2016 (representatives:
Eiji Akiyama, Daisuke Iono, Ken’ichi Tatematsu (Chile
Observatory), Masao Saito (NRO))- March 28-29, 2017
NRO Galactic Plane Survey Workshop 2016 (representative:
Tetsuhiro Minamidani)5. Education
NRO accepted three postgraduate students. The one is asecond-year Ph.D. student in SOKENDAI studying carbon chain
molecule chemical reactions. The others are visiting students
from Kagoshima University and the University of Tsukuba, andthey received Ph.D. degrees from their respective universities
based on the studies using the Nobeyama 45-m Radio Telescope.
SOKENDAI held the workshop on Radio Astronomical
Observation using the Nobeyama 45-m Radio Telescope form
June 6 to 10, with 12 undergraduate students in attendance. One
third of the participants were 4th year students, just about todecide their course after graduation. While guiding the students,from observations to presentation of the results requires
significant effort, the event offers an invaluable opportunity
for undergraduates to experience observations using a radio
telescope and think of their future career.

6. Misc. Activities(1) Hiring
Kazufumi Torii: Specially Appointed Assistant Professor(2) Resignation, Transfer
Masao Saito: Associate Professor to TMT-J Project
Hitoshi Arai: Research Supporter
Yoshio Tatamitani: Research Expert

II Status Reports of Research Activities077

4. Mizusawa VLBI Observatory
NAOJ Mizusawa VLBI Observatory operates VLBI (VeryLong Baseline Interferometry) facilities such as VERA (VLBI
Exploration of Radio Astrometry) and KaVA (KVN and VERA
Array), and provides these unique facilities to the internationaluser community to support the research activities at universities
and research institutes. In the meantime, astronomical researchusing these VLBI arrays is conducted mainly on the Galactic
structure, celestial masers, AGNs, and so on. Using the uniquedual-beam system which is capable of phase referencing byobserving two sources simultaneously, VERA conducts highaccuracy astrometry of maser sources and determines thedetailed structure of the Milky Way. In addition to the operationof VERA, maintenance and operation support were provided
to the Yamaguchi 32-m Radio Telescope and two Ibaraki 32-m
radio telescopes in collaboration with the local universities.
International collaboration has been promoted particularly in the
East Asia region through the joint operation of KaVA and theEast Asian VLBI Network, the latter of which is a joint VLBI
array between the People’s Republic of China, Japan, and theRepublic of Korea.
In addition to VLBI related activities, “The Central
Standard Time” is kept at the observatory as an obligation of
NAOJ, Esashi Earth Tides Station is operated for geophysicalresearch, and Ishigakijima Astronomical Observatory is jointly
operated with the local city for public outreach and astronomical
research.

1. VERA(1) Observations and Common Use Observations
The four stations of VERA were operated by remote control
from AOC (Array Operation Center) at NAOJ Mizusawa
Campus. In FY 2016, a total of 536 VLBI observations (4410
hours) were conducted with VERA, such as common use
observations, VERA project observations, fringe detection
observations for maser and reference sources, geodesy
observations, JVN (Japanese VLBI Network) observations,
KaVA (KVN and VERA Array) observations, and others. These
VLBI data, except for KaVA, were processed at the Mizusawa
correlation center in NAOJ Mizusawa Campus. The correlated
data were sent to each researcher for the case of common-use
and JVN observations and to persons in charge of data analyses
in the case of project data and geodesy data.
VERA common-use calls-for-proposals with the 43, 22, and
6.7 GHz bands for semesters 2016B and 2017A were releasedin May and October, respectively. A total of 9 proposals, which
requested a total time of 224 hours, were submitted, including 4
proposals for 82 hours from overseas. Based on the evaluations
by referees elected from scientists in related fields, the VLBI
program committee decided to accept a total of 5 proposals (138hours) in 2016B and 2017A.

078

II Status Reports of Research Activities(2) Science Research
In FY 2016, Mizusawa VLBI Observatory published a totalof 40 refereed journal papers for scientific achievements. Amongthem, four papers were published by the Observatory staff as
PIs. Nine papers were scientific results directly related to VERA
astrometry observations, one was the results from KaVA, andtwo were from the Japanese VLBI Network (JVN). In addition,
various scientific results from other VLBI arrays, ALMA,
and multi-wavelength time-domain studies on active galactic
nuclei (AGN) were published, which were developed based on
previous VERA sciences. It should be noted that there were 31
papers published through international collaboration.
For the VERA project results, a new research method for
distance measurements was reported. It utilized the accurate
proper motion and radial velocity measurements for the H2O
masers associated with a high-mass star-forming region
G7.47+0.06. The high accuracy (10 % error) distance, 20 ± 2 kpc,
was successfully determined demonstrating that the method canbe applied to sources farther than 10 kpc whose annual parallax
is barely measurable with VLBI. For star-formation studies, a
research group lead by Kagoshima University detected the jetdriven bow-shock structure in the outflow associated with thehigh-mass young stellar object S255. In the research field oflate-type stars, the first simultaneous VLBI observations of SiO
masers in four frequency bands were reported using the newly
developed wide-band VLBI backend system developed by the
Mizusawa VLBI Observatory. It is expected that the system will
be employed for combined VLBI observations with the NRO
45-m Telescope and KVN. There was a paper that reported thefirst KaVA imaging result for the SiO masers around a latetype star. The AGN research group reported the new synthesis
imaging method for interferometers utilizing the sparsemodelling.

2. The Japanese VLBI Network (JVN)
The university VLBI collaboration observation projectis carried out as a joint research project between NAOJ andsix universities. We organize the radio telescopes of VERA,
universities, and research institutes (JAXA / ISAS, NICT, GSI)
to make the Japanese VLBI Network (JVN), which is operated
at 3 bands of 6.7 GHz, 8 GHz, and 22 GHz. VLBI observations
were carried out for about 300 hours in total in 2016. In addition,
single-dish observations of up to 4,000 hours were carried out asresearch related to JVN. The main research subjects are active
galactic nuclei and maser / star formation.
In October 2016, the Astronomical Society of Japan releaseda special issue of PASJ on university collaboration. This volume
includes 8 papers based on JVN operations such as the results of
VLBI survey observations with small-number high-sensitivity
baselines (Fujinaga et al.), results of 6.7 GHz methanol-maser
monitoring by the East Asian VLBI network (EAVN) (Sugiyama
et al.), and a report on the Ibaraki telescopes (Yonekura et al.).

More than 10 papers including other related papers have been
published in 2016. Since the activities of university VLBI
collaboration have been appreciated, an Assistant Professor
position was established at Yamaguchi University, and filled by
Dr. Motoki, who obtained a Ph.D. by doing research using JVN
at Hokkaido University and worked as a postdoc at Mizusawa
VLBI.
In July 2016, the university collaborative workshop was heldat Ibaraki. Many participants attended, and white papers for the
future direction were created based on this discussion. A project,
entitled “high spatial resolution / time-domain astronomy in thecentimeter band,” was approved as a baseline of the university
collaboration. It is planned that maser / star formation study will
be mainly carried out at Ibaraki University, while active galactic
nuclei / black hole science will be mainly done at Yamaguchi
University. In particular, observations with a small number ofbaselines; time variation observations; and research with the
Ibaraki and Yamaguchi interferometers will play an importantrole in the future of the project.

3. Japan-Korea VLBI
(1) Observations and Common Use Observations
In 2016, a total of 158 VLBI observations (1234 hours),
common use observations, large program observations, and test
observations, were conducted by KaVA (KVN and VERA Array)with the 43 and 22 GHz bands. The data of the seven VLBI
stations were correlated at the Korea-Japan Correlation Center at
KASI Daejeon Campus in Korea.
KaVA common-use calls-for-proposals for semesters 2016B
and 2017A were made in May and October of 2016, respectively.
In total, 17 proposals requesting a total time of 582 hours were
submitted. Through the evaluations by referees elected fromscientists in related fields and subsequent decisions made by the
VERA and KVN combined Time Allocation Committee, a totalof 12 proposals (377 hours) were accepted in 2016B and 2017A.
(2) Results of Research
The number of science outcomes based on KaVA data is
steadily increasing since the opening of the KaVA common use
in FY 2014. In FY 2016, three research papers that made useof KaVA common-use data were published in peer-reviewed
journals. These are all related to AGN, where a variety of AGN
topics were explored: a follow-up monitoring of an opticallyviolent quasar (CGRsBS J0809+5341); radio imaging of highredshift (z > 5) quasars (e.g., J0131-0321); and a high-cadence
monitoring of a jet acceleration region (M87). In particular, theformer two are the first papers that were led by research groups
external to Korea/Japan, indicating that users of KaVA are
spreading into the world.
The three KaVA Large Programs (LP), which were launchedin late FY 2015, are continuing smoothly, and the analyses ofthese data are actively ongoing by each KaVA Science Working
Group (AGN, star-formation regions, late-type stars). For the
AGN LP, the acceleration profile of the M87 jet is beginningto be determined in higher detail. For the SFR LP, surveys of

87 water masers (22 GHz) and methanol masers (43 GHz) are
actively going on. For the LTS LP, roughly 90 % of the surveyof approximately 80 circum-nuclear masers was completed;work to narrow down the observational targets is ongoing. Someof these LP preliminary results were presented at international
conferences.

4. EAVN
To expand the capability of international VLBI throughout
East Asia, the commissioning of the East-Asian VLBI
Network (EAVN) is actively ongoing through collaboration
between Japan, Korea, and China. In FY 2016, a total of 8 test
observations were conducted with EAVN, and the first EAVN
image was successfully obtained (with KaVA plus Tianma at
Shanghai). The 9th EAVN Workshop was held at Guiyang,
China. Direct discussions were held with Chinese researchers,
particularly ones from Shanghai and Urumqi; and we reacheda consensus on the further acceleration of EAVN activities andcollaboration. As a result, the KaVA Science Working Groups
were expanded into the "EAVN Science Working Groups" byinviting Chinese researchers.
While the technical commissioning of the EAVN arrayis progressing, some science-oriented observations werealso launched, such as an EAVN monitoring of nearby
supermassive black holes near in time to the Event Horizon
Telescope observations. The program was performed with
KaVA+CVN+JVN at a high cadence of 1-2 weeks, and the array
operation went well without any major troubles. The common
use of EAVN is planned to open by 2018.

5. Geodesy and Geophysics
The regular geodetic sessions of VERA are allocated two or
three times every month to maintain the orientation and shapeof the array. VERA internal geodetic observations are performed
once or twice per month using K-band, and Mizusawa
participate in IVS sessions using S- and X-bands on a onceper-month basis. The 1-Gbps recording system of S/X bands
was newly developed to widen the recording bandwidth in IVS
sessions.
In FY 2016, we participated in 9 IVS sessions and performed
19 VERA internal geodetic sessions. The final estimation ofgeodetic parameters is derived by using the software developedby the VERA team.
After “The 2011 Earthquake off the Tohoku Pacific coast”(Mw = 9.0), VERA Mizusawa was displaced by co-seismic
crustal movement, and continuous post-seismic creeping was
detected in FY 2016. According to the newest analysis, the coseismic steps are X = −2.020 m, Y = −1.389 m, and Z = −1.060 m,
and displacement by creeping during FY 2016 is X = −0.075 m,
Y = −0.059 m, and Z = −0.014 m.
Continuous GPS observations at VERA stations are carriedout in order to detect short term coordinate variations andto estimate atmospheric propagation delays. The results of
GPS positioning also show a post-seismic motion to the East-

II Status Reports of Research Activities

079

Southeast of Mizusawa even though 6 years have passed since
the occurrence of the 2011 Earthquake off the Tohoku Pacificcoast. Continuous gravity observations with super-conducting
gravimeters were carried out at Mizusawa and Kamioka. The
observation at Kamioka was terminated in 2016. Gravity change
observation is also carried out at Ishigakijima as a joint projectwith other institutes and university groups. The features of theannual change are observed and studied by several techniques
including VLBI, GPS, and gravimeters. The strain and tilt
observation data obtained at the Esashi Earth Tides Station are
distributed in real time to several institutes based on the research
agreement between the Earthquake Research Institute, theUniversity of Tokyo and Mizusawa VLBI Observatory.

6. System Development
In 2016, we have developed two down-converters for dual
polarization receiving of the Q-band. We have performed a
VLBI experiment between KVN and VERA using OCTAD and
OCTADISK2 installed in KVN. The fringes of the experiments
are detected successfully in cooperation with VERA, KVN, andthe manufacturer. Fringes of an experiment between Italy and
VERA are also detected in all channels after data conversion
between domestic and international data formats. Upgrades to
OCTAD made AOV observations possible. We started discussionof the SKA project and high frequency VLBI as future plansof the observatory. We performed various basic design anddevelopment, including a low power consumption opticaltransmitter/correlator and balloon-borne radio interferometry.

7. Timekeeping Office Operations
The Timekeeping Office operates four cesium atomic
clocks together with a hydrogen maser atomic clock at
Mizusawa VERA Station. The facilities have been operating
stably, contributing to the determination of UTC (Coordinated
Universal Time) through continuous management and operationof the time system. The NTP (Network Time Protocol) Server at
the Timekeeping Office provides “Japan Central Standard Time”
on a network. This service has been in great demand; more than
1,500,000 daily visits have been recorded last year.

8. Ishigakijima Astronomical Observatory
FY 2016 was the 10th year of the Ishigakijima Astronomical
Observatory (IAO). In FY 2013, the “Starry Sky Study Room”
was established as an annex to screen the 4D2U (FourDimensional Digital Universe) theater by Ishigaki City, andthe number of visitors has increased to more than 15,000
people per year. The total number of visitors since FY 2006 has
exceeded 100,000. The observatory missions such as conducting
observational study, public outreach, and regional promotion
have been accomplished well. The 10th anniversary ceremony
was held in November. Special events including a science cafe,
photograph exhibition, and stargazing party were also given.
In terms of the research, observations of transient objects

080

II Status Reports of Research Activities

such as gamma-ray bursts, supernovae, and Solar System objects
were performed in collaboration with Japanese universities.
Three refereed papers using the observational data of IAO were
published, including studies of supernova SN 2016coi and comet
15P/Finlay. The total number of the papers has reached 19.
In FY 2016, the 15th “Southern Island Star Festival” washeld. The number of participants has also been increasing,and about 11,000 people attended the light-down stargazing
party. Special events to mark the 15th anniversary were held,
including a movie screening of “Welcome Home, HAYABUSA”
and the starry sky photo contest. The Japanese Tanka contest
on “Beautiful Stars” for which the judge was a famous Tanka
poet Machi Tawara was also held. In total, about 13,000 people
participated in the festival.
In terms of the education, the Chura-boshi Research Team
Workshop for high school students and the observational
experiment for undergraduate students of the University of the
Ryukyus were held. In the workshop, three new minor planets
candidates were found by the observations of the high school
students. One of these three objects was assigned the provisional
designation 2016 PH14 and was recognized as a discovery of
IAO by the IAU Minor Planet Center.
On the other hand, active interaction and collaboration withJapanese public astronomical observatories was performed. The
Nayoro Observatory in Hokkaido, with which IAO concluded
an agreement for cooperation, held a star festival in July; IAO
assisted with the star festival by providing a live relay of thelandscape and the starry sky from IAO.

9. Public Relations (PR) and AwarenessPromotion Activities(1) Open House Events
On April 17, 2016: the Seventh Open Observatory Eventheld at the Ibaraki University Center for Astronomy, and
NAOJ Mizusawa VLBI Observatory, Ibaraki Station, withapproximately 348 visitors in attendance.
On July 17: The Star Festival at the site of the 6 mantenna at Kinko Bay Park in Kagoshima City co-hosted with
Kagoshima City and Kagoshima University, with approximately
200 visitors.
On August 6–14: The Southern Island Star Festival
2016 held together with a special open house event at the
VERA Ishigakijima Station and Ishigakijima Astronomical
Observatory with approximately 11,000 visitors to the wholeStar Festival. Events included an astronomical observation
party at Ishigakijima Astronomical Observatory, attended by
338 visitors; and a special public opening of the VERA Station
attended by 252 visitors.
On August 7: Special open house of VERA Iriki station held
jointly with the Yaeyama Highland Star Festival 2016, withapproximately 4,500 visitors in attendance.
On August 20: Iwate Galaxy Festival 2016, open house of
NAOJ Mizusawa Campus, held with 2500 visitors in attendance.
On February 12, 2017: “Star Island 16”, open house event of
VERA Ogasawara Station held, with 227 visitors in attendance.

(2) Regular Public Visiting
Throughout the year, the following stations are open to the
public on a regular basis. The four VERA stations are open to
the public every day, 9 a.m. to 5 p.m., except during the New
Year’s season. Ishigakijima Astronomical Observatory is open
10 a.m. to 5 p.m. except during the New Year’s season and otherclosures.
The numbers of visitors to each facility is as follows,

Event” was held August 8–10 to use the VERA Mizusawa
antenna for observation. A total of 15 high school students
from the Tohoku region were accepted for research experience.
Continued from previous years, Mizusawa VLBI Observatory
supported the SSH (Super-Science High-school) research
activities for Yokote Seiryo High School in Akita Prefecture to
use the Mizusawa 20-m antenna.

a) VERA Mizusawa Observatory 18,100
The campus is regularly open to the general public with thecooperation of the Oshu Space and Astronomy Museum(OSAM: Yugakukan) located in the campus.
b) VERA Iriki Station 5,949c) VERA Ogasawara Station 9,930d) VERA Ishigakijima Station 2,442e) Ishigakijima Astronomical Observatory 15,061
Stargazing sessions: Evenings on Saturdays, Sundays.
The “Starry Sky Study Room” (featuring the 4D2U “FourDimensional Digital Universe”), constructed adjacent to
the observatory in 2013 by Ishigaki City, was very popular,
welcoming 4,317 guests.

10. Education(1) University and Post-Graduate Education
Regarding postgraduate education, Mizusawa VLBI
Observatory assisted two graduate students from the Universityof Tokyo and two from SOKENDAI for their Ph.D. research.
In addition, one Ph.D. student from oversees started Ph.D.
courses in SOKENDAI from autumn. One of the students
from SOKENDAI completed his Ph.D. thesis, and another
Ph.D. student found a job as a science communicator before
graduation. An undergraduate student from Nihon University
was accepted as a summer student of SOKENDAI. The
University of the Ryukyus and NAOJ have offered a joint
course on astronomy from FY 2009. Classroom lectures at
the university took place August 22–25 at the Nishihara main
campus and were opened to the public at the satellite campuses.
Observational workshops were held in Ishigakijima from August
29 to September 1, with about 30 participants. In addition, staff
members of Mizusawa VLBI Observatory give lectures at the
University of Tokyo, Tohoku University, and Teikyo Universityof Science as visiting professors.
(2) Research Experience for High School Students
During August 3–5, the VERA Ishigakijima station andthe Ishigakijima Astronomical Observatory held “The Churaboshi Research Team Workshop” for 17 high school students
from Ishigakijima, Okinawa main island, and Hyogo prefecture.
It was organized under support from JSPS. It is noteworthy
that observations carried out at Ishigakijima Astronomical
Observatory produced results including the discovery of a
new minor planet candidate which was assigned a provisional
designation. (Please refer to 8: Ishigakijima Astronomical
Observatory for more details.) “The 10th Z Star Research TeamII Status Reports of Research Activities081

5. Solar Observatory
The Solar Observatory primarily engages in the operationof solar observational facilities on the west side of Mitaka
Campus and in the development of new observational
instruments. It conducts both observational and theoreticalstudies of the structure of the solar outer atmosphere, including
the photosphere, chromosphere, corona, and solar wind; andactive phenomena such as sunspots, faculae, prominences,and flares. This observatory performs regular observations
using instruments such as the Solar Flare Telescope (SFT) andalso conducts expeditions to observe total solar eclipses. It
is also engaged in the planning of future ground-based solar
observations. Regular observations of sunspots and flares havebeen carried out for prolonged periods, and the resulting data areprovided to inter-university researchers.

1. Observational Facilities in Mitaka(1) Magnetic Field Observation
The SFT, which has been the main instrument of the
Observatory at Mitaka Campus, has kept observing photosphericvector magnetic fields at active regions and H-alpha flares
since its completion of 1992. The main instrument on the
SFT was updated to an infrared Stokes polarimeter in 2010.
Whereas previous magnetic field observations covered part ofthe solar surface, this new instrument was designed to obtainhigh accuracy vector magnetic field information over the fullsolar disk in order to elucidate the origins of the solar activity
cycle. This polarimeter is equipped with a 15-cm infrared lensand performs slit scanning observations using infrared spectral
lines (photosphere: iron, 1.565 μm line; chromosphere: helium,
1.083 μm line), which are sensitive to the magnetic field on
the Sun. This allows for constant acquisition of unprecedented
infrared polarization data for the photosphere and chromosphereof the entire solar disk. It had taken about two hours to cover the
full-disk Sun with a slit scan for each wavelength range, but a
two-camera system renewed in 2014 enables us to observe both
wavelength ranges simultaneously. The data acquisition is now
conducted more efficiently. However the system had a problem
in light path design; a camera could not sit in an optimal position
as designed and it was renovated this year by suspending theregular observations for several months. To further improve thepolarimetric data quality, the installation of an advanced infrared
camera with a large format and low read-out noise is being
conducted, and this year, the infrared detector H2RG EG-C andits control electric circuit SIDECAR+MACIE were procured
using a grant from the Project for Solar-Terrestrial Environment
Prediction (PSTEP), Grants-in-Aid for Scientific Research on
Innovative Areas.
(2) Regular Observation of Sunspots/Faculae/H-alpha Flares
Sunspot observations have been performed continuously
since 1929. These observations are currently conducted via
automatic detection of sunspots in digital images captured with

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a 10-cm refractor and a 2 k × 2 k pixel charge coupled device(CCD) camera mounted on the new (full-disk) sunspot telescope.
Observations were conducted for 241 days in FY 2016, from
April 2016 to March 2017.
Because full-disk solar image data are a widely demanded
resource in the astrophysics/geophysics researcher community,
some out-of-date synoptic instruments need to be upgraded.
Efforts are underway to update the photospheric andchromospheric imaging instruments and to further flesh out thedata. For instance, the SFT has started advanced observationsin the H-alpha line to acquire full-disk, high-resolution images.
It can obtain Doppler velocity information based on imaging
at multiple wavelengths around the H-alpha line center. High
temporal resolution enables the more complete capture ofactive phenomena, and a combination of multiple exposure
times allows for a wide dynamic range. Further improvement
in dynamic range and read-out noise was accomplished using
sCMOS cameras installed in FY 2015. This advancement hasenabled us to observe many phenomena, such as flares andprominence eruptions, even during the recent downturn insolar activity. The Observatory also uses the SFT to conduct
regular full-disk imaging observations in the G-band (430 nm)
and continuum wavelengths. In addition, CaII K (393 nm) filter
observation started in FY 2015.
The regular observational data described above, including
real-time images, are available on the website of the
Observatory. A spectrograph system with a coelostat is underdevelopment to perform long-term and full-disk observations.
An improvement to the spectrograph room was conducted thisyear. The Observatory maintains a coelostat and other existing
equipment to allow for velocity and magnetic field observations
more quantitative than everyday observation, as well as
experimental use.

2. Opening of Data Archives to the Public
The Solar Observatory has made nearly 16.2 TB of data
available to the public online, including data from the current
observations of white light, H-alpha, and magnetic fields aswell as those from nearly 100 years of various types of solar
observations. The various phenomena occurring in the solarterrestrial environment must be studied in terms of both sudden,
short-term events (space weather) and in terms of gradualchanges occurring over years or decades (space climate).
The Observatory will continue providing fundamental data
for these studies. The Observatory possesses nearly 100
years of accumulated records, including continuum images,
Ca II K-line images, and H-alpha images recorded on film,
photographic plates, and hand-drawn sketches, all of which havean importance of their own. The Observatory will make theseavailable to the public as well as soon as they are digitized andorganized. It is noted that there exist some of the world’s oldest
records of solar activities, which are expected to add particularinsight into future research. Higher bit digitization of old Ca II
K line images improving the data quality was conducted thisyear as a part of research activity for the PSTEP, Grants-in-Aid
for Scientific Research on Innovative Areas.
Data publicized via the website were previously stored ona server owned by the Observatory. The data have since beentransferred to the Astronomy Data Center, where all relevant
data servers have been managed in an integrated fashion. The
same data are stored at multiple locations in the data center,
serving as a backup in case of disaster.
The Observatory is also contributing to scientific verificationof data from the Nobeyama Solar Radio Polarimeters whichhave been maintained by Nobeyama Radio Observatory since
Nobeyama Solar Radio Observatory was shut down at the end of
FY 2014. To ensure the same data quality as before, a monthly
meeting is held for members from inter-university users,
Nobeyama Radio Observatory, and the Solar Observatory tocheck the obtained data.

2017. It included a session which served as the users meetingfor the Observatory where topics related to open use and futureplans were discussed.
Because the Observatory deals with fundamental solardata, there are often requests to use images from the Solar
Observatory database in school textbooks, to contribute toarticles in newspapers or magazines, and to help public events
held by museums. The Observatory actively responded to theserequests.
Regarding personnel transfers, Dr. Satoshi Morita wasselected as a specially appointed research specialist after theend of his term as a research expert at the end of FY 2016. It
was decided to start a new project “Solar Science Observatory”
by unifying the Solar Observatory with Hinode Science Centerfrom FY 2017 to promote more efficient research activity in thefield of solar physics.

3. Other Activities/Personnel Transfers
International cooperation includes support for the Japan–
Peru collaborative solar observations, with which the Solar
Observatory has been involved since 2004. In addition to thecollaboration in solar spectrograph installation and operationin Peru, relocation of the 10-cm coronagraph which had beenused in Norikura Solar Observatory is envisioned. For thispurpose, reassembling the coronagraph in the Observatory andsite selection in Peru are undergoing. The Solar Observatory
also supports the operation of another 10-cm coronagraphwith a NOGIS filter system in a Chinese observatory (3200m elevation) in the Yunnan province. This coronagraph was
relocated from Norikura in 2013 to observe two dimensional
intensity and velocity fields of the solar corona in the coronalgreen line of Fe XIV (530.3 nm). The Observatory supported
repair of a broken electric circuit board of the coronagraph thisyear. A new coronagraph reusing a 25 cm diameter lens fromthe coronagraph of Norikura Solar Observatory is planned in
China. The lens which has been displayed in a visitor facility of
Mitaka Campus was cleaned and stored in a container in caseof transportation to China in the near future. The Observatory
is participating the JSPS bilateral cooperative program between
Japan and Russia for FY 2016–2017 (Japanese representative:
Dr. Y. Yokoi, University of Tokyo) and is carrying out bilateral
joint research project in solar physics, by exchanging scientists
between the two countries.
The solar optical observations carried out at Hiraiso Solar
Observatory of the National Institute of Information andCommunications Technology are considered to be terminated.
To examine the possibility of utilizing the instruments in the
future at other institutes, the relevant equipment (H-alpha
Lyot filter and the telescope/coelostat for solar magnetic fieldmeasurements) were placed in storage at Mitaka until it has been
decided where to send them.
The solar research symposium for the entire solar
community was held at ISAS between February 20 and 22,

II Status Reports of Research Activities083

6. NAOJ Chile Observatory
The ALMA Project is a global partnership of East Asia
(led by Japan), Europe, and North America (led by the UnitedStates) in cooperation with other nations to operate a gigantic
millimeter/submillimeter radio telescope deploying 66 highprecision parabolic antennas in the 5000-m altitude Atacama
highlands in northern Chile. ALMA aims to achieve a spatial
resolution of nearly ten times higher than that of the Subaru
Telescope or the Hubble Space Telescope. Early scientificobservations with ALMA began in FY 2011 with a partial
number of antennas and full operation commenced in FY 2012.
This report describes the progress of the project, which includes
results of the open-use scientific observations and public
outreach activities. The ASTE telescope is a single-dish 10-m
submillimeter telescope located in the Atacama highlands andhas been operated to make headway into southern-hemisphere
submillimeter observations toward the ALMA Era. This report
also describes the progress of the ASTE telescope.

1. Progress of ALMA Project
ALMA scientific observations and commissioning
observations are currently underway. Commissioning
observations include polarization tests, solar observation tests
and observation tests using the newly installed Band 5 receiver,which are all making good progress. In these activities, East
Asian researchers have been taking initiatives in international
teams, as demonstrated by Koichiro Nakanishi and Hiroshi
Nagai for polarization, and Masumi Shimojo for solar
observation tests. Also, the sub-components developed by Japan,such as the antennas, correlators, and receivers (Bands 4, 8, and10), are working properly.

2. ALMA Open-Use and Scientific Observations
The fifth round of ALMA open-use observations commencedin October 2016 as Cycle 4. The main capabilities of Cycle 4
include: interferometric observations using forty 12-m antennas;
Atacama Compact Array (ACA) observations (interferometricobservation with ten 7-m antennas and single-dish observations
with three 12-m antennas); seven frequency bands (Bands 3,
4, 6, 7, 8, 9 and 10); and maximum baselines extended to 12.6
km (for Bands 3 to 6), 6.8 km (for Band 7), and 3.7 km (forBands 8 to 10). In addition to these, Cycle 4 also provides newopportunities for large programs that require long observations
over 50 hours, millimeter-wavelength VLBI, ACA stand-alonemode, solar observations, and polarization for spectral line
observations. In response to the Cycle 4 call for proposals, 1,571
proposals were submitted from all over the world.
The call for the sixth round of open-use observations
was issued as Cycle 5. The Cycle 5 capabilities will include:interferometric observations using forty-three 12-m antennas;
ACA observations (interferometric observation with ten
7-m antennas and single-dish observations with three 12-m

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antennas); eight frequency bands (Bands 3, 4, 6, 7, 8, 9, 10 and
newly-added Band 5), and maximum baselines of 16.2 km (forBands 3 to 6), 8.5 km (for Band 7), and 3.6 km (for Bands 8 to
10). It should also be noted as a remarkable development that
the ALMA maximum baseline will be made available for openuse observation with Bands 3 to 6. The call for proposals for
Cycle 5 is set to be closed at 00:00 JST on April 21, 2017. Cycle
5 is scheduled to start in October 2017.
Open-use of ALMA has already produced a numberof scientific results. This section describes some of theachievements, focusing mainly on East Asian projects. Aninternational team led by Akio Inoue at Osaka Sangyo University
detected emission lines from ionized oxygen in a distant galaxy
13.1 billion light-years away. The galaxy was first discovered
with the Subaru Telescope and observed with ALMA this time.
This is the most distant galaxy in which oxygen has ever been
detected and thought to be one type of source that triggered“cosmic reionization” in the early history of the Universe justseveral hundred millions of years to one billion years after thebirth of the Universe. This observation result is a very important
step towards understanding the cosmic reionization which has
yet to be explored. A team of Japanese astronomers led by
Takashi Shimonishi at Tohoku University revealed a hot corecontaining various molecular gases around a newborn massive
star in the Large Magellanic Cloud using ALMA. This is the first
hot molecular core that has ever been detected outside the Milky
Way Galaxy and has a very different composition than similar
objects found in the Milky Way. Studying complex organic
molecules contained in hot cores will be a key to unveiling thechemical diversity of the Universe. Since the Large Magellanic
Cloud is known to have lower metallicity compared with theMilky Way, this result provides an important clue to revealing
the distribution of organic molecules in the early Universe withlow metallicity. A research team led by Takashi Tsukagoshi
at Ibaraki University observed the young star TW Hydrae
using ALMA and revealed the detailed distribution of dust in
its protoplanetary disk. They made comparative analysis ofobservation results in two frequencies and found that larger dust
particles are absent in the most prominent gap with a radius of
22 astronomical units. Based on a theoretical model, the result
indicates that a possible Neptune-like planet is forming in thegap. These findings will help scientist identify what type ofplanet is forming in a specific location of a protoplanetary disk.

3. Educational Activities and Internship
During the summer vacation of universities, the NAOJ Chile
Observatory accepted five undergraduate students, three of
which conducted research activities in Mitaka and other two in
Chile, as well as four visiting researchers in total which include:
one Japanese graduate student each from Osaka Prefecture
University and the University of Tokyo and internationally one
post-doctoral fellow each from the University of Chile andLeiden University of Netherlands for a period of one month.

4. Public Outreach Activities
Achievements of ALMA scientific observations and test
observations were covered by nearly 40 newspaper/journal
articles and 11 television/radio programs, reporting ALMA
observation results in various fields of astronomy. In particular,
a news program called “Good Morning Japan” on NHK G
channel featured ALMA’s detection of the most distant oxygenin the Universe in June 2016, and another NHK program called“News Watch 9” introduced ALMA observation results of a
protostar in March 2017. The detection of the most distantoxygen was covered by more than 400 news websites worldwide
and the BBC website featured the observation results of TW
Hydrae achieved by Takashi Tsukagoshi (Ibaraki University) et
al. As seen in these examples, the scientific results by Japanese
researchers have been increasingly broadcast worldwide.
The NAOJ ALMA website posted 51 news articles and eightpress releases. A mailing-list-based newsletter has been issued ona monthly basis with approximately 2,500 subscribers. Updated,detailed information is available on Twitter (@ALMA_Japan),with nearly 33,250 followers as of the end of FY 2016.
In May 2016, the NAOJ Chile Observatory hosted a weeklong ALMA booth at the Japanese Geoscience Union Meeting
held in Makuhari Messe. The NAOJ Chile Observatoryorganized public lectures and Science Cafe events on 17
occasions in FY 2016 and gave talks on the progress of ALMA
to a large number of visitors. In particular, the 22nd ALMA
Public Lecture “Star and Planet Formation Explored by ALMA”
held in Nagoya City Science Museum on November 26,
2016 attracted a big audience of over 200, which was a great
opportunity to introduce the latest scientific results of ALMA to
the public.
The NAOJ Newsletter featured ALMA’s semiannual
achievements in the April and November 2016 issues.
From the mid-March 2015, ALMA started to accept public
visitors at the ALMA Operations Support Facility (OSF) at analtitude of 2900 meters. Every Saturday and Sunday, ALMA
is open to the public up to 40 people/day (advance registrationis required). Visitors to the OSF can have a guided tour of the
OSF including the control room and watch videos on ALMA.
The registration often reaches the full capacity soon after thestart of registration every weekend. Public visits to ALMA are
now becoming a good opportunity to provide many people live
experience at the workplace of ALMA researchers.

5. International Collaboration (committees, etc.)
On November 17, 2016, the Management Agreement
Concerning Operations of ALMA was signed in Santiago by
the representatives of NAOJ, the European Organization for
Astronomical Research in the Southern Hemisphere (ESO), andAssociated Universities Inc. (AUI) of the United States.
In the international ALMA project, meetings are held
frequently by various committees. In FY 2016, the ALMA

Board met face-to-face once, and the ALMA Scientific Advisory
Committee (ASAC) twice. In addition to these, teleconferences
have been held on a near-monthly basis among the members of
the ALMA Board and ASAC. The ALMA East Asian Science
Advisory Committee (EASAC) had meetings face-to-face or via
teleconferences on a quarterly basis. Each working group holds
meetings and teleconferences more frequently to maintain close
communication in implementing their respective tasks in theinternational project.

6. Workshops and Town Meetings• July 20 to 21, 2016 NAOJ Nobeyama Radio Observatory(NRO)
NRO-ALMA Science/Development Workshop 2016
• September 20 to 23, 2016 Renaissance Indian Wells Resort &Spa, Indian Wells, CA, USA
Half a Decade of ALMA: Cosmic Dawns Transformed• December 19 to 20, 2016 NAOJ Mitaka
ALMA/45 m/ASTE Users Meeting 2016
• March 24, 2017 Okayama University of Science
ALMA Cycle 4 Town Meeting

7. Obtained External Grants Other Than
Grants-in-Aid for Scientific Research including
Industry –University Collaboration Expenses• Satoru Iguchi: Grant for Basic Science Research Projects by
the Sumitomo Foundation• Seiji Kameno: International Research Support Program byFoundation for Promotion of Astronomy• Hitoshi Kiuchi: Funded externally by the Ministry of Internal
Affairs and Communications (Strategic Information andCommunications R&D Promotion Programme: SCOPE) R&D
for Promotion of Effective Radio Use (Advanced Effective
Radio Use-Phase 1)

8. Research Staff Changes(1) Hired• Xing Walker Lu: Specially Appointed Research Staff• Naslim Neelamkodan: Specially Appointed Research Staff• Natsuko Izumi: Specially Appointed Research Staff• Kazuki Tokuda: Specially Appointed Research Staff (assigned
to Osaka Prefecture University)• Sarolta Zahorecz: Specially Appointed Research Staff (assigned
to Osaka Prefecture University)• Takuya Hashimoto: Specially Appointed Research Staff(assigned to Osaka Sangyo University)• Sanemichi Takahashi: Specially Appointed Research Staff(assigned to Kogakuin University)(2) Departed or Transferred• Kana Morokuma: Specially Appointed Research Staff• Tatsuya Takekoshi: Specially Appointed Research Staff

II Status Reports of Research Activities085

9. Main Visitors• September 15, 2016
Mr. Toshiei Mizuochi, Vice Minister of Education, Culture,
Sports Science and Technology, visited the Santiago Office of
the Joint ALMA Observatory (JAO).
• October 13, 2016
Mr. Shigeharu Orihara, Counselor of the Japanese Embassy inChile, visited the OSF and AOS.
• October 18, 2016
Mr. Hiroshi Nagano (National Graduate Institute for Policy
Studies; former Chair of the OECD Global Science Forum)
visited the OSF and AOS.
• November 23, 2016
Director General of the National Astronomical Observatoriesof the Chinese Academy of Sciences (NAOC) and his party
visited the NAOJ Santiago Office.

10. Progress of ASTE Telescope
The ASTE telescope has been operated to promote fullfledged submillimeter astronomical research in the southernhemisphere and develop/verify observational equipment andmethods required for the submillimeter astronomy. Since
ALMA entered its operation phase in FY 2012, ASTE is usedmainly to provide observational evidence for strengthening
ALMA observation proposals and promote development for theenhancement of ALMA’s future performance.
Except for ALMA, there are only two large-scale
submillimeter telescopes in the world with a 10-meter-classantenna that can observe the southern sky: one is ASTE and theother is APEX operated by Europe. Therefore, having ASTE
operated by Japan will be a big advantage for strengthening
ALMA proposals and for implementing our strategies for further
extended capabilities with new observing instruments. For the
future, ASTE is also important since it provides opportunities
for nurturing young researchers who will play key roles in theequipment development for the next generation. In the near
future, ASTE will be incorporated into the open-use program tohave organic collaboration with the Nobeyama 45-m Telescope.
The open-use program in FY 2016 provided spectroscopic
observations in 345 GHz and 460 GHz bands for a period of
three months. To render support for researchers contributing
to the observational performance enhancement of ASTE,
the Guaranteed Time Observation (GTO) scheme has beenoffered since FY 2013, which allows them to exclusively makeproposals for the GTO slots. In addition to this, Joint slots
have been newly established to allow researchers to jointly
request observation time with ASTE and the Nobeyama 45-m
Telescope at the same time. A total of 14 proposals for openuse observations and GTO slots were submitted (including 9 foropen-use, 4 for Joint slots, and one for GTO). These proposals
were reviewed by the Millimeter/submillimeter Program
Subcommittee and 11 proposals were adopted including 6
for open use, 4 for Joint slots, and one for GTO in the first
call. Open-use observations were carried out from the ASTE

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Mitaka operations room or from other universities and research
institutes from September 26 to December 8, 2016.

7. Center for Computational Astrophysics (CfCA)
1. Overview
The Center for Computational Astrophysics (CfCA)
has been operating a system of open-use computers for
simulations centered around a general-purpose supercomputer
and the special-purpose computers for gravitational manybody problems, carrying out research and development ofcomputational astrophysics, and performing astronomical
research with simulations. The main supercomputer of thepresent system, ATERUI (Cray XC30), has the theoreticalpeak performance of 1 Pflops, which is the world’s fastest
supercomputer for astronomy. The center also continued
operation of other computers such as GRAPE-DR and GRAPE-9
that are dedicated for gravitational many-body problems, inaddition to general-purpose servers (PC clusters) for smallscale calculations.. Efforts in visualizing astronomical data also
continue.

2. Open Use(1) Computer Systems
This year marked the fourth year of the upgradedastronomical simulation system, which includes the openuse supercomputer Cray XC30. All the CPUs of the mainsupercomputer which is installed and under operation at
Mizusawa VLBI Observatory had been upgraded last year,
and the supercomputer’s theoretical peak performance is now
as high as 1 Pflops. The users have been making academicallysignificant progress as before.
While XC30 is leased for five years from Cray Japan Inc.,
the center has built the following equipment to aid the openuse computer operations: a series of dedicated computers forgravitational N-body problems, known as GRAPEs; PC clusters
for small to medium-scale computation; large-scale file servers;a group of servers for processing computational output data;and networking instruments to encompass the overall computer
system. These components are central to numerical simulations
by researchers in Japan and overseas. In particular, the GRAPE
system is promoted for its effective open use. The center
undertook development, improvement, and maintenance for both
hardware and software for the system this year.
Computational resources are allocated to the XC30,
GRAPEs, and smaller computational PC clusters in accordancewith a formal review process. The statistics of applications andapprovals for this year are listed below. Our center conducteda survey this year on the number of peer-reviewed papers
published in English in FY 2015 on studies that involved the
project's open-use computers. It turned out that 112 refereed
papers (written in English) were published in this fiscal year.
The center uses Drupal, a content management system
introduced for data exchange with users of open-use computers.
The acceptance of various applications and the management of
the users’ personal information are all handled through Drupal.

The regular CfCA News is an additional channel of information
dissemination. The center leverages this newsletter to inform
people of all useful and necessary information regarding
the computer system. A subsidy system for publishing andadvertising is continuing this year for research papers whose
major results were obtained by using the center's computers.
Two papers were accepted in FY 2015 for payout in FY 2016,
while two papers were accepted in FY 2016 for payout in thesame year at approximately 90,000 JPY.
□ Statistics on the Cray XC30
Operating hours- Annual operating hours: 8550.7- Annual core operating ratio: 89.84 %Users- Category S: 0 adopted in the first term, 0 in the second term;
total 0- Category A: 12 adopted at the beginning of the year, 1 in thesecond term; total 13- Category B+: 8 adopted at the beginning of the year, 1 in thesecond term; total 9- Category B: 91 adopted at the beginning of the year, 10 in thesecond term; total 101- Category MD: 13 adopted at the beginning of the year, 4 in thesecond term; total 17- Category Trial: 34, year total□ Statistics on the GRAPE system
Users- Category A: 2 adopted at the beginning of the year, 1 in thesecond term; total 3- Category B: 6 adopted at the beginning of the year, 0 in thesecond term; total 6- Category Trial: 1, year total□ Statistics on PC cluster
Operating hours- Annual operating hours: 8597.4- Annual job operating ratio: 72.9 %Total users: 41, year total(2) Tutorials and Users Meeting
The center organized various lectures and workshops
to provide the users of the open-use computer system witheducational and promotional opportunities, as well as to train
young researchers. The details are shown below. In addition,
the CfCA Users Meeting was held to serve as a forum for direct
information exchange. Many participated in the meeting, anddiscussions were fruitful.
□ Cray XC30 workshop for beginning users: August 29, 2016, 5
attendees

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□ IDL visualization workshop: August 30, 2016, 6 attendees□ Cray XC30 workshop for intermediate users: August 31, 2016,
7 attendees□ Hydrodynamics simulation school: February 18–21, 2017, 40
attendees□ N-body simulation Spring School: February 8–12, 2017, 12
attendees□ Users meeting: November 29–30, 2016, 67 attendees

3. PR Activities
In FY 2016, two press releases were issued from CfCA;“Avoiding ‘Traffic Jam’ Creates Impossibly Bright ‘Lighthouse’”(September 8, 2016, Tomohisa Kawashima and Ken Ohsuga,
CfCA/NAOJ), and “Mystery Solved Behind Birth of Saturn’sRings” (October 31, 2016, Ryuki Hyodo, Kobe University).
A Twitter account @CfCA_NAOJ and YouTube channel havebeen operated to provide the information on CfCA.
CfCA took part in the special open house of Mizusawa
Campus, Iwate Galaxy Festival 2015, held on August 20, 2016.
About 150 visitors attended the ATERUI guided tours andexperienced a close-up observation of the facility. In addition
CfCA assistant professor Ken Osuga gave one of the special
lectures, presenting the latest results of black hole researchusing ATERUI. At the Mitaka open house held on October 22,
2016, CfCA made the computer room accessible to the public
and introduced simulation astronomy with GRAPE and the PC
cluster. At this open house, the image panels which cover the
ATERUI body were displayed to introduce ATERUI to thosevisiting Mitaka. In addition to the open house, CfCA accepteda group of high school students to tour the computer room in
the Mitaka Campus. Moreover, in the NINS exhibition roomin Nobeyama Campus, CfCA displayed GRAPE boards andposters to introduce research results from simulation astronomy
calculated by the CfCA system.

4. 4D2U ProjectIn FY 2016, the 4D2U project continued to develop
and provide the movie contents and software. Simulation
movies titled “Dynamics of Saturn's Ring (II. Propeller
Structure),” “Giant Impact of Protoplanets,” and “Formationof Planetesimals” were released on the 4D2U website in July
2016. Two of these movies, "Giant Impact of Protoplanets"
and “Formation of Planetesimals”, as well as “Formation and
Evolution of Dark Matter Halos (II. Formation of the LargeScale Structure of the Universe) ver. 2” were published on the
4D2U YouTube channel with a format for VR on smartphones.
The updated version of the four-dimensional digital universe
viewer, “Mitaka,” was released in July 2016 (ver.1.3.2). Thisversion of Mitaka included new functions, e.g. displaying probes
like Juno and Kepler; and the topographic and toponomastic

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data of Mercury. Moreover, four languages (Italian, Indonesian,Portuguese, and Thai) were added. In February, 2017, the 4D2U
project put out a news release “Mitaka for VR” designed tooperate with VR headsets, like Oculus Rift CV1 and HTC Vive.
Mitaka for VR enabled us to enjoy the all-around view of thevirtual universe while walking through the virtual universe
freely and looking around celestial objects and space probes.
In FY 2016, demonstrations of Mitaka VR were given
during the open campus days of Mizusawa, Nobeyama, andMitaka; and the Inter-University Research Institute Corporation
Symposium. Many people were able to enjoy Mitaka outside of
the 4D2U Dome Theater.
4D2U contents were provided both domestically andinternationally for TV programs, planetarium programs, lecture
presentations, books, and so on. In FY 2016, all of the 4D2U
contents were provided to the 3D planetarium of Kurobe
Yoshida Science Museum in Toyama prefecture, which was
upgraded to stereoscopic projection in April 2016. In addition,
the 4D2U Theater of the NINS exhibition room in NobeyamaCampus installed all of the 4D2U contents.
A Twitter account @4d2u and YouTube Channel have been
operated to provide the information on 4D2U.

5. External Activities(1) Joint Institute for Computational Fundamental Science
The Joint Institute for Computational Fundamental
Science (JICFuS) is an inter-organizational instituteestablished in February 2009 as a collaboration base between
three organizations including the Center for Computational
Sciences (CCS) of the University of Tsukuba; the High Energy
Accelerator Research Organization, known as KEK; and NAOJ
to provide active support for computational scientific research(it has now expanded to include eight institutes). CfCA forms
the core of NAOJ’s contribution to JICFuS. In particular,
the institute engages primarily in computer-aided theoreticalresearch into the fundamental physics in elementary particle
physics, nuclear physics, and astrophysics. The scientificgoal of the institute is to promote fundamental research basedon computational science by encouraging interdisciplinary
research between elementary particle physics and astrophysics.
In addition to its ability as a single organization, a major
feature of the institute is the cooperation of their community toprovide considerate and rigorous support to present and future
researchers. Another important mission of the institute is toprovide researchers around Japan with advice regarding efficient
supercomputer use and the development of novel algorithms
for high-performance computing to meet research goals fromthe perspective of computer specialists. In addition, JICFuS
was chosen as the organization responsible for ‘Research andDevelopment, Application Development of scientific/social
issues that require particular attention by the use of the Post
K-computer’ in FY 2014. The program started last year.
In order to implement research plans, Hiroyuki Takahashi
was engaged as a project assistant professor. Takahashi
performed general relativistic radiation magnetohydrodynamics

(MHD) simulations of accretion disks and jets around black
holes/neutron stars. The simulation revealed that supercriticalaccretion is possible onto not just black holes, but neutron stars
as well. In the case of a strongly magnetized neutron star, amagnetosphere forms around the neutrons star. Then, the gasof the disk finally falls onto the magnetic poles and strong jets
appear around the rotation axis.
Representing CfCA, Professor Kohji Tomisaka and AssistantProfessors Ken Ohsuga of NAOJ participate in bimonthly
JICFuS steering committee meetings to engage in deliberations
on spurring computational science-based developments inastrophysics research through discussions with other committee
members who specialize in nuclear and elementary particle
physics.

(Research associates) Tomohisa Kawashima(2) HPCI Consortium
As a participant in the government-led High-Performance
Computing Infrastructure (HPCI) project since its planningstage in FY 2010, the center has engaged in the promotion of the
HPC research field in Japan, centering on the use of the national“K” supercomputer and the “Post-K” plan. Note that although
the center is involved with the JICFuS-led HPCI Strategic
Program Field 5 as well as Priority Issue 9 to be tackled using
the Post-K Computer as mentioned in (1), the activity in the
HPCI consortium is basically independent from them. The HPCI
consortium is an incorporated association established in April
2012, and the center is currently an associate member that is able
to express views, obtain information, and observe overall trends
in the planning, although we are devoid of voting rights as wellas the obligation to pay membership fees. Continuing from lastyear, a number of conferences and WGs have been held whereparticipants discuss a next-generation national supercomputing
framework to follow the “K”. The Post-K project has alreadystarted with some budget from the Ministry of Education,
Culture, Sports, Science, and Technology (MEXT). The primary
institutes and groups responsible for its development havebeen established. Now the detailed discussions as to how wefully exploit the resources of the post-K system have begun inrelevant communities and organizations. The post-K generationequipment is scheduled to commence operation in FY 2019 orlater. In principle, therefore, it is possible for the NAOJ to play acentral role in the post-K generation HPCI through participationin this discourse.

6. Contract Staff Transfers
The following staff members were hired on a contract basis in
this FY:(Research experts) n/a(Postdoctoral fellows) Yukari Ohtani(Research associates) Tomohisa Kawashima, Tetsuo Taki, Yuki
Tanaka, Satoki Hasegawa
The following contract staff members departed in this FY:(Research experts) Shoichi Oshino(Postdoctoral fellows) n/a

II Status Reports of Research Activities089

8. Hinode Science Center
The scientific satellite Hinode is an artificial satellite that was
launched on September 23, 2006, by the ISAS division of JAXA,
as Japan’s third solar observational satellite following Hinotori(1981) and Yohkoh (1991). NAOJ implemented this satellite
project under a joint research agreement with ISAS/JAXA. A
major theme of the scientific goals of the Hinode mission is toshed light on the coronal heating mechanism through a more
multifaceted understanding of magnetohydrodynamic (MHD)
phenomena occurring in the solar atmosphere. The satellite has
actually made a lot of discoveries related to these subjects.
Hinode is equipped with three telescopes including thesolar optical telescope (SOT), the X-ray telescope (XRT), andthe extreme ultraviolet (EUV) imaging spectrometer (EIS). It
engages in simultaneous observations of the detailed magnetic
fields and velocity fields on the surface of the photosphere andthe brightness and velocity fields from the chromosphere to thecorona. The onboard telescopes were developed as part of awide-ranging international collaboration with assistance from
ISAS/JAXA. SOT was developed mainly by NAOJ, and the
focal plane package (FPP) was developed by the US National
Aeronautics and Space Administration (NASA) and Lockheed
Martin.
With regard to the XRT, NASA and the Smithsonian
Astrophysical Observatory (SAO) are responsible for the
optics system and frame, and Japan (ISAS/JAXA, NAOJ)
is responsible for the focal plane camera. EIS is the resultof an even broader international cooperation. The structureand electrical system were developed by the UK Science andTechnology Facilities Council (STFC) and University College
London; the optics system was developed by NASA and theNaval Research Laboratory (NRL); and the University of Osloin Norway assisted with the terrestrial testing equipment and
the Quick Look system. NAOJ actively participated in thedevelopment of the EIS/satellite interface, satellite integration
testing, and launch experiments. After a successful launch,
NAOJ has continued its active involvement by acting as themain institution for collecting and analyzing data acquired by
the satellite.
The Hinode Science Working Group (SWG), composedof representatives from the international team, offers support
in scientific operation and data analysis. Together with two
members from the European Space Agency (ESA), the WG has
a total of 15 members, including two from the Hinode Science
Center (HSC): Suematsu, SOT; and Watanabe, EIS. Science
Schedule Coordinators have been organized to leverage theopen-use observation system. Many of the Japanese coordinators
are NAOJ staff members, including Watanabe (Co-chairman/
EIS) and Sekii (SOT).
FY 2016 marks the tenth year since the satellite's launch.
The mission extension has been approved in JAXA for four
more years until FY 2021. The NASA Senior Review is
expected to be held in July 2017 to approve the request of theNASA mission extension for three more years. The ESA Science090

II Status Reports of Research Activities

Program Committee also approved support at the current levelof funding until the end of FY 2018, possibly to be extended tothe end of FY 2020. The funding from STFC will be requested
in FY 2017 for an extension of two more years.

1. The Hinode Satellite: Onboard Telescopes
and Scientific Operation
The SOT is a telescope used for obtaining photosphericmagnetic field vectors via polarimetric observations ofabsorption lines. It has the capacity for continuous observation
at the diffraction limit with a spatial resolution of 0.2–0.3 arcsec
and an effective aperture of 50 cm without atmospheric seeing.
The focal plane package consists of three types of optics systems
and imaging functions for maintaining the desired performancelevel. Operational modifications have enabled long-term
maintenance of a sound field of view even in the narrow band
filter imager system, in which image degradation was initiallydetected in part of the field of view. The power supply for thefiltergraph (FG) camera failed on February 25, 2016. The FG
system has been powered off, and ceased operation since then.
The cause of the trouble was identified as a short circuit in the
FG power supply.
The XRT has the capacity of capturing the solar coronalplasma via soft X-rays. The telescope has inherited the grazing
incidence optics system and has improved in spatial resolution.
Its wavelength characteristics have been improved to allow
for observation of the solar coronal plasma over a broader
temperature range. Resolution is close to 1 arcsec. Calibration is
now possible for temporal variations in spectral characteristics
due to surface contamination on the detector, and the telescopeis available for analysis via its spectral characteristics.
The EIS obtains temperatures, densities, and velocitiesof the chromosphere, transition region, and coronal plasma
thorough the spectroscopic observation of EUV emission lines.
The instrument allows for spectroscopy and imaging at multiple
wavelengths via the operation of slits and slots. Its purpose is
to investigate the manner in which energy is conveyed from its
generation in the photosphere until its dissipation in the corona
by observing from the chromosphere (located between thephotosphere and the corona) through the transition region to thecorona.
A mission data processor (MDP) was installed to manage
observations and to acquire data via the three telescopes.
Coordinated observations using the three telescopes, in which
the MDP plays a crucial oversight role, are vital to achieve thescientific goals of the Hinode satellite. Particularly for the XRT,
functions such as the exposure time adjustment, the regionof interest (ROI) selection, and the flare detection logic arehandled by the MDP, which requires close coordination with thetelescopes.
Data from the Hinode satellite is primarily downlinked at
the Kagoshima station (USC) and at Norway’s Svalsat station

through collaboration with ESA, allowing for data acquisition
for every orbit. Scientific operation was again performed in FY
2016 via S-band data reception. The S-band reception frequency
was increased with help from ESA and NASA, allowing forcontinuation of regular, stable scientific operation.
Obtained data is collected at ISAS/JAXA, converted into the
FITS format, and provided to researchers around the world in
the form of Level-0 data, which is close to raw data. HSC staff
members and students took part in satellite operation for a totalof 218 days in FY 2016, 76 days of which were for contracted
work. Moreover, the contribution rates to the scientific operationof the HSC were 27.1% (domestic) and 17.1% (overall).
Instantaneous publication of all data acquired by Hinode began
on May 27, 2007, with stable continuation, implemented by
HSC.
Calls for Hinode Operation Plans (HOP), which encourage
proposals for open-use observations together with othersatellites and terrestrial observational equipment, promotejoint observations among solar researchers worldwide. As of
March 2017, a total of 337 applications have been accepted.
In particular, core HOP proposals made by members of thescientific instrument team became refined over multiple
implementations. Through systematic observations they haveproduced results which increase in significance as the solar cycle
progresses. And new HOPs were added aiming for collaborative
observations with the ALMA cycle-4 solar campaign.

2. Hinode Satellite Data Analysis
NAOJ HSC aims to construct an analytical environment anddatabase for scientific analysis of data from the Hinode satellite
in a central organization, allowing it to function as a research
center. The goals are to maximize the scientific outputs gained
from the Hinode satellite by offering researchers in Japan andother countries a data analysis environment; and to promoterigorous collaborative research between researchers in Japanand abroad by facilitating access to Hinode observational data
through distribution of the analyzed data and construction of adata search system.
As part of its educational and public outreach (E/PO)
activities, HSC also uses the latest observational data to raise
public awareness of the relationship between solar researchand everyday life so that the importance of solar research isappreciated. The Center has offered press releases, web releases,
and media appearances; responded to interview requests fromtelevision programs and journals; and provided materials for
publicizing scientific results.
In FY 2015, HSC staff members and students published 10
peer-reviewed papers related to Hinode, bringing the total to 260
papers by the end of March 2017. Cumulatively, a total of 942
peer-reviewed papers have been published on Hinode-related
topics in the six major journals (ApJ, AAP, SP, PASJ, Nature,and Science). Intensified collaborative research with newly
launched missions (SDO and IRIS) and advanced ground-based
facilities (ALMA) will further enhance the number of research
papers for pursuing the essence of solar activity.

3. Other Activities
In FY 2016, one postdoctoral fellow was engaged as amember of HSC.
The Hinode Science meetings for Japanese and international
researchers have been held regularly to advance research infields related to solar physics thorough use of the Hinodesatellite. We have taken turns at organizing the meetings, and thetenth Hinode Science meeting took place during September 5 –9, 2016, at Nagoya University, Nagoya (Japan). The number ofparticipants amounted to 153 from 14 overseas countries, and a
total of 161 papers were presented at the meeting.
To celebrate the tenth anniversary of the launch of the
Hinode mission, we have:
1. produced a movie (https://www.youtube.com/embed/
dqoIqXiz1Dk).
2. renewed the web pages of the project (http://hinode.nao.
ac.jp/).
3. held a public lecture on September 10, 2016 at Nagoya
University.
4. published a special issue of the Astronomical Herald (vol 109,
August-October edition).
5. published a special issue of NAOJ News (No. 282, 2017
January issue).
6. produced a poster as an insert in the above NAOJ News.
In addition to the aforementioned activities, HSC researchand educational staff members have presented scientificobservation results at numerous symposia on solar-related
subjects either by invitation or by active participation. HSC has
also invited international researchers to engage in collaborative
research. The following researchers have visited the Center fromoverseas on a long-term stay of at least one month:
Name

Organization (Country)

Rutten, Robert J.

Universiteit Utrecht(The Netherlands)

Table 1. Long-term Visitors.

II Status Reports of Research Activities091

9. Gravitational Wave Project Office2016 has been marked by the announcement of the firsttwo detections of gravitational waves from the coalescence andmerger of black holes binaries and by the operation iKAGRA,
the first 3-km long laser interferometer located underground at
Kamioka. These first detections demonstrate that KAGRA will
be able to detect the coalescence of binary black holes as soon
as its sensitivity reaches the order of 1 Gpc distance for stellar
mass binary black holes. The Gravitational Wave Project Office(GWPO) of NAOJ has pursued the construction of KAGRA at
Kamioka. In particular the office was one of the leading groups
in the operation of iKAGRA. The group has now entered an
intense phase of work on site to install the vibration isolation
system, one of the largest detector subsystems. To this end morethan ten NAOJ staff members are working at Kamioka on aregular basis.

1. Development of KAGRA
KAGRA is an interferometric gravitational wave detector
being constructed at an underground site in Kamioka, Gifu
prefecture. In addition to the quiet underground environment,
the use of cryogenic mirrors to reduce the thermal noise makes
KAGRA a unique instrument among other large gravitational
wave detectors.
KAGRA’s construction is planned to proceed in several
stages. Initial KAGRA (iKAGRA) was the first step of thephased development of the KAGRA detector, in which a room-

Figure 1: Sketch of gravitational wave space-time ripples impinging
upon the KAGRA detector.

092

II Status Reports of Research Activities

temperature Michelson interferometer was constructed. In
March 2016, iKAGRA detector installation was completed
and we successfully operated the first km-scale undergroundinterferometer ever built on the Earth. The test operation of
the iKAGRA interferometer started on March 25, 2016 andcontinued until April 25 with a short commissioning break inthe middle. This operation gave us an opportunity to checkthe validity of the KAGRA facility as well as accumulate a lotof experience in installing and commissioning a large-scaleprecision instrument underground. The next step of the KAGRA
development is called bKAGRA phase 1, in which we will build
a cryogenic Michelson interferometer. The efforts of the NAOJGWPO are now focused on the realization of bKAGRA phase 1.
The NAOJ GWPO is contributing to the project in several
aspects. The largest responsibilities are development andinstallation of ultra-high performance vibration isolation systems
for the interferometer mirrors. Other technical contributions
include the auxiliary optics, mirror characterization facility, andthe design of the optical configuration and the control strategy
for the main interferometer. NAOJ is also contributing to theproject management through the activities of the executive
office, the systems engineering office, the committee forpublication control, the publication relation committee, thesafety committee, and the KAGRA Scientific Congress (KSC)
board.
(1) Vibration Isolation Systems
The vibration isolation system (VIS) is composed of thesuspensions required to isolate all the interferometer mirrors andsome other optical components from ground vibrations. Fourdifferent types of suspensions, having different complexities tomeet the varied isolation requirements of different components,
have been developed at NAOJ for this purpose. We are now
installing mirror suspensions necessary for bKAGRA phase
1, including two 14-meter-long suspensions for cryogenic
mirrors, five large room-temperature suspensions, and two small
suspensions. Preparation of those suspensions progressed wellin FY 2016. In the latter half of the fiscal year, we started theinstallation of some of the suspensions. Currently more than 10
members of the GWPO are regularly working in Kamioka for
the installation works of the VIS.
(2) Auxiliary Optics
The Auxiliary Optics (AOS) subsystem is responsible forproviding optical components for stray light control, opticalangular sensors, beam reducing telescopes (BRTs), beam
monitoring cameras and optical windows. Highlights of theactivities in FY 2016 are relevant to the BRT and some of thelarge optical baffles. Prototyping of the BRT as well as thedesign of the vibration isolation stage for the BRT were mostly
finished by ATC. Two optical baffles with diameters of 1 m were
installed into KAGRA. Design of the wide-angle baffles was
mostly completed in collaboration with ATC and KEK. Twopapers were published on the optical baffles, and one of them
was nominated as a monthly highlighted paper by the OpticalSociety of America (OSA).
(3) Mirror Characterization
We are also developing a system to accurately measure theoptical absorption of mirrors, which is a critical characteristic
for the cryogenic mirrors of KAGRA. The system was originallycapable of measuring samples of up to 2-inch diameter. We
are now upgrading the system to be able to produce scanned
absorption maps of KAGRA sized (22 cm diameter) mirrors.
We made calibration checks on sapphire bulk absorption using
different measurement methods in collaboration with LMA(Laboratoire des Matériaux Avancés) in Lyon.

2. R&D(1) R&D for upgrades of KAGRA
While building bKAGRA, the GWPO pursues researchand development to investigate and prepare future upgradesof KAGRA. In this context the TAMA infrastructure is being
used to develop frequency dependent squeezing, one of themost promising solutions to improve the sensitivity of detectors
like KAGRA that are limited by quantum noise. To thispurpose a 300-meter-long high-finesse cavity and a squeezed
vacuum source are being built. Thanks to this experiment weestablished collaborations and received students from abroad.
The absorption measurement bench developed to characterize
the KAGRA mirror is also used to study the performancesof crystalline coatings, a possible solution to reduce coating
thermal noise. Thermal noise investigation is also the objectiveof another experiment now starting at ATC and aiming at
the direct measurement of mirror thermal noise at cryogenic
temperatures. Finally, crackling noise is being investigated incollaboration with ICRR.
(2) DECIGO
In this fiscal year, the DECIGO working group compiled
the Pre-DECIGO project; its scientific objectives and targets
along with the conceptual design of the satellite were publishedin a summary paper. After that, Pre-DECIGO was renamed“B-DECIGO” for some reasons including an attempt to show itwill have sufficient sensitivity to detect gravitational waves witha meaningful event rate (and so not just a simple precursor of
DECIGO). Taking advantage of outcomes from LISA Pathfinder,
the working group started to define several subprojects (orexperiments) to show/enhance technical feasibility of a
B-DECIGO satellite; in the near future, the working group willpropose B-DECIGO to JAXA by summarizing those efforts.

University of Tokyo/ICRR. We also received a master student
from Beijing Normal University for six months and we had threevisits by a Ph.D. student from CNRS/APC for a total duration of
three months. Finally, two of the GWPO members taught at the
Department of Astronomy of the University of Tokyo, at Hosei
University, and at the Osaka City University.

4. Outreach
Since the first detection of the gravitational waves, the public
interest in GW has increased significantly. In order to better
share and promote our activities to the public, we have opened
a completely renewed website for our group with a modern
design. We also updated the leaflet of GWPO with professionalgraphics and design.
We organized a Workshop for Popularizing CuttingEdge Astronomy in Toyama and Kamioka to provide the latest
developments in astronomy with emphasis on the GW to highschool teachers, curators of scientific museums, and so on. In
addition to this workshop, the members of the GWPO gave morethan 10 public lectures and talks about the GW astronomy andwrote 3 articles for popular magazines as well as 1 web article
about the first detection of the GW in the FY 2016.
The TAMA and KAGRA sites continued to get attention
from various people. We accepted more than 200 visitors
for TAMA (excluding the open-day visitors) and the GWPO
members took care of more than 150 visitors to KAGRA.
Among them are journalists from National Geographic
Magazine, NHK, and so on.

5. International Collaboration and Visitors
The GWPO is a member of the KAGRA collaboration,a scientific collaboration which includes also members fromabroad. Apart from KAGRA, the GWPO has a collaboration
with CNRS, Beijing Normal University (BNU), the Universityof Hamburg, and University of Trento in the context of R&D
for future upgrades to KAGRA. In this framework we received
the visits of Prof. Zhu from BNU, Dr. Leonardi from Trento,and Dr. Tacca from CNRS. We also had several exchanges with
the Virgo collaboration with which one of the office members
is affiliated. We received short visits from Dr. Vocca and Dr.
Travasso (University of Perugia) and from Dr. Arai (Caltech). As
usual we received several visitors at TAMA including the MEXT
financial Director, a delegation from the ministry of Economy
and the ministry of Education, the association of students in
Mathematics and/or Physics and Astronomy at the University of
Amsterdam, and the Japan Scientific Instruments Association.

3. Education

6. Publications, Presentations, and Workshop
Organization

In FY 2016 the office included two PhD students and two
master students among its members. In addition we received
two undergraduate students under the SOKENDAI summer
students program and we hosted three graduate students from the

The members of the office have authored 32 peer reviewed
publications including the paper reporting about “GW151226:
Observation of Gravitational Waves from a 22-Solar-Mass
Binary Black Hole Coalescence” which received a lot of interest

II Status Reports of Research Activities093

in the scientific community and a paper about “Vacuum andcryogenic compatible black surface for large optical baffles inadvanced gravitational-wave telescopes” which was highlighted
by OSA. Moreover 16 presentations were given by the officemembers at international conferences.

7. Acquisition of external funds
GWPO did not receive external funds apart from thoserelated to 6 grants allocated by JSPS.

8. Staff
One assistant professor moved to another group of NAOJ
and a new position was opened in the GWPO. One JSPS postdoc
moved to a specially appointed assistant professor position and a
specially appointed specialist was hired. Overall in FY 2016 theproject included 1 professor, 1 associate professor, 8 researchstaff, 5 engineers, 3 administrative staff, and 4 graduate students.

094

II Status Reports of Research Activities10. TMT-J Project Office
The TMT Project is a project to build an extremely large
30-meter telescope under the collaboration of five partnercountries including Japan, the United States of America, Canada,
China, and India. Heading the project for NAOJ is the TMT-J
Project Office. In 2014, an agreement was executed between
the participating organizations, TMT International Observatory
was founded to assume the construction and operation of
the observatory, and construction was commenced. Japan is
responsible for the fabrication of the telescope primary mirror;
the design and fabrication of the telescope structure as well as
performing its onsite installation and adjustment; and the design
and production of science instruments.
Maunakea on Hawai`i is the planned construction site
for TMT. The approval process for the use of the land in the
Maunakea Conservation District for TMT has proceeded.
In Fiscal Year 2016, with onsite construction scheduled tocommence in April 2018, Japan proceeded with the mass
production of the telescope primary mirror segments,
detailed design of the telescope structure, and the design anddevelopment of the science instruments.
By the end of the fiscal year, 3 Professors, 4 Associate
Professors, 1 Chief Research Engineer, 1 Specially Appointed
Associate Professor, 1 Assistant Professor, 3 Specially Appointed
Senior Specialists, 1 Research Administrator Staff, 1 Special
Senior Specialist, 1 Research Expert, 1 Research Supporter,
3 Specially Appointed Research Staff, 2 Administrative
Supporters, and 1 RCUH Staff held full-time positions. In
addition, 1 Professor, 5 Associate Professors, 2 AssistantProfessors, and 1 Research Engineer primarily assigned to the
Advanced Technology Center, Subaru Telescope, and the RISE
Project have concurrent positions in the TMT-J Project Officeand take part in activities that include the development of TMT
science instruments at the Advanced Technology Center.

1. TMT Project Progress and Status of the
Hawai`i Construction Site
The construction of TMT is spearheaded by participating
countries and organizations under the TMT International
Observatory established in 2014. The current officiallyparticipating countries and organizations are the National
Institute of Natural Sciences (Japan), National Astronomical
Observatories of Chinese Academy of Sciences, Universityof California, California Institute of Technology, Departmentof Science and Technology of India, and National ResearchCouncil of Canada. The Association of Universities for Researchin Astronomy (AURA, USA), participating as an Associate
Member, is currently taking steps for the U.S. to eventually
become an official participant. TMT International Observatory,
operated according to deliberations and decisions made inquarterly Board meetings of the TMT Board of Governors, isoverseeing the construction work performed in each country as
well as developing the onsite infrastructure. The board meetings

Figure 1: Conceptual image of a constructed TMT.

are attended by 3 representatives from Japan.
In December 2015, as the protest movement at Maunakea
continued to gain momentum, the supreme court of Hawai`i
ruled the permit approval process for the use of the landin the Maunakea Conservation District, the site of planned
construction, to be flawed and consequently invalidated thepermit, although full-fledged construction at the summit of
Maunakea was expected to have commenced by April 2015. As
a result of the judgment, a review process for permit approval
was reopened by the State of Hawai`i in February 2016. After aperiod of preparation that included the appointment of a hearing
officer and approval of interested parties, hearings, which area particularly important step in the review process, were helda total of 44 times between October 2016 and March 2017. At
the conclusion of the hearings, a judgment regarding permit
approval is submitted by the hearing officer to the Hawai`i
Board of Land and Natural Resources where the final judgment
is expected to be made. The TMT-J Project Office, with efforts
that included actual attendance at the hearing, collected detailed
information about the approval process and the hearing in orderto prepare for conferences concerning the TMT International
Observatory. The year 2016 also brought a surge in support for
TMT construction in Hawai`i. The TMT-J Project Office put inits own effort as well to garner more understanding by holding
dialogues with local stakeholders.
In parallel with this process, the TMT International
Observatory initiated a selection process for a backup
construction site in case construction at Maunakea becomes
impossible. Candidate sites included Spain, Mexico, China,
India, and 2 locations in Chile for a total of 6 locations. The
criteria for consideration included favorable conditions forscience observation, as well as the availability of the site forconstruction to commence by April 2018. Based on thesecriteria, TMT International Observatory selected La Palma in the
Canary Islands as the backup construction site. Japan, as part ofthis process, held meetings in 5 locations (Sendai, Tokyo, Kyoto,
Hiroshima, and Hilo) to explain the current situation in Hawai`iand to evaluate the alternate candidate construction sites. At
the GOPIRA (Group of Optical and Infrared Astronomers)
Symposium, the issue was deliberated and votes were cast by

II Status Reports of Research Activities095affiliated researchers for the selection of a backup site. Based on
the result of this process, Japan came to agree with the selectionof La Palma as the backup construction site.

2. Japan’s Progress on Its Work Share – theTelescope Structure, the Primary Mirror, andScience Instruments
For the construction of TMT, Japan is leading the design/
fabrication of the telescope structure and a portion of thefabrication of the primary mirror and science instruments. In
Fiscal Year 2016, the following progress was made.
(1) Fabrication of the mirror segments of the primary mirror
The TMT primary mirror is comprised of 492 mirror
segments. With replacements included, a total of 574 mirror
segments must be fabricated. The processes required in the
fabrication of mirror segments are: fabrication of the mirror
blanks, spherical grinding of the front and back surfaces,
aspherical grinding and polishing of the front surface,machining, and mounting of the mirror segments onto a
support assembly. These processes are followed by final surface
finish completed in the U.S. and coating with reflective metal
performed onsite before the mirror segments are finally installedon the telescope.
Of these processes, the plan calls for Japan to fabricate
the mirror blanks and to perform spherical grinding on all 574
segment mirrors. In Fiscal Year 2016, 49 mirror blanks were
fabricated and spherical grinding was completed on 60 mirror
blanks. With the share of work for the processes beginningfrom aspherical grinding/polishing and ending with mounting
the mirror segment on a support assembly distributed among 4
countries, the plan calls for Japan to be leading this work for 175of the mirror segments. In Fiscal Year 2016, ashperical grinding
was performed on 8 mirror segments and 5 were ashpericallypolished. In addition, with the U.S. scheduled to begin theirshare of work to make the mirror segments aspherical, shipmentof spherical mirror blanks to the U.S. was commenced.

Figure 2: Mirror segment blanks which have started to be shipped
overseas (Courtesy of Canon Inc.)

096

II Status Reports of Research Activities(2) Design of the telescope structure and its control system
Japan is leading the design and production of the telescope
structure which functions as the mount for the science
instruments and optics systems, including the primary mirror,
and points them in the direction of a target astronomical object.
Work on the detailed design of the telescope structure wasinitiated in Fiscal Year 2014 using the baseline design received
in Fiscal Year 2013. In continuation of the 3 international
reviews conducted by Fiscal Year 2015, an international review
was conducted for the Segment Handling System, Aerial Service
Platform, and Elevator in Fiscal Year 2016. With the completionof these reviews, the detailed design of the telescope structure
was completed.
(3) Science instruments
As part of the international collaboration, Japan is leading
the fabricating for a portion of 2 out of the 3 first-light science
instruments.
The Infrared Imaging Spectrometer (IRIS), for which Japanis assigned the task of creating its imaging components, iscurrently in the preliminary design phase. In Fiscal Year 2016,
the first preliminary design review was conducted for IRIS withthe focus primarily on its optics and mechanics. Preparation
work was performed to be ready for the final review of thepreliminary design, scheduled for the next fiscal year, which will
cover electronics, software, schedule, budget requirement, andissues indicated in the first review that require further study.
For the Wide Field Optical Spectrometer (WFOS), itsconceptual study is underway with Japan expected to take thelead on its camera system. In Fiscal Year 2016, design work forthe optics of the camera system was performed, and material
quality and polishing were studied for the optical elements
considered for selection.

3. Evaluation of Scientific Research by TMT
and Public Relations Activities
In 2016, the TMT Science Forum, held once a year since2013, was convened in Japan. This forum is a gathering todiscuss topics such as scientific research, science instrument
development, and the operation plan for the TMT. For the last
3 years, the forum was held in the U.S. with an important goalof developing a cooperative relationship with U.S. scientists for
the TMT Project with funding from the U.S. National Science
Foundation. This was the first time the TMT Forum was held
outside of the U.S. It was held in Kyoto from May 24 to 26 andwas attended by 140 participants who actively deliberated on
topics including 2nd generation science instruments.
The study of scientific research for TMT was facilitatedwith the Science Advisory Committee of TMT International
Observatory leading the way. Japan also made important
contributions through its continued participation in theInternational Science Development Teams (ISDTs) establishedin 2013.
In Japan, continued effort has been made for the project
to better reflect the opinions of the science communitycommunicated through forums such as the TMT-J Science
Advisory Committee. In Fiscal Year 2016, the effect of moving
the construction site elsewhere, particularly on scientificresearch and observatory operation, was evaluated through theaforementioned backup construction site candidate selection
process. Also, with the continuation of the strategic fundamental
research fund for the purpose of fundamental technology
research for the development and design of 2nd generation
science instruments, support funding for development was madeavailable and provided to 6 universities and other institutions
that applied to the public offering for the funding support.
Information on the TMT Project is provided in the TMT-J
Project Office website, including updates particularly regarding
the situation at the Maunakea construction site and the work
share progress made by Japan. Additionally, TMT Newsletters
No.46 through 50 were delivered. Efforts were made in public
relation through lectures held in various areas throughout Japanand exhibits at the National Institutes of Natural Sciences
Symposium and Inter-University Research Institute Symposium.
Approximately 50 lectures and requested classes were held forthe public.
Contributions were also made by making available an ondemand lecturer for the science/technology education and public
outreach event “Journey through the Universe” (March 2016)
held in Hawai`i where TMT is to be constructed.
TMT also assembled an international team that includes
Japan to study topics such as education and personnel training,
and as part of this project. In December, an international
workshop was held in Hilo, Hawai`i catering to the young
researchers and engineers that will lead the next generation.
40 graduate students and young researchers, that include 6
participants from Japan, learned about a wide range of topics
that encompassed not only scientific research and development,
but also international cooperation with people of different
cultural backgrounds and management and operation of large
scale projects.
Donations to the TMT Project have been raised continually;
2 corporations and 302 individuals provided donations in 2016
(from January to December).

Figure 3: TMT Science Forum in Kyoto.

II Status Reports of Research Activities097

11. JASMINE Project Office
1. Planning and Development of the JASMINE(Japan Astrometry Satellite Mission for
Infrared Exploration) Project(1) Overview
The JASMINE mission seeks to survey virtually the entire
20° × 10° Galactic Bulge around the center of the Galaxy andto perform infrared (Kw-band: 1.5–2.5 μm) measurements of
the annual parallaxes, proper motions, and celestial coordinatesof the stars at a high precision of 1/100,000 arcsecond (10 μas)
in order to determine with high reliability the distances andtransverse velocities of stars within approximately 10 kpc
of the Earth in the surveyed direction. Nearly 1 million stars
can be measured with a high precision in the Galactic Bulge
with a relative error for annual parallaxes less than 10 %. Thisis necessary for accurate distance determination. By using
observational data to construct a phase space distribution ofgravitational matter, astrometric surveys of the bulge of the
Milky Way promise to make major scientific breakthroughs in
our understanding of the structure of galactic bulges and thecauses of their formation; the history of star formation withinbulges; and the co-evolution of bulges and supermassive
black holes, which is closely related to the aforementioned
phenomena.
Prior to commencement of the JASMINE mid-sized scientificsatellite project, an ultra-small size project and a small size
project were implemented to progressively build up scientificresults and to accumulate the necessary technical knowledge andexpertise. The Nano-JASMINE micro-satellite project, with a
primary mirror aperture of 5 cm is currently underway. It aims
to test part of the technologies to be used in JASMINE and to
produce scientific results based on the astrometric information
for bright objects in nearby space. Despite its small aperture,
the satellite is capable of observational precision comparable to
the Hipparcos satellite. The combination of observational datafrom Nano-JASMINE and the Hipparcos Catalogue is expected
to produce more precise data on proper motions and annual
parallaxes. The satellite is scheduled for launch in the near
future. An additional plan is underway to launch a small-scale
JASMINE satellite (Small-JASMINE), with a primary mirror
aperture of about 30 cm, in FY 2022. This satellite will engage
in observations of a limited area around the nuclear bulge andcertain specific astronomical objects. This small-sized version
has the goal of obtaining advanced scientific results at an earlystage. The mid-sized JASMINE satellite, with a main apertureof approximately 80 cm, is designed for surveying the entire
bulge and is targeted for launch in the 2030’s. Internationally,
Japan shares responsibilities with ESA. With the Gaia Project,
ESA performs visible-light observation of the entire sky at a
precision of 10 μas, while Japan engages in infrared observationof the bulge, which is a method suitable for observations in the
direction of the Galactic Center.

098

II Status Reports of Research Activities(2) Major Progress in FY 20161) Organization of the Office
The JASMINE Project Office is composed of five full-time
staff members, six staff members with concurrent posts, one
research associate, one technical associate, and three graduate
students. Significant contributions were made by membersof the following organizations: Kyoto University’s Graduate
School of Science; ISAS at JAXA; the University of Tokyo’s
School of Engineering; Tokyo University of Marine Scienceand Technology; the University of Tsukuba; and the Institute of
Statistical Mathematics.
2) Progress of the Nano-JASMINE Project
The project will engage in spaceborne observations using
an ultra-small satellite to accomplish the following objectives:to make Japan’s first foray into space astrometry; to accumulate
the technical experience in onboard data acquisition, and thelike, necessary for the upcoming JASMINE project; to achievescientific results in the study of dynamical structures in thevicinity of the Solar System; and to analyze star formation basedon stellar motions in star formation regions.
The satellite was scheduled to be launched from a Brazilian
launch site operated by Alcantara Cyclone Space using a
Cyclone-4 rocket built by Yuzhnoye, a Ukrainian rocket
developer. The launch has been impossible due to the adverse
influence of international situations. On the other hand, we now
have the possibility that the Europena Space Agency (ESA)
can launch the Nano-JASMINE satellite, as well as anotherpossibility for the launch. We are now negotiating for the launch.
Assembly of the flight model that will actually be launched into
space was completed in FY 2010. The extra time yielded by
the launch delay has been used for additional testing to further
ensure project success. Maintenance of the satellite has also been
performed. Steady progress was also made in the developmentof the algorithms and software required to determine astrometric
information from raw observational data at the required level ofprecision. International cooperation with the data analysis teamfor the Gaia Project has been conducted smoothly. A Japanese
WG led by Ryoichi Nishi of Niigata University continued
to actively engage in investigating the scientific results to beobtained in the future by Nano-JASMINE.
3) Overview of Planning and Developing the Small-JASMINE
Project
The objective of the small-sized JASMINE project is to usea three-mirror optical system telescope with a primary mirror
aperture of 30 cm to perform infrared astrometric observations(Hw band: 1.1–1.7 μm). A goal is to measure annual parallaxes
at a precision of less than or equal to 20 μas and proper motions,or transverse angular velocities across the celestial sphere, at a
precision of less than or equal to 50 μas/year in the direction ofan area of a few degrees around the Galactic Center within thebulge and in the directions of a number of specific astronomical
objects of interest in order to create a catalogue of the positions
and movements of stars within these regions. The project is
unique in that unlike the Gaia Project, the same astronomical
object can be observed frequently and observation will be
performed in the near-infrared band, in which the effect ofabsorption by dust is weak. This project will help to achieve
revolutionary breakthroughs in astronomy and basic physics,
including the formation history of the superrmassive black holeat the Galactic Center; the gravitational field in the Galactic
Nuclear Bulge and the activity around the Galactic Center; theorbital elements of X-ray binary stars and the identification of
the compact object in an X-ray binary; the physics of fixed stars;
star formation; planetary systems; and gravitational lensing.
Such data will allow for the compilation of a more meaningful
catalog when combined with data from terrestrial observationsof the line-of-sight velocities and chemical compositions ofstars in the bulge. Conceptual planning and design of the
Small-JASMINE satellite system and detailed planning of thesubsystems began in November 2008 with cooperation fromnearly 10 engineers from JAXA’s SE Office (the Systems
Engineering Office), ARD (Aerospace R&D Directorate),and ISAS with a focus on the satellite’s vital elements such as
thermal structure, attitude control, and orbit.
Against this background, in-house discussions andmanufacturers’ propositions, which started in 2009, had continued
to consider the design of the satellite system to ascertain the target
precision in astrometric measurement as a general objective. The
SWG, led by Masayuki Umemura of the University of Tsukuba
and including volunteers from diverse fields in Japan, continued
to make scientific considerations. Other activities such asconceptual planning, design, technical testing, and international
project collaboration have been continued.
International partnerships to gain further understanding of
the Galactic Bulge have been formed with multiple overseas
groups engaging in terrestrial high-dispersion spectroscopic
observation to determine the line-of-sight velocities andchemical compositions for bulge stars. In particular, Steven
Majewski of the University of Virginia, the principal
investigator (PI) of the US Apache Point Observatory (APO)
Galactic Evolution Experiment (APOGEE) Project, offered ajoint proposal for the APOGEE-2 project as an extension of theoriginal APOGEE project to engage in bulge observations in thesouthern hemisphere because the project is suitable for bulge
observations. The telescope employed will be equipped with ahigh-dispersion spectroscope, identical to that of APOGEE. The
joint proposal has been submitted. An official memorandum of
understanding has been exchanged among the APOGEE-2 team,members of the fourth Sloan Digital Sky Survey (SDSS-IV)
Collaboration, and Small-JASMINE to strengthen international
partnerships and to achieve scientific goals related to the
Galactic Bulge.
As planning has progressed so far, the full mission proposal
was prepared and submitted in January 2016 to the ISAS call forsmall-sized scientific satellite mission proposals and the SmallJASMINE mission is going through the ISAS selection process.

II Status Reports of Research Activities099

12. Extra-Solar Planet Detection Project Office (Exoplanet Project Office, EPO)
The Extra-Solar Planet Detection Project Office cooperates
with researchers interested in extra-solar planet at various
universities, centered around NAOJ to promote the developmentof overall technologies and organize related observations withthe goal of observing exoplanets and their formation sites.
We conduct observational instrument development, researchpromotion, mission planning, and R&D to develop common
basic technologies. We also promote international partnerships
related to exoplanets, which are the focus of this project office.
Specifically, research and development have continued centeredaround the following 4 themes:(1) The development/maintenance/operation of high-contrast
observational instruments using the Subaru Telescope
to directly observe exoplanets: HiCIAO, SCExAO, and
CHARIS; and the promotion of the SEEDS survey and postSEEDS projects.
(2) The development of the new IR Doppler instrument IRD andplanning its observations.
(3) The development of the high-contrast instrument TMT/SEIT,and promoting technological review and related international
collaborations for the WFIRST/CGI, and HabEx missions.
(4) Research into star and planet formation and the interstellar
medium through wide field-of-view polarimetric imaging
with the IRSF telescope located in South Africa.
This project office is progressively dissolving and moving to
the Astrobiology Center. There have been 42 refereed papers in
English, 10 non-refereed papers in English, 13 presentations inEnglish, 5 non-refereed papers in Japanese, 3 books in Japanese,and 39 presentations in Japanese.

1. Development of the Subaru next generation
exoplanet instruments and exoplanet
observational research(1) HiCIAO (High Contrast Instrument for the Subaru Next
Generation Adaptive Optics)
HiCIAO is a coronagraph camera for direct imaging
of exoplanets and circumstellar disks for the 8.2-m Subaru
Telescope, which can simultaneously utilize various imaging
modes to differentiate by polarizations, multi-bands, andangle. It is a high-contrast, modular instrument. The first
Subaru Strategic Program SEEDS (Strategic Explorationsof Exoplanets and Disks with Subaru) with more than 100
participants continued from October 2009 to January 2015
without any serious troubles. Currently, we are continuing withthe development, maintenance and use of the extreme adaptive
optics instrument SCExAO and the CHARIS integral field unit
(IFU) as post-SEEDS activities.
(2) IRD (Infrared Doppler Instrument)
IRD is a high precision (~1 m/s) radial velocity spectrometerworking at near-infrared wavelengths, whose aim is to100

II Status Reports of Research Activities

detect habitable Earth-like planets around M dwarfs andbrown dwarfs. The budget is based on JSPS Grant-in-Aid forSpecially Promoted Research FY 2010–2014 (PI: Motohide
Tamura). Spectrograph, fiber experiments, laser frequency
comb completion, and total assemble were conducted. Science
discussions on habitable planets around M dwarfs are also
proceeding.
(3) SCExAO (Subaru Coronagraphic Extreme Adaptive Optics)
and CHARIS IFU
SCExAO is a 2000 element extreme adaptive optics
system. CHARIS IFU is an exoplanet observation instrument
for spectroscopy of giant exoplanets. EPO has been involvedin the development of these next-generation high-contrast
instrumentations.

2. Exoplanet instrument development for
future space and ground-based telescopes andinternational collaborations(1) WFIRST Coronagraph and HabEx (Habitable Planet Explorer)
These missions aim to directly image and characterize theEarth-like planets and super-Earths for signatures of life. As amember of the WACO working group (now the WFIRST WG),a coronagraph performance test at the JPL testbed is being
conducted with collaborators.
(2) SEIT (Second Earth Imager for TMT)The aim of this project is the direct imaging andcharacterization with the SEIT instrument on the Thirty Meter
Telescope (TMT). Both technical and science discussions are
made. The components have been considered and conceptual
design is proceeding.

3. Science research, education, and outreach
The SEEDS project successfully finished in January 2015
without any major troubles. Now we are expanding observations
using SCExAO and CHARIS. This fiscal year, 14 papers were
published on SEEDS alone. Highlights are given below.
SEEDS has discovered spiral arms in the disk of LkHα330
and revealed the distribution of large/small dust in them.
High-contrast direct imaging of intermediate-mass giants has
discovered 3 companions that cause long-term radial velocity
trends and set upper limits on any companions around 2 stars.
A comprehensive direct imaging survey of young (< 1 Myrs)
stars using the SEEDS data has indicated the frequency of wideorbit giant planets. A new companion brown dwarf has been
discovered in the Pleiades cluster.
About ten graduate students are supervised for exoplanetsand related topics. Many public talks, publication, and press
releases are made on exoplanets, disks, and other astronomical
fields.

Figure 1: HiCIAO high contrast imaging of intermediate-mass giants with long-term radial velocity trends. Central stars are within the white regions, while
the dots in circles are the newly discovered companions. Observing wavelength is near-infrared.

II Status Reports of Research Activities10113. RISE (Research of Interior Structure and Evolution of Solar System Bodies) Project Office
1. Project Overview
In FY 2016, operation preparation for the Laser Altimeter(LIDAR) of Hayabusa2 was carried out. And, a thermal test of
the APD detector of the Ganymede Laser Altimeter (GALA)
for the Jupiter Icy Moon Explorer (JUICE) mission was made.
Also the RISE Project Office proposed four option plans as
future directions for planetary sciences within NAOJ. The
Hayabusa2 asteroid explorer was launched on December 3,
2014; initial test operations finished in January; and Hayabusa2
is underway to C-type asteroid Ryugu. Before rendezvous withthe target asteroid start in the summer of 2018, the RISE Project
Office developed a scientific data production/analysis tool as apreparation necessary for operation of the laser altimeter. The
tool has been implemented, however a test using simulated
data has not been completed due to a delay in the Hayabusa2
project supplying the simulated data. For GALA, the RISE
Project Office members intensively tested an APD to confirm its
suitable temperature range, and acquired basic data for GALA
development. As for future directions for planetary science, theRISE Project Office held discussions and proposed 4 options
to the Planetary Science Subcommittee: (1) Lunar deep interior
exploration, (2) Small body studies, (3) Oscillation of planetaryatmospheres, and (4) Cosmo-hydrology. For lunar deep interior
exploration, we investigated the merits of 3 observational
methods to measure the lunar Q value and the size of the solid/
liquid core with high accuracy using lunar surface observation
instruments by making the most of the heritage of Kaguya
and the Geodetic research of RISE. For small body studies,
we considered research into the evolution of primitive Solar
System bodies and the delivery of water to the inner planets
by investigating main belt comets (MBC) with ground-based
observations and space probes by using the ongoing MartianMoon Explorer mission as a springboard. In the oscillationof planetary atmospheres, we are fostering the possibility ofcollaborative observations between France, Tokyo Institute ofTechnology, and NAOJ to measure Jupituer’s free oscillation.
For cosmo-hydrology we promoted Solar System bodies
research within NAOJ based on a long-term vision of planetaryscience activity in NAOJ.

2. Educational Activities/Internship
Seven RISE members delivered 18 lectures on a part-timebasis to graduate students at the University of Aizu. Also the
Office accepted four third-year undergraduate students of Iwate
University and Iwate Prefectual University for a week.

3. Outreach/PRIn FY 2016, one of the Office members volunteered for
the Kirari Oshu Astronomy class of Oshu City. Three members
participated in the 4D2U Astronomer’s Talks; lectures were102

II Status Reports of Research Activities

given 3 times. And 4 members participated in Fureai (Friendly)
Astronomy classes 6 times. One member was sent to the open
campus of VERA Ogasawara station to provide an introduction
to the research and 2 mini-lectures. Members also gave
public presentations at Anan City Science Center and Mitaka
Astronomy Pub.

4. Joint Research/International Collaborations
From Russia, Professor Alexander Gusev and Ms. Ekaterina
Kronrod visited the Office for three months and two months,
respectively, for joint research on thermo-mineralogicalmodeling of the lunar interior and future lunar and planetary
explorations. Jointly with The People’s Republic of China andthe Republic of Korea, the Offi ce member held a summer
school for planetary science and exploration in East Asia in
June in Wuhan City, China. Five Japanese graduate students
participated in the summer school to promote international
exchange of young scientists.

5. Career Development
One research staff member left the RISE Project Office in
September as his term ended. To fill this vacancy, the Officeopened an announcement of a job opportunity. The retired
research staff member is now employed as a specially appointed
associate professor at Aizu University.

14. Solar-C Project Office
The SOLAR-C Project Office has engaged in planning thenext solar observation satellite project SOLAR-C, promoting thesounding rocket experiment CLASP (the Chromospheric LymanAlpha SpectroPolarimeter), and also preparing for participationin the large balloon-borne experiment Sunrise3. In addition, theactivity for participation in the U.S. sounding rocket experiment
FOXSI3 has started since Fiscal Year (FY) 2016.

1. SOLAR-C Project
SOLAR-C is a planned project and may become Japan’s
fourth solar observation satellite, after Hinotori, Yohkoh, andHinode. The plan is to realize the launch in the latter half of the2020’s. The project is intended to investigate the solar magnetic
plasma activities that influence space weather and space climate
around the Earth. The investigations involve the measurementof magnetic fields in the chromosphere and high-resolution
imaging/spectroscopic observations that have not been achieved
to date. The themes include major problems in solar research: theheating mechanism of the chromosphere/corona, the origin ofsolar explosive events, and the mechanism of the solar magnetic
activity cycle. Since its establishment, the SOLAR-C project
WG has involved many non-Japanese specialists in addition to
Japanese researchers. Provisionally, Japan will be responsible
for the launch vehicle and satellite; and the science instruments
will be developed through the international collaborations with
the U.S. and European space agencies and institutions.

2. Small-sized Project(1) CLASP Project
The CLASP project is an observational sounding rocket
experiment aiming to detect solar magnetic fields in thechromosphere and transition region through polarization
observation at the far ultraviolet wavelengths. Planning andbasic development started in FY 2009. The project involves aninternational research team with participation from Japan, theU.S., and other countries. The spectropolarimeter was preparedin Japan with components provided by the U.S. and France,
and an American sounding rocket is used for the flight. The
CLASP project entered the development stage fully in the latter
half of FY 2012 and carried out the first flight experiment in
Sep 2015. The second flight experiment is scheduled for 2019
and will change the observed spectral line from H Lyα to thechromospheric Mg II line at 280 nm.
(2) Sunrise3 Project
The Sunrise3 project is the third balloon-borne experimentin the German Sunrise program. The preparation of the plan
started in FY 2015 for the flight experiment scheduled in 2020.
Under the international collaboration, the Japanese team will
jointly develop a high-resolution spectropolarimeter that isequivalent to the science instrument planned in SOLAR-C. The

project will tackle the development demonstration of a state-ofthe–art remote-sensing instrument and the challenges to frontline science studies ahead of the satellite observations.
(3) FOXSI3 Project
The FOXSI3 project is the approved third observationalsounding rocket experiment in the US FOXSI program withfocusing hard X-ray telescopes. One of the hard X-ray detectors
is to be replaced by the high-speed CMOS camera that wasdeveloped by the Japanese team for soft X-ray coronal imaging
spectroscopy. The soft X-ray energy spectrum is to be obtainedat each CMOS imaging pixel by photon counting.

3. Major Activity in FY 2016
The SOLAR-C proposal, which was submitted to JAXA in
Feb 2015, was not selected in the mission definition review as
the candidate for the 1st JAXA Strategic Middle-class Satellite
Mission. The SOLAR-C WG is refining the science objectives,
investigating the possibility of reducing the diameter of the large
optical telescope, and rebuilding the international collaboration
framework. In terms of the international collaboration, thescience objectives team for the next generation solar physics
mission, which has been formed at the request of the space
agencies JAXA, NASA, and ESA, has started to prioritize thepotential JAXA-led solar physics missions for launch in the
mid-2020’s.
While publishing the first science results from the flight
experiment in September 2015, the CLASP project has been
preparing for the second flight experiment. The proposal forthe second flight has been approved by NASA during FY
2016, and the next flight is scheduled for 2019. We are now
preparing for the flight. The Sunrise3 proposal to a German
funding agency has also been approved in this fiscal year, andthe Japanese team has submitted funding proposals to obtain thedevelopment funds. The team has defined the Sunrise3 sciencecases, and the basic optical design has been carried out tosatisfy the requirements. The FOXSI3 project has conducted thedevelopment of a high-speed CMOS camera and carried out thetest production of a 3D printed alloyed titanium optical baffle
for the stray light reduction.

4. Others
Although the SOLAR-C Project Office is reimbursed by
NAOJ for its general operation and emergencies, a large partof the expenses for supporting the project preparation is fundedby other sources including the Grant-in-Aid for Scientific
Research, JAXA’s strategic R&D fund for basic development
and experiments for onboard instruments, and research grants
from the private sector.
Dr. D. Song has been appointed as a Project Research
Fellow since January 2017.

II Status Reports of Research Activities10315. Astronomy Data Center
1. Introduction
The Astronomy Data Center (ADC), a central core ofcomputing and archiving for astronomical data, supports
scientists worldwide by providing a variety of data center
services. In addition, ADC is driving forward research anddevelopment programs for future generations of service.
Our activities consist of the DB/DA Project, Network
Project, JVO Project, HSC Data Analysis/Archiving Software
Development Project, and open-use computer system andservice.

2. DB/DA Project
The DB/DA-project conducts research and development
on astronomical Data Bases and Data Analysis. It also opens
various astronomical data to researchers and educators (http://
dbc.nao.ac.jp/).
SMOKA (http://smoka.nao.ac.jp/) is the core of the DB/
DA-project and provides archival data of Subaru Telescope,
OAO 188-cm Telescope, Kiso 105-cm Schmidt Telescope (theUniversity of Tokyo), MITSuME 50-cm Telescopes (Tokyo
Institute of Technology), and KANATA 150-cm Telescope(Hiroshima University). The total amount of opened data is
about 17 million frames (119 TB) as of May 2017. SMOKA
contributes to many astronomical products. The total number ofrefereed papers using SMOKA data is 203 as of May 2017.
Continuing from the previous year, in FY 2016, we
improved the system for improved operational efficiency and forthe development of SMOKA’s advanced retrieval functions (i.e.
supernova retrieval). In addition, the first Subaru Telescope HSC
SSP data release (observations up through November 19, 2015,
a total of 850,000 frames) was opened to the public in March2017.
As of May 2017, we are preparing the design of a newcomputer system scheduled to begin operation in March 2018
and examining the options for program and data transfer.

3. Network Project
The Network Project designs and operates NAOJ
information network infrastructure for the Mitaka Headquarters
and branch offices. Noteworthy topics of this fiscal year are as
follows.
1) Upgrading the Wide Area Network service: We have operated
the circuit service between Mizusawa and Sendai since 2015.
In 2016, the service bandwidth has been upgraded from 40
Gbps to 80 Gbps. Also, we made a 100 Gbps interconnection
between NAOJ and SINET operated by NII: National
Institute of Informatics.
2) Use of the 100 Gbps Transpac line to the U.S.A.: NAOJ andthe WIDE project are jointly operating the Transpac, the
US-JAPAN Academic research and education network. The

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II Status Reports of Research Activities

Transpac has 100 Gbps bandwidth of circuits between Tokyoand Seattle. In 2016, SINET, JGN, and Univ. of HAWAII
submitted applications to use this circuit. Also throughcooperation with the Univ. of HAWAII it became possible toextended the circuit from Seattle to the UH Hilo campus.
3) The Traffic analyzer system was installed: This system canmirror the inbound and outbound internet traffic based on
the filter rule conditions. We can make the information andnetwork security enforcement more cost efficient.

4. JVO Project
A new version of the JVO portal (v2), for which the usabilityof the user interface was greatly improved, was released. ALMAWebQL, a quick-look application for ALMA data, was updated.
The feature to query to the atomic/molecular line database was
implemented, which enables a user to see the line information
just below the spectrum data. The features to display thespectrum data in the rest frame of the target source and toselect the color map to be used for drawing an image were also
implemented.
A Gaia data search service was released. In comparison to
the data search service operated by the Gaia project, our systemprovides a more user-friendly GUI and also enables a user tosearch large amounts of data without a limit on the number ofsearch result.
A test version of Subaru WebQL was developed andreleased. This web application enables a user to adjust thecontrast of images so that they can examine the data for not only
bright sources but also for dim diffuse sources.
Total number of access counts to the JVO services was 3.6
million and a total of 1 TB was downloaded in the 2016 fiscal
year.

5. Project for HSC Data Analysis/Archiving
Software Development
This project started in January 2009, primarily to develop
the data analysis pipeline and data archiving software for Hyper
Suprime-Cam (HSC). Our main effort is concentrated on theimplementation of the software for effective data analysis/archiving by parallel and distributed processing, for the sake of
precise photometric and astrometric calibrations, by correcting
various effects originated from the camera system.
Since March 2014, the Subaru Strategic Program (SSP) with
HSC has been undertaken, producing stable large data output(about 300–400 GB per night). We preformed data analysis of
the SSP data, produced a database storing the processed results,
and made an internal data releases in August 2016 to the SSP
team collaborators. The image products involve 2.6 million
files and their total size reached about 200 TB. The catalog
database stores about 300 million objects in a 15 TB databasevolume. We have developed various user interface software forgetting image or catalog products using the database throughweb browsers, and many of these functions have been offered tocollaborators. The hardware and software for the data releases
are in stable operation. In February 2017, we made the firstworld-wide Public Data Release (PDR) based on the data set
that was distributed among the SSP collaborators in late January
2016. We have approximately 300 registered users, including
individuals from various institutes in about 25 countries. No
apparent major problems in the PDR have been reported to date.
The PDR is expected to greatly promote scientific outcomes.
Major problems in the pipeline software have been significantly
reduced, although further improvements to functions are stillnecessary to achieve the planned accuracies for calibrations/
measurements of celestial objects in the images. The on-site data
analysis system being developed since 2011 has been supporting
SSP and general observations by providing observing tools
such as an observation log viewer, which is used to monitor thedata analysis results through a web browser. This system has
been contributing much to the smooth operation of the Subaru
Telescope.

7. Others
As part of outreach and promotions activities, 97 issues of“ADC News” were published from No. 483 to No. 579 in FY
2016. The news was distributed by E-mail to users and appearedon the ADC web pages.

6. Open-use computer system and service
The new rental open-use computer system, “National
Astronomical Observatory of Japan: Data analysis, archive,
and service system,” has been in operation since March
2013. The system plays a leading role as part of the InterUniversity Research Institute. The system consists of “MultiWavelength data analysis subsystem”, “Large data archiveand service subsystem” (MASTARS, SMOKA, HSC science,
ALMA, VERA, NRO, Okayama and Catalog archive service),“JVO subsystem”, “Solar data archive, analysis and service
subsystem”, “Data analysis subsystem in Mizusawa Campus”,
and “Development subsystem”. The total storage, memory andnumber of CPU cores within the system are about 6 PB, 13
TB and 2000 cores, respectively. In FY 2016, the total numberof valid users was 364 (including 55 users from overseas
institutes). We are working to replace the rental computer systemin the current year.
In the course of the Inter-University Research we also heldand supported some workshops on using software and systems.
The dates and numbers of participants in FY 2016 were as
follows.
1. HSC-SSP Database school, Apr 11, 2016, 21 users
2. HSC imaging analysis school, Jul 20–21, 2016, 15 users
3. IDL School for FITS data analysis, Aug 2–3, 2016, 12 users
4. SOKENDAI summer student program (Support), Aug 7–31,
2016, 4 users
5. Autumn school “Approach from theory and observation: thecharacter and distribution of the dark matter” (Support), Nov
10–11, 2016, 10 users (analysis workshop)
6. SQL school in FY 2016, Dec 13–14, 2016, 5 users
7. N-body simulation school, Feb 8–10, 2017, 12 users
8. IDL School for the beginner, Feb 28–Mar 1, 2017, 4 users
The total number of participants of the schools in FY 2016
was 83 users.

II Status Reports of Research Activities10516. Advanced Technology Center (ATC)
1. Organization and Summary of Activities in ATC
At the Advanced Technology Center (ATC), we are working
on the development of astronomical observation equipment thatis requested and to be used in the projects driven forward by
the National Astronomical Observatory of Japan as “priority
area development” and development research contributing
to the future astronomical projects as “advanced technology
development.”
Furthermore, from this fiscal year, we have set up a new
R&D framework called “Basic Technology Development,”
which does not belong to either of the categories “priority
area development” or “advanced technology development.”
These research and development themes shall have a time
limit of two years. At the same time, the Advisory Committee
for ATC discusses the approach to research and development
issues to be tackled at the ATC; in particular, clarifying thedirectives for selecting the themes for “advanced technology
development” as well as how to approach them and making
guidelines for organizational building and restructuring “basic
technology development” projects.
For ALMA receivers (Bands 4, 8, 10), whose development
we have been supporting with the highest priority, shipping
was completed in FY 2013 (by March 2014), and then wereformed our organizational structure. From October 2014 we
moved to the new organizational structure and carried out not
only maintaining the ALMA receivers but also promoting the
research, development, and future upgrades to the receivers
as well as receivers to be installed on the 45-m reflector and
ASTE telescope. Under this organization structure in FY
2016, we have performed ALMA receiver troubleshooting andupgraded the FOREST receiver mounted on the Nobeyama
45-m telescope. In addition, we conducted a commissioning
observation with the radio camera on the ASTE telescope ledby the radio camera development group that joined ATC lastyear.
As high priority areas of development, the observation
instruments IRIS and WFOS were developed for TMT and thevibration damping, vibration isolator, mirror holders, etc. weresuccessfully developed for the gravitational wave telescope
KAGRA.
In the development of IRIS in FY 2016, we have moved
forward with the basic design phase (Preliminary designphase). We specified the interface conditions of the IRIS
imaging system to be handled by NAOJ/ATC, completed thebasic optical and opto-mechanical design and passed throughthe intermediate review (Preliminary Design Review 1, PDR- 1) in November 2016. Starting in December 2016, we havebeen making basic designs for electrical systems and software,cost estimates, and the schedule for the final design andmanufacturing phases.
We have been studying the concept of a camera system for
WFOS, a wide field-of-view multi-object spectroscope, which106

II Status Reports of Research Activities

is another TMT first generation observational instrument. We
have continued the concept review of the camera system in FY
2016.
In particular, mainly led by optical engineers at ATC,
we redesigned the optical system, analyzed stray light due tospecification changes, pointed out the problem of vignettingin the lens system when polycrystalline fluorite was adopted,
and then showed the effect on imaging performance and thenecessity of measures against stray light within WFOS.
For the KAGRA auxiliary optics, we designed the opticaltransmission monitoring system (TMS) and made some
prototypes last year. In April 2016, the test operation of theinitial phase of KAGRA (iKAGRA) was completed. Since
manufacturing and testing of almost all of the vibration
isolators used in the room temperature part of K AGR A
involved in the final design were mostly made by the ME shop
at ATC, we are proud that ATC is making a big contribution
to the success of KAGRA’s trial operation. This fiscal year,
continuing from the last fiscal year, we carried out assemblyof anti-vibration filters and pre-shipment tests in collaboration
with the project office. In addition, we proceeded with thedesign of the vibration isolation system of the wide-angle
scattering baffles to be installed in the immediate vicinity of
the cooling mirror.
For advanced technology development, the main themes ofresearch and development are “CLASP, Solar-C”, “Telescope
Receiver Development”, and “HSC”.
The CLASP observation rocket experiment is a pioneering
project of the solar magnetic field observation of the Sun in thefar ultraviolet region. After succeeding in the first experimentcarried out in September 2015, we have been preparing for thesecond flight experiment (planned to launch in 2019) in which
the observation wavelength is to be changed. In addition,
among the projects the SOLAR-C Preparation Project Officesupports, there is a balloon observation project, Sunrise-3,
scheduled to be implemented around 2020 after CLASP's
second flight. This fiscal year we successfully completed thereal optical design of the focal plane observation instrument,
SCIP, for Sunrise-3 to be provided by Japan.
In “Development of Telescope Receivers,” based on
the technology cultivated in the development of the ALMA
receivers, we have suppor ted not only evaluation andinstallation of the Nobeyama FOREST receiver but also
development and installation of receivers for 3 cartridge dewars
to be used in the ASTE telescope.
I n addit ion, we cooperated with Osa ka Prefect u reUniversity in GLT receiver development, continued technicalcooperation with Nagoya University for the NANTEN 2
telescope, and produced and shipped a three cartridge dewar
for the LLAMA Project based on a consignment business
contract.
We think that it is one of ATC’s important missions to
spread the technology and know-how accumulated in ATC toother projects and universities/research institutions to raise theoverall community technologically.
Hyper Suprime-Cam (HSC) started scientific observationfrom March 2014, and is being used for the observations in a
Subaru strategic program (SSP) and open-use observations.
Although it has basically worked well up to now, we had aproblem occur in the filter replacement mechanism. But wehave a prospect that it can be resolved by performing preventive
maintenance in a cycle shorter than assumed, because it ispartly due to the loosening of the fixation of the machineparts. In order to reduce the time overhead by shortening the
CCD readout time, a verification experiment in the laboratoryis under consideration with the aim of increasing the CCD
readout speed.
In the basic technology development, we will focus
on “radio camera development” and “infrared detector
development” as the themes of technology development aiming
for the development of basic technologies both for future
detectors and observational instruments.
At the Advisory Committee for ATC (including external
committee members), discussions on not only the project
promotion system at the Advanced Technology Center, but also
the method of research and development contributing to future
astronomy were started according to the request from the
Director General. In FY 2016 discussions were held primarily
about how to carry out advanced technology development
contributing to the future of radio camera and infrared detector
development.

2. Workshops and Development Support
Facilities(1) Mechanical Engineering Shop (ME shop)
T he Me ch a n ica l Eng i ne e r i ng ( M E) shop e ngage s
in a comprehensive manufacturing process to fabricate
experimental and observational instruments, from design tofabrication and verification. Three teams including design,
fabrication, and measuring/ultra-precision fabrication teams
cooperate to advance projects by leveraging their expertise.
The design team has mainly been working on mechanicaldesign for the K AGR A and TMT/IR IS projects. Major
contributions to the projects are as follows,[KAGRA project]- Mechanical design of the vibration isolation table for the
Beam Reducing Telescope.
- Mechanical design of the Beam Reducing Telescope.
- Assembly of Bottom Filters for the vibration isolation system.
- Mechanical design of the suspension system for wide angle
baffles.
[TMT/IRIS project]- Design and thermal structural analysis of an optical element
holder in cryogenic conditions.
- Thermal contraction analysis of the Imager structure.
- Seismic response analysis of overall IRIS structure.
- Cryogenic endurance test of mechanical components (ballbearing and ball screw) for the Imager.
- Attend preliminary design review.
The fabrication team has been working on the auxiliary
optical system of KAGRA since last year, and has fabricateda five-axis lens positioner (prototype) for the Beam Reducing
Telescopes. In addition, various parts of the vibration isolation
system, auxiliary optical system, and transmission monitor
system were delivered.
For TMT/ IR IS, mechanical par ts for the cr yogenic
endurance test were machined continuously in order to be able
to supply them upon request from the design team.
In addition, we completed the fabrication of the pupil
mirror array holder and the slit mirror array holder final model,
which are parts for the IFU (Integral Field Unit) of the Subaru
Telescope.
In collaborative development programs, we made the baseplate and other prototype parts for an ultra-wide-field highspeed CMOS camera (tomo-e) under development by the
University of Tokyo, Institute of Astronomy. Continuing on,
we are making the final one-quarter scale model. And, we aresupporting the development of a secondary mirror center cone
for the TAO project.
The ult ra-precision section of the fabr ication teamhas responded to fabrication requests. Development of the
wideband 37-pixel corrugated horn array has continued fromthe previous year. In the same way, trail fabrications for thecorrugated horn for the ALMA Band 10 receiver continued andmore data required for machining was obtained. Both topics
will be continued. A 37-pixel Si lens array with AR coating
was successfully finished as a prototype for the 109-pixel Silens array. This was successfully installed and took data on the
Nobeyama 45-m Radio Telescope. But new challenges have
Table 1: The requests in FY 2016.

From FY 2015

6

ATC

28

TMT/IRIS

7

KAGRA

32

ASTE

3

CLASP2,SOLAR-C

5

HSC

1

TMT

1

JASMINE

4

Division of Optical and Infrared Astronomy

1

Exoplanet Project office7

Public Relations Center2

Solar Observatory

1

Subaru Telescope3

Okayama Astrophysical Observatory

3

External Organizations
IoA, Univ. of Tokyo

2

Saitama University

2
Total
To FY 2016

102
5

II Status Reports of Research Activities

107

arisen in the AR coating, and development will be on going.
T he mea su re me nt t ea m ha s re sponde d t o not ju stmeasurement requests but also supported fabrication in order
to assure the high specifications. The main topic among
measurement only requests was the measurement of dummy
mirrors and connected parts for the KAGRA project. The main
topic in fabrication support was the pupil mirror array holder.
(2) Thin Film Processing Unit
Fundamental experiments continued to design and develop
the concrete processes of coating using inhomogeneous
multilayers. Data were obtained with a simple in-situ monitor
for thickness and refractive index during the deposition process.
These data were used to try to improve the performance of an
AR-multilayer, and it worked.
(3) Space Optics
Acquisition and accumulation of fundamental technologies
for space observations using platforms such as balloons,sounding-rockets, and satellites are progressing throughplanned or ongoing project activities. In FY 2016, Space
Optics primarily supported the development activities of solar
observation projects that are situated as Advanced Technology
Developments in ATC.
Space Optics has suppor ted the development of thepolar ization calibration system of the second CLASP
sounding-rocket experiment in which the target lines for thesolar chromosphreric magnetic field observations at FUV
wavelengths have changed. A new activity for developing
the focal plane instrument of the Sunrise-3 balloon project,which aims for vector magnetic field observations of the solar
photosphere and chromosphere from the altitude of the Earth’s
stratosphere, has started in this fiscal year.
(4) Optical Shop
Activity of the Optical Shop in 2016
1) Management• Me a su r i ng i n st r u me nt m ai nt e n a nce. (such a s d ai ly
inspections)• Technical consulting for users (29 cases)• Repair and upgrade.
- Exchange of the clean booth cover for the ZYGO
- Installation of Keyence VH-B18- Upgrade of PC for FT-IR
And others2) Common use of measurement instruments (April 2016 March 2017)• The number of annual user: 267
NAOJ: 223 (including 99 form ATC)
External organizations: 44 (including 9 from Institute of
Astronomy, University of Tokyo)• Use of LEGEX910 (large-scale 3-D measurement machine): 23
Number of operating days: 27

108

II Status Reports of Research Activities(5) Optical and Infrared Detector GroupWe have conduct ed t he se cond rou nd of t he joi ntpurchasing program for MESSIA6, a general purpose focal
plane array controller for astronomical instruments, as part ofshared use of the Advanced Technology Center. MESSIA6 wasbuild based on the electronics developed for Hyper SuprimeCam in cooperation with the University of Tokyo, and the HighEnergy Accelerator Research Organization (KEK). In this year,
a total of 6 sets were purchased for 4 organizations including
NAOJ divisions. We also supported the installation work of afully-depleted CCD manufactured by Hamamatsu Photonics
K.K. and MESSIA6 for the KOOLS observational instrumentof Kyoto University and Okayama Astrophysical Observatory
at our laboratory. We continue to provide the documentation of
MESSIA6, and support the users for installing MESSIA6 andCCDs onto their instruments.
(6) Facility Management Unit
The Facility Management Unit conducts the managementof ATC facilities including the buildings, electric facilities;
daily maintenance of the Cold Evaporator (CE); maintenanceof building equipment; oversight of const r uction; andmanagement of hazardous material and laboratory equipment.
We carried out renovation work on one draft chamber usedin washing work etc. in the laboratory to obtain a control windspeed satisfying the regulation value. Regarding the four draft
chambers used for cleaning work etc. in the clean room, we
have re-renovated three units that did not meet the regulation
values.
Also, we replaced the stainless steel discharge pipingwith PVC in the acid-treated draft chamber with the scrubber
decontamination device, as a countermeasure against corrosionof the piping. As the circulation cooling water facility and thewater pipeline become polluted due to aging, inspection andcleaning work including the outdoor cooling tower was carriedout to prevent deterioration of water quality.
With regard to the newly built No. 3 building (TMT
building), construction of circulating cooling water facilities
was considered in order to be able to use refrigerators in eachlaboratory, and Cold Evaporator (CE) piping connections arebeing considered.
There are many projects that use laboratory equipment,
including ATC, GWPO/KAGRA, TMT, Division of Radio
Astronomy/Chile Observatory, HSC, JASMINE, Division of
Optical and Infrared Astronomy, Extrasolar Planet Detection
Project Office, Subaru Telescope, Hinode Science Center, andSOLAR-C/CLASP. Projects that require high cleanliness inequipment development use clean rooms. In the 110 clean roomof the No.1 building and the 101 large clean room of the No.2
building, equipment related to KAGRA was developed. In
addition, the main body of the CLASP telescope, successfullylaunched in the United States in 2015, will return and new
equipment will be developed at the 101 large clean room of theNo.2 building as a new CLASP-2.

3. Prioritized Area Developments(1) ALMA receiver maintenance of Band 4, 8, 10
For the ALMA project, the mass-production and shipment
to Chile of the Band 4, 8, and 10 receiver cartridges, whichwere assigned to Japan, were completed in FY 2013. In Chile,
most of the receivers have been installed and operated in
the ALMA antennas, and many scientific results have been
published. At the Advanced Technology Center (ATC), the
ALMA receiver maintenance team has the responsibility ofmaintaining the defective receivers, and repaired four Band10
receivers during FY 2016.
Table 2: Total number of defective receivers.
Receiver Total

Breakdown
Initial failure

Repaired Remaining
Aging failure in FY 2016 for repair

Band 4

6

3

3

0

0

Band 8

17

14

3

0

0

Band 10

21

6

15

4

5

Table 2 shows the total number of defective receivers
broken down into “initial failure” and “aging failure.” And also
shown are the number of receivers repaired in FY 2016, and thenumber of receivers remaining to be repaired. These remaining
receivers are still inside of the antennas and will be replaced
during receiver system maintenance.
All of the initial failures of Band 10 receiver were fixed in
FY 2016. Thus, aging failure of electrical devices will dominate
future maintenance. We have continued good collaboration
with local engineers in Chile for careful maintenance such as“periodic health checks”, “preventative maintenance” and so on.
(2) TMTWe, the IRIS-Japan team at ATC, have been continuing
development of the first generation Thirty Meter Telescope(TMT) instrument IRIS since 2011.
The Preliminary Design Phase is continuing in FY2016.
We defined and released the design requirement documentof the IRIS imager, for which NAOJ/ATC has been taking
responsibility, and interface control documents between the
IRIS imager and other IRIS subsystem. Also we finished thepreliminary optical and opto-mechanical design of the IRIS
imager. All these designs and documents were reviewed andaccepted at the intermediate review (Preliminary Design
Review 1) in November, 2016. After the PDR-1, we started
working on the preliminary design of electronics, software, etc.
and producing a management plan, cost, and schedule for the
coming final design phase and fabrication phase.
In parallel, we have been continuing the protot y pe
experiment and trial fabrication looking ahead to the coming
final design phase and fabrication phase. The major issues are
the durability of the ball screw under the cryogenic conditions,the cooling characteristics of the surface shape of the opticalcoating, and trail fabrication of the high-precision asphericmirror.

We have been working on a conceptual study for the WFOS
camera system. WFOS is another first generation instrument of
TMT. In FY 2016, we figured out new optical designs that meet
new requirements. It was found that the vignetting fraction was
no less than 30 % as long as we employ a refractive system.
We also assessed an impact of polycrystal calcium fluoride
lenses on its image quality, and found that no more than one
polycrystal lens should be used in the camera. Thirdly, we
conducted a stray light analysis for WFOS, and confirmedthat during a full moon scattered light at the dome floor was asignificant stray light source. This suggests the importance ofinternal baffling. An optical designer in ATC contributed topart of the optical designing work and the stray light analysis.
(3) KAGRA
We have developed KAGRA's auxiliary optics subsystem(AOS) and vibration isolation subsystem (VIS) with theGravitational-wave Project Office (GWPO).
About AOS, we have continued the design and manufactureof some parts of the transmission monitor system (TMS). This
optical system will be located at the end of each 3-km arm
optical cavity of KAGRA to monitor the tilt and shift of thebeam line, and make feedback signals to the control system.
A prototype test of the beam reducing telescope (BRT), which
is a part of the TMS, has been done, and the test results havebeen reflected in the design of the actual setup. The BRTs need
to be isolated from vibrations as is done for the other mirrors
in the KAGRA interferometer, and the design of the vibration
isolation stages for BRTs has been ongoing. In addition, thedesign of the vibration isolation system for the wide-angle
baffles, which will be installed next to the main mirrors, hasbeen ongoing.
KAGRA-VIS is a subsystem to suspend mirrors required
for the KAGRA interferometer to isolate them from seismic
motions. T he system consists of multi-st age isolation
mechanical filters. Most of the parts of the isolation systemhave been brushed up, assembled, and tested by the ME
shop, so the ME shop is essential for KAGRA. With thesecontributions, the initial phase of KAGRA (iKAGRA) finished
its test run in April 2016. In this fiscal year we have continued
to assemble and test several mechanical filters cooperating with
the GWPO. For “standard filters,” 13 out of the required 19
pieces have been assembled, and for “bottom filters,” 2 out of
4 pieces have been assembled. Moreover, for work to upgrade
KAGRA (to bKAGRA) in this fiscal year, the GWPO asked us
to design a part called "bottom filter recoil mass" and propose
the installation procedure. The ME shop did the work, and thedesigned parts have been installed in KAGRA.
As shared use of the ATC facilities, “pre-isolators” were
tested by the GWPO in the large clean room. In addition,
researchers from KEK and ICRR tested hydrocatalysis bonding(HCB) of sapphire parts to a sapphire dummy mirror in theISO1 clean booth. The three-dimensional measurement system
was used several times to evaluate the test results.

II Status Reports of Research Activities

1094. Advanced Technology Developments(1) CLASP2/Sunrise/SOLAR-C
The CLASP sounding-rocket experiment is a pioneering
project of observing the solar magnetic fields at far ultraviolet
wavelengths. Af ter succeeding in the f irst experimentconducted in September 2015, the development team has
been preparing the new instr ument to observe different
chromospheric lines than those observed in the first f light.
This will be used for the second flight experiment scheduled in
2019. The major activities in this fiscal year were the modified
optical design and the development of the optical components
in response to the change of target lines.
The Solar-C Project Office is participating in a balloon
project, Sunrise-3, to be launched around 2020 after the
CLASP 2nd f light. The detailed optical design of the focal
plane instrument, SCIP, that the Japanese team is primarily
responsible for has been carried out in this fiscal year.

supported studies led by NRAO and ESO for the developmentof Band 2+ (67–95 GHz) and 2+3 (67–116 GHz) prototype
receivers, respectively. In the case of Band 2+, a corrugatedhorn and dielectric lens have been designed and fabricated.
Preliminary tests after integration in the Band 2+ prototype
receiver show good performance.
2. Ultra-Wideband receiver
In terms of RF bandwidth, we are developing SIS mixers
based on high-critical-current-density junctions with the goalof covering the full ALMA Band 7+8 (275-500 GHz). So far,
we have demonstrated a DSB mixer which satisfies ALMA
requirements in the full 300-500 GHz band. In addition, we
have designed and fabricated corrugated horns and waveguidecomponents for Band 7+8, and are currently evaluating theperformance of prototypes. In terms of IF bandwidth, we havesuccessfully achieved the direct connection of an SIS mixer
and an IF amplifier, and extended IF bandwidth to 3-18 GHz(currently, 4-8 GHz in ALMA).

(2) Telescope Receiver Developments
1) Telescope Receiver Developments
Based on the technical skills acquired through the ALMA
receiver developments, the “telescope receiver development”
team has responsibility for the development and support
for installation of the Nobeyama FOREST receiver andthe development, tests, and installation of receivers for a
3-cartridge receiver cryostat for the ASTE telescope. And also,
we maintain good collaboration with other radio telescopes
operated by universities, such as technical collaboration on
NANTEN2 with Nagoya University, cooperative production ofa receiver for the Greenland Telescope with Osaka Prefecture
University, and fabrication of a 3-cartridge receiver cryostat for
the LLAMA telescope through a manufacturing cooperation
contract with the Universidade de São Paulo.
ATC can i ncrease the tech nolog y st andards of thecommunity by giving feedback using the technologies andknowledge accumulated through development of specificprojects, and promote the technology development of otherprojects, universities, and research institutions. It is also
important to make the best use of the achievements of the
projects.
2) Development of advanced future receivers
In the field of future developments in heterodyne receivers,
we focus on two main activities. Firstly, we are involved ininternational collaboration for the development of the ALMA
receivers in frequency bands not implemented in the array yet:Band 1, Band 2+, and Band 2+3. Secondly, we have started
receiver development to support future upgrade plans for
ALMA in three main directions: ultra wideband, terahertz, andmultibeam receivers.
1. ALMA Band 1, 2+ and 2+3 receivers
We supported ALMA band 1 development and preparation
towards production through several technical studies. We also110

II Status Reports of Research Activities

3. Terahertz receiver
We have continued the development of optical components
and superconducting mixers for the 1.2–1.6 THz band. In FY
2015, we demonstrated the possibility to fabricate good quality
corrugated horns for these frequencies. Last year, based onthem, we completed the design of ALMA compliant optics.
With respect to superconducting mixers, we have worked on
the design of a quasi-optical mixer in collaboration with Paris
Observatory.
4. Multibeam receiver
We have worked on the concept of a multibeam receiver
based on superconducting integrated circuits, and started
fabrication of the f irst protot y pes. In addition, we arecollaborating with K ASI in Korea towards a wideband
multibeam receiver.
(3) SIS junction development
We have made steady progress in fabricating high current
density (Jc) SIS junctions with the goal of providing a steadysupply of high quality mixing devices to be used in receivers
installed in telescopes, first and foremost ALMA, as well
as future receiver development research. The devices are
implemented with a Jc as high as 25–45 kA/cm 2 , which is
2–4 times as high as that conventionally achievable. This
breakthrough happened one year ago when found an effective
way to protect the tunnel barrier from damage during counterelectrode deposition by applying a 5 nm thick cap Al layer
above the oxide barrier. The mixer devices fabricated inthis way have enabled a single receiver to operate across anoctave frequency range. With these devices, we demonstrated
a receiver operating across two ALMA bands (Band 7 andBand 8) with a sensitivity meeting ALMA specification.
This achievement proves the feasibility of improving ALMA
observation capability by merging ALMA receivers.
In parallel with the development of high-Jc junctions, wehave initialized an investigation into fabricating SIS mixers
on free-standing membranes. This technique is essential fornext-generation multi-pixel SIS receivers, which enable a large
field of view in a radio telescope. In order to carry out thisstudy, we have setup two sophisticated pieces of equipmentin the cleanroom: a deep-reactive-ion etching system (MUC21, Sumitomo Precision Co.) and a SUSS MA6 mask alignerthat enables backside alignment. We have established afabrication process of Si membranes from silicon-on-insulator
wafers and demonstrated 6-micrometer thick free-standing
Silicon membranes with a diameter of 3 mm and flat surface(the maximum bending is less than 5 micrometers). This
achievement brings us a bright outlook, especially for thedevelopment of multibeam receivers with a wider field of view
for ALMA.
(4) HSC
Hyper Suprime-Cam (HSC) started its science operationin March, 2014 and has been offered to the Subaru Strategic
Program (SSP) and general observer's programs. During thetwo years so far, 137 nights were allocated for SSP and asimilar number of nights were allocated for general observers.
The operation has been stable over this time, but during FY
2016, we encountered mechanical problems several times in
the actuators of the central unit (CU) of the filter exchanger
system. An ATC engineer found several loose bolts in the
CU. This suggests the importance and necessity of preventive
maintenance more frequently than we had originally planned.
We found the first CCD failure on April 2012 and the numberof failed CCDs grew to three by May 2015. No new trouble
in the CCDs was, however, reported in FY 2016. If we seemore detector failure, we will have to decrease the back bias
voltage to reduce the risk but this causes degradation of image
resolution. Careful trade-off studies should be made basedon the on-going lab experiments. After two years of SSP
observations were completed, it became evident that the survey
speed is about 80 % of the original plan. This is mainly because
the weather was worse than our estimate of the number of clear
nights. One possible solution is to reduce the CCD readout timeby paying a penalty of increased readout noise. In FY 2017,
we should work out optimization of the CCD clocking. This isworth spending time because even a moderate squeeze amounts
to big savings of observing times over the decades of HSC
operation. In fact, Suprime-Cam has been used over 19 years.
We planned to install the detection efficiency monitor in FY
2016 but it was postponed due to the delay of M1 re-coating.
We will set it up in October, 2017.

5. Basic Technology Development(1) MKID camera /CMB Instruments
We are developing a wide field of view, broadband, andhigh sensitivity millimeter / submillimeter wave instruments.
In collaboration with the University of Tsukuba and Saitama
University, we have developed a superconducting MKID
camera for a future Antarctica terahertz telescope. As apathfinder, the MKID camera was installed on the Nobeyama
45 m telescope. In collaboration with KEK, ISAS, Kavli IPMU,
and Riken, we are developing LiteBIRD and GroundBIRD
which observe B-mode polarizations of the cosmic microwave
background radiation (CMB). The LiteBIRD has been selected
as one of the higher priority projects of the master plan 2017of the Science Council of Japan. In this year, the following
research results were obtained.
1) Development of broadband corrugated horn array (S.
Sekiguchi et al. 2017 IEEE TST)
2) Broadband antireflection structure on Si (T. Nitta et al. 2017
IEEE TST)
3) Design of Octave-band OMT-MKID (S. Shibo et al. 2016
SPIE)
4) Confirmation of the interface between the data acquisition
system of the MKID camera and the Nobeyama 45-m Radio
Telescope by a test installation(2) Near-IR Imaging Sensor Developments
In this year, we have made a trial chip of small-pixel
and large-format Indium Gallium Arsenide (InGaAs) image
sensors in cooperation with KEK, Hiroshima University, andKagoshima University. The cost is expected to be lower thanexisting near-infrared sensors. We have successfully madefully-functional chips with a small number of bad pixels,
however the readout noise slightly increased. Near infrared
test observations were conducted with the manufactured chips
attached to Hiroshima University’s Kanata Telescope. We
continue to investigate making a low noise InGaAs image
sensor compatible with both small-pixels and large-format,
which is suitable for a near-infrared wide field camera.
(3) Multicolor Millimeter/Submillimeter Continuum Camera
Exploring a large patch of the sky in the millimeter/
submillimeter bands with a continuum camera will provide
the opportunities to effectively measure the redshifts ofsubmillimeter galaxies, the structure of the hot plasma inclusters of galaxies, and the physical properties of the dust in
star-forming regions. Thus, we are developing a Transition
Edge Sensor (TES) bolometer camera in collaboration with the
University of Tokyo, Hokkaido University, the University ofCalifornia Berkeley, and McGill University.
In FY 2016, science commissioning of the bolometer
camera, capable of simultaneous observation at 1.1 mm and 0.87
mm wavelengths, on board the ASTE telescope was conducted.
As a result, we have achieved the target mapping speed at the
0.87 mm wavelength, and demonstrated the effectiveness ofthe novel intensity calibration instrument. Our experiences areshared with the development projects such as DESHIMA and
A-Pol to enhance the continuum observation capability in EastAsia.
(4) Development of Terahertz Intensity Interferometry
New interferometer technology making use of intensity
fluctuations in astronomical sources has been developed in theterahertz frequency region. In collaboration with the National

II Status Reports of Research Activities

111

Institute of Advanced Industrial Science and Technology(AIST), low leakage superconducting tunnel junction detectors
are being developed, and their leakage current is evaluatedand fedback to the fabrication process. Compact sorption
coolers were developed to cool the wide bandwidth SIS photon
detectors, showing a cooling capacity of 400 uW at 0.8 K.
Our proposal for imaging intensity interferometry is basedon delay time measurement using photon bunches, which wasdemonstrated by simulation and presented in workshops. The
development of SIS photon detectors is made possible by the
grant-in-aid for challenging exploratory research programsfrom JSPS.

6. Open Use Programs, Joint Research, andDevelopment
In FY 2016, we accepted open use programs of ATC
facilities twice a year including 10 collaboration programs and
23 facility use programs. Applicant names and program titles
are listed in the section “Open Use Programs etc.” Results ofthe programs can be found on the ATC homepage.

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17. Public Relations Center
1. Overview
The Public Relations Center engages in the publication,
promulgation, and promotion of scientific achievements madenot only by NAOJ but also by others in the field of astronomy
in general to raise public awareness; responds to reportsof discoveries of new astronomical objects; and provides
the ephemeris and other astronomical information directly
related to people’s everyday activities, such as sunrise andsunset times. In FY 2016, the Center has been comprised of 6
offices and 1 unit: the Public Relations Office, the Outreachand Education Office, the Ephemeris Computation Office,the Library Unit, the Publications Office, the IAU Office for
Astronomy Outreach (OAO), and the General Affairs Office.

2. Personnel
In FY 2016, the Public Relations Center was composed of
Director Toshio Fukushima and the following staff members:
2 professors, 2 associate professors, 1 assistant professor (oneholds concurrent posts), 1 research engineer, 1 chief senior
engineer, 1 chief engineer, 1 Chief of the Library, 5 speciallyappointed senior specialists, 3 research experts, 21 public
outreach officials, 1 research supporter, and 2 administrative
supporters.
On April 1, 2016, Associate Professor Hitoshi Yamaoka
arrived and specially appointed senior specialist Hiroko
Tsuzuki arrived in the Public Relations Office on September 12.
On November 30, 2016, public outreach official Diaz Rosas
Elian Abril in the IAU Office of Astronomy Outreach finished
her term. On March 31,2017, public outreach official Takao
Ibaraki, public outreach official Kuninori Iwashiro, and public
outreach official Hiroshi Futami finished their terms.

3. Public Relations OfficeThrough press conferences and web releases, the Public
Relations Office actively developed public outreach activities
focused around the results of each research project, first andforemost ALMA and Subaru Telescope, including open-use
and collaborative results with other universities and research
institutes. In addition, our office hosted lectures to publicize
cutting-edge astronomy. In cooperation with the Outreach andMonthApril 2016
May 2016
June 2016
July 2016

Access counts
358,635
579,476
555,124
463,076

Education Office, the Public Relations Office also conducted
observation campaigns to promote astronomical phenomenaof interest to the public, like the meteor showers. Our officeorganized and held independent workshops with public relation
officials to improve the skills of outreach personnel.
(1) Online-Based Information Sharing
The Public Relations Office runs the NAOJ website (http://
www.nao.ac.jp/en/), disseminating information via the internet.
Table 1 shows the access counts for the website.
Last fiscal year, a special website “Multiwavelength
Universe”English version was opened. This website won the
WebAward 2016 Best Science Site.
For the NAOJ Chile Observatory, the Public Relations
Office reviewed and offered advice on the proposal for thewebsite renewal.
The office opened Twitter accounts and Facebook accounts
in Japanese and English sequentially from 2010. We havebeen actively disseminating information on social networking
services. Our office disseminates information on the status ofvarious NAOJ projects such as public visits, regular stargazing
parties at Mitaka Campus, and position openings, both inEnglish and Japanese. As of the end of March 2017, the numberof followers exceeds 80,000. From this fiscal year, we havestrengthened our English version of Twitter. In the second
half of the fiscal year, we started to post daily. Also, NAOJ
quizzes on Twitter were started and they made the Twitter
more interactive. Also, from this fiscal year, our office started
to disseminate visual images on Instagram.
NAOJ e-mail newslet ters No.159 –171 were issued,
introducing research results and NAOJ hosted events.
We continued to produce videos explaining research
results, videos explaining astronomical phenomena, and videos
introducing outreach activities. Including English versions,
19 original videos were produced. The videos are uploaded
mainly on YouTube. As of the end of March 2017, these videos
have accumulated a total of 459,139 minutes of play time and86,005 views. This fiscal year, as a new effort, our office twice
performed live stream broadcasting of heavenly bodies withthe 50-cm Telescope for Public Outreach. There were about
2,000 viewers in total. In addition, we conducted live internet
broadcasts including the lectures mentioned below and on
Mitaka Open House Day.

Month
Access counts
August 2016
1,237,959
September 2016
444,328
October 2016
430,131
November 2016
532,127
Total: 6,611,747

Month
December 2016
January 2017
February 2017
March 2017

Access counts
522,840
620,472
481,406
386,173

Table 1: Monthly website access statistics for the Public Relations Office website, NAOJ Public Relations Center (April 2016–March 2017).

II Status Reports of Research Activities

113

“Keiichi Kodaira Video Clip”for the digital book

English Version

Hunting Black HolesJapanese/English Versions“FUREAI (Friendly) Astronomy” PR movie

Japanese Version

HSC/M31 Video Clip
HSC/Virgo1 Video Clip
Dr. Flaminio interview about Breakthrough Prize in Fundamental Physics
Dr. Barton interview about Breakthrough Prize in Fundamental Physics
Project PR movie “Public Relations Center”
Perseid Meteor Shower (Aug.12, 2016)
CfCA “Pulsar Video Clip”
Project PR movie “Okayama Astrophysical Observatory”
Project PR movie “Subaru Telescope”
Project PR movie “NAOJ Chile Observatory”
Cultural Properties Protection Week Movie “NAOJ Solar Tower Telescope”

Japanese/English/Italian Versions
Japanese/English Versions
Japanese Version
Japanese Version
Japanese Version
Japanese Version
Japanese Version
Japanese/English Versions

Table 2: Summary of Produced Videos.

May 11, 2016
May 25, 2016

New Test by Deepest Galaxy Map Finds Einstein's Theory Stands True

June 7, 2016
July 26, 2016
August 12, 2016
September 5, 2016

Japan OISTER collaboration uncovers the origin of extraordinary supernovae
Ancient Eye in the Sky
Dense molecular gas disks drive the growth of supermassive black holes—Are supernova explosions the key?
Discovery of an Extragalactic Hot Molecular Core

October 31, 2016

A joint observation by solar observing satellites Hinode and IRIS quantitatively explores the formation of the solar
chromosphere

November 21, 2016

Discovery of Unexpected Supersonic Events Everywhere on the Sun - Results from 5-minute Flight of the Sounding
Rocket Experiment “CLASP” -November 22, 2016
November 28, 2016

Record-breaking Faint Satellite Galaxy of the Milky Way Discovered*
Timing the Shadow of a Potentially Habitable Extrasolar Planet Paves the Way to Search for Alien Life

December 5, 2016
January 16, 2017
January 24, 2017
January 31, 2017
February 24, 2017
February 28, 2017
March 8, 2017
March 29, 2017
January 15, 2016
February 4, 2016
February 25, 2016
February 25, 2016
March 3, 2016
March 10, 2016
March 10, 2016

ALMA measures size of seeds of planets

Footprints of Baby Planets Imprinted in a Gas Disk

Tail of Stray Black Hole hiding in the Milky Way
Micro spacecraft investigates cometary water mystery
Tracing the Cosmic Web with Star-forming Galaxies in the Distant Universe
Saturn’s Rings Viewed in the Mid-infraredFirst Public Data Release by the Hyper Suprime-Cam Subaru Strategic Program
Ancient Stardust Sheds Light on the First Stars — Most distant object ever observed by ALMA
Subaru Telescope Detects the Shadow of a Gas Cloud in an Ancient Proto-supercluster
Signs of Second Largest Black Hole in the Milky Way - Possible Missing Link in Black Hole Evolution
A Violent Wind Blown from the Heart of a Galaxy Tells the Tale of a Merger
Subaru-HiCIAO Spots Young Stars Surreptitiously Gluttonizing Their Birth Clouds
New Fast Radio Burst Discovery Finds ‘Missing Matter’ in the Universe
ALMA Spots Baby Star’s Growing Blanket
Deciphering Compact Galaxies in the Young Universe
Mysterious Infrared Light from Space Resolved Perfectly
Table 3: Web Releases.

June 16, 2016
September 6, 2016

ALMA Detected the Most Distant Oxygen
Avoiding “Traffic Jam” Creates Impossibly Bright “Lighthouse”*
Table 4: Press Conferences.

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(2) Research Result PR
There were 20 research result announcements (compared
to 27 in FY 2015 and 16 in FY 2014). For press releases
aimed towards overseas audiences, we have continued to use
the delivery services of American Astronomical Society,
AlphaGalileo, and EurekAlert! from AAAS. We released
almost all the research releases in both English and Japanese.
We made videos introducing the content indicated with a *mark.
In the perennially popular Astronomy Lectures for Science
Journalists program, the 23rd lecture entitled “ALMA Opens a
New Astronomy” was held on December 2, 2016. Thirty people(23 companies) participated in the lecture.
(3) Activities as NAOJ’s Public Relations Center
The following activities were pursued in addition to theCenter’s regular task of aiding research result releases.
The Public Relations Office organized lectures withresearch projects. On June 11, 2016, NAOJ and Riken Lecture“Origin of Materials told by the Universe;” on September 10,
Hinode 10th anniversary lecture “Exploring the Universe andthe Earth through Solar Observations;” and on November
26, the NAOJ lecture meeting/22nd ALMA public lecture“Exploring birth of stars and planets with ALMA” were held
respectively. In addition, the office persevered in helping
to organize and publicize the Subaru Telescope/ Shinshu
University public lecture “From Shinshu via Hawai‘i, aGalactic Research Journey” on November 23 and “The Subaru
Telescope/Hiroshima University public lecture” on November
27.
Furthermore, since the 23rd NINS Symposium “Frontiersof Modern Astronomy: a Second Earth and the Dark Universe”
was held on March 5, 2017 with NAOJ responsible for theplanning and operating, the Public Relations Center was at thecenter of holding the event, in cooperation with the General
Affairs Section, General Affairs Division.
To expand our public relation materials, our office took
photographs at Mizusawa VLBI Obser vator y, Okayama
Astrophysical Observatory, and KAGRA. For KAGRA, movies
were also taken simultaneously.
Our office organized workshops with public relation
officials inviting lectures from outside to improve the skills ofoutreach personnel. Training in photography was offered on
July 25, 2016, and training in science writing was offered on
January 18, 2017.
To publicize NAOJ abroad, we exhibited booths at oversea
meetings for the public and events where the press gathers(New Scientist Live in London: September 2016 and AAAS

April–June
July–September
October–December
January–March

Solar info Lunar info Ephemeris info
167
70
43
126
110
63
192
233
44
136
63
29

meeting in Boston, February 2017). In addition, we ordered an
outside film maker to make a 6 minute video for release at theAmerican Physical Society Annual Meeting and screened it inMarch 2017.
(4) New Astronomical Objects
From t h is f iscal ye a r, t he re s p on sibi l it y for New
Astronomical Objects moved from the Ephemeris Computation
Office to the Public Relations Office. Four staff members,
including one full-time and three part-time, handled reportsof new astronomical objects and other communications
submitted to NAOJ. In this fiscal year, there was a total of 15
reports including confirmation requests for new celestial object
candidates and other reports. The contents were: 4 novae/
supernovae, 6 variable stars/transient objects, 1 comet, 1 minor
planet, and 3 luminous objects. Among the many examples ofreporting a variable star or known asteroid as a new object, thereport of a transient object in September, was communicatedvia NAOJ to the IAU Central Bureau for Astronomical
Telegrams and was recognized as an independent discovery ofNova Scorpii 2016 No. 2 (V1656 Sco.)

4. Outreach and Education Office(1) Public Visits
A total of 20,522 people visited the Mitaka Campus
Visitors' Area in FY 2016. In addition, the group tours in
2016, consisted of 110 general tours (4,408 guests), and 36
workplace visits by schools (362 guests), for a total of 146 tours
accommodating 4,770 guests. Note that in the workplace visits,
lectures by researchers, question-and-answer sessions, andvisits to research facilities also took place. The office started
developing the audio guide in the Visitors’ Area. From October,
our office began experimental operation at the 20-cm Telescope
Dome, Repsold Transit Instrument Building, Gautier Meridian
Circle Building, and Astronomical Instrument Museum.
Regular stargazing parties were held twice a month (theday before the 2nd Saturday and the 4th Saturday) with the 50cm Telescope for Public Outreach. These were held regardlessof cloudy or rainy weather. Advance booking (300 people foreach session; a lottery system from April to September andadvanced reservations until filled system from October toMarch) was introduced in FY 2012 for these events. A total of
23 sessions were held with 4,671 participants this year. The
Regular Stargazing Parties celebrated their 20th anniversary
in April 2016. More than 60,000 guests have visited in these 20
years.

Time
28
15
4
6

Solar System Universe
330
92
209
149
276
121
225
112

Astronomy
147
134
137
107

Other
554
803
649
400

Total
1431
1609
1656
1078

Table 5: Telephone inquiries made to the Outreach and Education Office of the NAOJ Public Relations Center (April 2016–March 2017).

II Status Reports of Research Activities

115

The Outreach and Education Office changed the regularpublic screenings at the 4D2U Dome Theater from three times
a month to four times (1st, 2nd, 3rd Saturday, the day before
the 2nd Saturday). Advanced reservations were required forthese. A total of 47 screenings were held this year, with 5,432
guests participating. For five of the regular public screenings,
the office held “Astronomer’s Talks” where NAOJ researchers
talked about the latest research and these were popular. Group
screening used to only be performed on Fridays, but wechanged to Wednesdays and Fridays. Therefore, the number ofgroup tours became larger and 81 group screenings were heldwith 2,655 guests attending. Especially at Wednesday group
screenings, teacher training sessions were held. 96 tours wereorganized with 1,189 attendees. In total, 224 screenings were
held and a total of 9,276 guests enjoyed 4D2U’s stereoscopic
images.
The regular “Tangible Cultural Property Tours” ceased
operation at the end of March 2016. In 2016, the NAOJ Solar
Tower Telescope Special Open Days (November 3, November
5, and November 6, no reservations needed) and Tangible
Cultural Heritage Tours (November 3 and March 20, advancereservations needed) were held with 624 attendees.
(2) Telephone Inquiries
The office received inquiries from the media, government
offices, and the general public. The Outreach and Education
Office responded to 5,774 telephone inquiries (Table 5) and 134
letters, 52 of which were official documents.
(3) Educational and Outreach Activities
For the “Fureai (Friendly) Astronomy” project, now in its
7th year, a total of 49 lecturers provided events to 80 schoolsout of the 86 which applied, reaching 8,017 students.
We presented the results of the questionnaire performed
in Fiscal Year 2015, at the Japanese Society for Education and
Popularization of Astronomy Meeting and The Astronomical
Society of Japan Fall Meeting. Particularly noteworthy is thatfor the Astronomical Society of Japan meeting, we presented at
the press conference.
“Summer Nights: Let’s Count Shooing Stars, 2016” wasconducted in August 2016 and we received 2,311 reports. A
paper showing the possibility of obtaining observation results
close to skilled observers by collecting a large number ofreports from the general public was published in “Planetary
and Space Science.”
On August 16 (Tuesday) and August 17 (Wednesday),“Astronomy classes for kids in Summer” events were held forelementary and junior high school students. On the first day,there were lectures about the assembly and use of telescopes.
In cooperation with the JASMINE Project Office, the second
day was lectures about the distances of celestial bodies,
three-dimensional star handcrafts of the big dipper, and aninterpretation using the four-dimensional digital universe
viewer, “Mitaka.” Also, star gazing parties were scheduled forboth days (Cancelled on the first day due to the typhoon.) The
total number of attendees was 77.

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The Public Relations Center participated as the secretariat
for the Mitaka Open House Day, a special public event held at
Mitaka Campus and organized by the steering committee.
This two-day event was held on October 21 (Friday)
and October 22 (Saturday) with the theme “Gravitational
Waves, a new Frontier of Astronomy.” It was co-hosted
by the Astrobiology Center, National Institutes of Natural
Sciences; the Institute of Astronomy, the School of Science,
the University of Tokyo; and the Department of Astronomical
Science at the School of Physical Sciences of the Graduate
University of Advanced Studies. The event f lourished: 542
guests attended on pre-open day, 3,992 guests attended on
open day, 4,534 guests attended in total. Each Project offered aselection of activities based on their own expertise which weresuitable for a wide range of age groups. Activities included theviewing of facilities not normally open to the public, interactive
panel displays, minilectures, quizzes and games that are
popular among children, and a virtual reality experience.
From October 2 (Sunday) to October 4 (Tuesday), the“Workshop for Popularizing Cutting-Edge Astronomy” washeld with the theme of “Gravitational Wave Astronomy” forstaff members of science museums/museums, teachers, andscience communicators, who are doing astronomy outreachwork. Lectures were held at the University of Toyama andattendees also visited the Large-scale Cryogenic Gravitational
Wave Telescope KAGRA of the Institute for Cosmic Ray
Research, University of Tokyo; the Underground Neutrino
Detector Super-Kamiokande; and the Kamioka Liquid
Scintillator Antineutrino Detector (KamLAND, Tohoku
University). 64 guests attended.
On March 2 (Thursday) and March 3 (Friday), NAOJ, theInternational Planetarium Society, and others, co-hosted the“Data to Dome Workshop” at the Large Seminar Room and
4D2U Dome Theater. The aims of this international handson workshop were to enable easy visualization and extend
the possibility of science communication in planetariums. 52
guests attended including 9 invited speakers and 15 attendees
from overseas (U.S.A., Canada, Taiwan, Germany, South
Africa, Hong Kong, the Netherlands, and Sri Lanka.)(4) Community Activities
The “Mitaka Picture Book House in the Astronomical
Observatory Forest” welcomed 41,068 visitors in FY 2016.
The Outreach and Education Office supervised the exhibition“Ephemeris Counting Life (July 2016 – June 2017).” We also
cooperated with modern and traditional Tanabata events,
moon viewing event, and other events. In addition, through the“Mitaka Picture Book House in the Astronomical Observatory
Forest, Picture Book Original Drawings Hallway Exhibit
Contest” which started from FY 2013, the Outreach and
Education Office cooperated in the selection of 3 winningbooks.
The Out reach and Education Off ice conducted the
8th“Mitaka Solar System Walk” from Friday, September 23
to Sunday, October 23 in cooperation with Mitaka City andthe non-profit organization (NPO) Mitaka Network University

Promotion Organization. Stamps were placed at 170 shops and
67 facilities, including NAOJ Mitaka Campus and the Mitaka
City Municipal Office, for a total of 237 locations around
Mitaka. Adding 19 limited stamps, 256 stamps were placed andthis is a record number. Approximately 18,000 guide-maps/
stamp sheets were distributed, of which 3,379 people turned
theirs in for a prize. The number of participants who collected
all the stamps was 387. It was a good chance to tour the Solar
System while promoting commerce, industry, sightseeing andproviding families with a way to enjoy Mitaka and rediscover
the city’s charm.
The Outreach and Education Office also provided the venue
for “Astronomy Course for Apprentice Starry Sky Guides,Star Sommelier Mitaka - Let’s Become Apprentice Starry Sky
Guides! - ” hosted by Mitaka Network University and also
assisted by providing teachers and workshops.
The “Information Space of Astronomy and Science” forwhich Mitaka City, Mitaka Network University, and Mitaka
City Planning Board co-operate celebrated the second year
since its opening and 11 exhibitions were held in FY 2016. The
Public Relations Center had proposed 2 of these exhibitions
and helped with 3 lectures.
Also, the office offered outreach and monthly astronomical
information images through large-scale information displays
and “Cosmic Reading Bookstore Corner,” a display of sample
books available to read which changes themes (once every 2months), and cooperated on the “M Marche Project” conductedon the 4th Sunday of every month. We welcomed 21,674 guests
in the 2016 fiscal year and celebrated 20,000 visitors and
30,000 visitors since the opening. It has been acknowledged asa location in town where science can be easily accessed.

February 1, 2017). The Calendar and Ephemeris webpage was
updated to match what was published in the Reki Yoko.
(2) As for the website (http://eco.mtk.nao.ac.jp/koyomi/index.
html.en), ECO continuously updated the contents of theEphemeris Wiki and worked on checking the accessibility
se que nt ial ly. ECO coop e r at e d w it h t he a st ronom ical
phenomena awareness campaigns again this year. The radiantpoints of the Perseid, Geminid, and Quadrantid meteor showers
were published in the Astronomical Information section of thewebsite. There were about 24 million page views for this fiscal
year.
(3) The Japan Association for Calendars and Culture Promotion
hosted its 6th General Meeting, and the Calendar Presentation
Ceremony.
(4) ECO hosted regular exhibitions in collaboration with
the Library, selecting from NAOJ’s invaluable collection ofhistorical archives written in Japanese/Chinese. The themesof the 54th and 55th permanent exhibitions were “24 Sekki
and Calendar” and “Shigetomi Hazama” respectively. These
exhibits can also be viewed at the Rare Materials Exhibition of
the Library’s website, in Japanese only (http://library.nao.ac.jp/
kichou/open/index.html).
(5) New Astronomical Objects work was transferred to the
Public Relations Office this fiscal year.

(5) Merchandizing Business
The office cooperated with merchants who organized the
NAOJ original goods and aided in making 5 types of goods and
132 individual products, such as pin badges, cultural property
facility post cards, and T-shirts. In addition, the office invitedmerchants to place vending machines dispensing capsule toys
starting from August 2016. These were placed so that visitors
can buy goods when the Co-op store is closed on Saturdays andSundays. Also, the office invited booths selling goods at the
Mitaka Open House Day. A total of 1,230 items of these goods
were sold in the year.

5. Ephemeris Computation Office
The Ephemeris Computation Office (ECO) estimates
calendrical phenomena such as the apparent positions of theSun, Moon, and planets on the basis of international standards
and publishes the “Calendar and Ephemeris” as part of thecompilation of almanacs, which is one of NAOJ’s raisons d’être.
(1) ECO published the 2017 edition of the Calendar andEphemeris, the 2017 version of the calendrical section of the
Rika Nenpyo (Chronological Scientific Tables), and the 2018
edition of the Reki Yoko (posted in the official gazette on

Figure 1: Pageview Statistics of ECO Website.

6. Library Unit
The Library Unit collects and sorts scientific journals andbooks in order to make them available for the research and

II Status Reports of Research Activities

117

study of NAOJ researchers and students. In recent years, withthe continuing digitalization of scientific materials, the portionof the materials in electronic format has increased.
For non-NAOJ personnel who wish to use the Mitaka
Librar y materials, the Librar y is open to the public on
weekdays. In FY 2016, 249 non-NAOJ personnel came to use
the Library. Also for researchers and students belonging toother organizations, we loan books or provide photocopies via
the institute’s library. In FY 2016, photocopies or loans were
provided in a total of 96 cases.
Important documents, especially those originating from theEdo Era Tenmonkata (Shogunate Astronomer), are preserved
while taking into account the environment of a specialized
library. Images of some of the important documents areavailable to the public on the Library Unit homepage.
During the Mitaka Open House Day festivities in October,
we used to open part of the Mitaka Library to the public, but in
Fiscal Year 2016, we extended the subject themes. In addition
to materials for general and young readers, we actually allowed
visitors to take a look at many specialized books related toastronomy.
The number of books and journals owned by Mitaka
Library and each observatory and the condition of continuing
NAOJ publications are published in Section XI Library,
Publications.

7. Publications Office
The Publications Office continued its activities in planning,
editing, and printing NAOJ’s original materials for PR andpromotions. The following periodicals were also published thisyear:
• Annual Report of the National Astronomical Observatory ofJAPAN Volume 28 Fiscal 2015 (Japanese)• Annual Report of the National Astronomical Observatory ofJAPAN Volume 18 Fiscal 2015 (English)• Report of the National Astronomical Observatory of JAPAN
Volume 18 (Japanese)• NAOJ Pamphlet (Japanese)• NAOJ Pamphlet (English)• NAOJ News, No. 273 – No. 284 (April 2016–March 2017)• R a d io Ast ronomy P ubl ic Relat ion s com ic “A l ma r’s
Adventure” (#6)
• NAOJ Publicity Poster Series (#4, #5, #6)
Continuing from the previous year, in FY 2015 thePublications Office strove to strengthen its international
publication ability and digital publication ability. Regarding
the production of an international edition of the Rika Nenpyo(Chronological Scientific Tables), the authors performed
the first check of the English translation and it is in layout.
In digitalization efforts, the Office brushed up the “NAOJUniversal Multi-Publication System (NAO-JUMPS),” which
includes research highlight of the Annual Report of the
NAOJ and fixed layout articles from NAOJ News. Together
with this, the first book Makali‘i in Hawai‘i ”(ISBN978-4-

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II Status Reports of Research Activities

908895-01-2) was published using the generalized electronic
book platform “NAOJ-Delivering next-generation e-books(NAOJ-Deneb).” In normal business, the Office produced
and distributed the NAOJ pamphlets and the Annual Reportof the National Astronomical Observatory of JAPAN. In thesystematic production of special editions with the goal ofdeveloping project outreach support in NAOJ News, extra
copies of each of the special editions (“The Subaru Telescope
Special Edition 2016” July; “Mizusawa VLBI Observatory
Special Edition” December; “Hinode Solar Observatory 10th
Anniversary Special Edition” January; and “People Involvedin the TMT Project Vol.01 Special Edition” March) wereprinted and these aided the outreach efforts of each project.
The TMT Special Edition is especially noteworthy because
the office conducted international interviews in California and
Hawai‘i. The March issue was the California issue, including
12 articles published in both Japanese and English, making a
concerted effort towards content internationalization. From
now on, to develop and share NAOJ News articles as a resource
to be used as outreach content for each project, we plan topromote the production of overall, basic articles throughclose cooperation with researchers and promote internationalmagazine compiling. Other than periodicals, the 2017 calendar“SUBARU Telescope” (the 12th since 2005) was created. The
Office provided native check services to the Public Relations
Office; General Affairs Division, Administration Department;
and Hinode Science Center for English language publications,contributing to the expansion and enhancement of NAOJ’s
international information dissemination. In addition, like inother years support was also given to the publication of the“Rika Nenpyo, (Chronological Scientific Tables).”

8. International Astronomical Union Office for
Astronomy Outreach (IAU/OAO)
T he Of f ice for Ast ronomy O ut reach (OAO) of t he
International Astronomical Union (IAU), which is established
as an office in the Public Relations Center, communicatedwith National Outreach Contacts (NOC’s) (windows foroutreach in each country) in an effort to strengthen cooperative
relationships, communication, and coordination with 69 NOC’s
as of the end of the 2016 fiscal year. Significant progress wasmade between 17 NOC’s this fiscal year. In relation to this, IAU
OAO announced that from the next fiscal year we would begin
discussing outreach systems for each country that would be
more effective in achieving the objectives in the near future.
For international information provision, the office posted a
total of 550 postings from OAO on IAU social media during FY
2016. The Facebook community grew by 33 % and the Twittercommunity by 40 %. Meanwhile, the IAU Astronomy Outreach
Newsletter (e-mail news) was delivered 24 times and 300 items
of information were provided to 4,500 subscribers all over theworld. The newsletter has been translated and redistributed
into four different languages by collaborators in the respective
countries.
On May 16 –20, 2016, the Inter national Conference

CAP2016 of the IAU C2 committee was held in Medellín
City, Colombia with 140 participants from 30 countries. OAO
contributed to the management of the conference as one of
the Executive Chairs, and many staff members participatedand deepened international relations through presentations,workshops, etc. In cooperation with the Out reach and
Education Office and others, the Office successfully invitedthe international conference CAP 2018 to Fukuoka and isproceeding on preparatory work in cooperation with theconvention organizing committee members, Fukuoka City, andothers.
From September 24 to September 26, NAOJ and theJapanese Societ y for Education and Popular ization of
Astronomy co-hosted “The 3rd Symposium on Universal
Design for Astronomy Education” at NAOJ Mitaka Campus
with 131 attendees from 15 countries.
Our office also conducted a survey on the translation
network and summarized the key issues for OAO stakeholders
and the astronomy outreach community in establishingtranslation services and language translation requests as part of
OAO's activities. We held several evaluation meetings during
FY 2016 and begin experimental translation network projects
from FY 2017.
IAU OAO received international evaluation by IAU and
NAOJ from August 31 to September 2. This is because theagreement on OAO between the IAU and NAOJ was set
to expire at the end of the current fiscal year. A thoroughand fruitful evaluation process was carried out. The main
recommendation from the evaluators was that the scope ofastronomy outreach is very wide, so OAO should focus on
narrowing down its priorities, and performing projects in asystematic way. In response to the evaluation, OAO reviewed
its organization and division of labor, and after having attended
the Intercultural Communication Seminar, OAO is pursuing
its activities under a new organization structure. In February
2017, IAU and NAOJ exchanged new agreements for 2017-2021
based on the evaluation results.

II Status Reports of Research Activities11918. Division of Optical and Infrared Astronomy
1. Overview
The primary objectives of divisions in NAOJ are facilitating
and invigorating projects and individual research throughpersonnel exchanges to place researchers in environments moresuitable for their individual projects. While pursuing challenging
exploratory research on observation and development, thedivision furthers these goals by launching new projects asnecessary. The division also actively engages in graduate
education efforts to foster next-generation talent. These activities
are based on the concept that the Division of Optical andInfrared Astronomy is a center for personnel exchange between
Subaru Telescope, which engages in open use, and universities
and research institutes in Japan, which focus on developmental
research into new instruments and observational research. This
fundamental principle has been developed since the Subaru
Telescope was constructed.
The Division of Optical and Infrared Astronomy oversees
OAO (Okayama Astrophysical Observatory) and Subaru
Telescope (C Projects); the TMT-Japan (TMT-J) Project Officeand the Gravitational Wave Project Office (B Projects); and the
JASMINE Project Office and the Extrasolar Planet Detection
Project Office (A Projects). The Division and the Projects
carry equal weight in organizational terms. Almost all NAOJ
members in optical- and infrared-related fields have positionsin the Division with either the Division or one of the A, B, or
C Projects as the primary appointment. At times, they may
also have concurrent positions in other projects. The primarystaff of the Division of Optical and Infrared Astronomy in FY
2016 consisted of two professors, and four assistant professors(including one specially appointed assistant professor).
The Division coordinates educational, research, andadministrative activities for Subaru Telescope Mitaka Office andthe Extrasolar Planet Detection Project Office. Since personnel
transfer often occurs within the Division of Optical and Infrared
Astronomy, the Division plays an increasingly important role incoordinating between Subaru Telescope and the TMT-J Project
Office. The Division as a whole maintains and operates facilities
which are auxiliary to research, such as mailing lists and web
servers for Division of Optical and Infrared Astronomy-related
projects such as Subaru Telescope, TMT-J, Extrasolar Planet
Detection Project Office, Gravitational Wave Project Office, andJASMINE Project Office. The remainder of this report will focus
on the research projects conducted by the primary staff of theDivision of Optical and Infrared Astronomy and the activities ofprojects that support open use.

2. Observational Research(1) Observational Research Using Various Types of Telescopes
Observational research utilizing the Subaru Telescopefocuses on a wide variety of fields such as cosmology; galaxy120

II Status Reports of Research Activities

formation and evolution; the formation of stars and planets; thestructure and evolution of the Milky Way; stellar spectroscopy;
Solar System bodies; and the search for exo-planets. A surveyof high-z quasars was conducted in the survey data of Hyper
Suprime-Cam (HSC) on the Subaru Telescope. A comet which
was accidentally captured in a queue observation was analyzed
and utilized as data about the dust trail. Comets were observedat the Kiso Observatory of the University of Tokyo. The data
reduction in the search for extrasolar planets using direct
imaging methods continued. Based on the infrared observationsof protoplanetary disks by the Subaru Telescope, observations
were proposed to ALMA, and some data were obtained
successfully.
(2) International Cooperative Observational Research
The Division also engages in international collaborative
studies with overseas researchers.
Planning of the observations and the collaboration with the
Fessenkov Astrophysical Institute at Kazakhstan was promoted
for a cooperative observations with the East Asian Core
Observatories Association (EACOA) medium-size telescope andthe Optical and Infrared Synergetic Telescopes for Education
and Research (OISTER). In the OISTER workshop held on
November 21–22, 2016 at Kyoto University, a talk was given
by an attendee from the Fessenkov Astrophysical Institute. A
Kazakhstan-Japan Mini Workshop was held at the Fessenkov
Astrophysical Institute at Almaty, Kazakhstan during March 28–
April 1.
The site survey in western Tibet continued in cooperation
with the National Astronomical Observatories, Chinese Academyof Sciences (NAOC). Discussions for the site assessment andconstruction of a telescope were held with researchers of NAOC,
the Purple Mountain Observatory, and Hiroshima University.
A study on extended ionized gas in the Leo cluster was
conducted with researchers in Italy. A study on extended
ultraviolet regions around galaxies continued with researchers in
the USA.
(3) Research Using Archives
Researches on the verification of astronomical phenomena
described in the New Testament started jointly with the
National Institutes for the Humanities. Studies of astronomical
phenomena based on other old ephemerides and documents
continued. A statistical study on Ultra Diffuse Galaxies in the
Coma Cluster was conducted using archive data from the Subaru
Telescope.
The image data of the Kiso Ultraviolet-excess Galaxies(KUG) catalog and the corrections of the positions based on
the images were made available on the web page of the Kiso
Observatory. A paper on the update was submitted. Digitizationof Kiso Schmidt plates continued.

3. Observational Instrument Development
The effect of the environment inside the dome on seeing sizeat the Subaru Telescope has been studied through collaboration
with Chofu Aerospace Center of JAXA (Japan Aerospace
Exploration Agency), Tokyo Denki University, and RIKEN.
The procedure to compare the results of a fluid calculation and awater-flow experiment with the data from the Subaru Telescope
environment sensors in the dome was investigated. Analysis of
the ghost images of bright stars in the data of Hyper SuprimeCam at the Subaru Telescope was conducted and a presentation
was made about correction methods. Commissioning and testsof the Hosei Twin Astronomical Telescopes (HOTATE) andobservations using it were supported.

4. Operational Support for Subaru Telescope
The Division of Optical and Infrared Astronomy offers
support for the open use of the Subaru Telescope. This includes
organizing open calls for open-use programs, program selection,
administration, management of open-use-related travel expenses,
and promoting PR activities for Subaru Telescope. The Divisionalso provides support for various research conferences held at
Mitaka Campus.

postgraduate education to 23 graduate students from the
Graduate University of Advanced Studies, the University ofTokyo, Tokyo Institute of Technology, Nihon University, Hosei
University, and the University of Electro-Communications.
Division staff members made active contributions to seminars
and self-directed studies. Since April 2015 we have held a30-minute seminar in the afternoon every day throughout theyear. In December, we held the annual workshop of the Divisionof Optical and Infrared Astronomy so that staff members
and graduate students can understand the current studies andinterests of each other. The Division participated in the “Fureai(Friendly) Astronomy” project, dispatching lecturers to various
schools around the country, providing pupils at elementaryand junior high schools with opportunities to learn about andappreciate astronomy.
In collaboration with M-JEED, which is a project by
Mongolia and Japan for a higher engineering education
development promoted by the Japan International Cooperation
Agency (JICA), research abilities and human training were
improved through collaborations between teachers andresearchers in the National University of Mongolia and NAOJ.
In FY 2016, three NAOJ academic staffs visited the National
University of Mongolia during September 5-10 and lectured on
astronomy.

5. Research Environment Maintenance
The Division manages the printers and rented multi-function
photocopiers; sub-networks; and data backup servers for Subaru
Telescope Mitaka Office as part of its efforts to maintain the
research environment. The Division maintains the web servers
and their contents, and also gives assistance for setting-up
computers for new administrative supporters.

6. Planning of Next-generation Large-Scale Projects
The Division is engaged in planning post-Subaru large
projects in optical and infrared astronomy, such as TMT and
the JASMINE series. The preparation for the assessment of
new infrared detectors by the maintenance of old instruments
continued.

7. PR, Outreach, and Discovery of New
Astronomical Objects
The Division cooperates with the Public Relations Center insupporting matters related to the discovery of new astronomical
objects and PR/outreach activities such as publications andpress conferences related to Subaru Telescope research results.
A Tanabata talk event at Koganei was supported. The Division
actively participates in a special public event held at Mitaka
Campus (Mitaka Open House Day).

8. Educational Activities
The Division of Optical and Infrared Astronomy provides

II Status Reports of Research Activities12119. Division of Radio Astronomy
The Division of Radio Astronomy oversees Nobeyama
Radio Observatory, Mizusawa VLBI Observatory, the RISE
Lunar Exploration Project, and NAOJ Chile Observatory
operating the Atacama Large Millimeter/submillimeter Array(ALMA) and Atacama Submillimeter Telescope Experiment(ASTE). The scientists and engineers of these projects areattached to the Division of Radio Astronomy, which promotes
radio astronomy research to harmonize these radio astronomy
projects. The research themes of the Division of Radio
Astronomy are represented by keywords such as Big Bang, early
Universe, galaxy formation, black holes, galactic dynamics, starformation, planetary system formation, planets and satellites, theMoon, the evolution of interstellar matter, and the origin of lifein the context of the evolution of the Universe. Radio astronomy
unravels mysteries and phenomena in the Universe through radio
waves, which are invisible to human eyes. The detailed research
results are reported in each project’s section and in the researchhighlights. The Radio Astronomy Frequency Subcommittee has
been established within the division, engaging in discussions onprotection against artificial interference generated by electricalequipment, which causes major obstacles in radio astronomical
observations.

1. Radio Astronomy Frequency Subcommittee
The mission of the Radio Astronomy Frequency
Subcommittee is to protect the environment for radio astronomy
observations. In 1932, Karl Jansky of the U.S.A. first discovered
radio waves emitted by astronomical objects, albeit accidentally.
Since then, dramatic advances have been made in radio
observation methods, showing us new perspectives of the
Universe invisible at the optical spectrum. The fact is that four
Novel Prizes have been awarded to achievements made in thefield of radio astronomy.
Just as light pollution from artificial light sources is an
obstacle in optical observation, artificial radio interference
generated by the electronic devices which surround us is amajor obstacle in radio observations. Breathtaking advancement
has been achieved in wireless communication technologies inrecent years, and wireless commercial products such as mobile
phones, wireless LANs, and automotive radars are widelyused. The areas of radio applications will further expand in
the future owing to their ubiquitous nature. But because of
its unique capabilities, compatibility among various radio
services, including both active and passive ones, will become aserious issue. Frequency is a finite resource and its sharing is anunavoidable issue. Therefore, further efforts will be necessary
for maintaining the sky free from artificial interference for betterradio astronomy observations.
(1) Role and Organization
The purpose of the Radio Astronomy Frequency
Subcommittee is to ensure that radio astronomical observations

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are free from artificial interference and to raise public awarenessof the importance of the protection activities. Radio astronomical
observation does not emit radio waves; thus, it does notinterfere with other wireless communications. A proactive
approach is needed to widely raise awareness of the efforts
to protect the environment for radio observations. Regularexplanatory sessions are provided at the Ministry of Internal
Affairs and Communications (MIC) and regional Bureaus of
Telecommunications to solicit appreciation of the importance ofprotecting the field.
The coordination between the community of radio astronomy
and commercial wireless operators is led by MIC within Japanand internationally by the International Telecommunication
Union (ITU) Radiocommunication Sector (ITU-R) of the United
Nations. As part of the activities for FY 2016 the Subcommittee
took an active role in formulating the opinion of the Japaneseradio astronomical community (on behalf of the Japanese radio
astronomers) in these coordination efforts.
The Subcommittee is composed of members from NAOJ
and representatives of universities and research institutes inJapan.
(2) Current Challenges
A sharing study between active radio services and radio
astronomy is crucial for compatibility under the conditionof limited availability of frequency resources. Some rules
and regulations have been established to address the issue ofinterference cooperatively. The Radio Astronomy Frequency
Subcommittee remains responsible for taking measures for
new developments in wireless services including the following
challenges:- Significant increase in wireless activities in response to natural
disasters. After the Great East Japan Earthquake in 2011,
risk of radio interference has increased due to new wirelesscommunication services prepared for natural disasters.
- Development of new radio applications. There has been a rapid
increase in demand for higher frequencies. 76 GHz automobile
radars have become common. Wide band radars up to 81 GHz
may become more popular as they may reduce car accidents
resulting in injury or death. And, transportation of highspeed and high volume data, such as HDTV quality video, isbecoming possible through 60 GHz radio transmission systems.
Some satellite operators launched new plans for improving
broad-band communication to ships and planes globally.
- Reassigning of vacant frequency bands resulting fromenhanced efficiency in radio use. The digitization of television
broadcasting has created vacant frequency bands, which havebeen reassigned for mobile phones and other applications.
The effect of interference arising from such radio
applications (e.g. wireless business) varies widely depending on
the frequency band used. Radio astronomy observations havebeen given priority in a number of frequency bands within therange between 13.36 MHz and 275 GHz under the ITU Radio

Regulations (RR). However, negotiations will be necessary
between some radio services and radio astronomy if the samepriority level is to be shared within a certain band or underadjacent/proximity conditions. Even faint signals, of negligible
significance to general radio services, can have a chance of
substantial adverse effects on radio astronomy observations.
Sources of interference that need to be addressed continue
to increase and include the following devices and systems:
the 23 GHz CATV wireless transmission system used inemergencies, where ammonia observations are affected; 21
GHz next-generation satellite broadcasting, where water maser
observations are affected; 1.6 GHz mobile satellite phones for
emergencies, where the observation of pulsars and the likeare affected; a number of new UWB wireless applications
used by logistics and manufacturing industries, where
geodetic observations are affected; and Ka-band broad-bandcommunication from airliners to satellites, where water maser
observations are affected. 79 GHz automotive radars aroundNobeyama Radio Observatory have considerable impact on theobserving conditions. Although radio astronomy observationsin the 60 GHz band are not common because of the high rateof absorption in the atmosphere, the 60 GHz system must be
watched closely because its second harmonic can have adverse
effects on CO observations in the 115 GHz band.
(3) International Activities
The ITU Radio Regulations (RR), which allocate radio
frequencies to wireless applications, are revised once every three
to four years in the World Radiocommunication Conference(WRC). The RR includes frequency bands in which radio
astronomy observation is prioritized. Among these meetings,
the Radio Astronomy Frequency Subcommittee is regularly
involved in the WP7D (radio astronomy) and WP1A (frequency
management) meetings. The Subcommittee also takes part invarious international conferences, representing the Japanesecommunity of radio astronomy researchers.
In FY 2016, the Subcommittee participated in the ITU-R
WP7D meetings in April and October and the WP1A meetingsin May and November held in Geneva; and APG19-1 meetingin July in Chengdu, China. In these meetings, the following
items were discussed as major agenda items related to radio
astronomy: modernization of Global Maritime Distress Safety
Systems (GMDSS) utilizing 1.6 GHz satellite communication;
upgrading the maritime radio communication system utilizing
the 160 MHz maritime mobile-satellites, establishment ofa correspondence group for compatibility studies to ensurecompatibility between vehicle radars and the radio astronomy
activities, identification of frequency band candidates for the
new International Mobile Telecommunications (IMT2020)and so on. The WRC-19, which is scheduled for 2019, aims toidentify frequency bands for IMT2020 from eleven candidate
frequency bands ranging from 24 GHz to 86 GHz and to allocate
active services to frequencies above 275 GHz.
(4) Activities in JapanThe three major domestic activities of the Radio

Astronomy Frequency Subcommittee include: participationin various committees and working groups hosted by MIC,
direct negotiations for MIC’s authorization with wirelessoperators who generate radio interference, and promotion
to raise public awareness about radio interference to radio
astronomical observations. Negotiations with wireless operators
to reduce interference sources represent a major part of the
Subcommittee’s activities in Japan.
The committees and working groups hosted by MIC are
held to organize domestic tactics in preparation for international
conferences, defining Japan’s positions on various wirelessissues. Other MIC-related meetings provide opportunities
for discussing the radio application technologies related to
MIC’s wireless policy, and for negotiating with wirelessoperators on interference issues under MIC authorization.
Negotiations directly affecting the protection of radio astronomy
observations have been conducted concurrently to dealing with
the interference problems related to societal and technologicaltrends.
Several examples of the interference problems discussed in
section (2) above are given below.
For 24 GHz automotive radars, new regulations have been
prepared to make an automatic turn-off function a mandatory
standard feature so that the device is disabled upon reachingcertain areas around radio observatories.
In November 2015 WRC-15 resolved to allocate 77.5–78
GHz to the radiolocation service, allowing automotive vehicles
to utilize the whole 76–81 GHz band for their radar, while there
is a predicted increase in the use of 76 GHz and 79 GHz highresolution automobile radars. Of particular concern are thepossible effects of interference from these radars on the 45-m
radio telescope at Nobeyama Radio Observatory, which engages
in observations of the spectral-lines of deuterated compounds
and other molecules in interstellar matter. The observations
with the Nobeyama 45-m Radio Telescope located in Japan willcontinue to carry significance in relation to the international
project ALMA, which deploys 66 high-performance radio
telescopes at an altitude of 5,000 m in Chile. Since automotive
radars are highly relevant to human life safety, negotiations
have been conducted with careful analysis in order to reach amutually acceptable agreement.
A new radio wave application is being planned for 21 GHz
next-generation satellite broadcasting with a picture resolution
16-fold higher than that of the current HDTV. This band is nearthe 22 GHz radio astronomy band, which is important for watermaser observation. The radio signals from the satellite comefrom outer space. Their detrimental effects need to be alleviatedwith a filter at the output stage of the satellite. The NHK Science& Technology Research Laboratories developed a prototype
bandpass filter to suppress spurious signals to an acceptablelevel. NHK plans to verify its performance further on a futuresatellite set to launch in December, 2017.
Radio observations in the 60 GHz band are not common
because of the high atmospheric absorption rate in thatfrequency range. Albeit in fact, the 60 GHz system must be
watched closely in terms of its proliferation in the market, since

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123

interference from it may affect CO observations in the 115 GHz
band, which is within the band of the second harmonics of the
60 GHz radio system.
Following the MIC discussion for improving disastermeasures, the committee discussed with Globalstar Inc. (USA)and signed the revision to the operating condition agreement
to establish guard channels and radio quiet zones considering
the risk of interference to the radio astronomy (OH maser
observation) band from spurious emissions from the 1.6 GHz
satellite uplink signal.
In a MIC working group, the Subcommittee was originallyconcerned that Ka-band broad-band satellite communication
services may cause interference to radio astronomy observatories
in Japan. However, the evaluation of both the 22 GHz downlink
and airliners’ 30 GHz uplink signal resulted in developing
appropriate operating conditions with no risk of interference tothe observatories including Nobeyama Radio Observatory. The
working group plans to make a similar evaluation of operating
conditions for other satellite operator systems in FY 2017.
Additionally, radio astronomy observations could be
adversely affected by some of the new wireless technologies:
wireless power transmission (WPT) for electric vehicle
energy charging (non-beam); next generation railway radio
communication systems between bullet trains and trackside; andso on. The Subcommittee continues to monitor their progressand shares this information with related radio astronomers.
Moreover, the Subcommittee has been engaged in making
applications to the MIC to request frequency protection for
the NAOJ telescopes as well as other telescopes owned by theJapanese community of radio astronomers on their behalf.
Collecting actual interference cases at various observatories
is also important. To raise public awareness about “Interference
to Radio Astronomy,” these collected cases are effectively
used in presentations by our community members. We are also
preparing tutorial materials for the general public. As opticalastronomers are actively working to protect their observation
environment against artificial light, we, radio astronomers, aremaking the same efforts for the sake of continuing observations
in radio astronomy in coming ages.

124

II Status Reports of Research Activities20. Division of Solar and Plasma Astrophysics
The Division of Solar and Plasma Astrophysics is mainly
made of staff members from the Solar Observatory, the Hinode
Science Center, and the Solar-C Project Office. It conducts
research on the Sun in close coordination with these projects.
An NAOJ fellow and graduate students supervised by the staffof the above-mentioned projects also belong to the Division.
All of the permanent staff of these projects is affiliated with theDivision.
The Division conducts both theoretical and observational
research into the inner structure of the Sun and outer solar
atmosphere including the photosphere, chromosphere, corona,and solar wind; and various phenomena in the magnetizedplasma such as flares, sunspots, solar faculae, and prominences.
The Division’s theoretical research includes helioseismology
studies of the internal structure of the Sun, and applicationsof plasma physics and magnetohydrodynamics to various
phenomena on the Sun as well as on Sun-like stars. The solargroup at NAOJ started observations from space in the very earlystages of Japan’s space program. The Division has participatedin the development of the Hinode satellite, which is currently
in orbit, and is playing a major role in its scientific operation.
In ground based observations, the Division conducted research
to introduce and utilize new technologies in the Solar Flare
Telescope and has been conducting long-term monitoring
observations of solar activity, and the obtained data are open to
the community.

visited solar-related research organizations and experienced thelatest research in the field.

3. International Cooperation
Y. Katsukawa has been a member of the Science Working
Group of the Daniel K. Inouye Solar Telescope, a 4-m telescope
under construction at Haleakala, Hawai`i. Some members of
the Instituto de Astrofísica de Canarias of Spain came to Japanto promote the construction of another 4-m solar telescope,
which is now in the planning stage in Europe, and a meeting todiscuss the collaboration was held. Several plans are also underconsideration for future ground-based telescopes that would
involve collaborations with East Asian countries and Peru.

1. Research in Solar Physics
NAOJ fellow S. Toriumi published two papers in refereed
journals as lead author. One is about the statistical analysisof the flare-productive active regions, while the other is on
the coordinated observation of small-scale energy releasing
events in a developing active region by Hinode and IRIS. He
also published one refereed paper on flare statistics as a coauthor. Toriumi has been promoting collaborative research withinternational partners; he invited Prof. R. Rutten of Lingezicht
Astrophysics/University of Oslo/Utrecht University andorganized a scientific meeting on the formation of the solar
spectrum.
The Division has a seminar (on Friday afternoon, roughly
twice a month) whose speakers are from both inside and outsideof the Division. The organizer for this year was S. Toriumi.

2. Educational Activities
The teaching staff of the Division supervised three graduate
students from the Graduate University for Advanced Studies(SOKENDAI). Among them, N. Kambara and M. Yoshidapassed the examination for the Master’s degree. The Division,in cooperation with Kyoto University and Nagoya University,
supported the annual “Leading-edge Solar Research-Experience
Tour” in March for undergraduate students; eight students

II Status Reports of Research Activities12521. Division of Theoretical Astronomy

126

1. Overview

2. Current Members and Transfers

The Division of Theoretical Astronomy (DTA) engaged
in research activities for FY 2016 with the aim of achieving
internationally outstanding research results both in quality andquantity to accomplish of the following four goals that were set
by NAOJ:- Advance world class cutting-edge theoretical research.
- Pursue theoretical astronomy research, particularly inareas that utilize the NAOJ supercomputers or large-scaleobservational instruments to give further insight into their
future development.
- Encourage collaborations among researchers in Japan andstrengthen domestic theoretical astronomy research.
- Invigorate postgraduate education.
The division handles a wide variety of themes in theoreticalastronomy research, addressing a diversity of hierarchicalstructures of the Universe in terms of formation and evolution
processes, dynamics, and physical state of matter, coveringa span from the early Universe to galaxies, stars, planetary
formation, activities of compact objects, the origins of spacetime, and plasma phenomena in astronomy and astrophysics;
joint research with observational astronomy using observational
instruments of various frequency bands such as the Subaru
Telescope, ALMA, and Nobeyama radio telescopes; andinterdisciplinary research with neutrino cosmology, gravitational
wave astronomy, physics of elementary particles and atomic
nuclei.
The Division of Theoretical Astronomy aims to facilitate
Japan’s high competitiveness on the international plane throughcontinuous production of world-leading research results andoffers a superb research environment as a base for theoreticalresearch accessible to researchers in Japan and overseas. It
has accepted a wide range of both Japanese and international
researchers as visiting professors, visiting project research
fellows, and long-term research fellows who actively engage
in various research projects in the division. In particular,
the division has fostered research developments to create an
influential research center for young researchers and is actively
engaged in personnel exchanges with many universities andresearch institutes. In addition, the division actively organizes
numerous cross-disciplinary international conferences, domestic
meetings, and seminars for the fields of theoretical astronomy
and astrophysics, observational astronomy, and experimental
physics; and it leads research activities in various related fields
of astronomical science. The division’s full-time professors,
associates, assistants, and project assistant professors, together
with NAOJ postdoctoral fellows and EACOA fellows, researchexperts, specially appointed research staff, JSPS fellows, andresearch supporters conduct theoretical astronomy research andeducation involving postgraduate students from the Graduate
University of Advanced Studies, the University of Tokyo, and
the Graduate School of Japan Women’s University.

In FY 2016, the dedicated faculties of the Divisionof Theoretical Astronomy included two professors, two
associate professors, and four assistant professors in addition
to one adjunct professor and one adjunct assistant professor
who concurrently held primary positions at the Center for
Computation Astrophysics. In addition to these research andeducational members, the division was served by five project
assistant professors, including one research associate, two JSPS
fellow, two EACOA fellows, and in addition one administration
associate who gave full support to all activities of the division.
Among them Takeshi Inoue, an assistant professor, moved to
Nagoya University as an associate professor from November in
2016.

II Status Reports of Research Activities

3. Research Results
The research papers and presentations in international
conferences carried out by the division members as author(s)or presenter(s) are listed below. Categories with fewer than 5
publications have been omitted.
- Peer-reviewed papers in English: 91- Reports in English (talks at international conferences): 71(invited talks: 16)- Reports in Japanese (talks at national meetings, etc.): 42
Some of the research results are presented as the researchhighlights listed at the beginning of this report. The following
highlights include research in which the division members tookleading roles:- Impact of New Gamow-Teller Strengths on Explosive Type Ia
Supernova Nucleosynthesis (Mori, K., Kajino, T. et al.)- New Electron Orbits in Collisionless Magnetic Reconnection(Zenitani, S. et al.)- Kilonova Emission from Compact Binary Mergers (Tanaka, M.
et al.)- Chemodynamical Evolution of Dwarf Galaxies Deduced fromr-process Elements (Hirai, Y., Kajino, T. et al.)
- H0LiCOW - Lens Mass Model of HE 0435-1223 and Blind
Measurement of Its Time-delay Distance for Cosmology(Wong, K. C. et al.)- Properties of Interstellar Dust Responsible for Steep Extinction
Curves toward Type Ia Supernovae (Nozawa, T. et al.)- Circumstellar and Explosion Properties of Type Ibn
Supernovae (Moriya, T. et al.)- Radio Transients Associated with Accretion-induced Collapseof White Dwarfs (Moriya, T.)- Supernovae Powered by Magnetars that Transform into Black
Holes (Moriya, T. et al.)- Properties of Magnetars Mimicking 56Ni (Moriya, T. et al.)- Formation of Spiral Arm in Galaxies by Swing Amplification(Kokubo, E. et al.)- Planetesimal Formation by Gravitational Instability of PorousDust Aggregates (Kokubo, E. et al.)
- N-Body Simulation of Chariklo's Ring (Kokubo, E. et al.)- Heavy Element Production in Type II Supernovae: Sensitivity
to Nuclear Equation of States (Kajino, T. et al.)- Relativistic Screening Effects on Big Bang Nucleosynthesis
and Low-lying Resonances (Kajino, T. et al.)- Detectability of Cosmic Dark Flow in the Type Ia Supernova
Redshift-Distance Relation (Kajino, T. et al.)- Impact of Sterile Neutrino Dark Matter on Core-collapse
Supernovae (Kajino, T. et al.)- Neutrino Antineutrino Pair Emissions in Strongly Magnetized
Neutron-Star-Matter in Relativistic Quantum Approach(Kajino, T. et al.)- Possible Measurements of Reaction Cross Sections for
Explosive Nucleosynthesis using Laser -Driven γ-ray Pulses(Kajino, T. et al.)- Isomer Production Ratio of 113Cd following Neutron-Capture
Reactions to Investigate the Origin of 115Sn (Kajino, T. et al.)- Solving the Red Supergiant and Supernova Rate Problems via
Relic Supernova Neutrino Spectrum (Kajino, T. et al.)- Non-Extensive Statistics Solution to the Cosmological Lithium
Problem (Kajino, T. et al.)The following research results are released on the division’s
website (http://th.nao.ac.jp/) as research highlights:- Japan OISTER collaboration uncovers the origin of
extraordinary supernovae (Tanaka, M. et al.)
- Avoiding “Traffic Jam” Creates Impossibly Bright “Lighthouse”(Kawashima, T., Ohsuga, K. et al.)- New classes of electron orbits in magnetic reconnection(Zenitani, S. et al.)- Cosmic lenses Bring the Universe’s Expansion into Sharper
Focus (Wong, K. C. et al.)- Metallic Iron Grains Hardly Exist in the Universe (Nozawa, T.
et al.)- Mystery of Nucleosynthesis in Type Ia Supernova: Challenge
from Precise Nuclear Physics (Mori, K., Kajino, T. et al.)- Early evolutionary histories of galaxies deduced from r-processelements (Hirai, Y., Kajjino, T. et al.)- An Elegant Solution of the Big-Bang Lithium Problem?
(Kajino, T. et al.)

4. Domestic Collaborations
The Division of Theoretical Astronomy played leading roles
in organizing the following domestic conferences:- 5th TDA Symposium on “Pre-solar Grains, Evolution ofInterstellar Dust, and the Origin of the Solar System”, NAOJ
Mitaka Campus, September 26 - 27 in 2016. (Participants; 38)- Japan SKA Joint Science Forum on “Cosmic Magnetic Field:
from Intra-Galactic Phenomena to Large Scale Structure”,

Yamagata Zao, October 27 - 29 in 2016. (Participants; 35)- 6th TDA Symposium on “Role of the Magnetic Field in Stellar
Formation and its Observational Evidence”, NAOJ Mitaka
Campus, November 24 - 25 in 2016. (Participants; 37)- 29th RIRONKON Symposium on “Cosmic Hierarchical
Structure driven by Gravity”, NAOJ Mitaka Campus,
December 20 – 22 in 2016. (Participants; 153)

5. International Collaborations
Toshitaka Kajino performed duties of the following posts:
international referee for the National Sciences and Engineering
Research Council of Canada (NSERC); international referee
for Partnership for Advanced Computing in Europe (PRACE);
international associate for the European Centre for Theoretical
Studies in Nuclear Physics and Related Areas (ECT*); andinternational referee for the Swiss National Science Foundation(SNSF). Eiichiro Kokubo served on the organizing committeeof Commission A4 (Celestial Mechanics and Dynamical
Astronomy) of IAU.
The Division of Theoretical Astronomy played leading roles
in organizing the following international conferences:- The 4th DTA Symposium on Compact Stars and Gravitational
Wave Astronomy, NAOJ Mitaka Campus, May 13 – 14 in
2016. (Participants; approx. 20)- NIC XIV School on Nuclear Astrophysics, Niigata University,
June 13 – 17 in 2016. (Participants; approx. 70)- 14th International Symposium on Nuclei in the Cosmos(NIC XIV), Toki Messa in Niigata, June 19 – 24 in 2016.
(Participants; approx. 300)
- 2nd NAOJ-ECT* International Workshop on Many Riddles
About Core-Collapse Supernovae: 1 Bethe and Beyond, NAOJ
Mitaka Campus, June 27 – July 1 in 2016. (Participants; 52)- 9th Meeting on Cosmic Dust, Aobayama Campus in Tohoku
University, August 15 – 19 in 2016. (Participants; 51)- Japan-Germany Planet and Disk Workshop, Ishigaki in
Okinawa, September 25 – 30 in 2016. (Participants; approx. 50)- Quarks and Compact Stars 2017 (QCS2017), Yukawa Institutein Kyoto University, February 19 – 22 in 2017. (Participants;
approx. 70)

6. Educational Activities
The lecture subjects are listed below to supplement Section
III on activities of research and educational adjunct lecturer-ship
at the universities and graduate schools:· Toshitaka Kajino: Lectures on fundamentals of theoreticalastronomy at the Graduate University for Advanced Studies;science of time, space, and matter, and fundamentals of physics
at Gakushuin University; astrophysics and modern physics at
Japan Women’s University; astrophysics at Jissen Women’s
University; nuclear physics at Meiji University; astronomy
investigation I & II, reading papers in turn I & II, and special

II Status Reports of Research Activities

127

astronomy investigation II at the Graduate School of the
University of Tokyo.
· Eiichiro Kokubo: Earth and Planetary Sciences I at the
University of Tokyo, Solar System and Exoplanetary Systems at
the University of the Ryukyu.
· Masashi Tanaka: Introduction to observational astronomy Iat the Graduate University for Advanced Studies; advanced
astrophysics at Chiba University; advanced stellar physics II at
Tohoku University.
· Takashi Hamana: Geology at the Tokyo University ofAgriculture and Technology.
Tomoya Takiwaki and Eiichiro Kokubo also delivered SSH
lectures on “Supernovae, culminating their Stellar Evolution"
at Aichi prefectural high school and “Solar System andExoplanetary Systems” at Kanazawa Izumigaoka high school,
respectively, and contributed much to high school education.

7. Outreach Activities
The Division of Theoretical Astronomy actively engaged inpublic promotions and outreach activities by offering lectures to
the general public. The following lectures were delivered thisyear:
· Toshitaka Kajino: “Cosmology towards the Origin of Matter
and Time and Space” (International Conference NIC2017
Commemorative Lecture, Hitotsubashi Auditorium, Tokyo);“Origin of Heavy Elements” (Cosmo-Nuclear Physics Forum,
RIKEN, Wako)· Eiichiro Kokubo: “Solar System” and “Exoplanetary Systems”
at Niigata Citizen University; “From Stardust to the Earth” at
Osaka Prefectual University; “The Blue Planet” at Yokohama
Aasahi Culture Center; “Form Stardust to the Earth and Moon”
at Discovery Park Yaizu; “Exoplanet Zoo” at Ikebukuro
Community College; “Introduction to Planet Formation Theory”
and “Solar System and Exoplanetary Systems” at Waseda
University Extension Center; “The Origin of the Earth” atKonan University· Takiwaki Tomoya: “Science Frontier of Core-Collapse
Supernovae” (Asahi Culture Center Tokyo); “Supernovae,
culminating their Stellar Evolution” (Asahi Culture Center
Yokohama); “Universe” (Shimadoromu General Lecture,
Science and Technology Museum, Tokyo)· Masaomi Tanaka: “The Life of a Star and Supernova
Explosions” (Asahi Culture Center Shinjuku); “Following
the Moment of a Supernova Explosion” (Mitaka Network
University); “Science Frontier of Core-Collapse Supernova
Observation” (Asahi Culture Center Shinjuku); “What is the
Death of Massive Stars like – Approaching the Mysteries ofSupernova Explosions” (Sundai Gakuen Sundai Astronomy
Seminar); “What is the Death of Massive Stars like – Exploring
the Moment of a Supernova Explosion” (Science Cafe Orion)

128

II Status Reports of Research Activities

8. Awards
Tomoya Takiwaki was awarded the ASJ Young Astronomer
Award 2016. Seiji Zenitani and Masaomi Tanaka were given
the MEXT Young Scientists’ Awards. Masato Shirasaki and
Masaomi Tanaka received awards from the Inoue Foundation for
Science.

9. Main Visitors from Overseas
The Division of Theoretical Astronomy strives to fulfill its
roles as a center of excellence in Japan for theoretical studies inastronomy and astrophysics and also as an international research
institution by providing an excellent research environment.
It engages in various joint research projects with visiting
researchers from overseas, with the help of Grants-in-Aid
for Scientific Research, government subsidies for operating
expenses, the NAOJ budget for guest visitors, and others. The
main international visitors of FY 2016 to the division are listed
below:
Akif B. Balantekin (University of Wisconsin–Madison, US)
Carmen Adriana Martinez Barbosa (Leinden University,
Netherlands)
Melina Bersten (National University of La Plata, Argentina)
Myung-Ki Cheoun, (Soongsil University, South Korea)
Emmanouil Chatzopoulos (Lousiana State University, USA)
Vivien Chen (National Taiwan University, Taiwan)
Chau Ching Chon (Academia Sinica, Taiwan)
Silvio Cherubini (Catania University, Italy)
Roland Diehl (Max Planck Institute/Technical University of
Munich, Germany)
Kevin Ebinger (University of Basel, Switzerland)Marius Eichler (University of Basel, Switzerland)
Michael A. Famiano (Western Michigan University, USA)
Morgan Fraser (University College Dublin, Ireland)
Gaston Folatelli (National University of La Plata, Argentina)
Carla Frohlich (University of North Carolina, USA)
Federico Garcia (Argentine Institute of Radio Astronomy,
Argentina)
Tristan Guillot (Nice Observatory, France)
Ji-an Jiang (University of Cambridge, UK)
Oliver Just (Max Planck Institute, Germany)
Kostas Kokkotas (University of Tübingen, Germany)
Takami Kuroda (University of Basel, Switzerland)
Kyunjin Kwak, (Ulsan National Institute of Science &Technology, Korea)
Shih-Ping Lai (National Taiwan University, Taiwan)
Sheng-Jun Lin (National Taiwan University, Taiwan)
Doug Lin (University of California Santa Cruz, USA)
Andreas Lohs (University of Darmstadt, Germany)
Grant J. Mathews, (University of Notre Dame, USA)
Gail Mclaughlin (University of North Carolina, USA)
Annabella Mondino Llermanos (National University of Cordoba,
Argentina)
Bernhard Mueller (The Queen's University Belfast, UK)Quang Nygen-Luong (Korea Astronomy and Space Science
Institute, Korea)
Valerio Pirronello (Catania University, Italy)
Yoshito Shimajiri (Saclay Nuclear Research Centre, France)
Benjiamin Wehmeyer (University of Basel, Switzerland)

II Status Reports of Research Activities12922. Office of International Relations
The Office of International Relations strives to promote andfacilitate further internationalization at NAOJ by maintaining
an environment where multi-cultural researchers and students
can engage cooperatively in research and educational activities.
Specifically, the Office’s main activities include supportinginternational collaborative projects; managing Security
Export Control; liaising with overseas astronomical researchorganizations; gathering and providing information oninternational activities; offering support for hosting international
conferences, workshops, and seminars; providing support for
visiting international researchers and students; and assisting
Japanese universities and research organizations for international
partnerships. In FY 2016 the Office continued to work closelywith the Executive Advisor to the Director General in charge ofinternational research coordination.

1. International Collaborative Project Support

130

Furthermore, the Office supported the activities of the Officefor Astronomical Outreach of the IAU (IAU OAO) and the IAU
Office for Astronomy Development (OAD, located in South
Africa).
The Office cooperated with the IAU OAO during the review
of OAO activity from the end of August to early September.
The Office also supported the NAOJ Public Relations Officewith its exhibit at New Scientist Live held in London during
September 28–October 1. Additionally, the Office displayed an
exhibit to present NAOJ’s projects and research results together
with recruitment information at the EAMA10 (10th East Asian
Meeting on Astronomy) held September 26–30 at Seoul, South
Korea.
The Office supported the organization of the JCMT TAC
held in Mitaka during November 21–23, and the East Asian
Astro Statistics Workshop held in Mitaka during February 27–
March 2.
Pursuant to the reorganization of the Public Relations
Office, it has been decided that the Public Relations Office will
be responsible for overseas activities in relation to the generalpublic, while the Office of International Relations will be incharge of activities related to overseas researchers.

The Office of International Relations serves as a liaison
point for international activities, engages in international
agreements or provides support for doing so, and accumulates
procedural and administrative knowledge, through consultations
or investigations on individual cases to enter into and implement
collaboration with overseas universities or research institutions.
Other matters handled by the Office include administrative
coordination in approval processes to sign agreements andmemoranda for international collaborations, conducting
preliminary reviews for legal documentation, supporting
signing ceremonies, and managing Security Export Control
for export of goods or transfer of technology. In FY 2016,
nine international agreements, new and renewed, were signed
including ones under the name of NINS. In the area of Security
Export Control, activities included review and processing of
70 cases (121 items), and an Security Export Control briefing
was held in October at Mitaka (15 attendees including 1 from
Nobeyama through TV conference connection) for improving
the knowledge and awareness of NAOJ staff.

The Office of International Relations offers support forthe planning and implementation of international research
conferences, workshops, and seminars hosted or supportedby NAOJ. The work involves consultation and responses toinquiries regarding administrative issues. The Office alsooffers advice about which organizations or individuals tocontact as appropriate, coordinates between organizations, andgathers relevant information. In FY 2016 the Office supported
international research conferences and other events by preparing
documentation for Japanese visa applications for 36 foreign
participants in total.

2. Liaison Work for Overseas Astronomical
Research Organizations

4. Support for Hosting International
Researchers and Students

The Office of International Relations supported theorganization of the East Asian Observatory (EAO) Board
meeting and the JCMT Board and users’ meeting, both held at
Mitaka during April 13–14, 2016, and April 15–18, respectively.
At the same time, the Office organized the annual directorate
meeting of the East Asian Core Observatories Association(EACOA). The four institutions forming the EACOA include
NAOC (China), NAOJ (Japan), KASI (South Korea), and
ASIAA (Taiwan). The Office also assisted the Executive Advisor
to the Director General in charge of international researchcoordination in coordinating with the other 3 institutions forselection of the 2017 EACOA postdoctoral fellowship program.

The Office enhanced its framework for offering organizational
support for research, education, and living arrangements forforeign researchers and exchange students. The Support Desk
offers support services to ease difficulties for foreigners living
in Japan. It supports, on-site if required, covering various
matters such as administrative procedures at municipal and othergovernmental offices; finding and moving into an apartment andother various procedures and applications for starting up a newlife; consultation on shopping, children’s education, health andothers; and gathering/providing useful information relating toeveryday life. The Support Desk has been highly appreciatedby users. The Office continued the Japanese language lessons,

II Status Reports of Research Activities

3. Support for Hosting International Research
Conferences, Workshops, and Seminars

helping foreign members of NAOJ acquire beginner level
capability, and for FY 2016, a combination of E-learningfeatures and classroom lessons were provided, as was introducedin the previous year. The Office also provided support for visa
applications, and including renewals; support was given to 48
applications: 12 for staff and family members, 18 for invitedresearchers, and 18 for visitor/long stay researchers.
• The Office continued its activities to support non-Japanese
speaking staff, by translating various forms for applications
and notices, including e-mail text and explanations ofprocedures (67 documents).

5. Assistance in International Partnerships
Involving Japanese Research Organizations
The Office of International Relations assists universities andother educational and research organizations in Japan to engage
in international partnerships. It also liaises with the International
Strategy Headquarters and the International Cooperation
Office at NINS to coordinate international collaborations. The
Office oversaw the Optical and Infrared Synergetic Telescopesfor Education and Research (OISTER) project conducted by
Okayama Astrophysical Observatory, Ishigakijima Astronomical
Observatory, and nine Japanese universities.
Although the budget for the OISTER project will betransferred to the Research Promotion Division from FY 2017
onward, the Office will continue to provide administrative
support.

II Status Reports of Research Activities

131

III Organization
1. Organization

Projects(C Projects)

Subaru Telescope
Okayama Astrophysical Observatory
Nobeyama Radio Observatory
Advisory Committee for Research and Management

Mizusawa VLBI Observatory
Solar Observatory
NAOJ Chile Observatory
Center for Computational Astrophysics
Hinode Science Center

Director General(B Projects)

Vice-Director General (on General Affairs)

Gravitational Wave Project Office
TMT-J Project OfficeVice-Director General (on Finance)
Director of Engineering
Director of Research Coordination(A Projects)

JASMINE Project Office
Extrasolar Planet Detection Project Office
RISE Project
SOLAR-C Project Office

Executive Advisors to the Director General

Centers
Astronomy Data Center
Advanced Technology Center
Public Relations Center
Divisions
Division of Optical and Infrared Astronomy
Division of Radio Astronomy
Division of Solar and Plasma Astrophysics
Division of Theoretical Astronomy
Research Enhancement Strategy Office
Research Evaluation Support Office
Office of International Relations
Human Resources Planning Office
Safety and Health Management Office
Engineering Promotion Office
Administration Department

132

III Organization

2. Number of Staff Members(2017/3/31)
Regular Employees
Director General
Research and Academic Staff
Professor
Executive Engineer
Associate Professor
Chief Research Engineer
Assistant Professor
Research Associate
Research Engineer
Engineering Staff
Administrative Staff
Research Administrator Staff
Employees on Annual Salary System
Fixed-term Employees
Full-time Contract Employees
Part-time Contract Employees

1
152
27
0
39
11
59
0
16
36
57
7
117
56
131

3. Executives
Director General
Vice-Director General
on General Affairs
on FinanceDirector of Engineering
Director of Research Coordination

Watanabe, Jun-ichi
Kobayashi, Hideyuki
Takami, Hideki
Gouda, Naoteru

Executive Advisor to the Director General
Executive Advisor to the Director General

Ogasawara, Ryusuke
Sekiguchi, Kazuhiro

Hayashi, Masahiko

III Organization

133

4. Research Departments
Projects
C Projects

Subaru Telescope
Director
Arimoto, Nobuo
Professor
Arimoto, Nobuo
Professor
Ohashi, Nagayoshi
Associate Professor
Hayashi, Saeko
Associate Professor
Iwata, Ikuru
Associate Professor
Kodama, Tadayuki
Associate Professor
Noumaru, Junichi
Associate Professor
Takato, Naruhisa
Associate Professor
Takeda, Yoichi
Chief Research Engineer Iwashita, Hiroyuki
Assistant Professor
Imanishi, Masatoshi
Assistant Professor
Komiyama, Yutaka
Assistant Professor
Koyama, Yusei
Assistant Professor
Minowa, Yosuke
Assistant Professor
Okita, Hirofumi
Assistant Professor
Onodera, Masato
Assistant Professor
Pyo, Tae-soo
Specially Appointed
Hayashi, Masao
Assistant Professor
Specially Appointed
Tanaka, Masayuki
Assistant Professor
Research Engineer
Bando, Takamasa
Senior Engineer
Namikawa, Kazuhito
Senior Engineer
Omata, Koji
Chief Engineer
Tamura, Tomonori
Engineer
Sato, Tatsuhiro
Specially Appointed
Niino, Yuu
Research Staff
Specially Appointed
Takagi, Yuhei
Research Staff
Specially Appointed
Toshikawa, Jun
Research Staff
Specially Appointed
Hayashi, Yusuke
Senior Specialist
Specially Appointed
Ikeda, Hiroyuki
Senior Specialist
Specially Appointed
Oishi, Yukie
Senior Specialist
Specially Appointed
Taniguchi, Akimitsu
Senior Specialist
Research Expert
Kawanomoto, Satoshi
Research Expert
Koike, Michitaro
Research Expert
Mineo, Sogo
Research Expert
Yamada, Yoshihiko
Research Expert
Yamanoi, Hitomi
Administrative Supporter Kuwata, Hitomi
Administrative Supporter Noguchi, Masumi
Administrative Supporter Suehiro, Yoko134

III Organization

Administrative Supporter Takamoto, Masami
Administrative Supporter Yamada, Narumi
Administrative Supporter Yoshida, Chie
Administration Department
ManagerSeto, Yoji
General Affairs Section
Chief
Chiba, Satoko
Accounting Section
Senior Staff
Sugawara, Satoshi
RCUH
RCUH
Alpiche, Dex
RCUH
Aoki, Kentaro
RCUH
Aso, Yusuke
RCUH
Balbarino, Michael
RCUH
Berghuis, Jennie
RCUH
Bulger, Joanna
RCUH
Castro, Timothy
RCUH
Clergeon, Christophe
RCUH
Currie, Thayne
RCUH
Conol, JonahRCUH
Cook, David
RCUH
Doi, Yoshiyuki
RCUH
Doughty, Danielle
RCUH
Elms, Brian
RCUH
Endo, Mari
RCUH
Ferreira, James
RCUH
Finet, Francois
RCUH
Formanek, Keiko
RCUH
Fujiwara, Hideaki
RCUH
Fujiyoshi, Takuya
RCUH
Gaskin, Roberta
RCUH
Gorman, William
RCUH
Guthier, Debbie
RCUH
Guyon, Olivier
RCUH
Hasegawa, Kumiko
RCUH
Hattori, Takashi
RCUH
Hopkins, James
RCUH
Inagaki, Takeshi
RCUH
Jeschke, Eric
RCUH
Jovanovic, Nemanja
RCUH
Kackley, Russell
RCUH
Kakazu, Yuko
RCUH
Kerns, Michael
RCUH
Kim, Ji Hoon
RCUH
Koshida, Shintaro
RCUH
Kudo, Tomoyuki
RCUH
Kyono, Eiji
RCUH
Lee, Chien-Hsiu
RCUH
Lemmen, Michael
RCUH
Letawsky, Michael
RCUH
Lozi, Julien
RCUH
Morris, Marita
RCUH
Murai, Rieko

RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH
RCUH

Nabeshima, Yoshitake
Nakata, Fumiaki
Niimi, Yuka
Nishimura, Reid
Nishimura, Tetsuo
Otsuki, Noriko
Pathak, Prashant
Ramos, LucioRoth, Noriko
Rousselle, Julien
Schubert, Kiaina
Spencer, Robin
Sur, Ryoko
Suzuki, Yuko
Tait, Philip
Tajitsu, Akito
Takiura, Koki
Tamae, Richard
Tanaka, Makoto
Tanaka, Yoko
Terai, Tsuyoshi
Tomono, Daigo
Toyofuku, Ralph
Tsang, Emiko
Weber, Mark
Williams, Joshua
Winegar, Tom
Wung, Matthew
Yoshiyama, Naomi

Okayama Astrophysical Observatory
Director
Izumiura, Hideyuki
Associate Professor
Izumiura, Hideyuki
Associate Professor
Ukita, Nobuharu
Specially Appointed
Kanbe, Eiji
Associate Professor
Assistant Professor
Yanagisawa, Kenshi
Engineer
Tsutsui, Hironori
Specially Appointed
Matsubayashi, Kazuya
Research Staff
Specially Appointed
Fukui, Akihiko
Senior Specialist
Research Expert
Kuroda, Daisuke
Research Expert
Maehara, Hiroyuki
Research Supporter
Toda, Hiroyuki
Administration Office
Administration Section
Chief
Tanabe, Keizo
Administrative Supporter Katayama, Kumiko
Administrative Supporter Shibukawa, Hiroko
Administrative Supporter Yamashita, Ayako
Administrative
Koyama, Shoji
Maintenance Staff
Administrative
Watanabe, Noriaki
Maintenance Staff

Nobeyama Radio Observatory
Acting Director
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
EngineerEngineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Senior Specialist
Research Expert
Research Expert
Research Expert
Research Expert
Technical Expert
Technical Expert
Administrative Supporter
Administrative Supporter
Research AssistantResearch Assistant
Administration Office
Deputy Manager
General Affairs Section
Chief
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative
Maintenance Staff
Administrative
Maintenance Staff
Administrative
Maintenance Staff
Administrative
Maintenance Staff
Administrative
Maintenance Staff
Administrative
Maintenance Staff
Administrative
Maintenance Staff
Administrative
Maintenance Staff

Kobayashi, Hideyuki
Kanzawa, Tomio
Ishizuki, Sumio
Minamidani, Tetsuhiro
Umemoto, Tomofumi
Torii, Kazufumi
Mikoshiba, Hiroshi
Handa, Kazuyuki
Miyazawa, Kazuhiko
Miyazawa, Chieko
Shinohara, Noriyuki
Kurakami, Tomio
Nishitani, Hiroyuki
Wada, Takuya
Kaneko, Hiroyuki
Miyamoto, Yusuke
Oya, Masaaki
Kinugasa, Kenzo
Maekawa, Jun
Takahashi, Shigeru
Tatamitani, Yoshio
Hayashi, Mitsuru
Nishioka, Makiko
Hatakeyama, Eiko
Ide, Hidemi
Fujita, Shinji
Matsuo, Mitsuhiro
Otsuka, Tomoyoshi
Otsuka, Tomoyoshi
Kikuchi, Kikue
Shinkai, Hisako
Yoda, Chizuko
Fuji, Shigeru
Hinata, Shigeto
Ide, Hiroko
Kadoshima, Junko
Kikuchi, Michiko
Kikuchi, Tsuyoshi
Koike, Ikuko
Saito, Arayo

III Organization

135

Administrative
Maintenance Staff
Administrative
Maintenance Staff
Accounting Section
Chief
Senior Staff
Administrative Supporter
Administrative Supporter
Administrative Supporter
Administrative Supporter
Mizusawa VLBI Observatory
Director
Professor
Professor
Associate Professor
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Chief Engineer
Engineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Technical Expert
Research Supporter

136

III Organization

Tsuchiya, Junko
Yokomori, Yasuyuki

Miyabara, Yasuhide
Iijima, Kunio
Kodaira, Toshiko
Takasawa, Mitsue
Takemura, Miwako
Tokui, Chisato

Honma, Mareki
Honma, Mareki
Kobayashi, Hideyuki
Shibata, Katsunori
Sato, Katsuhisa
Hada, Kazuhiro
Hirota, Tomoya
Jike, Takaaki
Kameya, Osamu
Kono, Yusuke
Sunada, Kazuyoshi
Tamura, Yoshiaki
Ishikawa, Toshiaki
Suzuki, Syunsaku
Ueno, Yuji
Hirano, Ken
Matsumoto, Naoko
Sakai, Nobuyuki
Tazaki, Fumie
Wu, Yuanwei
Kanaguchi, Masahiro
Miura, Mitsuo
Nagayama, Takumi
Oyama, Tomoaki
Asakura, Yu
Funayama, Hiroshi
Hachisuka, Kazuya
Kim, Jeoung Sook
Matsukawa, Yuki
Nishizawa, Akihisa
Sato, Kaori
Takahashi, Ken
Yamashita, Kazuyoshi
Yoshida, Toshihiro
Matsueda, Chika

Administrative Supporter Komori, Akiyo
Administrative Supporter Uekiyo, Hatsue
Administration Office
Deputy Manager
Hommyo, Susumu
General Affairs Section
Chief
Hommyo, Susumu
Staff
Iida, Naoto
Administrative Supporter Oizumi, Yuka
Administrative Supporter Sasaki, Mie
Administrative Supporter Sasaki, Mie
Accounting Section
Chief
Ito, Hiromasa
Administrative Supporter Kikuchi, Sachiko
Administrative Supporter Takahashi, Yumi
Ishigakijima Astronomical Observatory
Director
Honma, Mareki
Research Expert
Hanayama, Hidekazu
Time Keeping OfficeDirector
Sato, Katsuhisa
Solar Observatory
Director
Associate Professor
Senior Engineer
Specially Appointed
Research Staff
Research Expert
Research Expert
Research Expert
Administrative Supporter
NAOJ Chile Observatory
Director
Professor
Professor
Professor
Professor
Professor
Professor
Specially Appointed
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor
Specially Appointed
Associate Professor
Specially Appointed
Associate Professor
Specially Appointed
Associate Professor

Suematsu, Yoshinori
Hanaoka, Yoichiro
Shinoda, Kazuya
Joshi, Anand Diwakar
Hagino, Masaoki
Morita, Satoshi
Yaji, Kentaro
Sugimoto, Junko

Sakamoto, Seiichi
Iguchi, Satoru
Kameno, Seiji
Mizuno, Norikazu
Ogasawara, Ryuusuke
Sakamoto, Seiichi
Tatematsu, Kenichi
Hasegawa, Tetsuo
Asaki, Yoshiharu
Asayama, Shinichiro
Iono, Daisuke
Kiuchi, Hitoshi
Kosugi, George
Okuda, Takeshi
Muller, Erik Michael
Espada Fernandez,
DanielKawamura, Akiko
Nagai, Hiroshi

Specially Appointed
Associate Professor
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Assistant Professor
Specially Appointed
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Engineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff

Nakanishi, Koichiro
Kikuchi, Kenichi
Nakamura, Kouji
Watanabe, Manabu
Ezawa, Hajime
Gonzalez Garcia,
AlvaroHiramatsu, Masaaki
Hirota, Akihiko
Ishii, Shun
Kamazaki, Takeshi
Matsuda, Yuichi
Sawada, Tsuyoshi
Shimojo, Masumi
Takahashi, Satoko
Akiyama, Eiji
Egusa, Fumi
Miura, Rie
Okamoto, Joten
Saigou, Kazuya
Ashitagawa, Kyoko
Nakazato, Takeshi
Yamada, Masumi
Kato, Yoshihiro
Kobiki, ToshihikoNakamura, Kyoko
Ito, Tetsuya
Shizugami, Makoto
Ao, Yiping
Hashimoto, Takuya
Izumi, Natsuko
Lu, Xing
Kroug, Matthias Nils
Morokuma, Kana
Neelamkodan, Naslim
Sanhueza Nunez,
Patricio Andres
Takahashi, Sanemichi
Takekoshi, Tatsuya
Tokuda, Kazuki

Specially Appointed
Research Staff
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Research Expert
Research Expert
Administrative Expert
Research Supporter
Research Supporter
Technical Supporter
Administrative Supporter
Administrative Supporter

Zahorecz, Sarolta
Fujimoto, Yasuhiro
Fukui, Hideharu
Furutani, Akio
Horie, Yosaku
Ikeda, Emi
Kawakami, Kazuyuki
Kawasaki, Wataru
Konuma, Mika
Kuniyoshi, Masaya
Matsui, Takayuki
Miel, Renaud Jean
Christophe
Morita, Eisuke
Nakamoto, Takashi
Niizeki, Yasuaki
Nukatani, Sorahiko
Okumura, Yuji
Otawara, Kazushige
Saito, Motoi
Shimoda, Takanobu
So, Ryoken
Sugimoto, Kanako
Uemizu, Kazunori
Yoshino, Akira
Sakuma, Naoko
Tomimuro, Hisashi
Kamada, Masako
Uchida, Ayako
Yamazaki, Toshitaka
Hayashi, Ritsuko
Kono, Izumi
Otawara, Hikaru

III Organization

137

Administrative Supporter
Chile Employees
Chile Employee
Chile Employee
Chile Employee
Chile Employee
Administration Department
Manager
General Affairs Section
Chief
Accounting Section
Chief
Staff

Saito, Naoko
Aguilera, Javier
Krapivka, Gabriela
Toro, Lorena
Zenteno, Javier
Okumura, Yuji
Tsukano, Satomi
Okumura, Yuji
Hiramatsu, Naoya

Center for Computational Astrophysics
Director
Kokubo, Eiichiro
Professor
Kokubo, Eiichiro
Assistant Professor
Ohsuga, Ken
Specially Appointed
Takahashi, Hiroyuki
Assistant Professor
Specially Appointed
Asahina, Yuta
Research Staff
Specially Appointed
Ohtani, Yukari
Research Staff
Research Expert
Kato, Tsunehiko
Research Expert
Nakayama, Hirotaka
Research Expert
Oshino, Shoichi
Research Expert
Wakita, Shigeru
Research Supporter
Fukushi, Hinako
Research Supporter
Hasegawa, Satoki
Research Supporter
Taki, Tetsuo
Research Supporter
Tanaka, Yuki
Administrative Supporter Kimura, Yuko
Hinode Science Center
Director
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Research Staff
Technical Expert
Research Supporter
Research Supporter
Administrative Supporter

B Projects

Watanabe, Tetsuya
Sekii, Takashi
Suematsu, Yoshinori
Ishikawa, Ryoko
Katsukawa, Yukio
Kubo, Masahito
Lee, Kyoung Sun
Inoue, Naoko
Ishii, Shuichi
Tsuchiya, Chie
Kano, Kaori

Gravitational Wave Project OfficeDirector
Flaminio, RaffaeleSpecially Appointed
Flaminio, Raffaele
Professor
Associate Professor
Aso, Yoichi
Affiliated AssociateAndo, Masaki
Professor

138

III Organization

Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Specially Appointed
Assistant Professor
Research Engineer
Chief Engineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Administrative Expert
Research Supporter
Administrative Supporter
Administrative Supporter
Research Assistant
TMT-J Project OfficeDirector
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Specially Appointed
Associate Professor
Chief Research Engineer
Assistant Professor
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Research Expert
Special Senior Specialist
Research Supporter

Akutsu, Tomotada
Ohishi, Naoko
Takahashi, Ryutaro
Tatsumi, Daisuke
Shoda, Ayaka
Ishizaki, Hideharu
Tanaka, Nobuyuki
Barton, Mark Andrew
Pena Arellano,
Fabian Erasmo
Zeidler, Simon
Hirata, Naoatsu
Tapia, San Martin Enzo
NicolasOhyama, Megumi
Harada, Mikiko
Sakamoto, Eri
Yoshizumi, Mizuho
Guo, Yuefan

Usuda, Tomonori
Usuda, Tomonori
Saito, Masao
Yamashita, Takuya
Aoki, Wako
Kashikawa, Nobunari
Sugimoto, Masahiro
Terada, Hiroshi
Oya, ShinMiyashita, Takaaki
Yasui, Chikako
Harakawa, Hiroki
Kubo, Mariko
Ozaki, Shinobu
Schramm, Malte
Chapman, Junko
Kozu, Akihito
Kusumoto, Hiroshi
Sugiyama, Motokuni
Ishii, Miki
Inatani, Junji
Tajima, Toshiyuki

Administrative Supporter Haranaka, Miyuki
Administrative Supporter Yamaguchi, Chiyu
RCUH
Iye, Masanori

A Projects

JASMINE Project OfficeDirector
Professor
Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Supporter
Technical Supporter

Gouda, Naoteru
Gouda, Naoteru
Kobayashi, Yukiyasu
Tsujimoto, Takuji
Ueda, Akitoshi
Yano, Taihei
Utsunomiya, Shin
Kashima, Shingo

Extrasolar Planet Detection Project OfficeDirector
Tamura, Motohide
Affiliated Professor
Tamura, Motohide
Assistant Professor
Kotani, Takayuki*
Assistant Professor
Nakajima, Tadashi*
Assistant Professor
Nishikawa, Jun
Assistant Professor
Suto, Hiroshi*
Affiliated Assistant
Narita, Norio
Professor
Specially Appointed
Hashimoto, Jun*
Assistant Professor
Specially Appointed
Hori, Yasunori*
Assistant Professor
Specially Appointed
Konishi, Mihoko
Research Staff
Specially Appointed
Omiya, Masashi
Research Staff
Specially Appointed
Kusakabe, Nobuhiko*Senior Specialist
Research Supporter
Kurokawa, Takashi*concurrently appointed in NINSRISE Project
Director
Namiki, Noriyuki
Professor
Namiki, Noriyuki
Associate Professor
Hanada, Hideo
Associate Professor
Matsumoto, Koji
Chief Research Engineer Tsuruta, Seiitsu
Assistant Professor
Araki, Hiroshi
Assistant Professor
Noda, Hirotomo
Research Engineer
Asari, Kazuyoshi
Research Engineer
Tazawa, Seiichi
Specially Appointed
Kawamura, Taichi
Research Staff
Specially Appointed
Yamamoto, Keiko
Research Staff
Administrative Supporter Sato, Sayaka
SOLAR-C Project OfficeDirector
Professor

Ichimoto, Kiyoshi
Ichimoto, Kiyoshi

Professor
Watanabe, Tetsuya
Associate Professor
Goto, Motoshi*
Associate Professor
Hara, Hirohisa
Associate Professor
Kano, Ryouhei
Assistant Professor
Narukage, Noriyuki
Specially Appointed
Song, Donguk
Research Staff
Administrative Supporter Fujiyoshi, Marie*concurrently appointed in NINS

Centers
Astronomy Data Center
Director
Associate Professor
Associate Professor
Associate Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Research Expert
Research Expert
Research Expert
Research Supporter
Research Supporter
Research Supporter
Administrative Supporter
Research Assistant
JVO Project
Director
Advanced Technology Center
Director
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer

Takata, Tadafumi
Ichikawa, Shinichi
Ohishi, Masatoshi
Takata, Tadafumi
Furusawa, Hisanori
Ito, Takashi
Oe, Masafumi
Shirasaki, Yuji
Inoue, Goki
Homma, Hidetomo
Sorahana, Satoko
Kamegai, Kazuhisa
Makiuchi, Shinichiro
Ozawa, Takeaki
Zapart, Christopher
Andrew
Furusawa, Junko
Isogai, Mizuki
Tanaka, Nobuhiro
Fujikawa, Makiko
Noda, Sachiyo
Utsumi, Motomu
Ishii, Yuko
Suzuki, Taiki
Mizumoto, Yoshihiko

Noguchi, Takashi
Noguchi, Takashi
Takami, Hideki
Hayano, Yutaka
Matsuo, Hiroshi
Miyazaki, Satoshi
Sekimoto, Yutaro
Shan, Wenlei
Fujii, Yasunori

III Organization

139

Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
Chief Engineer
EngineerEngineer
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Specially Appointed
Research Staff
Research Expert
Technical Expert
Technical Expert
Administrative Supporter
Administrative Supporter
Administrative Supporter
Research AssistantResearch AssistantResearch AssistantPublic Relations Center
Director
Professor
Professor
Associate Professor
Associate Professor
Research Engineer
Chief Senior Engineer
Chief Engineer
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist

140

III Organization

Okada, Norio
Kojima, Takafumi
Nakaya, Hidehiko
Oshima, Tai
Suzuki, Ryuji
Fukushima, Mitsuhiro
Noguchi, Motokazu
Obuchi, Yoshiyuki
Sato, Naohisa
Kamata, Yukiko
Kubo, Koichi
Takahashi, Toshikazu
Fukuda, Takeo
Ikenoue, Bungo
Inata, Motoko
Iwashita, Hikaru
Kaneko, Keiko
Mitsui, Kenji
Uraguchi, Fumihiro
Waseda, Koichi
Ezaki, Shohei
Tsuzuki, Toshihiro
Dominjon,Agnes Micheline
Hasebe, Takashi
Uchiyama, Mizuho
Saito, Sakae
Nishino, Tetsuo
Suzuki, Yoshinori
Kuroda, Kyoko
Murakami, Hiromi
Yoshida, Taeko
Abdelouahab,
Valentin Adel
Gobin, Nicolas
Kozuki, Yuto

Fukushima, Toshio
Fukushima, Toshio
Watanabe, Jun-ichi
Agata, Hidehiko
Yamaoka, Hitoshi
Katayama, Masato
Matsuda, Ko
Nagayama, Shogo
Cheung, Sze Leung
Ishikawa, Naomi
Lundock, Ramsey Guy
Pires Canas, Lina Isabel

Specially Appointed
Tsuzuki, Hiroko
Senior Specialist
Research Expert
Ono, Tomoko
Research Expert
Takata, Hiroyuki
Research Expert
Usuda, Kumiko
Research Supporter
Kume, Kaori
Public Outreach Official Endo, Isao
Public Outreach Official Fujita, Tokiko
Public Outreach Official Futami, Hiroshi
Public Outreach Official Hamura, Taiga
Public Outreach Official Hatano, Satomi
Public Outreach Official Ibaraki, Takao
Public Outreach Official Ishizaki, Masaharu
Public Outreach Official Iwashiro, Kuninori
Public Outreach Official Koike, Akio
Public Outreach Official Kubo, Maki
Public Outreach Official Mikami, Naotsugu
Public Outreach Official Naito, Seiichiro
Public Outreach Official Natsugari, Satomi
Public Outreach Official Nemoto, Shiomi
Public Outreach Official Ogoe, Osamu
Public Outreach Official Oguri, Junko
Public Outreach Official Shibata, Yukiko
Public Outreach Official Shioya, Yasuhisa
Public Outreach Official Takabatake, Noriko
Public Outreach Official Takeda, Takaaki
Administrative Supporter Aoki, Makiko
Administrative Supporter Noguchi, Sayumi
Public Relations OfficeDirector
Yamaoka, Hitoshi
Outreach and Education OfficeDirector
Agata, Hidehiko
Ephemeris Computation OfficeDirector
Katayama, Masato
Library
ChiefTodoriki, Tatsuya
Publications OfficeDirector
Fukushima, Toshio
The Office for Astronomy Outreach of the IAU
Director
Agata, Hidehiko
Administration OfficeDirector
Matsuda, Ko

Divisions
Division of Optical and Infrared Astronomy
Director
Mizumoto, Yoshihiko
Professor
Arimoto, Nobuo
Professor
Gouda, Naoteru
Professor
Kobayashi, Yukiyasu
Professor
Mizumoto, Yoshihiko
Professor
Ohashi, Nagayoshi
Professor
Saito, Masao
Professor
Sekiguchi, Kazuhiro
Professor
Usuda, Tomonori

Professor
Yamashita, Takuya
Associate Professor
Aoki, Wako
Associate Professor
Aso, Yoichi
Associate Professor
Hayashi, Saeko
Associate Professor
Iwata, Ikuru
Associate Professor
Izumiura, Hideyuki
Associate Professor
Kashikawa, Nobunari
Associate Professor
Kodama, Tadayuki
Associate Professor
Noumaru, Junichi
Associate Professor
Sugimoto, Masahiro
Associate Professor
Takato, Naruhisa
Associate Professor
Takeda, Yoichi
Associate Professor
Terada, Hiroshi
Associate Professor
Ukita, Nobuharu
Chief Research Engineer Iwashita, Hiroyuki
Chief Research Engineer Miyashita, Takaaki
Assistant Professor
Akutsu, Tomotada
Assistant Professor
Imanishi, Masatoshi
Assistant Professor
Komiyama, Yutaka
Assistant Professor
Koyama, Yusei
Assistant Professor
Minowa, Yosuke
Assistant Professor
Morino, Jun-ichi
Assistant Professor
Nishikawa, Jun
Assistant Professor
Ohishi, Naoko
Assistant Professor
Okita, Hirofumi
Assistant Professor
Onodera, Masato
Assistant Professor
Pyo, Tae-soo
Assistant Professor
Sôma, Mitsuru
Assistant Professor
Takahashi, Ryutaro
Assistant Professor
Tatsumi, Daisuke
Assistant Professor
Tsujimoto, Takuji
Assistant Professor
Ueda, Akitoshi
Assistant Professor
Yagi, Masafumi
Assistant Professor
Yanagisawa, Kenshi
Assistant Professor
Yano, Taihei
Assistant Professor
Yasui, Chikako
Research Engineer
Bando, Takamasa
Research Engineer
Ishizaki, Hideharu
Senior Engineer
Omata, Koji
Senior Engineer
Namikawa, Kazuhito
Chief Engineer
Tamura, Tomonori
Chief Engineer
Tanaka, Nobuyuki
Engineer
Sato, Tatsuhiro
Engineer
Tsutsui, Hironori
Administrative Supporter Kimura, Hiroko
Research AssistantOnoue, Masafusa
Research Assistant
Shimakawa, Rhythm
Research AssistantSuzuki, Tomoko
Division of Radio Astronomy
Director
Professor
Professor
Professor
Professor
Professor

Iguchi, Satoru
Honma, Mareki
Iguchi, Satoru
Kameno, Seiji
Kawabe, Ryohei
Kobayashi, Hideyuki

Professor
Professor
Professor
Professor
Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Associate Professor
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Chief Research Engineer
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Assistant Professor
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Research Engineer
Senior Engineer
Senior Engineer
Senior Engineer

Mizuno, Norikazu
Namiki, Noriyuki
Ogasawara, Ryusuke
Sakamoto, Seiichi
Tatematsu, Kenichi
Asaki, Yoshiharu
Asayama, Shinichiro
Hanada, Hideo
Iono, Daisuke
Kiuchi, Hitoshi
Kosugi, George
Matsumoto, Koji
Okuda, Takeshi
Shibata, Katsunori
Kanzawa, Tomio
Kawashima, Susumu
Kikuchi, Kenichi
Nakamura, Kouji
Sato, Katsuhisa
Tsuruta, Seiitsu
Watanabe, Manabu
Araki, Hiroshi
Ezawa, Hajime
Gonzalez Garcia,
AlvaroHada, Kazuhiro
Hiramatsu, Masaaki
Hirota, Akihiko
Hirota, Tomoya
Ishii, Shun
Ishizuki, Sumio
Jike, Takaaki
Kamazaki, Takeshi
Kameya, Osamu
Kono, Yusuke
Matsuda, Yuichi
Minamidani, Tetsuhiro
Miyoshi, Makoto
Noda, Hirotomo
Sawada, Tsuyoshi
Shimojo, Masumi
Sunada, Kazuyoshi
Takahashi, Satoko
Tamura, Yoshiaki
Umemoto, Tomofumi
Asari, Kazuyoshi
Ashitagawa, Kyoko
Ishikawa, Toshiaki
Mikoshiba, Hiroshi
Nakazato, Takeshi
Suzuki, Syunsaku
Tazawa, Seiichi
Yamada, Masumi
Handa, Kazuyuki
Kato, Yoshihiro
Kobiki, Toshihiko

III Organization

141

Senior Engineer
Senior Engineer
Senior Engineer
Senior Engineer
Chief Engineer
Chief Engineer
Chief Engineer
EngineerEngineerEngineerEngineer
Specially Appointed
Senior Specialist
Research Supporter

Miyazawa, Chieko
Miyazawa, KazuhikoNakamura, Kyoko
Shinohara, Noriyuki
Ito, Tetsuya
Kurakami, Tomio
Ueno, Yuji
Hirano, Ken
Nishitani, Hiroyuki
Shizugami, Makoto
Wada, Takuya
Takebayashi, Yasuo
Tsuneyama, Junko

Division of Solar and Plasma Astrophysics
Director
Hanaoka, Yoichiro
Professor
Watanabe, Tetsuya
Associate Professor
Hanaoka, Yoichiro
Associate Professor
Hara, Hirohisa
Associate Professor
Kano, Ryouhei
Associate Professor
Sekii, Takashi
Associate Professor
Suematsu, Yoshinori
Assistant Professor
Ishikawa, Ryoko
Assistant Professor
Katsukawa, Yukio
Assistant Professor
Kubo, Masahito
Assistant Professor
Narukage, Noriyuki
Specially Appointed
Toriumi, Shin
Assistant Professor
Senior Engineer
Shinoda, Kazuya
Division of Theoretical Astronomy
Director
Tomisaka, Kohji
Professor
Kokubo, Eiichiro
Professor
Tomisaka, Kohji
Professor
Yoshida, Haruo
Associate Professor
Kajino, Toshitaka
Associate Professor
Nakamura, Fumitaka
Assistant Professor
Hamana, Takashi
Assistant Professor
Ohsuga, Ken
Assistant Professor
Takiwaki, Tomoya
Assistant Professor
Tanaka, Masaomi
Specially Appointed
Moriya, Takashi
Assistant Professor
Specially Appointed
Nozawa, Takaya
Assistant Professor
Specially Appointed
Ogihara, Masahiro
Assistant Professor
Specially Appointed
Sotani, Hajime
Assistant Professor
Specially Appointed
Zenitani, Seiji
Assistant Professor
Specially Appointed
Kawashima, Tomohisa
Research Staff
Administrative Supporter Izumi, Shioko

142

III Organization

5. Research Support Departments
Research Enhancement Strategy OfficeDirector
Kobayashi, Hideyuki
Specially Appointed
Chapman, Junko
Senior Specialist
Specially Appointed
Senior Specialist

Fukui, Hideharu

Specially Appointed
Senior Specialist

Hasuo, Ryuichi

Specially Appointed
Senior Specialist

Hori, KunikoSpecially Appointed
Senior Specialist

Lundock, Ramsey Guy

Specially Appointed
Senior Specialist

Miura, Mitsuo

Specially Appointed
Senior Specialist

Yamamiya, Osamu

Research Evaluation Support OfficeDirector
Watanabe, Jun-ichi
Specially Appointed
Hori, Kuniko
Senior Specialist
Office of International Relations
Director
Specially Appointed
Senior Specialist
Specially Appointed
Senior Specialist
Research Expert
Support Desk
Research Supporter

Hasuo, Ryuichi
Hasuo, Ryuichi
Komiyama, Hiroko
Yoshida, Fumi
Shirato, Reiko

Human Resources Planning OfficeDirector
Yamamiya, Osamu
Safety and Health Management OfficeDirector
Takami, Hideki
Technical Expert
Kashiwagi, Yuji
Engineering Promotion OfficeDirector
Takami, Hideki
Chief Research Engineer Kawashima, Susumu
Administration Department
General Manager
General Affairs Division
Manager
Deputy Manager
Senior Specialist
Specialist (Information
Technology)
Specialist (Personnel
Accounting)

Sasagawa, Hikaru
Harada, Eiichiro
Furuhata, Tomoyuki
Onishi, Tomoyuki
Chiba, Yoko
Watanabe, YukikaSpecially Appointed
Senior Specialist

Noguchi, Koki

Specially Appointed
Yamamoto, Chieko
Senior Specialist
General Affairs Section
Chief
Chiba, Yoko
Staff
Morita, Akitsugu
Staff
Yoshimura, Tetsuya
Vehicle Driver
Amemiya, Hidemi
Administrative Expert
Murakami, Sachiko
Administrative Expert
Noguchi, Utako
Administrative Supporter Kobayashi, Kayo
Administrative Supporter Seki, Kumi
Personnel Section
Chief
Yamanouchi, Mika
Staff
Isozaki, Yuka
Staff
Sakamoto, Misato
Payroll Section
Chief
Watanabe, Yukika
Staff
Furukawa, Shinichiro
Staff
Inoue, Miyuki
Administrative Supporter Aiba, Narukazu
Administrative Supporter Momma, Yoko
Employee Affairs Section
Chief
Yamaura, Mari
Staff
Saito, Masahiro
Administrative Expert
Noguchi, Megumi
MEXT Trainee
Staff
Matsukura, Koji
Maternity Leave
Staff
Ouchi, Kaori
Spouse Accompaniment Leave
Staff
Mochimaru, Shiori
Research Promotion Division
Acting Manager
Sasagawa, Hikaru
Furuhata, Tomoyuki
Senior Specialist(International Relations)
Administrative Supporter Torii, Makiko
Research Support Section
Chief
Goto, Michiru
Staff
Yamafuji, Yasuto
Administrative Expert
Haruki, Mutsumi
Administrative Supporter Hagimoto, Miya
Administrative Supporter Komoda, Chizuru
Administrative Supporter Urushibata, Kozue
Administrative Supporter Yasuda, Masako
Graduate School Section
Chief
Kikkawa, Hiroko
Administrative Expert
Inoue, Mizuho
International Academic Affairs Section
Staff
Takada, Miyuki
Administrative Supporter Ito, Yoshihisa

III Organization

143

Financial Affairs Division
Manager
Deputy Manager
Specialist (Audit)
General Affairs Section
Chief
Administrative Supporter
Budget Section
Chief
Staff
Administrative Supporter
Asset Management Section
Chief
Staff
Purchase Validation Center
Chief
Administrative Supporter
Administrative Supporter
Administrative Supporter
Accounting Division
Manager
Specialist (Contract)
Accounting Section
Chief
Staff
Administrative Supporter
Administrative Supporter
Administrative Supporter
Procurement Section
Chief
Staff
Staff
Staff
Consultant
Administrative Expert
Administrative Supporter
Facilities Division
Manager
Administrative Expert
General Affairs Section
Chief
Staff
Administrative Supporter
Planning Section
Chief
Administrative Supporter
Maintenance Section
Chief
Senior Staff

144

III Organization

Nemoto, Nobuyuki
Ikeda, Hiroshi
Ishikawa, Junya
Yamamoto, Shinichi
Sasaki, Sayuri
Akaike, Makoto
Masuda, Akio
Ishida, Mikiko
Sato, Kanako
Takahashi, SachikoSato, Kanako
Hosoi, Chiho
Nakagomi, Kimitoshi
Tsukamoto, Satoko
Tanaka, Masaru
Yamazaki, Go
Sato, Yoko
Miyata, Yusuke
Kobayashi, Rina
Nagasawa, Fumi
Suzuki, Yukiko
Yamazaki, Go
Kayamori, Shinji
Sugimoto, Naomi
Takai, Tetsuya
Hyuga, Tadayuki
Sato, Masako
Ochiai, Nana
Watanabe, Matsuo
Asada, Tsuneaki
Kawashima, Ryota
Nakagawa, Yukie
Hasegawa, Chisato
Murakami, Kazuhiro
Nagata, Yomogi
Narisawa, Hiroyuki
Hayashigura, Koji

6. Personnel change
Research and Academic Staff
Date
Name

Change2016/4/1

Yamaoka, Hitoshi

HiredPublic Relations Center, Associate Professor

2016/4/1

Gonzalez Garcia,
Alvaro

Hired

Division of Radio Astronomy (NAOJ Chile
Observatory), Assistant Professor(Advanced Technology Center,
Specially Appointed Assistant Professor)

2016/4/1

Yamada, Masumi

Hired

Division of Radio Astronomy (NAOJ Chile
Observatory), Research Engineer(NAOJ Chile Observatory, Specially
Appointed Senior Specialist)

2016/5/1

Yasui, Chikako

HiredDivision of Optical and Infrared Astronomy(TMT-J Project Office), Assistant Professor

2016/7/1

Narukage, Noriyuki

Hired(Advanced Technology Center,
Division of Solar and Plasma Astrophysics(SOLAR-C Project Office), Assistant Professor Specially Appointed Research Staff)

2016/7/1

Nakamura, Kouji

Hired

Division of Radio Astronomy (NAOJ Chile
Observatory), Chief Research Engineer

2016/10/1

Ishii, Shun

Hired

Division of Radio Astronomy (NAOJ Chile
Observatory), Assistant Professor

2016/7/31

Espada Fernandez,
DanielResigned(NAOJ Chile Observatory Specially
Appointed Associate Professor)

Division of Radio Astronomy(NAOJ Chile Observatory),
Associate Professor

2016/10/31

Inoue, Tsuyoshi

Resigned(Nagoya University Graduate School of
Science, Associate Professor)

Division of Theoretical Astronomy,
Assistant Professor

2017/3/31

Arimoto, Nobuo

RetiredDivision of Optical and Infrared
Astronomy (Subaru Telescope),
Professor

2017/3/31

Kobayashi,
Yukiyasu

RetiredDivision of Optical and Infrared
Astronomy (JASMINE Project
Office), Professor

2017/3/31

Mizumoto,
Yoshihiko

RetiredDivision of Optical and Infrared
Astronomy, Professor

2017/3/31

Noguchi, Motokazu

RetiredAdvanced Technology Center,Research Engineer

2017/3/1

Mizuno, Norikazu

Promoted

Division of Radio Astronomy (NAOJ Chile
Observatory), Professor

Division of Radio Astronomy(NAOJ Chile Observatory),
Associate Professor

2017/3/1

Saito, Masao

Promoted

Division of Optical and Infrared Astronomy(TMT-J Project Office), Professor

Division of Radio Astronomy(Nobeyama Radio Observatory),
Associate Professor

2016/4/1

Nakajima, Tadashi

National Institutes of Natural Sciences
Reassigned Astrobiology Center Extrasolar Planet
Detection Project Office, Assistant Professor

New Affiliated Institute, Position

Previous Affiliated Institute, Position(Kyushu University Graduate Schoolof Science, Assistant Professor)(NAOJ Chile Observatory, Specially
Appointed Senior Specialist)

Division of Optical and Infrared
Astronomy (Extrasolar Planet Detection
Project Office), Assistant Professor

Engineering Staff
Date

Name

Change2016/12/1

Ezaki, Shohei

Hired2016/6/30

Negishi, Satoru

Resigned

New Affiliated Institute, Position
Advanced Technology Center, Engineer

Previous Affiliated Institute,
Position(NAOJ Chile Observatory,Specially Appointed Senior Specialist)
Division of Optical and Infrared
Astronomy (Subaru Telescope),
Chief Engineer

III Organization

145

2016/4/1

Namikawa,
Kazuhito

Promoted

Division of Optical and Infrared Astronomy(Subaru Telescope), Senior Engineer

Division of Optical and Infrared
Astronomy (Subaru Telescope),
Chief Engineer

2016/4/1

Kato, Yoshihiro

Promoted

Division of Radio Astronomy (NAOJ Chile
Observatory), Senior Engineer

Division of Radio Astronomy (NAOJ
Chile Observatory), Chief Engineer

2017/3/1

Omata, Koji

Promoted

Division of Optical and Infrared Astronomy(Subaru Telescope), Senior Engineer

Division of Optical and Infrared
Astronomy (Subaru Telescope),
Chief Engineer

2017/3/1

Kamata, Yukiko

Promoted

Advanced Technology Center, SeniorEngineer

Advanced Technology Center, Chief
Engineer

Administrative Staff

146

Name

2016/4/1

Sasagawa, Hikaru

HiredGeneral Manager

2016/4/1

Ikeda, Hiroshi

HiredAdministration Department Financial
Affairs Division, Deputy Manager(The University of Tokyo)

2016/4/1

Yamazaki, Go

Hired

Administration Department Accounting
Division Procurement Section, Chief(Tokyo Gakugei University)

2016/4/1

Narisawa, Hiroyuki

HiredAdministration Department Facilities
Division Maintenance Section, Chief(The University of Tokyo)

2016/4/1

Tanabe, Keizo

HiredOkayama Astrophysical Observatory
Administration Office Administration
Section, Chief(Okayama University Hospital)

2016/4/1

Morita, Akitsugu

Hired

Administration Department General Affairs
Division General Affairs Section, Staff

2016/4/1

Inoue, Miyuki

HiredAdministration Department General Affairs
Division Payroll Section, Staff

2016/4/1

Takahashi, Sachiko

HiredAdministration Department Financial Affairs
Division Asset Management Section, Staff

2016/8/1

Miyabara, Yasuhide

Hired

Nobeyama Radio Observatory Administration(Shinshu University)
Office Accounting Section, Chief

2016/7/31

Shimizu, Hidetoshi

Resigned(Shinshu University)

Nobeyama Radio Observatory
Administration Office Accounting
Section, Chief

2017/3/31

Nemoto, Nobuyuki

Resigned(Ministry of Education, Culture, Sports,
Science and Technology-Japan)

Administration Department
Financial Affairs Division, Manager

2017/3/31

Watanabe, Yukika

Resigned(Tokyo Gakugei University)

Administration Department General
Affairs Division Payroll Section, Chief

2017/3/31

Sato, Kanako

Resigned(Tokyo Gakugei University)

Administration Department
Financial Affairs Division AssetManagement Section, Chief

2017/3/31

Hayashigura, Koji

Resigned(Tokyo National Museum)

Administration Department
Facilities Division Maintenance
Section, Senior Staff

2017/3/31

Yoshimura, Tetsuya

Resigned(The University of Tokyo)

Administration Department General
Affairs Division General Affairs
Section, Staff

2017/3/31

Miyata, Yusuke

Resigned(The Graduate University for Advanced
Studies)

Administration Department
Accounting Division Accounting
Section, Staff

2017/3/31

Watanabe, Matsuo

RetiredIII Organization

ChangeNew Affiliated Institute, Position

Previous Affiliated Institute,
Position(Japan Society for the Promotion of
Science)

Date

Administration Department
Facilities Division, Manager

2016/4/1

Kawashima, Ryota

Promoted

Administration Department Facilities
Division General Affairs Section, Chief

Administration Department
Facilities Division General Affairs
Section, Senior Staff

2016/4/1

Hayashigura, Koji

Promoted

Administration Department Facilities
Division Maintenance Section, Senior Staff

Administration Department
Facilities Division Maintenance
Section, Staff

2016/7/1

Goto, Michiru

Promoted

Administration Department General Affairs
Division Research Support Section, Chief

Administration Department
General Affairs Division Research
Support Section, Senior Staff

2016/8/1

Furuhata, Tomoyuki

Promoted

Administration Department General Affairs
Division, Deputy Manager

Subaru Telescope Administration
Department Accounting Section,
Chief

2016/8/1

Sugawara, Satoshi

Promoted

Subaru Telescope Administration
Department Accounting Section, Senior
Staff

Subaru Telescope Administration
Department General Affairs
Section, Staff

2016/7/1

Yokota, Banri

National Institutes of Natural Sciences
Administration Department
Reassigned Administrative Bureau Liaison and Planning Financial Affairs Division Budget
Division Research Support Section, Staff
Section, Staff

Masuda, Akio

National Institutes of Natural
Administration Department Financial Affairs Sciences Administrative Bureau
Reassigned
Division Budget Section, Staff
Liaison and Planning Division
Research Support Section, Staff

2016/7/1

Employee on Annual Salary System
ChangePrevious Affiliated Institute,
Position
NAOJ Chile Observatory, Specially Appointed (Division of Radio Astronomy
Professor (Distinguished Professor)(NAOJ Chile Observatory), Professor)

Date

Name

New Affiliated Institute, Position

2016/4/1

Hasegawa, Tetsuo

Hired2016/4/1

Hayashi, Masao

Hired

Subaru Telescope, Specially Appointed
Assistant Professor

2016/4/1

Okamoto, Takenori

Hired

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

2016/4/1

Moriya, Takashi

HiredDivision of Theoretical Astronomy,
Specially Appointed Assistant Professor

2016/4/1

Ogihara, Masahiro

Hired

Division of Theoretical Astronomy,
Specially Appointed Assistant Professor

2016/4/1

Niino, Yuu

HiredSubaru Telescope, Specially Appointed
Research Staff

2016/4/1

Takagi, Yuhei

Hired

Subaru Telescope, Specially Appointed
Research Staff

2016/4/1

Joshi,
Anand Diwakar

HiredSolar Observatory, Specially Appointed
Research Staff

2016/4/1

Kroug, Matthias Nils Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2016/4/1

Izumi, Natsuko

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2016/4/1

Ohtani, Yukari

HiredCenter for Computational Astrophysics,
Specially Appointed Research Staff

2016/4/1

Lee, Kyoung Sun

Hired

Hinode Science Center, Specially Appointed
Research Staff

2016/4/1

Ozaki, Shinobu

Hired

TMT-J Project Office, Specially Appointed
Research Staff

2016/4/1

Kubo, Mariko

Hired

TMT-J Project Office, Specially Appointed
Research Staff

2016/4/1

Schramm, Malte

Hired

TMT-J Project Office, Specially Appointed
Research Staff
III Organization

147

148

2016/4/1

Konishi, Mihoko

Hired

Extrasolar Planet Detection Project Office,Specially Appointed Research Staff

2016/4/1

Yamamoto, Keiko

HiredRISE Project, Specially Appointed Research
Staff

2016/4/1

Homma, Hidetomo

Hired

Astronomy Data Center, Specially Appointed
Research Staff

2016/4/1

Hasebe, Takashi

HiredAdvanced Technology Center, Specially
Appointed Research Staff

2016/4/1

Uchiyama, Mizuho

Hired

Advanced Technology Center, Specially
Appointed Research Staff

2016/4/1

Taniguchi, Akimitsu

Hired

Subaru Telescope, Specially Appointed
Senior Specialist

2016/4/1

Oya, Masaaki

HiredNobeyama Radio Observatory, Specially
Appointed Senior Specialist

2016/4/1

Fujimoto, Yasuhiro

Hired

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2016/4/1

Kusumoto, Hiroshi

Hired

TMT-J Project Office, Specially Appointed
Senior Specialist

2016/4/1

Makiuchi,Shin'ichiro

HiredAstronomy Data Center, Specially Appointed
Senior Specialist

2016/4/1

Ozawa, Takeaki

HiredAstronomy Data Center, Specially Appointed
Senior Specialist

2016/4/1

Kamegai, Kazuhisa

Hired

Astronomy Data Center, Specially Appointed
Senior Specialist

2016/4/1

Komiyama, Hiroko

Hired

Office of International Relations, Specially
Appointed Senior Specialist

2016/5/1

Torii, Kazufumi

HiredNobeyama Radio Observatory, Specially
Appointed Assistant Professor

2016/7/1

Kanbe, Eiji

Hired

Okayama Astrophysical Observatory,Specially Appointed Associate Professor

2016/7/1

Egusa, Fumi

Hired

NAOJ Chile Observatory, Specially
Appointed Assistant Professor(NAOJ Chile Observatory, Specially
Appointed Research Staff)

2016/8/1

Espada Fernandez,
DanielHired

NAOJ Chile Observatory, Specially
Appointed Associate Professor(Division of Radio Astronomy(NAOJ Chile Observatory),
Associate Professor)

2016/8/1

Lu, Xing

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2016/9/1

Saigou, Kazuya

Hired

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

2016/9/12

Tsuzuki, Hiroko

HiredPublic Relations Center, Specially Appointed
Senior Specialist

2016/9/21

Neelamkodan,
NaslimHired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2016/10/1

Kawashima,
Tomohisa

Hired

Division of Theoretical Astronomy, Specially
Appointed Research Staff

2016/10/1

Fukui, Akihiko

HiredOkayama Astrophysical Observatory,Specially Appointed Senior Specialist

2016/10/25

Tapia San Martin,
Enzo Nicolas

Hired

Gravitational Wave Project Office, Specially
Appointed Senior Specialist

2016/11/1

Matsubayashi,
Kazuya

Hired

Okayama Astrophysical Observatory,Specially Appointed Research Staff

2016/11/1

Kawamura, Taichi

Hired

RISE Project, Specially Appointed Research
Staff

2016/11/1

Sorahana, Satoko

Hired

Astronomy Data Center, Specially Appointed
Research Staff

III Organization(Okayama AstrophysicalObservatory, Specially Appointed
Research Staff)

2016/12/1

Zapart, Christopher
Andrew

Hired

Astronomy Data Center, Specially Appointed
Senior Specialist

2017/1/16

Hashimoto, Takuya

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/1/16

Song, Donguk

Hired

SOLAR-C Project Office, Specially
Appointed Research Staff

2017/2/1

Tokuda, Kazuki

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/2/1

Zahorecz, Sarolta

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2017/3/1

Shoda, Ayaka

Hired

Gravitational Wave Project Office, Specially
Appointed Assistant Professor

2017/3/31

Takahashi,
Sanemichi

Hired

NAOJ Chile Observatory, Specially
Appointed Research Staff

2016/4/30

Higuchi, Yuichi

Resigned

2016/6/30

Egusa, Fumi

Resigned(NAOJ Chile Observatory, Specially
Appointed Assistant Professor)

2016/6/30

Narukage, Noriyuki

Resigned

Advanced Technology Center,(Division of Solar and Plasma Astrophysics
SOLAR-C Project Office, Assistant Professor) Specially Appointed Research Staff

2016/7/1

Nakamura, Kouji

Resigned(Division of Radio Astronomy (NAOJ Chile
Observatory), Chief Research Engineer)

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2016/9/30

Motogi, Kazuhito

Resigned(Yamaguchi University Graduate School of
Sciences and Technology for Innovation,
Assistant Professor)

Mizusawa VLBI Observatory,Specially Appointed Research Staff

2016/11/30

Zapart, Christopher
Andrew

Resigned(Astronomy Data Center, Specially Appointed Astronomy Data Center, Specially
Senior Specialist)
Appointed Research Staff

2016/11/30

Kobayashi, Tsuyoshi

Resigned

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2016/11/30

Ezaki, Shohei

Resigned(Advanced Technology Center, Engineering
Staff)NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2016/12/31 Hatsukade, Bun'yo

Resigned(The University of Tokyo Graduate School of
Science Department of Astronomy, AssistantProfessor)

NAOJ Chile Observatory, Specially
Appointed Assistant Professor

2017/1/15

Matsuoka, Yoshiki

Resigned

2017/2/28

Karatsu, Miki

Resigned

2017/3/31

Tazaki, Fumie

Resigned

2017/3/31

Kanaguchi, Masahiro Resigned

2017/3/31

Furutani, Akio

Resigned(NAOJ Chile Observatory, Specially
Appointed Senior Specialist)

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

2016/9/30

Fukui, Akihiko

Contract
Expired(Okayama Astrophysical Observatory,Specially Appointed Senior Specialist)

Okayama AstrophysicalObservatory, Specially Appointed
Research Staff

2016/9/30

Yamada, Ryuhei

Contract
ExpiredRISE Project, Specially Appointed
Research Staff

2016/11/30 Kim, Jeoung Sook

Contract
ExpiredMizusawa VLBI Observatory,Specially Appointed Research Staff

2017/3/31

Contract
ExpiredDivision of Theoretical Astronomy,
Specially Appointed Assistant Professor

Zenitani, Seiji(Astronomy Data Center, Specially
Appointed Research Staff)

Astronomy Data Center, Specially
Appointed Research Staff
NAOJ Chile Observatory, Specially
Appointed Research Staff

Division of Optical and Infrared(Ehime University Research Center for Space
Astronomy, Specially Appointed
and Cosmic Evolution, Associate Professor)
Assistant Professor
NAOJ Chile Observatory, Specially
Appointed Senior Specialist(Mizusawa VLBI Observatory, Specially
Appointed Research Staff)

Mizusawa VLBI Observatory,Specially Appointed Research Staff
Mizusawa VLBI Observatory,Specially Appointed Senior Specialist

III Organization149

2017/3/31

Matsumoto, Naoko

Contract
ExpiredMizusawa VLBI Observatory,Specially Appointed Research Staff

2017/3/31

Toshikawa, Jun

Contract
ExpiredSubaru Telescope, Specially
Appointed Research Staff

2017/3/31

Morokuma, KanaContract
ExpiredNAOJ Chile Observatory, Specially
Appointed Research Staff

2017/3/31

Takekoshi, Tatsuya

Contract
ExpiredNAOJ Chile Observatory, Specially
Appointed Research Staff

2017/3/31

Otawara, Kazushige

Contract
Expired(NAOJ Chile Observatory, Specially
Appointed Senior Specialist)

NAOJ Chile Observatory, Specially
Appointed Senior Specialist

Research Administrator Staff
Date
2016/7/1

2016/7/31

2017/1/31

Name
Hasuo, Ryuichi

Hired

New Affiliated Institute, Position

Previous Affiliated Institute,
Position

Research Enhancement Strategy Office,
Office of International Relations, Specially
Appointed Senior Specialist

Yamaguchi, Takahiro

Resigned

Research Enhancement Strategy
Office, Office of International
Relations, Specially Appointed
Senior Specialist

Ota, Masahiko

Contract
ExpiredResearch Enhancement Strategy
Office, Safety and HealthManagement Office, Specially
Appointed Senior Specialist

Foreign Visiting Researcher
Name
Kokkotas, Konstantinos
Packham, Christopher Charles
Koda, Jin
Overzier, Roderik Adriaan
Chibueze, James Okwe

150

ChangeIII Organization

2016/4/26
2016/5/16
2016/4/1
2016/4/2
2016/7/1

Period~ 2016/6/3~ 2016/8/17~ 2016/8/12~ 2016/5/1~ 2016/9/29

Affiliated InstituteEberhard Karls University of Tuebingen (Germany)
University of Texas at San Antonio (USA)The State University of New York at Stony Brook (USA)National Observatory, Rio de Janeiro (Brazil)
University of Nigeria (Nigeria)7. Advisory Committee for Research and Management
Members
From universities and related institutes
Ichimoto, Kiyoshi

Hida Observatories,
Graduate School of Science,
Kyoto University

Kajita, Takaaki

Institute for Cosmic Ray Research,
The University of Tokyo

Sugita, Seiji

School of Science, The Universityof Tokyo

Chiba, Seiji

Graduate School of Science andFaculty of Science, Tohoku
University

Doi, Mamoru

School of Science, The Universityof TokyoFujisawa, Kenta

The Research Institute for Time
Studies at Yamaguchi University

Matsushita, Kyoko

Faculty of Science Division 1,
Tokyo University of Science

Mitsuda, Kazuhisa

Institute of Space and Astronautical
Science

Murakami, Izumi

National Institute for Fusion
Science○ Momose, Munetake

College of Science, Ibaraki
University

From NAOJ
Arimoto, Nobuo
Usuda, Tomonori
Gouda, Naoteru
Kokubo, Eiichiro
Kobayashi, Hideyuki
Sakamoto, Seiichi
Takami, Hideki
Tomisaka, Kohji
Hasegawa, Tetsuo
Honma, Mareki● Watanabe, Jun-ichi

Subaru Telescope
TMT-J Project Office
JASMINE Project Office
Center for Computational
Astrophysics
Mizusawa VLBI Observatory
NAOJ Chile Observatory
Advanced Technology Center
Division of Theoretical Astronomy
NAOJ Chile Observatory
Mizusawa VLBI Observatory
Public Relations Center● Chairperson ○ Vise-Chairperson
Period: April 1, 2016 – March 31, 2018

III Organization

1518. Professors Emeriti
Professors Emeriti (NAOJ)
Kakuta, Chuichi
Hiei, Eijiro
Yamashita, Yasumasa
Nishimura, Shiro
Kozai, Yoshihide
Hirayama, Tadashi
Miyamoto, Masanori
Nariai, Kyouji
Okamoto, Isao
Nakano, Takenori
Kodaira, Keiichi
Yokoyama, Koichi
Oe, Masatsugu
Kinoshita, Hiroshi
Nishimura, Tetsuo
Kaifu, Norio
Ishiguro, Masato
Inoue, Makoto
Kawano, Nobuyuki
Andou, Hiroyasu
Karoji, Hiroshi
Chikada, Yoshihiro
Noguchi, Kunio
Fujimoto, Masakatsu
Manabe, Seiji
Miyama, Shoken
Kawaguchi, Noriyuki
Iye, Masanori
Shibasaki, Kiyoto
Sakurai, Takashi
Professors Emeriti (Tokyo Astronomical Observatory)
Moriyama, Fumio
Kozai, Yoshihide152

III Organization

IV Finance
Revenues and Expenses (FY2016)
Revenues
Management Expenses Grants
Facilities Maintenance Grants
Subsidy Income
Miscellaneous Income
Industry-Academia Research Income and Donation Income
Reversals of Reserves for Specific Purposes
Total
Expenses
Management Expenses
Employee Personnel Expenses
Operating Expenses
Facilities Maintenance Expenses
Subsidy Expenses
Industry-Academia Research Expenses and Donation Expenses
Total
Revenues-Expenses

Budget11,443,115
828,611
48,40045,901
373,239
550,000
13,289,266
Budget12,039,016
3,700,453
8,338,563
828,611
48,400373,239
13,289,266
Budget0

Final Account11,907,321
718,864
48,40059,937
573,8090
13,308,331
Final Account
11,711,869
3,675,932
8,035,937
718,865
48,400384,672
12,863,806
Final Account444,525(Unit: ¥1,000)
Budget − Final Account−464,206
109,7470−14,036−200,570
550,000−19,065
Budget − Final Account327,147
24,521
302,626
109,746
0−11,433
425,460
Budget − Final Account−444,525

IV Finance153

V KAKENHI (Grants-in-Aid for Scientific Research)
1. Series of Single-year Grants for FY 2016
Research Categories

Number of Selected Projects

Scientific Research on Innovative Areas(Research in a proposed research area)
Scientific Research (S)Scientific Research (A)Scientific Research (B)Young Scientists (A)JSPS Research Fellows
JSPS International Research Fellows
Research Activity Start-up
Publication of Scientific Research Results
Total

Budget (Unit: ¥1,000)
Direct Funding Indirect Funding

Total

10

42,80012,84055,640

1
11
5
2
7
1
3
1
41

20,40087,70030,700
9,700
8,000
500
3,100
500
203,400

6,120
26,310
9,210
2,910
2,400
0
930
0
60,72026,520114,010
39,91012,61010,400
500
4,030
500
264,120

Budget (Unit: ¥1,000)
Direct Funding Indirect Funding
20,400
6,120
8,200
2,460
15,7004,710
44,30013,290Total
26,520
10,66020,41057,5902. Multi-year Fund for FY 2016
Research Categories

Number of Selected Projects

Scientific Research (C)Challenging Exploratory Research
Young Scientists (B)
Total

18
8
17
43

3. Partial Multi-year Fund for FY 2016154

Research Categories

Number of
Selected Projects

Young Scientists (A)
Total

1
1

Budget (Series of Single-year Grants)(Unit: ¥1,000)
Direct Funding Indirect Funding
Total
0
0
0
0
0
0

V KAKENHI (Grants-in-Aid for Scientific Research)

Budget (Multi-year Fund)(Unit: ¥1,000)
Direct Funding Indirect Funding Total
100
30
130
100
30
130

VI Research Collaboration
1. Open Use
TypeProject/Center

Okayama
AstrophysicalObservatory

Category

Number of
Total
Accepted Number of
Proposal Researcher

188-cm Reflector Telescope(Project Program)

2

31 (0)

2 Institutes

188-cm Reflector Telescope(Normal Program)30

184 (10)16 Institutes, 5 Countries

188-cm Reflector Telescope(Student Program)

0

0 (0)

0 Institute

2

2 (0)

1 Institute

2
72

3 (0)
308 (43)

2 Institutes
57 Institutes, 11 Countries*
173 (55)
58 (7)
11 (3)*
48 Institutes, 11 Countries
18 Institutes, 5 Countries
5 Institutes, 2 Countries

62 (42)

21 Institutes, 7 Countries

109 (68)

32 Institutes, 15 Countries

188-cm Reflector Telescope(Miscellaneous Program)
188-cm Reflector Telescope (ToO Program)
Subaru Telescope
Solar Observatory
Nobeyama Radio
Observatory
Open Use at
Project/Center

Mizusawa VLBI
Observatory

45-m Telescope (Regular Program)
45-m Telescope (Short Program)
45-m Telescope (Back-up Program)
45-m Telescope (Large Program)
45-m Telescope (Director’s Discretionary Time)
VERA

*

23
12
1
0
2
18

Astronomy Data Center

364

Center for Computational Astrophysics
Hinode Science Center
Facility Use
Advanced
Technology Center Joint Research and Development

225
94
24
10

NAOJ Chile
Observatory
Nobeyama Radio
Observatory/NAOJ
Chile Observatory
Joint Development Research
Joint Research
Research Assembly
NAOJ Symposium

Note

ALMA (Cycle3)

402

ASTE

7

45-m/ASTE Joint program

4
9
2
20
1

364 (55
at foreign 34 Institutes, 17 Countries
institutes)
225 50 Institutes, 11 Countries
94 (36) 39 Institutes, 11 Countries
93
36 Institutes
59
21 Institutes
4,064
310 Institutes, 38 Countries(3,517)42 (2) 12 Institutes, 2 Countries

39 (8)

15 Institutes, 2 Countries
7 Institutes
2 Institutes
12 Institutes
1 Institute

The number of foreign researchers shown in brackets ( ) is included in the total.
Notes show the number of institutes and foreign countries represented by the proposal PIs. The country count does not include Japan.
The period of ALMA (Cycle3) is September, 2016 from October, 2015.
* The observation data is open to the public on the web. No application is needed to use the data.

VI Research Collaboration

1552. Commissioned Research Fellows
Visiting Scholars (Domestic)
Period: April 1, 2016 – March 31, 2017
Name

Position at NAOJ

Uzawa,Yoshinori

Visiting Professor

Otsubo, Toshimichi
Onishi, Toshikazu
Oka, Tomoharu
Nagao, Toru
Hayashi, Yoshiyuki
Momose, Munetake
Oshima, Akitoshi
Kobayashi, Kaori
Komugi, Shinya
Sagawa, Hideo
Sekine, Yasuhito
Sorai, Kazuo
Niinuma, Koutaro
Hirata, Naru
Kurayama, Tomoharu

Visiting Professor
Visiting Professor
Visiting Professor
Visiting Professor
Visiting Professor
Visiting Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Associate Professor
Visiting Research Fellow

Sakai, Takeshi

Visiting Research Fellow

Hayama, Kazuhiro

Visiting Research Fellow

Baba, Yukie

Visiting Research Fellow

Affiliated Institute
Terahertz Technology ResearchCenter, NICT
Hitotsubashi University
Osaka Prefecture University
Keio University
Ehime University
Kobe University
Ibaraki University
Chubu University
Toyama University
Kogakuin University
Kyoto Sangyo University
The University of Tokyo
Hokkaido University
Yamaguchi University
The University of Aizu
Teikyo University of Science
The University of ElectroCommunications
Institute for Cosmic Ray Research,
The University of Tokyo
Ochanomizu University

Host Project/Center/Division
NAOJ Chile Observatory
RISE Project
NAOJ Chile Observatory
NAOJ Chile Observatory
TMT-J Project Office
Center for Computational Astrophysics
NAOJ Chile Observatory
Center for Computational Astrophysics
NAOJ Chile Observatory
NAOJ Chile Observatory
NAOJ Chile Observatory
RISE Project
Nobeyama Radio Observatory
Mizusawa VLBI Observatory
RISE Project
Mizusawa VLBI Observatory
NAOJ Chile Observatory
Gravitational Wave Project OfficeMizusawa VLBI Observatory

JSPS (Japan Society for the Promotion of Science) Postdoctoral Research Fellows
Name
Arimatsu, Kou

Host Researcher
Research Subject
Exploring the outer Solar System by stellar occultations observed with wideWatanabe, Jun-ichi
field high-speed cameras

Uchiyama, Mizuho

Studying stellar evolution of forming massive young stellar objects with the midYamashita, Takuya
infrared variability observations

Shouda, Ayaka

Development of the multi-messenger observation system for a gravitational-wave
Flaminio, Raffaele
detector

Shirasaki, Masato

Probing Cosmic Dark Matter and Dark Energy with Higher-Order Statistics of Weak
Hamana, Takashi
Gravitational Lensing

Shinnaka, Yoshiharu

Physicochemistry of the early solar nebula: Thermal history of cometary dust and
Watanabe, Jun-ichi
isotopic fractionation of cometary volatiles

Yamauchi, Aya

Research in the structure of a distant region of our galaxy using a new distance
Honma, Mareki
measurement method with VERA

Ichikawa, Kohei

Revealing the coevolution of black holes and galaxies through the newly discovered
Imanishi, Masatoshi
population of AGN

JSPS (Japan Society for the Promotion of Science) Foreign Research Fellows
Name
Cataldi, Gianni
Wu, Benjamin156

VI Research Collaboration

Period2016/11/21 ~ 2018/11/20
2016/9/27 ~ 2017/9/26

Host Researcher
Ohashi, Nagayoshi
Nakamura, Fumitaka

VII Graduate Course Education
1. Department of Astronomical Science, School of Physical Sciences,
SOKENDAI (The Graduate University for Advanced Studies)
SOKENDAI (The Graduate University for Advanced
Studies) was established in 1988 as an independent graduate
university without undergraduate courses via partnerships withinter-university research institutes for the sake of advancing
graduate education.
There used to be four schools – Cultural and Social
Studies, Mathematical and Physical Sciences, Life Science,and Advanced Sciences before the reorganization of the Schoolof Mathematical and Physical Sciences into the schools ofPhysical Sciences, High Energy Accelerator Science, andMultidisciplinary Sciences in April 2004. Now the total ofsix schools are offering doctoral education and research
opportunities.
NAOJ has been accepting three-year doctoral-course
students since FY 1992 and five-year students since FY 2006
for the Department of Astronomical Science at the School ofPhysical Sciences. (The School of Mathematical and PhysicalSciences was reorganized into the School of Physical Sciencesin April 2004.)(1) Objective of the Department of Astronomical Science
The Department of Astronomical Science aims to train
students, through observational, theoretical, or instrument
development research in astronomy or in related fields, in anenvironment with the most advanced observational instruments
and supercomputers, as researchers who work at the forefrontof world-class research; experts who carry out development ofadvanced technology; and specialists who endeavor in educationand public outreach activities equipped with advanced andspecialized knowledge.
Numbers of students to be admitted:
Two (per year in the five-year doctoral course)
Three (per year in the three-year doctoral course)
Degree: Doctor of Philosophy(2) Admission Policy
The Department of Astronomical Sciences seeks students
with a strong interest in astronomy and the Universe; apassion for unraveling scientific questions through theoretical,
observational, and instrument development research; andstudents who have not only basic academic skills, but also
theoretical and creative aptitude required for advanced research.

(3) Department Details (Course Offerings)
Optical and Near Infrared Astronomy[Educational and Research Guidance Field]
Ground-based astronomy / Optical and infrared telescope
system / Planets / Sun, stars and interstellar matter /Galaxies and cosmology
Radio Astronomy[Educational and Research Guidance Field]
Ground-based astronomy / Radio telescope system / Sun,stars and interstellar matter / Galaxies
General Astronomy and Astrophysics[Educational and Research Guidance Field]
High-precision astronomical measurement / Astronomy
from space / Data analysis and numerical simulation / Earthand planets / Sun, stars and interstellar matter / Galaxies
and cosmology(4) Course-by-Course Education Program to Cultivate
Researchers in Physical Sciences with Broad Perspectives
The School of Physical Sciences began its “Course-byCourse Education Program to Develop Student Research
Capability and Aptitude” in FY 2009 as a part of MEXT’s
Program for “Enhancing Systematic Education in Graduate
Schools.” Since FY 2012 the School has been carrying out its
succeeding program, “Course-by-Course Education Program
to Cultivate Researchers in Physical Sciences with Broad
Perspectives”, offering four specific courses to the students:
the Basic Course, the Advanced Research Course, the Project
Research Course, and the Development Research Course. In FY
2015, the Department of Astronomical Science accepted five
students in the Basic Course and two students in the Advanced
Research Course. The Department also offered the e-learningclass “Introduction to Observational Astronomy II” as aschool-wide common basic subject, as well as the “Exercise in
Scientific English” class, in order to provide a good foundation
for students at the graduate school.
In order to better prepare students for the international stage,
the Department hosted the Asia Winter School during December
7 to 9, 2016, as well as the 2016 Summer Student programs at
Mitaka, Mizusawa, Kamioka, Okayama and Chile campuses toallow undergraduate students a chance to experience researchat the Department of Astronomical Science. In addition to
the existing Research Assistant system, the Department also
provided Associate Researcher positions for the students of the
Department of Astronomical Science.

VII Graduate Course Education

157

(5) Number of Affiliated Staff (2017/3/31)
Chair of the Department of Astronomical Science
Optical and Near Infrared Astronomy Course
Professors
Associate Professors
Lecturer
Assistant Professors
Radio Astronomy Course
Professors
Associate Professors
Assistant Professors
General Astronomy and Astrophysics Course
Professors
Associate Professors
Assistant Professors
Total

1
10
14
1
16
8
9
19
6
14
14
112

(6) Graduate Students (33 students)
1st year (6 students)
Name

Principal Supervisor

Ishikawa, Hiroyuki

Usuda, Tomonori

Hayashi, Saeko

Kawamura, Yuta

Matsuo, Hiroshi

Ezawa, Hajime

Tanioka, Satoshi

Aso, Yoichi

Flaminio, Raffaele

Hatta, Yoshiki

Sekii, Takashi

Hosokawa, Ko

Kotani, Takayuki

Watanabe, Tetsuya
Takami, Hideki
Usuda, Tomonori

Research Theme
Detailed study of the habitable exoplanets as candidates where
actual life can be found
Basic development of Photon Counting Terahertz Interferometer
Direct measurement of the coating thermal noise using
cryogenic optical cavities
Helio- and asteroseismology
Development of a new high-resolution spectrograph with aspatial resolution and study of an exoplanet characterization

Watanabe, Noriharu

Usuda, Tomonori

Takami, Hideki
Aoki, Wako

Observational Studies of Orbital Evolution of Various
Exoplanets System

2nd year (5 students)
Name

Principal SupervisorAndo, Misaki

Iono, Daisuke

Kambara, Nagaaki
Kikuta, Satoshi

Sekii, Takashi
Imanishi, Masatoshi

Supervisor
Saito, Masao
Espada, Daniel
Watanabe, Tetsuya
Kodama, Tadayuki

Matsuno, Tadafumi

Aoki, Wako

Arimoto, Nobuo

Yoshida, Masaki

Suematsu, Yoshinori Hara, Hirohisa

3rd year (3 students)
Name

Principal Supervisor

Michiyama, Tomonari Iono, Daisuke

158

Yamamoto, Moegi

Kodama, Tadayuki

Kim, Jungha

Honma, Mareki

VII Graduate Course Education

Supervisor

Research Theme
Observing Colliding Galaxies Using ALMA
Local helioseismology
AGN feedback to low-mass galaxy formation at high redshift
Observational study of metal-poor stars to reveal the history of
the near-field UniverseOn the Structure and Heating Mechanism of Solar
Chromosphere and Corona

Supervisor
Research Theme
Kodama, Tadayuki
Observing Starburst Galaxies Using ALMA
Nakanishi, Koichiro
Iwata, Ikuru
Searching for distant clusters with Subaru/HSC
Understanding the circumstellar structure of high-mass young
Shibata, Katsunori
stellar objects based on KaVA observations

4th year (6 students)
Name
Okutomi, Koki
Onoue, Masafusa

Principal Supervisor
Supervisor
Aso, Yoichi
Flaminio, Raffaele
Kashikawa, Nobunari Miyazaki, SatoshiBaba, Haruka

Aoki, Wako

Usuda, Tomonori

Ryu, Tsuguru

Hayashi, Saeko

Usuda, Tomonori

High-Contrast Imaging for Intermediate-Mass Giants with
Long-Term Radial Velocity Trends

Uchiyama, Hisakazu

Kashikawa, Nobunari Matsuda, Yuichi

The study of large-scale structures based on wide-imaging
observations of Subaru telescope

Taniguchi, Kotomi

Saito, Masao

Chemical evolution and mechanisms of carbon-chain moleculesin star-forming regions

5th year (13 students)
Name

Principal Supervisor

Yang, Yi

Hayashi, Saeko

Ishikawa, Shogo

Kashikawa, Nobunari Kodama, Tadayuki

Onishi, Kyoko

Iguchi, Satoru

Onitsuka, Masahiro

Usuda, Tomonori

Sakurai, Junya

Miyazaki, Satoshi

Shimakawa, Rhythm

Kodama, Tadayuki

Arimoto, Nobuo

Suzuki, Taiki
Min, Cheul Hong
Pathak, Prashant

Ohishi, Masatoshi
Honma, Mareki
Takami, Hideki

Saito, Masao
Shibata, Katsunori
Minowa, Yosuke

Kobayashi, Hiroshi

Ohsuga, Ken

Tomisaka, Kohji

Suzuki, Tomoko

Kodama, Tadayuki

Iono, Daisuke

Shino, Nagisa

Honma, Mareki

Shibata, Katsunori

Sukom, Amnart

Tomisaka, Kohji

Hayashi, Saeko

Ohishi, Masatoshi

Supervisor
Usuda, Tomonori

Research Theme
Development of laser interferometer module torwards DECIGOStudies on High-z quasars by wide-field imaging observation
Development of infrared instruments and observational researchfor exploring Earth-like exoplanets

Research Theme
Direct Imaging of Circumstellar Disks and Planets in Binary
Systems
Measurement of dark halo mass by clustering analysis of starforming galaxies

Observational study towards black-hole mass: resolving thecoevolution process of black hole and galaxy
Observational Studies of the Structure and Evolution of Exoplantes
Takato, Naruhisa
Study of large scale structures in the universe through wide
Kobayashi, Yukiyasu
field imaging
Iono, Daisuke

Environmental and mass dependence of galaxy properties at thecosmic noon
Research on Organic Molecules in the Universe
Research for a symbiotic star using VERA
Chromaticity effects on high resolution imaging
Radiation Hydrodynamics Simulations of Clumpy Outflows
from Black-hole Accretion disks
Galaxy formation beyond the peak epoch probed by [OIII] emitters
Testing the massive-star formation scenario via methanol maser
observations
Study of star and planetary formation process and theexoplanets based on infrared observations

VII Graduate Course Education

159

2. Education and Research Collaboration with Graduate Schools
Name
Inooka, Kota
Choi, Insa

Affiliated InstituteSupervisor
The University of Tokyo Yamashita, Takuya
The University of Tokyo Ohashi, Nagayoshi

Shimizu, Takayuki

The University of Tokyo Sekimoto, YutaroMori, Kanji

The University of Tokyo Kajino, Toshitaka

Yamaguchi, Masayuki The University of Tokyo Kawabe, Ryohei
Kurose, Ippei
The University of Tokyo Ohashi, Nagayoshi

Impact of New GT Strengths on Explosive SN Ia
Nucleosynthesis
mm/sub-mm Study of Planet and Star Formation
Observational Study of Star Forming Regions
The performance evoluation of Nano-JASMINE’s CCD withradial rays

Sakai, Iori

The University of Tokyo Kobayashi, Yukiyasu

Sasaki, Hirokazu

The University of Tokyo Kajino, Toshitaka

Fujii, Yoshinori

The University of Tokyo Flaminio, Raffaele

Fujita, Ayato
Tatsuuma, Misako
Luo, Yudong

The University of Tokyo Gouda, Naoteru
The University of Tokyo Kokubo, Eiichiro
The University of Tokyo Kajino, Toshitaka

Shu, Shibo

The University of Tokyo Sekimoto, Yutaro

Kuramochi, Kazuki

The University of Tokyo Kobayashi, Hideyuki

Lee, Minju

The University of Tokyo Kawabe, Ryohei

Kato, Yuta

The University of Tokyo Sakamoto, Seiichi

Sakai, Daisuke

The University of Tokyo Kobayashi, Hideyuki

Dynamical study of molecular clouds in the Galactic centerwith radio observations

Hirai, Yutaka

The University of Tokyo Kajino, Toshitaka

Exploring galactic chemo-dynamical evolution throughr-process elements

Marchio, Manuel

The University of Tokyo Flaminio, RaffaeleAso, Yusuke

The University of Tokyo Ohashi, Nagayoshi

Ohashi, Satoshi

The University of Tokyo Sakamoto, Seiichi

Saito, Toshiki

The University of Tokyo Kawabe, Ryohei

Shibagaki, Shota

The University of Tokyo Kajino, Toshitaka

Shibata, Takashi

The University of Tokyo Kokubo, Eiichiro

Sekiguchi, Shigeyuki The University of Tokyo Sekimoto, Yutaro
Tagawa, Hiromichi
Koyamatsu, Shin

160

ThesisObservational research of exoplanets
A study on Star Formation using radio interferometer
Development of the instruments for the cosmic microwave
background observation.

The University of Tokyo Gouda, Naoteru
The University of Tokyo Ohashi, Nagayoshi

VII Graduate Course Education

Collective neutrino oscillations and application to
nucleosynthesis in core-collapse supernovae
Development of the vibration isolation system for the
KAmioka GRavitational-wave Antenna
Dynamical Structure and its Evolution of the Milky Way
Planetary System Formation
Field Theory and Cosmology
Development of superconducting MKID camera for CMB
B-mode polarization
Observational demonstration of RIAF with sub-mm VLBI
using Sparse Modeling
Environmental effect on galaxy evolution using dense gas tracer
Star forming activity in the z=2-3 proto-clusters with Infrared
Space telescope

Development, characterization and improvement of themirrors for the KAGRA gravitational wave detector
A study on Star Formation using radio interferometer
Chemical evolution of the star-forming cores in the giant
molecular clouds
Star Formation and Super Massive Black Hole in Merging
Galaxies through Dense Molecular Gas Observations
Revealing the origin of r-process elements with astrophysicalsimulations
Terrestrial Planet Formation
Development of broadband dual polarimetry MKID camera
for observation of CMB B-mode polarization
Early cosmic merger of multiple black holes
Formation and Evolution of Protoplanetary Disks

3. Commissioned Graduate Students
Doctoral Course

Affiliated Institute
Osaka Prefecture
University

Period2016/4/1 ~2017/3/31

Silva, Andrea

Tufts University

2016/4/1 ~2017/3/31

Iono, Daisuke

ALMA Observations of Starburst Galaxies

Fujita, Shinji

University of Tsukuba

2016/4/1 ~2017/3/31

Saito, Masao

Studying of processes of clump formation in
GMCs

Matsuo, Mitsuhiro

Kagoshima University

2016/4/1 ~2017/3/31

Saito, Masao

Observations of molecular clouds in the outergalaxy with a wideband digital spectrometer

Master’s Course

Affiliated Institute

PeriodSupervisor

ThesisKozuki, Yuto

Supervisor
Noguchi, Takashi

Thesis100 GHz SIS Mixer with wide RF and IF
bandwidth

Kokubo, Tsukasa

Tokyo Universityof Agriculture andTechnology

2016/4/1 ~2017/3/31

Watanabe, Jun-ichi

Optical processing and evaluation for exoplanet
exploration system

Ito, Ayaka

Hosei University

2016/4/1 ~2017/3/31

Usuda, Tomonori

Observational Studies of Exoplanets

Takumi, Asami

The Open University ofJapan

2016/4/1 ~2017/3/31

Watanabe, Jun-ichi

Observational researches on Small Solar System
BodiesTani, Ryo

The University of Electro- 2016/10/1 ~Communications
2017/3/31

Kashikawa,Nobunari

Circum galactic medium probed by Lyman-alphaintensity mapping

Morozumi,
Tatsuhiko

The University of Tokyo

2016/10/1 ~2017/3/31

Aso, Yoichi

Development of Beam Reducing Telescope

Oyamada, Shuri

Japan Women's
University

2016/10/1 ~2017/3/31

Nakamura,
FumitakaObservational Study of Orion Molecular Cloudwith a dense gas tracer

Komeda, Satoshi

Kyushu University

2016/10/1 ~2017/3/31

Fukushima, Toshio

Research of X-ray objects using archive datafrom X-ray satellites

4. Degrees Achieved with NAOJ Facilities
Name

DegreeThesisInvestigation of the Coevolution between Supermassive Blackholes
and Galaxies at Redshift 3 through Subaru Near-Infrared Observations

Saito, Yuriko

Doctor of Philosophy, SOKENDAI

Matsuzawa, Ayumu

Doctor of Philosophy, SOKENDAIIshikawa, Shogo

Doctor of Philosophy, SOKENDAI

Onishi, Kyoko

Doctor of Philosophy, SOKENDAI

Onitsuka, Masahiro
Shimakawa, Rhythm

Doctor of Philosophy, SOKENDAI
Doctor of Philosophy, SOKENDAI

Suzuki, Taiki

Doctor of Philosophy, SOKENDAI

Suzuki, Tomoko

Doctor of Philosophy, SOKENDAI

Accelerated Star-Forming Activity before the Peak Epoch as Revealed
by Galaxies Emitting Strong Lines of Doubly Ionized Oxygen

Min, Cheulhong

Doctor of Philosophy, SOKENDAIVERA Observations of 43GHz SiO Masers toward a Symbiotic Star R
Aquarii

Study on the Verification Method of Pointing Performance ofSubmillimeter Wavelength Antenna through the ALMAThe Galaxy–Halo Connection Across Cosmic History
Black-Hole Mass Measurements in Nearby Galaxies Using Molecular
Gas Dynamics
A Study of the Transit-Like Phenomena around a T-Tauri StarThe Forming Galaxy Clusters at the Cosmic NoonA Study on Evolution of N-bearing Complex Organic Molecules
towards Glycine

VII Graduate Course Education

161

VIII Public Access to Facilities
1. Mitaka Campus

2. Mizusawa Campus[Open year-round]
Dates: April to March, 10:00–17:00
Every day except for the New Year ’s season(December 28–January 4)
Visitors: 20,413
Open Facilities: Observatory History Museum (65-cm
Telescope Dome), 20-cm Telescope Dome, Solar
Tower Telescope, Exhibit Room, Repsold Transit
Instrument Building (Transit Instrument Museum),
Astronomical Instruments Museum, Gautier Meridian
Circle Building, Old Library[Open year-round]
Dates: April to March (except for New Year’s season), 9:00–
17:00 daily
Visitors: 18,100
Open Facilities: Kimura Hisashi Memorial Museum, VERA
20-m antenna, 10-m VLBI antenna[Regular Star Gazing Parties]
Dates: Friday before second Saturday; fourth Saturday
Visitors: 4,671 (23 events)
Open Facility: 50-cm Telescope for Public Outreach[4D2U Theater Showings]
Dates: Friday before second Saturday; first, second, andthird Saturdays
Visitors: 5,432 (47 events)
Open Facility: 4D2U Dome Theater[Special Open-House Event] Mitaka Open House Day
Dates: October 21 (Fri.), 2016, 14:00–19:00
October 22 (Sat.), 2016, 10:00–19:00
Topic: Gravitational Waves, a new Frontier of Astronomy
Visitors: 4,534
This event is jointly sponsored by NAOJ, the Universityof Tokyo School of Science Institute of Astronomy, the
SOKENDAI Department of Astronomical Science, and the
NINS Astrobiology Center. It has been held for 2 days each year,
starting from 2010. The perennially popular lectures related tothis year’s theme were hosted by the Institute of Astronomy,
University of Tokyo (“The Universe Observed in Kiso’s Sky
by Tomo-e Gozen” Shigeyuki Sakoh, Assistant Professor) and
NAOJ (“Listening to the Universe with Gravitational Waves”
Raffaele Flaminio, NAOJ Specially Appointed Professor; and“Seeing Gravitational Waves with Electromagnetic Waves?
Pursuing the true Nature of Gravitational Wave Sources throughElectromagnetic Follow-up Observations” Michitoshi Yoshida,
Professor, Hiroshima University).
* Guided tours corresponding to group tours (Dantai Kengaku)
and cultural property events were also held. In addition the“Information Space of Astronomy and Science” was openedin 2015 near the south entrance of Mitaka Station to distributeinformation.

162

VIII Public Access to Facilities

The open house event is held at the campus with thecooperation of the Oshu Space and Astronomy Museum (OSAM:
Yugakukan) located in the campus.
[Special Open Day] Held as part of Iwate Galaxy Festival 2016
(Hours: 10:00-20:30)
Date: August 20 (Sat.), 2016, 10:00–20:30
Visitors: Approximately 2,500
Same as last year, the Open Day was co-hosted with
Ihatov Space Action Center / the Oshu Space and Astronomy
Museum (OSAM: Yugakukan) and the city of Oshu. The event
was opened with a performance by a marching band from a
local elementary school. NAOJ offered such attractions as
exhibits about the research results of VERA, RISE, and CfCA;
tours of the 20-m parabolic antenna; commemorative photobooth; plastic bottle rocket launch; a quiz game; tours of thesupercomputer "Aterui;" and a special guided tour of the Array
Operations Center (AOC) and the VLBI correlator.
Special lectures about black holes were given by Ms. Arisa
Kuroda of TV fame, Masaki Ando, Associate Professor of
University of Tokyo, Mareki Honma, Director of the Mizusawa
VLBI Observatory and Ken Osuga, Assistant Professor of theCenter for Computational Astrophysics, and were enormously
well received.
OSAM (Yugakukan) offered various experiments in thescience stalls, workshops, etc., which were carried out by thestudent interns. The Open Day was a great success with close
ties to the local people.

Iriki: VERA Iriki Station[Open year-round]
Dates: April to March (except for New Year’s season)
Visitors: 5,949[Special Open Day]
Date: August 7 (Sun.), 2016, 12:00–20:00
Visitors: Approximately 4,500
This special open event was held in conjunction with
“Yaeyama Highland Star Festival 2016” hosted by the executive
committee primarily formed by members of Satsuma-Sendai
city hall and Kagoshima University.

At the NAOJ VERA 20-m radio telescope and the Kagoshima
University 1-m optical/infrared telescope facilities, guided toursof telescopes and observation buildings were held. NAOJ
offered such attractions as parent-child science experiments,
plastic bottle rocket launching, 4D2U (4-Dimentional Digital
Universe screening), and a stargazing party at night. This time
JAXA supported a chance to try on a spacesuit, which was wellreceived.
The special lecture of the year was given by Takumi
Nagayama, Specially Appointed Senior Specialist from
Mizusawa VLBI Observatory. All visitors had fun and weresatisfied with scientific programs offered in this festival.

Ogasawara: VERA Ogasawara Station[Open year-round]
Dates: April to March (except for New Year’s season)
Visitors: 9,930[Special Open Day]
Date: February 12 (Sun.), 2017, 10:00–16:30
Visitors: 227
A special open house event was held this year again under
the name “Star Island 16”. Same as last year, the free shuttle
buses were appreciated by the visitors. The number of visitors
was 227, which was more than last year. Because the number ofthe resident in the island is about 2,000, more than 10 % of theislanders visited this event.
NAOJ offered such attractions as exhibits about the research
results of VERA and RISE, 20-m parabolic antenna driving
experience, quiz games, a commemorative photo booth, andshort lectures.
On the night before the special open house, Space Lectures
were given at the Ogasawara Visitor Center by Director General
Masahiko Hayashi and Kazuhiro Hada, Assistant Professor at
Mizusawa VLBI Observatory, and were attended by 46.
A stargazing party was held by the local Ogasawara
astronomy club on the day following the special open house,
February 13, and NAOJ members also assisted. Thanks to good
weather, the stargazing party was well received and the numberof visitors was 50.

Ishigakijima: VERA Ishigakijima Station[Open year-round]
Dates: April to March (except for the New Year’s season);premises are open to the public 24 hours/day, andthe observation rooms are open during the hours of
10:00–16:30.
Visitors: 2,442

Same as previous years, attractions like antenna tours, acommemorative photo booth, merchandise, commemorative
lectures, and exhibits were offered.

Ishigakijima: Ishigakijima Astronomical Observatory[Open year-round]
Dates: April to MarchOpen Hours: Wednesdays through Sundays (Except for the
New Year’s season; when Monday / Tuesday is anational holiday, it is open and then closes on thenext day.), 10:00–17:00
Stargazing Sessions: Evenings on Saturdays, Sundays,
Holidays, and Star Festival weekdays (19:00–22:00),
two 30-minute sessions per evening, with support of
NPO Yaeyama Star Club
4D2U Screening: from 15:00 to 15:30 every day when theobservatory is open
Visitors: 15,061 (903 during the Star Festival of the Southern
Island)Open Facilities: Murikabushi 105-cm optical/infrared
telescope, Starry Sky Study Room (featuring the
4D2U “4-Dimensional Digital Universe”), interior ofobservation dome (including exhibits of astronomical
images)The Starry Sky Study Room, constructed adjacent to theobservatory in 2013 by the Ishigaki city, was very popular,
welcoming 6,186 guests.

[Star Festival of the Southern Island 2016]
Dates: August 6 (Sat.) to August 14 (Sun.), 2016
Visitors: Approximately 11,000
This year is the 15th anniversary of both the completion of
VERA Ishigakijima Station and the Star Festival of the Southern
Island. Approximately 11,000 visitors attended the dimmed-lightstargazing event blessed with better weather than ever before.
The annual planetarium screening was attended by 623.
The activities at Ishigakijima Astronomical Observatory
boost regional development like school education, lifelong
learning, and sightseeing. The cooperation agreement between
NAOJ and the Ishigaki-city tourism exchange association has
been finalized. And it is widely recognized that the starry sky
can be used as a tourism resource. Considering this situation, we
will continue to strengthen our ties with other associations.

[Special Open day] The Special Open Day was held as a part of
the Star Festival of the Southern Island.
Dates: August 7 (Sun.), 2016, 10:00–17:00
Visitors: 194 (252 during the Star Festival of the Southern
Island)VIII Public Access to Facilities1633. Nobeyama Campus[Regular Open]
Open Time: 8:30–17:00 (every day except during New
Year’s Season (Dec. 29 to Jan. 3), open until 18:00
during the summer (Jul. 20 to Aug. 31))
Visitors: 44,961
Open Facilities: 45-m Radio Telescope, Nobeyama
Millimeter Array, Nobeyama Radioheliograph, etc.
(just viewing) and NINS Nobeyama exhibition room
(just July to September)[Open House Day]
Date: August 27 (Sat.), 2016, 9:30–16:00
Visitors: 1,675
The theme of the 2016 Open House Day was “Let’s go on ajourney to look for a Black Hole”. We have two lectures on thetheme, which attract large audiences every year. This year one
was “Pursuing Objects Emitting Gravitational Waves” by Dr.
Tanaka, Masaomi (NAOJ). The other was “Objects lurking in
the Galactic Center” by Prof. Oka, Tomoharu (Keio University).
However, we had only 1,675 visitors due to stormy weather onthat day. Several events, such as the chance to touch the mainreflector panel of the 45-m Radio Telescope, had to be canceled.
It was severe conditions for visitors and staff members. In spiteof the bad weather, we had some established hands-on events
such as the antenna handicrafts, radio detector handicrafts,
and the antenna origami. At the NINS exhibition room, thepresentation of the 4D theater, exhibits of other institutes,
and the Mitaka VR system operated by the CfCA team were
offered. In addition, the ALMA team offered the ALMA VR
system and some short lectures. Moreover, we had balloons forchildren presented by the NRO character, Dr. Nobeyama, andthe NRO original panel for taking commemorative pictures. We
had unfortunate weather, but felt some hope because we were
supported by many people from other projects of NAOJ as wellas other institutes of NINS.
[Jimoto Kansha Day] (Thanks Day for the locals)
Date: February 11 (Sat.), 2017, 13:30–16:00
Visitors: 45
It is difficult for the local people to join the Open House Day
during the farming season. They do not know so much what we,not only NRO but also Tsukuba and Shinshu Universities, study
in Nobeyama. In response to these comments, we establishedthis event in cooperation with Shinshu University, Faculty ofAgriculture, Education and Research Center of Alpine Field
Science and Tsukuba University, Agricultural and Forestry
Research Center, Yatsugatake Forest. At the Vegetaball Withhosted by Shinshu University, we also had an exhibition on
the “scarlet runner bean” project, which is studied by Shinshu
University in cooperation with Minamimaki Village. The
exhibitions by elementary school students and a “scarlet runnerbean” sampling party were held out. Also, we had three lectures,

164

VIII Public Access to Facilities“Nagano is Astro-Prefecture” by NAOJ, “Talk about various
plants in the local area” by Tsukuba University and “Introduction
to the scarlet runner bean project” by Shinshu University.
It appeared to be a local-based event.

4. Okayama Campus

5. Subaru Telescope

Okayama Astrophysical Observatory[Open year-round]
Dates: 9:00–16:30 daily
Visitors: 10,102
Open Facilities: Window view of Okayama 188-cm Reflector
Telescope[Summit Facility Tour]• Dates open for public tour: 55 (these dates are listed in the
public tour program page at the Subaru Telescope’s web
site, only 1 day was canceled due to the hurricane; no tours
scheduled during the winter months of December to March,
the weather was particularly bad in December, January andMarch)• Public tour visitors: 456• Special tour visitors: 127 groups, 592 visitors[Special Stargazing Party]
Date: April 2 (Sat.), 2016, 18:30–22:25
Visitors: 79
133 applications for 348 applicants were received. Pollux ofGemini and Jupiter were viewed.
Date: July 30 (Sat.), 2016, 18:30–22:25
Visitors: 81
124 applications for 359 applicants were received. Mars andSaturn were viewed.

[Base Facility Tour]• Special tour visitors: 40 groups, 398 visitors[Public information]• Primary means of disseminating public information is
posting at the official website http://subarutelescope.org○ Science results from the Subaru Telescope – 9 Japaneseand 10 English articles○ Depicting special activities or announcing Calls for
Proposals, recruitment – 46 Japanese and 30 English
articles. Japanese topics include 22 articles in a series
introducing the Subaru Telescope.
• Web postings are supplemented by social media via official
accounts○ Twitter accounts – SubaruTelescope (for Japanese),
SubaruTel_Eng (for English)○ Facebook pages – 国立天文台 (for Japanese), National
Astronomical Observatory of Japan (for English, started
February 2015)○ YouTube channels – Subaru Telescope NAOJ (forJapanese), Subaru Telescope NAOJe (for English)[Outreach]
1. Lectures at the Subaru Telescope’s base facility in Hilo: 18
cases, reached 281 people
2. Remote presentations, mainly to Japan: 11 cases, reached1,349 people
3. Lectures, demonstrations, workshops etc. in the vicinity: 16
cases, reached 482 people
4. Lectures in Japan: 13 cases, reached 4,933 people
5. Others - Exhibits etc.: 8 cases, reached approximately 1,905
people
6. Media coverage
23 Japanese media visits. No English media visits.

VIII Public Access to Facilities165

IX Overseas Travel
Research and Academic Staff Overseas Travel(Including employees on annual salary system)
country/area

category

Business Trip

South Korea
43
China
37
Thailand5
Taiwan29
Hong Kong
1
Singapore
1
Indonesia
1
Philippines
0
Other areas in Asia
23
Hawai`i
68
U.S.A.
94
Australia
6
Italy
26
U.K.
33
France13
Canada5
Guam, Saipan0Germany
37
Other areas in Europe and Oceania
50
Mexico2
Brazil0Africa4
Other areas in South and Central America *
46
Total
524
* Most travelers to South and Central America went to Chile.

166

IX Overseas Travel

Training

Total

0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0
0

43
37
5
29
1
1
1
0
23
68
94
6
26
33
13
5
0
37
50
2
0
4
46
524

X Award Winners
Award Recipients

Affiliated Division

Job TitleAward
The 2nd SOKENDAI Future Scientist
Award

Date

Onishi, Kyoko

SOKENDAI

Student

Saito, Masao; Mizuno,
Norikazu; Iguchi,
Satoru; et al.

Nobeyama Radio
Observatory/NAOJ Chile
Observatory/NAOJ Chile
Observatory/et al.

FY2016 The Commendation for Science
Associate
and Technology by the Minister ofProfessor/Associate
Education, Culture, Sports, Science
Professor/
and Technology, Prizes for Science andProfessor/et al.
Technology (Development Category)

2016/4/12

Assistant Professor

FY2016 The Commendation for Scienceand Technology by the Minister of
Education, Culture, Sports, Scienceand Technology, The Young Scientists’Prize

2016/4/21

Assistant Professor

FY2016 The Commendation for Scienceand Technology by the Minister of
Education, Culture, Sports, Scienceand Technology, The Young Scientists’Prize

2016/4/21

Special Breakthrough Prize In
Fundamental Physics

2016/5/2

Spotlight on Optics (from the OpticalSociety, OSA)

2016/5/26

Zenitani, Seiji

Division of Theoretical
Astronomy

2016/4/4

Tanaka, Masaomi

Division of Theoretical
Astronomy

Flaminio, Raffaele;
Barton, Mark; et al.

Gravitational Wave Project
OfficeAkutsu, Tomotada

Gravitational Wave Project
OfficeAssistant Professor

Fukagawa, Misato

NAOJ Chile Observatory

Specially
The 5th NINS Young Researcher'sAppointed
Prize
Associate Professor

Flaminio, Raffaele; et al.

Gravitational Wave Project
Office2016 Gruber Cosmology Prize

2016/7/12

Public Relations Center
Web Team

Public Relations Center

WebAward 2016 Best Science Website

2016/9/12

Hara, Hirohisa;
Watanabe, Tetsuya;
Toriumi, Shin

SOLAR-C Project Office/Hinode Science Center/
Division of Solar andPlasma Astrophysics

Associate Professor/
Professor/Specially
Daiwa Adrian Prize 2016
Appointed
Assistant Professor

2016/11/15

Iye, Masanori

TMT-J Project Office

RCUH/Professor
emeritus

SPIE FELLOW

2017/1/31

Tanaka, Masaomi

Division of Theoretical
Astronomy

Assistant Professor

The 9th Inoue Science Research Award

2017/2/3

CLASP Project TeamSOLAR-C Project Office/Hinode Science Center2016 NAOJ Director General Prize

2017/3/7

Nobeyama
45m-Telescope
Improvement Team

Nobeyama Radio
Observatory/Advanced
Technology Center2016 NAOJ Director General Prize

2017/3/7

Okamoto, Joten

NAOJ Chile Observatory

Specially
Appointed
Assistant Professor

The 9th SPSS Award

2017/3/9

Nakamura, Koji

Gravitational Wave Project
OfficeResearch Affiliate

Particle Physics Scholarships 11th
Seitaro Nakamura Prize

2017/3/17

Hada, Kazuhiro

Mizusawa VLBI
Observatory

Assistant Professor

ASJ Young Astronomer Awards 20162017/3/17

Takiwaki, Tomoya

Division of Theoretical
Astronomy

Assistant Professor

ASJ Young Astronomer Awards 20162017/3/17

2016/6/5

X Award Winners

167

XI Library, Publications
1. Library
Number of books in each library (2017/3/31)
Japanese Books
Mitaka17,462
Okayama
222
Nobeyama
1,225
Mizusawa
4,972
Hawai`i
1,605
Total
25,486

Foreign Books
45,823
3,363
6,294
18,083
4,534
78,097

Total
63,285
3,585
7,519
23,055
6,139
103,583

Number of journal titles in each library (2017/3/31)
Japanese Journals
Foreign Journals
Mitaka638
775
Okayama4
18
Nobeyama
16
82
Mizusawa
659
828
Hawai`i
17
17
Total
1,334
1,720

Total
1,413
22
98
1,487
34
3,054

2. Publication
Here we list continuing publications produced by NAOJ in FY 2016.
Mitaka01) Report of the National Astronomical Observatory of Japan, Vol. 18: 1 issue02) Annual Report of the National Astronomical Observatory of Japan (in Japanese), no. 28, Fiscal Year 2015: 1 issue03) Annual Report of the National Astronomical Observatory of Japan (in English), vol. 18 Fiscal Year 2015: 1 issue04) National Astronomical Observatory Reprint, No. 2749–2885; 137 issues05) Calendar and Ephemeris, 2017; 1 issue06) NAOJ News, No. 273–284; 12 issues07) Guide to the National Astronomical Observatory of Japan pamphlet (Japanese); 1 issue08) Guide to the National Astronomical Observatory of Japan pamphlet (English); 1 issue09) Rikanenpyo (Chronological Scientific Tables), 2017; 1 issue

168

XI Library, Publications

XII Important Dates
April 1, 2016 – March 31, 20172016
April 2Spring 2016 Special Stargazing Party held at Okayama Astrophysical Observatory, with 79 visitors in attendance(out of 348 applicants).

April 12

Japanese ALMA Antenna Development Team won Commendation for Science and Technology by the Minister of
Education, Culture, Sports, Science and Technology (Prizes for Science and Technology, Development Category).

April 17

Seventh Open Observatory event held at the Ibaraki University Center for Astronomy and the NAOJ Mizusawa
VLBI Observatory Ibaraki Station, with 348 visitors in attendance.

April 21

The ALMA Observatory issued the ALMA Cycle 4 call for proposals for early scientific observations which starts
from October 2016 and received by the deadline a total of 1610 observation proposals from astronomers around theworld.

May 7
May 17
May 20
May 28Subaru Telescope staff interacted with the public during the AstroDay event in a shopping mall in Hilo.
The Japan-Chile Chamber of Commerce and Industry held its monthly meeting and invited NAOJ Chile
Observatory Director Seiichi Sakamoto as a speaker to give a lecture.
A NAOJ Chile Observatory staff member gave a lecture at the Japanese School of Buenos Aires, Argentina.
“Starry Sky Photo Session in NAOJ Nobeyama” was held in Nobeyama Radio Observatory. There were 31
participants from many places in Japan.

June 6~
June 10Observation training of Radio Astronomy at Nobeyama Radio Observatory for Undergraduate Students was
performed; there were 12 participants.

June 11NAOJ and Riken Lecture “Origin of Materials told by the Universe” held at Hitotsubashi Hall with 325 guests in
attendance.

Early July
July 7
July 15~
September 18
July 17

Subaru Telescope staff’s visual work was part of the exhibit at the Tokyo train station during the star festival
program.
A NAOJ Chile Observatory staff member gave a lecture as a Tanabata event at the Japanese School in Santiago.
An exhibit “The Sun” held at the Information Space of Astronomy and Science.
Star Festival held using the 6-m antenna at the NAOJ Mizusawa VLBI Observatory Kagoshima station in
Kagoshima City Kinko Bay Park, co-hosted with Kagoshima City and Kagoshima University, with approximately
200 visitors in attendance.

July 25~July 29 Facility Guide Week for Educational Organization was carried out at Nobeyama Radio Observatory.
Summer 2016 Special Stargazing Party held at Okayama Astrophysical Observatory, with 81 visitors in attendanceJuly 30(out of 359 applicants).
August 3~
August 5

Chura-boshi Research Team workshop for high school students held at VERA Ishigakijima Station and Ishigakijima
Astronomical Observatory, with 15 participants from Ishigakijima,one participant from the main island of Okinawa
and one participant from Hyogo Prefecture in attendance. The team using radio-waves couldn't discover anything
but the second team using visible light observations with the Murikabushi Telescope discovered 3 candidates.

August 6~
August 14

The Star Festival of the Southern Island 2016 held together with a special open house event at the VERA
Ishigakijima Station and Ishigakijima Astronomical Observatory with approximately 11,000 visitors to the wholeStar Festival. Events including an astronomical observation party at Ishigakijima Astronomical Observatory,
attended by 338 visitors; and a special public opening of the VERA Station attended by 252 visitors.

August 7

Special open house of VERA Iriki station held jointly with the Yaeyama Highland Star Festival 2016, withapproximately 4,500 visitors in attendance.

August 8~
August 10

Tenth Z-star Research Team event held for high school students in the six Tohoku prefectures, with 15 participants
attending. The participants were divided into two groups, made a astronomical obsevation, and analyzed data using
the VERA Mizusawa 20-m radio telescope. However, neither team could find any maser celestial objects.

August 10~
September 6

As a part of the summer student program held by NAOJ and the Department of Astronomical Science of the
Graduate University for Advanced Studies (SOKENDAI), two undergraduate students from Kyoto Sangyo
University stayed at the Chile Observatory and conducted research with ALMA data.

August 16~
August 17“Astronomy classes for kids in Summer 2016” held in Mitaka Campus.

XII Important Dates

169

August 20
August 20
August 27
September 10

Iwate Galaxy Festival 2016, a special open house day of Mizusawa Campus, held with approximately 2,500 visitors
in attendance.
A lecture “What is the Sun?” held at the Information Space of Astronomy and Science.
Open House day of Nobeyama Radio Observatory. There were 1,675 visitors for this event.
Hinode 10th anniversary lecture “Exploring the Universe and the Earth through Solar Observations” held at
Nagoya University with 228 guests in attendance.

September 12~
8 undergraduate students participated in the observation experience program at the Subaru Telescope.
September 17
September 15

Mr.Toshiei Mizuochi, State Minister for Ministry of Education, Culture, Sports, Science and Technology visitedthe Santiago Central Office of the Joint ALMA Observatory.

September 23~ An exhibit “Mitaka Solar System Walk - Let’s Realize the Size and Distance of Each Planet -” opened at theNovember 6
Information Space of Astronomy and Science.
NAOJ, International Astronomical Union Office for Astronomy Outreach, and Japanese Society for Education and
September 24~
Popularization of Astronomy co-hosted “The 3rd Symposium on Universal Design for Astronomy Education” with
September 26
131 guests (including 25 handicapped persons and 15 foreigners).
October 2~
October 4

The 12th Workshop for Popularizing Cutting Edge Astronomy held with the theme of “Gravitational Wave
Astronomy” at University of Toyama and the Institute for Cosmic Ray Research, University of Tokyo.

October 12~
November 6

An exhibit “Solar Tower Telescope” opened at the Information Space of Astronomy and Science.

October 21~
October 22

Mitaka Open House Day held, with 4,534 visitors in attendance.

November 17

The Management Agreement Concerning Operations of ALMA was signed by the National Astronomical Observatoryof Japan, the Associated Universities Inc., and the European Southern Observatory in the Santiago Central Office of
the Joint ALMA Observatory.

November 21

A ceremony for FY 2016 continuous service recognition was held. 10 NAOJ staff members were recognized: Hitoshi
Yamaoka, George Kosugi, Satoshi Miyazaki, Fumitaka Nakamura, Tadafumi Takata, Hiroshi Araki, Tomofumi
Umemoto, Yoji Seto, Hiroyuki Narisawa, and Tatsuya Todoriki.

November 23

The first “Nagano is Astro-Prefecture” meeting was held in Matsumoto Campus of Shinshu University by the
executive committee consisting of staff members of Nobeyama Radio Observatory, Kiso Observatory in the
University of Tokyo, Shinshu University, and so on.There were about 100 participants.

November 23

The Subaru Telescope/Shinshu University public lecture “From Shinshu via Hawai`i, a galactic Research Journey”
held at Shinshu University with 350 guests in attendance.

November 26
November 27

NAOJ lecture meeting/22nd ALMA public lecture “The Birth of Stars and Planets Explored by ALMA” held at
Nagoya City Science Museum with 225 guests in attendance.
“The Subaru Telescope/Hiroshima University public lecture” held at Hiroshima Children's Museum.

2017
January 6~
January 10
January 14
January 26
January 28

170

Graduate students from the Department of Astronomical Science, SOKENDAI (Graduate University for Advanced
Studies) and astronomy major students from the University of Hawaiʻi at Hilo worked together to observe with the
Subaru Telescope.
Honorable Hirokazu Matsuno, the minister of the Ministry of Education, Culture, Sports, Science and Technology Japan, visited the Subaru Telescope’s facilities at Hilo and Maunakea.
NAOJ Chile Observatory staff members visited a summer camp held by Santiago Japanese School to give a lecture.
Staff of the Subaru Telescope held science workshops and put on an interactive booth at the annual Onizuka Science
Day at the University of Hawaiʻi at Hilo.

February 11“Jimoto kansha Day (Thanks Day for the locals)” was held at the Vegetaball With hosted by Shinshu University. It
was carried out by 3 Nobeyama Institutes (Tsukuba and Shinshu Universities and Nobeyama Radio Observatory).
There were 45 participants.

February 12

Star Island 16 open house event of VERA Ogasawara Station held, with 227 visitors in attendance (more than the
average year).

March 2~
March 3

NAOJ/The International Planetarium Society (IPS) and others co-hosted the “Data to Dome Workshop” with 52
guests from 8 oversea countries in attendance.

March 5The 23rd NINS Symposium “Frontiers of Modern Astronomy: a Second Earth and the Dark Universe” held at Tokyo
International Exchange Center (TIEC) with 273 guests in attendance.

March 13~
March 17

Staff of the Subaru Telescope and TMT-J Project Office visited classes in the public schools in Hilo and vicinity
during the Journey through the Universe program.

XII Important Dates

March 31

A ceremony for FY 2016 continuous service recognition for retiring staff members was held. 5 staff members wererecognized: Yoshihiko Mizumoto, Nobuo Arimoto, Yukiyasu Kobayashi, Motokazu Noguchi, and Matsuo Watanabe.

NAOJ staff participated in the “Fureai (Friendly) Astronomy” program by visiting schools to talk about their work
Throughout theand the telescope. This outreach program started seven years ago and was spearheaded by Dr. Nobuo Arimoto, theyear
Director of the Subaru Telescope.

XII Important Dates

171

XIII Publications, Presentations
1. Refereed Publications
Abbott, B. P., et al. including Tanaka, M., Yanagisawa, K.: 2016,
Localization and Broadband Follow-up of the Gravitational-wave
Transient GW150914, ApJL, 826, L13.
Abbott, B. P., et al. including Tanaka, M., Yanagisawa, K.: 2016,
Supplement: “Localization and Broadband Follow-up of theGravitational-wave Transient GW150914” (2016, ApJL, 826, L13),
ApJS, 225, 8.
Abbott, B. P., et al. including Flaminio, R.: 2016, Upper Limits On The
Rates of Binary Neutron Star and Neutron Star-black Hole Mergers
from Advanced Ligo’s First Observing Run, ApJL, 832, L21.
Abbott, B. P., et al. including Flaminio, R.: 2016, Supplement: “TheRate of Binary Black Hole Mergers Inferred from Advanced Ligo
Observations Surrounding GW150914” (2016, ApJL, 833, L1), ApJS,
227, 14.
Abbott, B. P., et al. including Flaminio, R.: 2016, Characterization ofTransient Noise in Advanced LIGO Relevant to Gravitational Wave
Signal GW150914, Classical Quant. Grav., 33, 134001.
Abbott, B. P., et al. including Flaminio, R.: 2016, GW150914: First
Results from the Search for Binary Black Hole Coalescence with
Advanced LIGO, Phys. Rev. D, 93, 122003.
Abbott, B. P., et al. including Flaminio, R.: 2016, Observing
Gravitational-Wave Transient GW150914 with Minimal Assumptions,Phys. Rev. D, 93, 122004.
Abbott, B. P., et al. including Flaminio, R.: 2016, Search for Transient
Gravitational Waves in Coincidence with Short-duration Radio
Transients during 2007-2013, Phys. Rev. D, 93, 122008.
Abbott, B. P., et al. including Flaminio, R.: 2016, High-energy Neutrino
Follow-up Search of Gravitational Wave Event GW150914 with
ANTARES and IceCube, Phys. Rev. D, 93, 122010.
Abbott, B. P., et al. including Flaminio, R.: 2016, Comprehensive Allsky Search for Periodic Gravitational Waves in the Sixth Science Run
LIGO Data, Phys. Rev. D, 94, 042002.
Abbott, B. P., et al. including Flaminio, R.: 2016, Directly Comparing
GW150914 with Numerical Solutions of Einstein’s Equations for
Binary Black Hole Coalescence, Phys. Rev. D, 94, 064035.
Abbott, B. P., et al. including Flaminio, R.: 2016, First Targeted Search
for Gravitational-wave Bursts from Core-collapse Supernovae in
Data of First-generation Laser Interferometer Detectors, Phys. Rev. D,
94, 102001.
Abbott, B. P., et al. including Flaminio, R.: 2016, Properties of the
Binary Black Hole Merger GW150914, Phys. Rev. Let., 116, 241102.
Abbott, B. P., et al. including Flaminio, R.: 2016, GW151226:
Observation of Gravitational Waves from a 22-Solar-Mass Binary
Black Hole Coalescence, Phys. Rev. Let., 116, 241103.
Abbott, B. P., et al. including Flaminio, R.: 2016, Tests of General
Relativity with GW150914, Phys. Rev. Let., 116, 221101.
Abbott, B. P., et al. including Flaminio, R.: 2016, Binary Black Hole
Mergers in the First Advanced LIGO Observing Run, Phys. Rev. X, 6,
041015.
Abbott, B. P., et al. including Flaminio, R.: 2016, Improved Analysis of172

XIII Publications, Presentations

GW150914 Using a Fully Spin-Precessing Waveform Model, Phys.
Rev. X, 6, 041014.
Abbott, B. P., et al. including Flaminio, R.: 2017, The Basic Physics ofthe Binary Black Hole Merger GW150914, Ann. Phys.-Berlin, 529,
1600209.
Abbott, B. P., et al. including Flaminio, R.: 2017, All-sky Search for
Short Gravitational-wave Bursts in the First Advanced LIGO Run,
Phys. Rev. D, 95, 042003.
Abbott, B. P., et al. including Flaminio, R.: 2017, Upper Limits on the
Stochastic Gravitational-Wave Background from Advanced LIGO’s
First Observing Run, Phys. Rev. Let., 118, 121101.
Abbott, B. P., et al. including Flaminio, R.: 2017, Directional Limits
on Persistent Gravitational Waves from Advanced LIGO’s First
Observing Run, Phys. Rev. Let., 118, 121102.
Akiyama, E., et al. including Hashimoto, J., Hasegawa, Y., Kudo, T.,
Kusakabe, N., Kuzuhara, M., Ohashi, N., Egner, S., Guyon, O.,
Hayano, Y., Hayashi, M., Hayashi, S. S., Ishii, M., Iye, M., Kandori,R., Morino, J., Nishimura, T., Pyo, T., Suenaga, T., Suto, H., Suzuki,R., Takahashi, Y. H., Takato, N., Terada, H., Tomono, D., Takami,
H., Usuda, T., Tamura, M.: 2016, Spiral Structure and Differential
Dust Size Distribution in the LKHα 330 Disk, AJ, 152, 222.
Akiyama, K., Kuramochi, K., Ikeda, S., Fish, V. L., Tazaki,F., Honma, M., Doeleman, S. S., Broderick, A. E., Dexter, J.,Mościbrodzka, M., Bouman, K. L., Chael, A. A., Zaizen, M.: 2017,
Imaging the Schwarzschild-radius-scale Structure of M87 with the
Event Horizon Telescope Using Sparse Modeling, ApJ, 838, 1.
Akiyama, K., Stawarz, L., Tanaka, Y. T., Nagai, H., Giroletti, M.,
Honma, M.: 2016, EVN Observations of HESS J1943+213:
Evidence for an Extreme TeV BL Lac Object, ApJL, 823, L26.
Akutsu, T., Saito, Y., Sakakibara, Y., Sato, Y., Niwa, Y., Kimura,N., Suzuki, T., Yamamoto, K., Tokoku, C., Koike, S., Chen, D.,
Zeidler, S., Ikeyama, K., Ariyama, Y.: 2016, Vacuum and Cryogenic
Compatible Black Surface for Large Optical Baffles in Advanced
Gravitational-wave Telescopes, Opt. Mater. Exp., 6, 1613
Alexander, D. M., et al. including Matsuda, Y.: 2016, ALMA Observationsof a z ≈ 3.1 Protocluster: Star Formation from Active Galactic Nuclei
and Lyman-alpha Blobs in an Overdense Environment, MNRAS, 461,
2944–2952.
Alonso-Herrero, A., et al. including Packham, C., Ichikawa, K.,
Imanishi, M.: 2016, The Complex Evolutionary Paths of Local
Infrared Bright Galaxies: A High-angular Resolution Mid-infrared
View, MNRAS, 463, 2405–2424.
Arai, A., Kawakita, H., Shinnaka, Y., Tajitsu, A.: 2016, Origins of
Absorption Systems of Classical Nova V2659 CYG (NOVA CYG
2014), ApJ, 830, 30.
Arai, H., et al. including Fujita, S., Yamauchi, A., Kaneko, H.,
Miyamoto, Y.: 2016, A Multi-Line Ammonia Survey of the Galactic
Center Region with the Tsukuba 32 m Telescope. I. Observations andData, PASJ, 68, 76.
Araki, H., Kashima, S., Noda, H., Kunimori, H., Chiba, K., Mashiko, H.,
Kato, H., Otsubo, T., Matsumoto, Y., Tsuruta, S., Asari, K., Hanada,
H., Yasuda, S., Utsunomiya S., Takino, H.: 2016, Thermo‑optical

Simulation and Experiment for the Assessment of Single, Hollow, andLarge Aperture Retroreflector for lunar Laser Ranging, Earth Planets
Space, 68, 101.
Asahina, Y., Kawashima, T., Furukawa, N., Enokiya, R., Yamamoto, H.,
Fukui, Y., Matsumoto, R.: 2017, Magnetohydrodynamic Simulationsof the Formation of Molecular Clouds toward the Stellar Cluster
Westerlund 2: Interaction of a Jet with a Clumpy Interstellar Medium,
ApJ, 836, 213.
Asensio-Torres, R., et al. including Currie, T., Kudo, T., Akiyama, E.,
Egner, S., Guyon, O., Hayano, Y., Hayashi, M., Hayashi, S. S., Ishii,
M., Iye, M., Kandori, R., Morino, J.-I., Nishimura, T., Pyo, T.-S.,
Serabyn, E., Suto, H., Suzuki, R., Takahashi, Y., Takato, N., Terada,
H., Takami, H., Usuda, T., Tamura, M.: 2016, Polarimetry and Flux
Distribution in the Debris Disk around HD 32297, A&A, 593, A73.
Baba, J., Morokuma-Matsui, K., Miyamoto, Y., Egusa, F., Kuno, N.:
2016, Gas Velocity Patterns in Simulated Galaxies: Observational
Diagnostics of Spiral Structure Theories, MNRAS, 460, 2472–2481.
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Fabricius, M., Walawender, J., Arimoto, N., Cook, D., Elms, B.,
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Feinberg, L., Rioux, N., Bolcar, M., Liu, A., Guyon, O., Stark, C.,
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Flaminio, R.: 2016, The Cryogenic Challenge: Status of the KAGRA
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Fujii, Y., Sekiguchi, T., Takahashi, R., Aso, Y., Barton, M., Erasmo, F.,
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Giono, G., Katsukawa, Y., Ishikawa, R., Narukage, N., Kano,
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Honda, S., Notsu, Y., Maehara, H., Notsu, S., Shibayama, T., Nogami, D.,
Shibata, K.: 2017, Lithium Abundance of the Solar-Type SuperflareStars, JPS Conf. Proc. 14 (NIC2016), Eds. S. Kubono, et al., 020303.
Huang, Y., et al. including Iguchi, S., Asayama, S., Iono, D., Gonzalez,A.: 2016, The Atacama Large Millimeter/sub-millimeter Array band1 receiver, Proc. SPIE 9911, Eds. G. Z. Angeli, P. Dierickx, 99111V.
Iguchi, S., Saito, M.: 2016, Large Aperture Millimeter/Submillimeter
Telescope: Which is More Cost-Effective, Aperture Synthesis
Telescope Versus Large Single Dish Telescope?, Proc. SPIE 9906,
Eds. H. J. Hall, R. Gilmozzi, H. K. Marshall, 99062T.
Ishigaki, M. N., Tsujimoto, T., Shigeyama, T., Aoki, W.: 2016, Chemical
Evolution of r-process Elements in the Draco Dwarf Spheroidal
Galaxy, Proc. IAU Symp. 317, Eds. A. Bragaglia, M. Arnaboldi, M.
Rejkuba, D. Romano, 310–311.
Ishikawa, S., Shimizu, T., Kano, R., Bando, T., Ishikawa, R., Giono,G., Beabout, D. L., Beabout, B. L., Nakayama, S., Tajima, T.: 2016,
In-Flight Performance of the Polarization Modulator in the CLASP
Rocket Experiment, Proc. SPIE 9905, Eds. J.-W. A. den Herder, T.
Takahashi, M. Bautz, 99052U
Ishino, H., et al. including Hasebe, T., Noguchi, T., Sekimoto, Y.: 2016,
LiteBIRD: Lite Satellite for the Study of B-mode Polarization and
Inflation from Cosmic Microwave Background Radiation Detection,
Proc. SPIE 9904, Eds. H. A. MacEwen, G. G. Fazio, M. Lystrup,
99040X.
Ishizuka, M., Kotani, T., Nishikawa, J., Tamura, M., Kurokawa, T.,
Mori, T., Kokubo, T.: 2016, Fiber Mode Scrambler Experiments for
the Subaru Infrared Doppler Instrument (IRD), Proc. SPIE 9912, Eds.

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189

R. Navarro, J. H. Burge, 99121Q.
Izumi, N., Kobayashi, N., Yasui, C., Tokunaga, A. T., Saito, M., Hamano,
S.: 2017, Star-Formation Efficiency in the outer Galaxy, Proc. IAU
Symp. 321, Eds. A. Gil de Paz, J. H. Knapen, J. C. Lee, 31–33.
Jenniskens, P, Borovicka, J., Watanabe, J., Jopek, T., Abe, S.,
Consolmagno, Guy J., Ishiguro, M., Janches, D., Ryabova, Galina
O., Vaubaillon, J., Zhu, J.: 2016, Division F Commission 22:
Meteors, Meteorites, and Interplanetary Dust, Proc. IAU, 11, T29A
(Transactions IAU), Ed. T. Montmerle, 365–379.
Jike, T.: 2016, VERA Geodetic VLBI with a Newly Developed Highspeed Sampler and Recorder, IVS 2016 General Meeting Proceedings,
Eds. D. Behrend, K. D. Baver, K. L. Armstrong, 159–162.
Jovanovic, N., Cvetojevic, N., Schwab, C., Norris, B., Lozi, J., Gross,S., Betters, C., Singh, G., Guyon, O., Martinache, F., Doughty, D.,
Tuthill, P.: 2016, Efficiently Feeding Single-mode Fiber Photonic
Spectrographs with an Extreme Adaptive Optics System: On-sky
Characterization and Preliminary Spectroscopy, Proc. SPIE 9908,
Eds. C. J. Evans, L. Simard, H. Takami, 99080R.
Jovanovic, N., et al. inluding Guyon, O., Lozi, J., Currie, T., Pathak, P.,
Doughty, D., Goebel, S., Kudo, T., Kotani, T., Minowa, Y., Takato,N., Tamura, M., Takami, H., Hayashi, M.: 2016, The SCExAO HighContrast Imager: Transitioning from Commissioning to Science, Proc.
SPIE 9909, Eds. E. Marchetti, L. M. Close, J.-P. Véran, 99090W.
Jovanovic, N., Guyon, O., Kawahara, H., Kotani, T.: 2017, Application ofMulticore Optical Fibers in Astronomy, Optical Fiber Communications
conference 2017, W3H.3.
Kakiuchi, K., Suzuki, T. K., Fukui, Y., Torii, K., Machida, M.,
Matsumoto, R.: 2017, Vertical Flows and Structures Excited by
Magnetic Activity in the Galactic Center Region, Proc. IAU Symp.
322, Eds. R. M. Crocker, S. N. Longmore, G. V. Bicknell, 220–221.
Katsukawa, Y., Kamata, Y., Anan, T., Hara, H., Suematsu, Y., Bando,
T., Ichimoto, K., Shimizu, T.: 2016, Development of a Near-Infrared
Detector and a Fiber-optic Integral Field Unit for a Space Solar
Observatory SOLAR-C, Proc. SPIE 9904, Eds. H. A. MacEwen, G. G.
Fazio, M. Lystrup, 99045I.
Kawabe, R., Kohno, K., Tamura, Y., Takekoshi, T., Oshima, T., Ishii, S.:
2016, New 50-m-class Single-dish Telescope: Large Submillimeter
Telescope (LST), Proc. SPIE 9906, Eds. H. J. Hall, R. Gilmozzi, H. K.
Marshall, 990626.
Kitagawa, Y., Yamagata, Y., Morita, S., Motohara, K., Ozaki, S.,
Takahashi, H., Konishi, M., Kato, N. M., Kobayakawa, Y., Terao, Y.,
Ohashi, H.: 2016, Fabrication of a Wide-field NIR Integral Field Unit
for SWIMS Using Ultra-precision cutting, Proc. SPIE 9912, Eds. R.
Navarro, J. H. Burge, 991225.
Kiuchi, H., Hills, R., Whyborn, N. D., Asayama, S., Sakamoto, S.,
Iguchi, S., Corder, S. A.: 2016, Artificial Calibration Source for
ALMA Radio Interferometer, Proc. SPIE 9914, Eds. W. S. Holland, J.
Zmuidzinas, 99142O.
Kokubo, T., Mori, T., Kurokawa, T., Kashiwagi, K., Tanaka, Y., Kotani,T., Nishikawa, J., Tamura, M.: 2016, 12.5-GHz-spaced Laser
Frequency Comb Covering Y, J, and H Bands for Infrared Doppler
Instrument, Proc. SPIE 9912, Eds. R. Navarro, J. H. Burge, 99121R.
Komiyama, Y., Nakaya, H., Kashikawa, N., Uchida, T.: 2016, Conceptual
Design of Wide-field Focal Plane with InGaAs Image Sensors, Proc.
SPIE 9908, Eds. C. J. Evans, L. Simard, H. Takami, 99085X.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,

190

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K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2016, GRB
160624A: MITSuME Ishigakijima Upper Limits, GRB Coordinates
Network, Circular Service, 19571, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2016, GRB
160623A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 19572, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2016, GRB
160625B: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 19599, 1.
Kuroda, D., Hanayama, H., Miyaji, T., Watanabe, J., Yanagisawa,
K., Nagayama, S., Yoshida, M., Ohta, K., Kawai, N.: 2016, GRB
160703A: MITSuME Ishigakijima Optical Observation, GRB
Coordinates Network, Circular Service, 19653, 1.
Labadie, L., Berger, J.-P., Cvetojevic, N., Haynes, R., Harris, R.,
Jovanovic, N., Lacour, S., Martin, G., Minardi, S., Perrin, G., Roth,M., Thomson, R. R.: 2016, Astronomical Photonics in the Context ofInfrared Interferometry and High-resolution Spectroscopy, Proc. SPIE
9907, Eds. F. Malbet, M. J. Creech-Eakman, P. G. Tuthill, 990718.
Li, H.-N., Aoki, W., Honda, S., Zhao, G., Suda, T., Christlieb, N.:
2017, Exploring the Early Chemical Evolution of the Milky Waywith LAMOST and Subaru, JPS Conf. Proc. 14 (NIC2016), Eds. S.
Kubono, et al., 010201.
Lozi, J., Guyon, O., Jovanovic, N., Singh, G., Goebel, S., Norris,
B., Okita, H.: 2016, Characterizing and Mitigating Vibrations for
SCExAO, Proc. SPIE 9909, Eds. E. Marchetti, L. M. Close, J.-P.
Véran, 99090J.
Males, J., et al. including Guyon, O., Jovanovic, N., Lozi, J.: 2016,
The Path to Visible Extreme Adaptive Optics with MagAO-2K and
MagAO-X, Proc. SPIE 9909, Eds. E. Marchetti, L. M. Close, J.-P.
Véran, 990952.
Martinache, F., Jovanovic, N., Guyon, O.: 2016, Subaru Coronagraphic
eXtreme Adaptive Optics: On-sky Performance of the Asymmetric
Pupil Fourier Wavefront Sensor, Proc. SPIE 9909, Eds. E. Marchetti,
L. M. Close, J.-P. Véran, 990954.
Matsuo, M., Minamidani, T., Umemoto, T., Nishimura, A., Nakahishi,
H., Kuno, N., Fujita, S., Tosaki, T., Tsuda, Y., Yamagishi, M., Kohno,
M., FUGIN team: 2017, A Survey of Molecular Clouds in the Outer
Galaxy with the Highest Spatial Resolution, Proc. IAU Symp. 321,
Eds. A. Gil de Paz, J. H. Knapen, J. C. Lee, 44–44.
Mawet, D., et al. including Guyon, O.: 2016, Keck Planet Imager andCharacterizer: Concept and Phased Implementation, Proc. SPIE 9909,
Eds. E. Marchetti, L. M. Close, J.-P. Véran, 99090D.
Mennesson, B., et al. including Guyon, O., Tamura, M.: 2016, The
Habitable Exoplanet (HabEx) Imaging Mission: preliminary sciencedrivers and technical requirements, Proc. SPIE 9904, Eds. H. A.
MacEwen, G. G. Fazio, M. Lystrup, 99040L.
Miller, K., Guyon, O.: 2016, Linear Dark Field Control: Simulation for
Implementation and Testing on the UA Wavefront Control Testbed,
Proc. SPIE 9909, Eds. E. Marchetti, L. M. Close, J.-P. Véran,99094G.
Minamidani, T., Nishimura, A., Miyamoto, Y., Kaneko, H., Iwashita,H., Miyazawa, C., Nishitani, H., Wada, T., Fujii, Y., Takahashi, T.,
Iizuka, Y., Ogawa, H., Kimura, K., Kozuki, Y., Hasegawa, Y., Matsuo,
M., Fujita, S., Ohashi, S., Morokuma-Matsui, K., Maekawa, J.,Muraoka, K., Nakajima, T., Umemoto, T., Sorai, K., Nakamura, F.,
Kuno, N., Saito, M.: 2016, Development of the New Multi-Beam 100
GHz Band SIS Receiver FOREST for the Nobeyama 45-m Telescope,Proc. SPIE 9914, Eds. W. S. Holland, J. Zmuidzinas, 99141Z.
Minamidani, T., Umemoto, T., Nishimura, A., Matsuo, M., Tsuda, Y.,
Ohashi, S., Tosaki, T., Kuno, N.: 2016, Nobeyama CO Galactic Plane
Survey: New Chapter of the Nobeyama 45-m Telescope, EAS Publ.
Ser., 75–76, 193–194.
Minowa, Y., Takato, N., Iwata, I., Hattori, T.: 2016, An Overview ofCurrent and Future Instrumentation at the Subaru Telescope, Proc.
SPIE 9908, Eds. C. J. Evans, L. Simard, H. Takami, 990806.
Mitsuda, K., Hashiba, Y., Minowa, Y., Hayano, Y., Sugai, H., Shimono,A., Matsubayashi, K., Hattori, T., Kamata, Y., Ozaki, S., Doi, M.,
Sako, S.: 2016, CCD System Upgrading of the Kyoto3DII and
Integral Field Spectroscopic Observation with the New System, Proc.
SPIE 9908, Eds. C. J. Evans, L. Simard, H. Takami, 99082M.
Miura, N., Oh-ishi, A., Kuwamura, S., Baba, N., Hanaoka, Y., Ueno, S.,
Nakatani, Y., Ichimoto, K.: 2016, Status of Hida Solar Adaptive Optics
System and Experiment of Tomographic Wavefront Sensing, Proc.
SPIE 9909, Eds. E. Marchetti, L. M. Close, J.-P. Véran, 99092N.
Miyamoto, Y., Nakai, N., Seta, M., Salak, D., Nagai, M., Ishii, S.,
Yamauchi, A.: 2016, Hot Gas in the Center of the Seyfert Galaxy
NGC 3079, Proc. IAU Symp. 315, Eds. P. Jablonka, Ph. Andre, F. van
der Tak, E55.
Montmerle T., et al. including Cheung, S.-l.: 2016, Executive Committee
Working Group: Public Naming of Planets and Planetary Satellites,
Proc. IAU, 11, T29A (Transactions IAU), Ed. T. Montmerle, 539–548.
Morokuma-Matsui, K., Koda, J., Takekoshi, T., Saito, M., Nakanishi,
H., Boissier, S., Madore, B. F., Boselli, A., Gil de Paz, A., Thilker,
D., Yagi, M., Sorai, K., Kuno, N.: 2017, Search for Molecular Gas in
XUV Disk of M83, Proc. IAU Symp. 321, Eds. A. Gil de Paz, J. H.
Knapen, J. C. Lee, 268–268.
Motohara, K., et al. including Koshida, S., Uchiyama, M.: 2016,
NIR Camera and Spectrograph SWIMS for TAO 6.5 m Telescope:
Overview and Development Status, Proc. SPIE 9908, Eds. C. J.
Evans, L. Simard, H. Takami, 99083U.
Murakami, N., Nishikawa, J., Akaiwa, N., Komuro, Y., Baba, N.,
Tamura, M.: 2016, Fiber Mode Scrambler Experiments for the
Subaru Infrared Doppler Instrument (IRD), Proc. SPIE 9912, Eds. R.
Navarro, J. H. Burge, 99121Q.
Murakami, N., Nishikawa, J., Akaiwa, N., Komuro, Y., Baba, N.,
Tamura, M.: 2016, A Three-layer Eight-octant Phase Mask towards
Broadband High-contrast Observations, Proc. SPIE 9912, Eds. R.
Navarro, J. H. Burge, 99126G.
Murthy, J., Witt, A., Baggaley, W. J., Dwek, E., Levasseur-Regourd, A.-C.,
Mann, I., Mattila, K., Watanabe, J.: 2016, Division G Commission
21: Galactic and Extragalactic Backgrounds Radiation, Proc. IAU,
11, T29A (Transactions IAU), Ed. T. Montmerle, 522–524.
Naito, H., Watanabe, F., Sano, Y., Kuramoto, K., Itagaki, K., Kiyota, S.,
Arai, A., Matsumoto, K., Kojiguchi, N., Sugiura, Y., Maehara, H.,
Nishiyama, K., Kabashima, F., Henze, M., Darnley, M. J., Shafter,
A. W., Kato, M.: 2016, Optical Photometric Observations of M31N
2008-12a: Pre- and Post-maximum of the 2016 Eruption, The
Astronomer’s Telegram, 9891.
Nakai, Y., Baba, N., Murakami, N., Miura, N., Tamura, M.: 2016, Image
restoration for a hypertelescope, Proc. SPIE 9907, Eds. F. Malbet, M.

J. Creech-Eakman, P. G. Tuthill, 99073F.
Nakaya, H., Komiyama, Y., Kashikawa, N., Uchida, T., Nagayama, T.,
Yoshida, M.: 2016, Low Temperature Performance of a Commercially
Available InGaAs Image Sensor, Proc. SPIE 9915, Eds. A. D.
Holland, J. Beletic, 99151O.
Narukage, N., et al. including Ishikawa, R., Kubo, M., Kano,
R., Suematsu, Y., Yoshida, M.: 2016, Chromospheric LAyer
SpectroPolarimeter (CLASP2), Proc. SPIE 9905, Eds. J.-W. A. den
Herder, T. Takahashi, M. Bautz, 990508.
Newman, K., Sirbu, D., Belikov, R., Guyon, O.: 2016, Development of
PIAA Complex Mask Coronagraphs for Large Aperture Ground-based
Telescopes, Proc. SPIE 9912, Eds. R. Navarro, J. H. Burge, 99126L.
Nishikawa, J., Oya, M., Murakami, N., Tamura, M., Kurokawa, T.,
Tanaka, Y., Kotani, T.: 2016, Contrast Improvement with Imperfect
Pre-coronagraph and Dark-hole, Proc. IAU, 11, T29A (Transactions
IAU), Ed. T. Montmerle, 213.
Nishikawa, J., Oya, M., Murakami, N., Tamura, M., Kurokawa, T.,
Tanaka, Y., Kotani, T.: 2016, Contrast Improvement with Imperfect
Pre-coronagraph and Dark-hole, Proc. SPIE 9904, Eds. H. A.
MacEwen, G. G. Fazio, M. Lystrup, 99043E.
Nishimura, A., Umemoto, T., Minamidani, T., Kuno, N., Tosaki, T.,
Fujita, S., Matsuo, M., Tsuda, Y., Ohashi, S., NRO-GPS team: 2016,
Nobeyama 45 m CO Galactic Plane Survey: Filament Properties andStar Formation in M17, Proc. IAU Symp. 315, Eds. P. Jablonka, Ph.
Andre, F. van der Tak, E58.
Ohishi, M.: 2016, Search for Complex Organic Molecules in Space, J.
Phys.: Conf. Ser., 728, 052002.
Ohsawa, R., et al. including Watanabe, J.: 2016, Development of a
Real-time Data Processing System for a Prototype of the Tomo-eGozen Wide Field CMOS Camera, Proc. SPIE 9913, Eds. G. Chiozzi,
J. C. Guzman, 991339.
Oka, T., Mizuno, R., Miura, K., Takekawa, S.: 2017, Signature of anIntermediate-Mass Black Hole in the Central Molecular Zone of Our
Galaxy, Proc. IAU Symp. 322, Eds. R. M. Crocker, S. N. Longmore,
G. V. Bicknell, 119–122.
Oka, T., Mizuno, R., Miura, K., Takekawa, S.: 2017, Posiible Detection of
Quasi-Periodic Oscillations from Sgr A* at 43 GHz, Proc. IAU Symp.
322, Eds. R. M. Crocker, S. N. Longmore, G. V. Bicknell, 50–51.
Onishi, T., Nishimura, A., Tokuda, K., Harada, R., Dobashi, K.,
Shimoikura, T., Kimura, K., Ogawa, H.: 2016, Large-Scale Molecular
Gas Survey in 12CO, 13CO and C18O (J = 2–1) with the Osaka 1.85 m
mm-submm Telescope, Proc. IAU Symp. 315, Eds. P. Jablonka, Ph.
Andre, F. van der Tak, E62.
Ozaki, S., Miyazaki, S., Tsuzuki, T., Tanaka, Y.: 2016, Polishing Testof a Poly-crystal Calcium Fluoride Lens: toward the Developmentof TMT WFOS, Proc. SPIE 9908, Eds. C. J. Evans, L. Simard, H.
Takami, 99089N.
Pathak, P., Guyon, O., Jovanovic, N., Lozi, J., Martinache, F., Minowa,
Y., Kudo, T., Takami, H., Hayano, Y., Narita, N.: 2016, First Onsky Closed Loop Measurement and Correction of Atmospheric
Dispersion, Proc. SPIE 9909, Eds. E. Marchetti, L. M. Close, J.-P.
Véran, 990956.
Pehlivan, Y., Subasi, A. L., Birol, S., Ghazanfari, N., Yuksel, H.,
Balantekin, A. B., Kajino, T.: 2016, Can We Scan the Supernova
Model Space for Collective Oscillations?, CETUP* 2015 – Workshop
on Dark Matter, Neutrino Physics and Astrophysics & PPC 2015 –XIII Publications, Presentations

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IXth International Conference on Interconnections between Particle
Physics and Cosmology, AIP Conf. Proc. 1743, Eds. B. Szczerbinska,
R. Allahverdi, K. Babu, B. Balantekin, B. Dutta, T. Kamon, J. Kumar,
F. Queiroz, L. Strigari, R. Surman, 040007.
Rains, A., Ireland, M., Jovanovic, N., Feger, T., Bento, J., Schwab, C.,
Coutts, D., Guyon, O., Arriola, A., Gross, S.: 2016, Precision Single
Mode Fibre Integral Field Spectroscopy with the RHEA Spectrograph,Proc. SPIE 9908, Eds. C. J. Evans, L. Simard, H. Takami, 990876.
Rezaei, M., Park, M.-S., Wheaton, S., Tan, C. L., Fathipour, V., Guyon,O., Ulmer, M. P., Mohseni, H.: 2016, New Progress in Electroninjection Detectors for NIR Imagers with Low Noise and High Frame
Rates, Proc. SPIE 9915, Eds. A. D. Holland, J. Beletic, 99150P.
Saito, T., Iono, D., Ueda, J., Yun, M. S., Nakanishi, K., Sugai, H.,
Imanishi, M., Hagiwara, Y., Kaneko, H., Motohara, K., Espada,D., Yamashita, T., Lee, M., Michiyama, T., Kawabe, R.: 2016,
Molecular Gas Excitation and Chemistry in VV 114 and NGC 1614with ALMA, Proc. IAU Symp. 315, Eds. P. Jablonka, Ph. Andre, F.
van der Tak, E71.
Sako, S., et al. including Watanabe, J.: 2016, Development of a
Prototype of the Tomo-e Gozen Wide-field CMOS Camera, Proc.
SPIE 9908, Eds. C. J. Evans, L. Simard, H. Takami, 99083P.
Salak, D., Nakai, N., Miyamoto, Y.: 2016, Evolution of Molecular
Clouds in the Starburst Galaxy NGC 1808 Revealed with ALMA,EAS Publ. Ser., 75–76, 69–70.
Schwab, C., Jovanovic, N., Feger, T., Bakovic, M., Gurevich, Y. V.,
Stürmer, J., Apodaca, R., Vanzi, L., Rukdee, S., Lawrence, J. S.,
Coutts, D. W., Cvetojevic, N., Mahadevan, S., Stefánsson, G. K.,
Halverson, S. P., Guyon, O.: 2016, Adaptive Optics Fed Single-mode
Spectrograph for High-precision Doppler Measurements in the Nearinfrared, Proc. SPIE 9912, Eds. R. Navarro, J. H. Burge, 991274.
Sekimoto, Y., Sekiguchi, S., Shu, S., Sekine, M., Nitta, T., Naruse, M.,
Dominjon, A., Hasebe, T., Shan, W., Noguchi, T., Miyachi, A.,
Mita, M., Kawasaki, S.: 2016, Design of Corrugated-horn-coupled
MKID Focal Plane for CMB B-mode Polarization, Proc. SPIE 9914,
Eds. W. S. Holland, J. Zmuidzinas, 99142A.
Shu, S., Sekiguchi, S., Sekine, M., Sekimoto, Y., Nitta, T., Dominjon, A.,
Noguchi, T., Naruse, M., Shan, W.: 2016, Development of Octaveband Planar Ortho-mode Transducer with Kinetic Inductance Detector
for LiteBIRD, Proc. SPIE 9914, Eds. W. S. Holland, J. Zmuidzinas,
99142C.
Singh, G., Lozi, J., Choquet, E., Serabyn, E., Guyon, O.: 2016, PSF
Calibration Using the Lyot-based Low Order Wavefront Sensor
Telemetry: First Simulations, Proc. SPIE 9909, Eds. E. Marchetti, L.
M. Close, J.-P. Véran, 99097K.
Sôma, M., et al.: 2016, NOVA SCORPII 2016 No. 2 = PNV J172251123158349, CBET 4320, Ed. D. W. E. Green.,
Stoehr, F., Manning, A., Moins, C., Jenkins, D., Lacy, M., Leon, S.,
Muller, E., Nakanishi, K., Matthews, B., Gaudet, S., Murphy, E.,
Ashitagawa, K., Kawamura, A.: 2017, The ALMA Science Archive,
The Messenger, 167, 2–6.
Suematsu, Y., Saito, K., Koyama, M., Enokida, Y., Okura, Y., Nakayasu,
T., Sukegawa, T.: 2016, Development of Compact Metal-mirror
Image Slicer Unit for Optical Telescope of the SOLAR-C Mission,
Proc. SPIE 9904, Eds. H. A. MacEwen, G. G. Fazio, M. Lystrup, N.
Batalha, N. Siegler, E. C. Tong, 990411.
Suematsu, Y., Solar-C Working Group: 2016, The SOLAR-C Mission:

192

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Science Objectives and Current Status, ASP Conf. Ser. 504, Eds. I.
Dorotovic, C. E. Fischer, M. Temmer, 299–308.
Sugai, H., Kashima, S., Kimura, K., Matsumura, T., Inoue, M., Ito, M.,
Nishibori, T., Sekimoto, Y., Ishino, H., Sakurai, Y., Imada, H., Fujii,
T.: 2016, Optical Designing of LiteBIRD, Proc. SPIE 9904, Eds. H. A.
MacEwen, G. G. Fazio, M. Lystrup, 99044H.
Suzuki, T. K., Fukui, Y., Torii, K., Machida, M., Matsumoto, R.,
Kakiuchi, K.: 2017, Investigating Magnetic Activity in the Galactic
Centre by Global MHD Simulation, Proc. IAU Symp. 322, Eds. R. M.
Crocker, S. N. Longmore, G. V. Bicknell, 137–140.
Takakuwa, S., Phashi, N., Yen, H.-W., Chou, T.-L., Saigo, K., Saito, M.,
Aso, Y., Aikawa, Y., Koyamatsu, S., Machida, M. N., Takahashi, S.
Z., Tomida, K., Tomisaka, K.: 2016, SMA and ALMA Studies ofProtoplanetary Disk Formation around Low-Mass Protostars, Proc.
IAU Symp. 315, Eds. P. Jablonka, Ph. Andre, F. van der Tak, 126–129.
Takekawa, S., Oka, T., Tanak, K.: 2017, Physical Contact between the+20 km s−1 Cloud and the Galactic Circumnuclear Disk, Proc. IAU
Symp. 322, Eds. R. M. Crocker, S. N. Longmore, G. V. Bicknell,
145–146.
Tanaka, M., Chiba, M., Komiyama, Y., Tanaka, M., Okamoto, S.,
Okamoto, T.: 2017, The Missing Satellite Problem Outside of the
Local Group, Proc. IAU Symp. 321, Eds, A. Gil de Paz, J. H. Knapen,
J. C. Lee, 196–198.
Tanaka, M., Chiba, M., Komiyama, Y.: 2016, Discovery of New Dwarf
Galaxies around NGC4631 with Subaru/Hyper Suprime-Cam, Proc.
IAU Symp. 317, Eds. A. Bragaglia, M. Arnaboldi, M. Rejkuba, D.
Romano, 350–351.
Tokuyama, S., Oka, T., Takekawa, S., Yamada, M., Iwata, Y., Tsujimoto,S.: 2017, Statistical Study of High-Velocity Compact Clouds Basedon the Complete CO Imagings of the Central Molecular Zone, Proc.
IAU Symp. 322, Eds. R. M. Crocker, S. N. Longmore, G. V. Bicknell,
154–155.
Walawender, J., Wung, M., Fabricius, M., Tanaka, I., Arimoto, N.,
Cook, D., Elms, B., Hashiba, Y., Hu, Y.-S., Iwata, I., Nishimura, T.,
Omata, K., Takato, N., Wang, S.-Y., Weber, M.: 2016, The nuMOIRCS
Project: Detector Upgrade Overview and Early Commissioning Results,
Proc. SPIE 9908, Eds. C. J. Evans, L. Simard, H. Takami, 99082G.
Wizinowich, P., Chun, M., Mawet, D., Agapito, G., Dekany, R., Esposito,
S., Fusco, T., Guyon, O., Hall, D., Plantet, C., Rigaut, F.: 2016, Nearinfrared wavefront sensing, Proc. SPIE 9909, Eds. E. Marchetti, L. M.
Close, J.-P. Véran, 990915.
Yamada, M., Oka, T., Tanaka, K., Nomura, M., Takekawa, S., Iwata,Y., Tokuyama, S., Tanabe, K., Tsujimoto, S., Furusawa, M.: 2017,
Kinematics of the Ultra-High-Velocity Gas in the Expanding
Molecular Shell Adjacent to the W44 Supernova Remnant, Proc. IAU
Symp. 322, Eds. R. M. Crocker, S. N. Longmore, G. V. Bicknell,
151–153.
Yamanaka, M., Nakaoka, T., Kawabata, M., Kawabata, K. S., Tanaka, M.,
Tominaga, N., Maeda, K., Hashimoto, O., Kinugasa, K., Takayama,M., Morihana, K., Oister Collaboration: 2016, Spectroscopic FollowUp Observations of AT 2016coi (ASASSN-16fp) : Possible Detectionof Helium, The Astronomer's Telegram, 9124.
Yamaoka, H., Green, D. W. E., Samus, N. N., Aksnes, K., Gilmore, A. C.,
Nakano, S., Sphar, T., Tichá, J., Williams, G. V.: 2016, Division
B Commission 6: Astronomical Telegrams, Proc. IAU, 11, T29A
(Transactions IAU), Ed. T. Montmerle, 90–98.

Yasui, C., Izumi, N., Saito, M., Kobayashi, N.: 2017, A SpatiallyResolved Study of Initial Mass Function in the Outer Galaxy, Proc.
IAU Symp. 321, Eds. A. Gil de Paz, J. H. Knapen, J. C. Lee, 34–36.
Yatsu, Y., Kawai, N., Fujiwara, T., Tachibana, Y., Yoshii, T., Harita, S.,
Muraki, Y., Ohuchi, H., Kuroda, D., Yanagisawa, K., Hanayama, H.:
2016, Recent progress of the Robotic Telescope System “MITSuME”,
IV Workshop on Robotic Autonomous Observatories, Revista
Mexicana de Astronomía y Astrofísica (Serie de Conferencias) Vol.
48, Eds. M. D. Caballero-García, S. B. Pandey, D. Hiriart, A. J.
Castro-Tirado, 24–26.
Yilmaz, M., Selam, S. O., Sato, B., Bikmaev, I., Izumiura, H., Keskin,V., Kambe, E.: 2016, The Line Bisectors of G Type Giant Star
HD199719, The 19th Cambridge Workshop on Cool Stars, Stellar
Systems, and the Sun, Ed. G. A. Freiden, 69.
Yoneta, K., Murakami, N., Kotani, T., Kawahara, H., Matsuo, T., Baba,N., Tamura, M.: 2016, Development of Speckle Nulling Technique
for the Savart-plate Lateral-shearing Interferometric Nuller for
Exoplanets (SPLINE), Proc. SPIE 9912, Eds. R. Navarro, J. H.
Burge, 99126I.
Yoshii, Y., et al. including Koshida, S.: 2016, The University of Tokyo
Atacama Observatory 6.5 m Telescope: Project Overview and Current
Status, Proc. SPIE 9906, Eds. H. J. Hall, R. Gilmozzi, H. K. Marshall,
99060R.
Zacharias, N., Brown, A., Evans, D., Chen, L., Gouda, N., Makarov,
V., Shulga, A., Souchay, J., Teixeira, R., Unwin, S.: 2016, Division a
Commission 8: Astrometry, Proc. IAU, 11, T29A (Transactions IAU),
Ed. T. Montmerle, 46–59.

5. Publications in English
Kubono, S., Kajino, T., Nishimura, S., Isobe, T., Nagataki, S., Shima,T., Takeda, Y. (Ed.): 2017, Proceedings of 14th International
Symposium on Nuclei in the Cosmos (NIC2016), JPS, Japan.
Valtonen, M., Anosova, J., Kholshevnikov, K., Mylläri, A., Orlov, V.,
Tanikawa, K.: 2016, The Three-body Problem from Pythagoras to
Hawking, Springer International Publishing, Switzerland.
Yamada, M., Yoo, J., Zenitani, S.: 2016, Magnetic Reconnection: Energy
Conversion and Inventory of a Prototypical Magnetic Reconnection
layer (Astrophysics and Space Science Library book series 427),
Springer International Publishing, Switzerland.

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6. Conference Presentations
Agata, H., Canas, L., Karino, S.: 2016, Astronomy Education Standard
Curriculum, CAP2016, (Medellín, Colombia, May 16–20, 2016).
Agata, H., Canas, L., Karino, S.: 2016, Astronomy Education Standard
Curriculum, Global Hands-On Universe (GHOU) Conference
2016 with Galileo Teacher Training Program (GTTP) International
Workshop 2016, (Stord, Norway, Aug. 22–28, 2016).
Agata, H., Canas, L., Usuda-Sato, K., Kato, T.: 2016, Workshop: Mitaka
Software - from Your Classroom to the Universe, Global Hands-On
Universe (GHOU) Conference 2016 with Galileo Teacher Training
Program (GTTP) International Workshop 2016, (Stord, Norway, Aug.
22–28, 2016).
Agata, H.: 2016, Astronomy Education in Mongolia, International
Educational Workshop on Space Science in Mongolia 2016, (Selenge,
Mongolia, Sep. 8, 2016).
Agata, H.: 2016, Activity of IAU Outreach (OAO) and NAOJ - Astronomy
for Everyone!, International Educational Workshop on Space Sciencein Mongolia 2016, (Ulaanbaatar, Mongolia, Sep. 6, 2016).
Agata, H.: 2016, Exploring the Universe with Mitaka software &Outreach strategy NAOJ, Global Hands-On Universe (GHOU)
Conference 2016 with Galileo Teacher Training Program (GTTP)
International Workshop 2016, (Stord, Norway, Aug. 22–28, 2016).
Akiyama, E., Hashimoto, J., Liu, H. B., Li, I. J., Motohide, T.: 2016,
Differential Grain Growth in the Spiral Structure of the LkHα 330
Disc, Star Formation 2016, (Exeter, UK, Aug. 21–26, 2016).
Akiyama, E., Sitko, M., Liu, H. B., Grady, C., Hashimoto, J., Muto,
T.: 2017, Disk Structure in a Large Hole of a Pre-transitional Disk
around Sun-like PDS 70 Young Star, East-Asian ALMA Science
Workshop 2016, (Hsinchu, Taiwan, Mar. 10–12, 2017).
Antolin, P., Okamoto, J., De Pontieu, B., Van Doorsselaere, T.,
Yokoyama, T., De Moortel, I.: 2016, Alfvénic Waves in Prominences
and Associated Instabilities and Heating, AOGS 2016, (Beijing,
China, Jul. 31–Aug. 5, 2016).
Antolin, P., Okamoto, J., De Pontieu, B., Van Doorsselaere, T.,
Yokoyama, T., De Moortel, I.: 2016, Resonant Absorption as Feeding
Mechanism for Alfvenic Turbulence - Observable Signatures in a
Solar Prominence, IRIS-6: The Chromosphere, (Stockholm, Sweden,
Jun. 20–23, 2016).
Aoki, W.: 2016, Spectroscopic approach to Galactic Archaeology with
Subaru, Panoramas of the Evolving Cosmos, The 6th Subaru Int.
Conf., (Hiroshima, Japan, Nov. 28–Dec. 2, 2016).
Aoki, W.: 2016, Observational Constraints on the Astrophysical Site of
the r-Process, 14th Int. Symp. on Nuclei in the Cosmos (NIC2016),(Niigata, Japan, Jun. 19-24, 2016).
Aso, Y., KAGRA collaboration: 2016, R&D for the gravitational
wave detector KAGRA, 21st Int. Conf. on General Relativity andGravitation (GR21), (New York, USA, Jul. 10–25, 2016).
Aso, Y., KAGRA collaboration: 2017, Status of the KAGRA project,
LVC Meeting in Pasadena, (Pasadena, CA, USA, Mar. 13–16, 2017).
Aso, Y.: 2017, Room Temperature Vibration Isolation Systems of
KAGRA, 5th ELiTES Meeting, (Toyama, Japan, Feb. 8–10, 2017).
Bento, J., Feger, T., Ireland, M., Rains, A., Jovanovic, N., Coutts, D.,
Schwab, C., Arriola, A., Gross, S.: 2016, Performance and Future
Developments of the RHEA Singlemode Spectrograph, SPIE Groundbased and Airborne Instrumentation for Astronomy VI, (Edinburgh,

194

XIII Publications, Presentations

UK, Jun. 26–30, 2016).
Canas, L., Cheung, S.-l., Shibata, Y.: 2016, National OutreachContacts (NOC): IAU’s Outreach Network Program Case Study,
Communicating Astronomy with the Public 2016, (Medellin,
Colombia, May 16–20, 2016).
Canas, L., Cheung, S.-l., Shibata, Y.: 2016, IAU Outreach (OAO) bringing together formal education and outreach, Global Hands-On
Universe (GHOU) Conference 2016 with Galileo Teacher Training
Program (GTTP) International Workshop 2016, (Stord, Norway, Aug.
22–28, 2016).
Canas, L., Perez, A., Gil, A., Carcia, B., Merced, W., Usuda-Sato, K.:
2016, Astronomy for Inclusion: Network and Hands-on Workshop,
Communicating Astronomy with the Public 2016, (Medellin,
Colombia, May 16–20, 2016).
Canas, L., Shibata, Y.: 2016, Making tactile planetarium from lowsost materials, 3rd Symposium on Universal Design for Astronomy
Education, (Tokyo, Japan, Sep. 24–26, 2016).
Canas, L., Simmons, M., McMonigal, C., Doran, R.: 2016, Big &Global4Local: Micro-Crowdfunding Local Astronomy Outreach and
Education Projects, Communicating Astronomy with the Public 2016,(Medellin, Colombia, May 16–20, 2016).
Canas, L., Usuda-Sato, K., Perez, A., Gil, A., Garcia, B., Merced, W.:
2016, Workshop: Accessible Astronomy - Take an Inclusion Program
to Your Country, Global Hands-On Universe (GHOU) Conference
2016 with Galileo Teacher Training Program (GTTP) International
Workshop 2016, (Stord, Norway, Aug. 22–28, 2016).
Canas, L.: 2016, IAU Office for Astronomy Outreach: Astronomy for
Everyone, Southeast Asia Astronomical Network (SEAAN) 2016,(Hanoi, Viet Nam, Dec. 12–13, 2016).
Cheung, S.-l.: 2016, The IAU Office for Astronomy Outreach —its mission and the beyond NameExoWorlds and Cosmic Light,
Communicating Astronomy with the Public 2016, (Medellin,
Colombia, May 16–20, 2016).
Cheung, S.-l.: 2016, IAU Office for Astronomy Outreach, Latin America
IAU Regional Meeting 2016, (Cartagena de Indias, Colombia, Oct.
2–7, 2016).
Currie, T. M., Guyon, O., Jovanovic, N., Lozi, J., Tamura, M., Kudo, T.,
Uyama, T., Garcia, E.: 2017, SEEDS: Direct Imaging of Exoplanets
and Their Forming Disks with the Subaru Telescope, AAS Meeting#229, (Grapevine, TX, USA, Jan. 3–7, 2017).
Ebizuka, N., Okamoto, T., Hosobata, T., Yamagata, Y., Sasaki, M.,
Uomoto, M., Shimatsu, T., Sato, S., Hashimoto, Kirino, O., N.,
Tanaka, I., Hattori, T., Ozaki, S., Aoki, W.: 2017, Current Statusof Novel Gratings for Next Generation Astronomical Instruments IV,
Subaru Users’ Meeting FY2016, (Tokyo, Japan, Jan. 10–12, 2017).
Ebizuka, N., Okamoto, T., Hosobata, T., Yamagata, Y., Sasaki, M.,
Uomoto, M., Shimatsu, T., Sato, S., Hashimoto, N., Tanaka, I.,
Hattori, T., Ozaki, S., Aoki, W.: 2016, Novel Diffraction Gratings for
Next Generation Spectrographs with High Spectral Dispersion, SPIE
Advances in Optical and Mechanical Technologies for Telescopes
and Instrumentation II, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Egusa, F., Mentuch Cooper, E., Koda, J., Baba, J.: 2016, Offsets between
Gas and Stellar Spiral Arms in M51, Discs in Galaxies, (Garching,
Germany, Jul. 11–15, 2016).
Egusa, F.: 2016, Gas Disk Dynamics, Extensitve CO Survey of Nearby
Galaxies, (Mitaka, Japan, Dec. 7–9, 2016).

Egusa, F.: 2016, Extensive CO Survey of Nearby Galaxies with ACA,
ALMA/45m/ASTE Users Meeting 2016, (Mitaka, Japan, Dec. 19–20,
2016).
Ezawa, H., Matsuo, H., Ukibe, M., Fujii, G., Shiki, S.: 2016, Developments
towards the terahertz intensity interferometry, SPIE Astronomical
Telescopes + Instrumentatio, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Flaminio, R.: 2016, Observation of Gravitational Waves from a Binary
Black Hole Merger: results and perspectives, 4th DTA Symp.,(Mitaka, Japan, May 13–14, 2016).
Flaminio, R.: 2016, Observation of Gravitational Waves: Latest Results
and Perspectives, Ultimate Subaru Science Workshop 2016, (Tokyo,
Japan, Jun. 16–17, 2016).
Flaminio, R.: 2016, Gravitational Wave Astronomy: Status andPerspectives, 2nd NAOJ-ECT Workshop on Many Riddles About
Core-Collapse Supernovae: Bethe and Beyond, (Mitaka, Japan, Jun.
27–Jul. 1, 2016).
Flaminio, R.: 2016, Gravitational Wave Detectors: Status of the Art andPerspectives, Irago Conferecne 2016, (Tokyo, Japan, Nov. 1–2, 2016).
Flaminio, R.: 2016, Status of KAGRA, The 2nd International Meetingon KAGRA, (Beijing, China, Nov. 10–12, 2016).
Fujii, Y., Adams, T., Marion, F., Flaminio, R.: 2016, Localization of
Coalescing Binaries with a Hierarchical Network of Gravitational
Wave Detectors, Gravitational-Wave Astrophysics in the High Event
Rate Regime, (Tokyo, Japan, Dec. 5–6, 2016).
Fujita, C., Ozeki, H., Kobayashi, K.: 2016, The Microwave Spectroscopyof Aminoacetonitrile in the Vibrational Excited States 2, 71st
International Symposium on Molecular Spectroscopy, (UrbanaChampagne, IL, USA, Jun. 20–24, 2016).
Fujiwara, H., Morishima, R., Fujiyoshi, T., Yamashita, T.: 2017,
Seasonal Variation of the Radial Brightness Contrast of Saturn’sRings Viewed in Mid-infrared by Subaru/COMICS, Ice in the Solar
System, (Madrid, Spain, Jan. 23–26, 2017).
Fujiwara, H.: 2016, Dust in Warm Debris Disks, Seach for Life: From
Early Earth to Exoplanets, (Quy Nhon, Vietnam, Dec. 11–16, 2016).
Fujiwara, H.: 2016, Introduction to Research with Subaru Telescope,
Tropical School in Undergraduate Astronomy: Astronomical
Observations, (Quy Nhon, Vietnam, Dec. 11, 2016).
Fujiwara, H.: 2017, Dust in Warm Debris Disks, NARIT Friday
Seminar, (Chiang Mai, Thailand, Feb. 17, 2017).
Fukui, A.: 2016, Characterizations of Transiting Exoplanets with Multiband Camera MuSCAT, Japan-Germany Planet and Disk Workshop,(Ishigaki, Japan, Sep. 25–30, 2016).
Fukui, A.: 2016, MuSCAT & MuSCAT2: New Multiband Imagers for
Precise Photometry, 21st Int. Microlensing Conf. Ushering in the
New Age of Microlensing from Space, (Pasadena, CA, USA, Feb.
1–3, 2017).
Fukushima, K., Kobayashi, K., Hirota, T.: 2016, Methanol Maser
Survey Observation with the Nobeyama 45 m Telescope, Workshop
for Interstellar Matter 2016, (Sapporo, Japan Oct. 19–21, 2016).
Gee, W. T., Guyon, O., Walawender, J., Jovanovic, N., Boucher, L.:
2016, Project PANOPTES: a Citizen-scientist Exoplanet Transit
Survey Using Commercial Digital Cameras, SPIE Ground-based andAirborne Instrumentation for Astronomy VI, (Edinburgh, UK, Jun.
26–30, 2016).
Giono, G., Katsukawa, Y., Ishikawa, R., Narukage, N., Kano, R., Kubo,
M., Ishikawa, S., Bando, T., Hara, H., Suematsu, Y., Winebarger,

A., Kobayashi, K., Auchere, F., Trujillo Bueno, J.: 2016, Optical
Alignment of the Chromospheric Lyman-Alpha SpectroPolarimeter
Using Sophisticated Methods to Minimize Activities Under Vacuum,
SPIE Astronomical Telescopes + Instrumentatio, (Edinburgh, UK, Jun.
26–Jul. 1, 2016).
Goebel, S. B., Guyon, O., Hall, D. N. B., Jovanovic, N., Atkinson, D.
E.: 2016, Evolutionary Timescales of AO-produced Speckles at NIR
Wavelengths, SPIE Adaptive Optics Systems V, (Edinburgh, UK, Jun.
26, 2016).
Gonzalez, A., Asayama, S., Tapia, V., Finger, R., Monasterio, D., Reyes,
N.: 2016, Effects of Cryostat Infrared Filters on the Performance of
ALMA band 1 (35–52 GHz) Receiver Optics, IEEE Antenna andPropagation Symposium/ USNC URSI 2016, (Fajardo, Puerto Rico,Jun. 26–Jul. 1, 2016).
Gonzalez, A., Kaneko, K., Asayama, S.: 2017, Recent Work on (sub-)mm-wave Ultra WideBand Corrugated Horns for Radio Astronomy,
11th European Conf. on Antennas and Propagation (EuCAP 2017),(Paris, France, Mar. 19–24, 2017).
Gonzalez, A., Kaneko, K., Kojima, T., Asayama, S., Uzawa, Y.: 2016,
Corrugated Horns for ALMA band 11 (1.25–1.57 THz), 27th Int. Symp.
on Space Terahertz Technology, (Nanjing, China, Apr. 12–15, 2016).
Gonzalez, A., Kojima, T., Fujii, Y., Asayama, S.: 2016, Reconfigurable
Beam Measurement System and Use for ALMA band 11 (1.25–1.57
THz), 27th Int. Symp. on Space Terahertz Technology, (Nanjing,
China, Apr. 12–15, 2016).
Gonzalez, A., Kojima, T., Kaneko, K., Asayama, S.: 2017, Developmentof a wideband waveguide diplexer to provide LO power in the
275–500 GHz band, 28th Int. Symp. on Space Terahertz Technology,(Cologne, Germany, Mar. 13–15, 2017)
Gonzalez, A., Tapia, V., Reyes, N., Mena, F. P., Nesti, R., Villa, F.,
Cuttaia, F., de Rosa, A., di Giorgio, A. M., Morbidini, A., Yagoubov,
P.: 2016, ALMA Band 2+3 (67–116 GHz) optics design and firstmeasurements, IEEE Antenna and Propagation Symposium/ USNCURSI 2016, (Fajardo, Puerto Rico, Jun. 26–Jul. 1, 2016).
Gonzalez, A.: 2016, Optics work for the band 2 and 2+3 receivers at
NAOJ, ALMA bands 2/2+3 Workshop, (Gothenburg, Sweden, May
23–24, 2016).
Gonzalez, A.: 2016, Optics Research for Future Receivers at NAOJ, ALMA
Developer’s workshop, (Gothenburg, Sweden, May 25–27, 2016).
Gouda, N.: 2016, Small-JASMINE, Gaia-JASMINE joint meeting,(Mitaka, Japan, Dec. 6–9, 2016).
Groff, T., Chilcote, J., Kasdin, J., Brandt, T., Galvin, M., Loomis, C.,
Carr, M., Knapp, G., Guyon, O., Jovanovic, N., Lozi, J., Takato, N.,
Hayashi, M.: 2017, On-Sky Performance Verification of the CHARISIFS, AAS Meeting #229, (Grapevine, TX, USA, Jan. 3–7, 2017).
Groff, T., Chilcote, J., Kasdin, J., Galvin, M., Loomis, C., Carr, M.,
Brandt, T., Knapp, G., Limbach, M., Guyon, O., Jovanovic,
N., McElwain, M., Takato, N., Hayashi, M.: 2016, Laboratory
Testing and Performance Verification of the CHARIS Integral Field
Spectrograph, SPIE Ground-based and Airborne Instrumentation for
Astronomy VI, (Edinburgh, UK, Jun. 26–30, 2016).
Gusev, A., Hanada, H., Kosov, A., Meng, Z., Ping, J.: 2016, Dynamics
and Interior of the Inner Solid and Outer Liquid Cores of the Moon
for ChangE-4/5/6, Luna-25/26/27, ILOM Projects, AOGS 2016,(Beijing, China, Jul. 31–Aug. 5, 2016).
Gusev, A., Hanada, H., Meng, Zh., Ping, J.: 2016, Tidal-librational

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Dissipative Dynamics of the Multi-layers Moon, AstroKazan 2016,(Kazan, Russia, Aug. 25–29, 2016).
Guyon, O.: 2016, Where are our Closest Neighbours? Looking for Lifeon Nearby Exoplanets, Conf. on Lasers and Electro-Optics 2016, (SanJose, USA, Jun. 5–10, 2016).
Guyon, O.: 2016, Imaging and Characterization of Rocky Planets in the
Habitable Zones of Nearby Stars with ELTs, Fourth Annual GMT
Community Science Meeting, (Asilomar, CA, USA, Sept. 26–28,
2016).
Hada, K.: 2016, Report on EAVN Imaging Test Observations and Future
Prospects, East Asia VLBI Workshop 2016, (Guiyang, Guizhou,
China, Nov. 7–11, 2016).
Hada, K.: 2016, Millimeter VLBI with ALMA and Its User Support,
ALMA/45m/ASTE/Mopra Users Meeting 2016, (Mitaka, Japan, Dec.
19–20, 2016).
Hada, K.: 2016, M87 Jet Imaged at Highest Sensitivity: An Improved
View of the Transverse Structure, M87 Workshop, (Taipei, Taiwan,
May 23–27, 2016).
Hada, K.: 2016, The Structure and Propagation of the Misaligned Jet
M87, Blazars Through Sharp Multi-wavelength eyes, (Malaga, Spain,
May 30–Jun. 3, 2016).
Hada, K.: 2016, Radio Imaging of M87 at Low Frequencies, EHT
Collaboration Meeting 2016, (Boston, MA, USA, Nov. 29–Dec. 3,2016).
Hada, K.: 2017, The East Asian VLBI Network, Black Hole Astrophysics
with VLBI - Past, Present and Future, (Mitaka, Japan, Mar. 27–29,
2017).
Hada, K.: 2017, An Improved View of the M87 Jet: Radio Imaging of
the Spine-sheath Structure, Challenges of AGN Jets, (Mitaka, Japan,
Jan. 17–20, 2017).
Hanada, H., Araki H., Tsuruta, S., Asari, K., Noda, H., Kashima, S.,
Funazaki, K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Sasaki,
H., Hasegawa, T., Gusev, A.: 2016, Results of Ground Experiments
Using a Small Telescope Like PZT for Observation of Lunar Rotation
and a New Proposal for Miniaturization, AOGS 2016, (Beijing,
China, Jul. 31–Aug. 5, 2016).
Hanada, H., Araki H., Tsuruta, S., Asari, K., Noda, H., Kashima, S.,
Funazaki, K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M., Sasaki,
H., Hasegawa, T., Gusev, A.: 2016, Expected Accuracy of a Small
Telescope Like PZT for Observations of Vertical Gravity Gradientand Lunar Rotation, 4th IAG Symposium on Terrestrial Gravimetry:
Static And Mobile Measurements, (Saint Petersburg, Russia, Apr.
12–15, 2016).
Hanada, H., Tsuruta, S., Asari, K., Araki, H., Noda, H., Kashima,S., Funazaki, K., Satoh, A., Taniguchi, H., Kato, H., Kikuchi, M.,
Sasaki, H., Hasegawa, T., Gusev, A.: 2016, Evaluation of Accuracy ofa Small Telescope Like PZT for Observation of Lunar Rotation and a
New Proposal for Future Missions, AstroKazan 2016, (Kazan, Russia,
Aug. 25–29, 2016).
Hanaoka, Y., Sakurai, T., IRMag Group: 2016, Statistical Study of theMagnetic Field in Solar Filaments, 8th Solar Polarization Workshop,(Firenze, Italy, Sep. 12–16, 2016).
Hanaoka, Y.: 2016, NAOJ’s Synoptic Solar Observations, Theoreticaland Observational Approaches to the Solar Magnetic Field, (Tokyo,
Japan, May 27, 2016).
Hanaoka, Y.: 2017, Direct Observations of the Magnetic Field in Solar

196

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Filaments, 2nd PSTEP International Symposium, (Kyoto, Japan, Mar.
23–24, 2017).
Hanayama, H.: 2016, Ishigaki Observatory ~Ishigakijima Astronomical
Observatory and Murikabushi 105 cm Telescope~, JOVIAL Kick-off
Meeting, (Nice, France, Apr. 18–20, 2016).
Hara, H.: 2016, Hinode EUV Imaging Spectroscopy at the Site ofMagnetic Reconnection in Solar Flares, 10th Hinode Science
Meeting, (Nagoya, Japan, Sep. 5–8, 2016).
Hara, H.: 2016, Solar Corona: Recent Progress from Space Observations,International Congress on Plasma Physics (ICPP)-2016, (Kaohsiung,Taiwan, Jun. 27–Jul. 1, 2016).
Hara, H.: 2017, Hinode EUV Imaging Spectroscopy at the Site ofMagnetic Reconnection in Solar Flares, Magnetic Reconenction
2017, (Matsuyama, Japan, Mar. 19–22, 2017).
Harada, Y., Goossens, S., Matsumoto, K., Yan, J., Ping, J., Noda, H.,
Haruyama, J.: 2016, The Deep Lunar Interior with a Low-Viscosity
Zone: Revised Constraints from Recent Geodetic Parameters on the
Tidal Response of the Moon, AOGS 2016, (Beijing, China, Jul. 31–
Aug. 5, 2016).
Harada, Y., Goossens, S., Matsumoto, K., Yan, J., Ping, J., Noda, H.,
Haruyama, J.: 2016, The Deep Lunar Interior with a Low-viscosity
Zone: Revised constraints from Recent Geodetic Parameters on the
Tidal Response of the Moon, Japan Geoscience Union Meeting 2016,(Chiba, Japan, May 22–26, 2016).
Harada, Y., Goossens, S., Matsumoto, K., Yan, J., Ping, J., Noda, H.,
Haruyama, J.: 2016, The Deep Lunar Interior with a Low-Viscosity
Zone: Revised Constraints from Recent Geodetic Parameters on the
Tidal Response of the Moon, ISLPS2016, (Wuhan, China, Jun. 9–10,
2016).
Hayakawa, T., Toh, Y., Shizuma, T., Kimura, A., Nakamura, S., Harada,
H., Iwamoto, N., Kajino, T., Chiba, S.: 2016, Neutron Capture
Reaction on 112Cd to Study of the s-process Origin of 115Sn, 14th Int.
Symp. on Nuclei in the Cosmos (NIC2016), (Niigata, Japan, Jun.
19–24, 2016).
Hayashi, M.: 2016, Physical Conditions of the Interstellar Medium inStar-forming Galaxies at z~1.5, The Changing Face of Galaxies:
uncovering transformational physics, (Hobart, Tasmania, Australia,
Sep. 19–23, 2016).
Hayashi, M.: 2016, Probing Star Forming Galaxies at z<1.5 with Widefield HSC-SSP Narrowband Data, Panoramas of the Evolving Cosmos,
The 6th Subaru Int. Conf., (Hiroshima, Japan, Nov. 28–Dec. 2, 2016).
Hidaka, J., Kajino, T., Mathews, G. J.: 2016, Study of Red Supergiant
and Supernova Rate Problems via Relic Supernova Neutrino
Spectrum, 14th Int. Symp. on Nuclei in the Cosmos (NIC2016),(Niigata, Japan, Jun. 19–24, 2016).
Hirai, Y., Ishimaru, Y., Saitoh, T. R., Fujii, M. S., Hidaka, J., Kajino, T.:
2016, Chemo-dynamical Evolution of r-process Elements in the Local
Group Galaxies, 14th Int. Symp. on Nuclei in the Cosmos (NIC2016),(Niigata, Japan, Jun. 19–24, 2016).
Hiramatsu, M., Shirasaki, Y.: 2017, Japanese Virtual Observatory’s
ALMA FITS Data Archive, Data to Dome Workshop, (Tokyo, Japan,
Mar. 2–3, 2017).
Hirota, T., Motogi, K., Honma, M., Machida, M. N., Matsushita, Y.:
2016, High Resolution Imaging of disk/outflow System in Orion
Source I, Half a Decade of ALMA: Cosmic Dawns Transformed,(Indian Wells, CA, USA, Sep. 20–23, 2016).

Hirota, T.: 2016, Interstellar and Circumstellar Maser Observations with
KaVA, TVN, and beyond, TVN2016: Thai VLBI Network (TVN)
Collaborative Workshop, (Krabi, Thailand, Sep. 5-9, 2016).
Hirota, T.: 2016, Hot Water Disk around Orion Source I, Water in the
Universe: From Clouds to Oceans, (Noordwijk, Netherland, Apr.
12–15, 2016).
Hirota, T.: 2016, A Survey of the Vibrationally Excited H2O lines in
Nearby Massive YSOs, JCMT Users Meeting, (Mitaka, Tokyo, Japan,
Apr. 17–19, 2016).
Hirota, T.: 2016, KaVA Large Program for Star-Formation, East Asia
VLBI Workshop 2016, (Guiyang, Guizhou, China, Nov. 7–11, 2016).
Hirota, T.: 2016, CASA Users Committee Report, ALMA/45m/ASTE/
Mopra Users Meeting 2016, (Mitaka, Japan, Dec. 19–20, 2016).
Hirota, T.: 2016, Hot water molecule around Orion source I, Workshop
for Interstellar Matter 2016, (Sapporo, Japan Oct. 19–21, 2016).
Hirota, T.: 2017, Maser Sciences with ALMA Band 1, ALMA Band 1
Science Workshop, (Taipei, Taiwan, Jan. 16–20, 2017).
Hirota, T.: 2017, High Resolution Observational Studies of Starformation, NARIT-CMU Mini-Colloquia on Masers & Starformation, (Chiang Mai, Thailand, Feb. 15, 2017).
Hirota, T.: 2017, VERA and ALMA Observations of Orion KL, NARIT
Friday Seminar, (Chiang Mai, Thailand, Feb. 17, 2017).
Honma, M.: 2016, Astrometry with VERA and Future of EAVN,
TVN2016: Thai VLBI Network (TVN) Collaborative Workshop,(Krabi, Thailand, Sep. 5–9, 2016).
Honma, M.: 2016, Discussion: Future Possible Collaboration of KaVA
and EAVN Science Working Group in East-Asian Region, East Asia
VLBI Workshop 2016, (Guiyang, Guizhou, China, Nov. 7–11, 2016).
Honma, M.: 2016, Status Report from Mizusawa VLBI, East Asia VLBI
Workshop 2016, (Guiyang, Guizhou, China, Nov. 7–11, 2016).
Honma, M.: 2016, Imaging the Event-horizon-scale Structure of Sgr A*
with Sparse Modeling, M87 Workshop, (Taipei, Taiwan, May 23–27,
2016).
Honma, M.: 2017, Imaging Black Hole Shadow with Sparse Modeling,
Black Hole Astrophysics with VLBI - Past, Present and Future,(Mitaka, Japan, Mar. 27–29, 2017).
Hori, Y., Iwasawa, M., Oshino, S., Fujii, M. S.: 2016, Towards Highresoultion N-body Simulations for Planet Formation, Japan-Germany
Planet and Disk Workshop, (Ishigaki, Japan, Sep. 25–30, 2016).
Hori, Y., Liu, S.-F., Lin, D. N. C.: 2016, Impact of Giant Impacts on
Planetary Interiors, New Directions in Planet Formation, (Leiden,
The Netherlands, Jul. 11–15, 2016).
Hori, Y.: 2017, The Primordoal Atmosphere on a Terrestrial Planet
in a Habitable Zone, Astrobiology Center Internatioal Workshop,(Hiroshima, Japan, Mar. 22–24, 2017).
Huang, Y.-D., et al. including Iguchi, S., Asayama, S., Iono, D.,
Gonzalez, A.: 2016, The Atacama Large Millimeter/sub-millimeter
Array (ALMA) band-1 receiver, SPIE conference on Astronomical
Telescopes + Instrumentation 2016, (Edinburgh, UK, Jun. 10–15,
2016).
Hwang, Y.-J., et al. including Gonzalez, A.: 2016, Band 1 Receiver
Front-end Cartridges for Atacama Large Millimeter/submillimeter
Array (ALMA): Design and Development toward Production, SPIE
conference on Astronomical Telescopes + Instrumentation 2016,(Edinburgh, UK, Jun. 10–15, 2016).
Ichikawa, K.: 2016, Discovery of a Dead AGN in Arp 187, East Asia

AGN workshop 2016, (Seoul, Korea, Sep. 22, 2016).
Ichikawa, K.: 2016, 3–500 μm Infrared Properties of 70-month Swift/BAT
AGN Catalog, Hidden Monsters: Obscured AGN and Connections toGalaxy Evolution, (Hanover, NH, USA, Aug. 8–12 2016).
Ichikawa, K.: 2016, Science Case of MICHI from AGN/BH Physics
Group, TMT/MICHI science workshop, (Kyoto, Jpaan, May 23,2016).
Ichikawa, K.: 2016, Key AGN Science Cases with MICHI, TMT Science
Forum 2016, (Kyoto, Japan, May 24–26, 2016).
Imanishi, M.: 2016, ALMA Molecular Gas Observations of Luminous
Infrared Galaxies as a Tool to Scrutinize Elusive Deeply-Buried
AGNs, Molecular Gas in Galactic Environments, (Charlottesville,
USA, Apr. 4–7, 2016).
Imanishi, M.: 2016, ALMA Molecular Gas Observations of Luminous
Infrared Galaxies as a Tool to Scrutinize Elusive Deeply Buried
AGNs, Hidden Monsters: Obscured AGN and Connections to Galaxy
Evolution, (Hanover, NH, USA, Aug. 8–12 2016).
Imanishi, M.: 2016, ALMA Molecular Line Observations of the
Ultraluminous Infrared Galaxies and Optical Seyfert Galaxies, Half a
Decade of ALMA: Cosmic Dawns Transformed, (Indian Wells, CA,
USA, Sep. 20–23, 2016).
Ishihara, Y., Hareyama, M., Honda, C., Hirata, N., Morota, T., Ohtake,M.: 2017, Highland Crust of the Orientale Basin Region Based on
Unsupervised Classification of Absroption Specrtra of the Moon, 48th
Lunar and Planetary Science Conference, (the Woodlands TX, USA,
Mar. 20–24, 2017).
Ishihara, Y., Kawamura T., Yamada, R., Ogawa, K., Takeuchi, N., Araya,
A,. Lognonné, P., Shirai, K., Tsuji, T.,Kobayashi, T., Nishikawa,Y., Drilleau, M., Tanaka, S.: 2016, Investigation and Developmentof Seismic Observation Package for Asteroid and Small Body
Explorations, Japan Geoscience Union Meeting 2016, (Chiba, Japan,
May 22–26, 2016).
Ishikawa, R., Kano, R., Kubo, M., Narukage, N., Katsukawa, Y.,
Giono, G., Bando, T., Hara, H., Suematsu, Y., Ishikawa, S., Tsuneta,
S., Trujillo Bueno, J., Stepan, J., Uitenbroek, H., Winebarger, A.,
Kobayashi, K., Auchere, F.: 2016, Comparison of the scatteringpolarization observed by CLASP; Possible indication of the Hanle
effect, 8th Solar Polarization Workshop, (Firenze, Italy, Sep. 12–16,
2016).
Ishikawa, R., Kano, R., Winebarger, A., Auchere, F., Trujillo Bueno,J., Narukage, N., Kobayashi, K., Bando, T., Katsukawa, Y., Kubo,
M., Ishikawa, S., Giono, G., Hara, H., Suematsu, Y., Shimizu, T.,
Sakao, T., Tsuneta, S., Ichimoto, K., Goto, M., Cirtain, J., De Pontieu,
B., Casini, R., Manso Sainz, R., Asensio Ramos, A., Stepan, J.,
Belluzzi, L., Carlsson, M.: 2016, The Chromosphere and Transition
Region as Seen with CLASP, IRIS-6: The Chromosphere, (Stockholm,
Sweden, Jun. 20–23, 2016).
Ishikawa, S., Kajino, T., Shibagaki, S., Balantekin, B. A., Famiano, M.
A.: 2016, Three-Body Model Calculation of 9Be Formation Rate andApplication to Supernova Nucleosynthesis, 14th Int. Symp. on Nuclei
in the Cosmos (NIC2016), (Niigata, Japan, Jun. 19–24, 2016).
Ishikawa, S., Kubo, M., Katsukawa, Y., Kano, R., Narukage, N.,
Ishikawa, R., Winebarger, A., Kobayashi, K., Trujillo Bueno, J., Bando,T., Auchere, F.: 2016, CLASP/SJ Observation of Time Variations of
Lyman-alpha Emissions in a Solar Active Region (poster), 10th Hinode
Science Meeting, (Nagoya, Japan, Sep. 5–8, 2016).

XIII Publications, Presentations

197

Ishikawa, S., Shimizu, T., Kano, R., Bando, T., Ishikawa, R., Giono,G., Beabout, D. L., Beabout, B. L., Nakayama, S., Tajima, T.: 2016,
In-flight Performance of the Polarization Modulator in the CLASP
Rocket Experiment, SPIE Astronomical Telescopes + Instrumentatio,(Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Izumiura, H.: 2016, The Situation That the Observatories and Telescopes
at Okayama are Placed in, Software and Observational Strategy
for Precise Radial Velocity Work with Medium Size Telescopes,(Munchen, Germany, Dec. 1–3, 2016).
Izumiura, H.: 2016, Robotic RV Explorer and Possible Collaborations,
Software and Observational Strategy for Precise Radial Velocity
Work with Medium Size Telescopes, (Munchen, Germany, Dec. 1–3,
2016).
Izumiura, H.: 2017, A Census of Mass-losing Long Period Variables
Showing SiO Masers in the Direction of the Galactic Nuclear Star
Cluster with ALMA Band 1, ALMA Band 1 Science Workshop,(Taipei, Taiwan, Jan. 16–20, 2017).
Joshi, A. D., Forbes, T. G., Park S.-H., Cho, K.-S.: 2016, Poster - A
Trio of Confined Flares in AR 11087, 10th Hinode Science Meeting,(Nagoya, Japan, Sep. 5–8, 2016).
Jovanovic, N., Cvetojevic, N., Schwab, C., Norris, B., Lozi, J., Gross,S., Betters, C., Singh, G., Guyon, O., Martinache, F., Doughty, D.,
Tuthill, P.: 2016, Efficiently feeding single-mode Fiber Photonic
Spectrographs with an Extreme Adaptive Optics System: On-sky
Characterization and Preliminary Spectroscopy, SPIE Astronomical
Telescopes + Instrumentatio, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Jovanovic, N., et al. including Guyon, O., Lozi, J., Currie, T., Pathak, P.,
Doughty, D., Goebel, S., Kudo, T., Kotani, T., Minowa, Y., Takato,N., Tamura, M., Takami, H., Hayashi, M.: 2016, The SCExAO HighContrast Imager: Transitioning from Commissioning to Science, SPIE
Adaptive Optics Systems V, (Edinburgh, UK, Jun. 26, 2016).
Jovanovic, N., Guyon, O., Kawahara, H., Kotani, T.: 2017, Application ofMulticore Optical Fibers in Astronomy, Optical Fiber Communications
conference 2017, (Los Angeles, USA, Mar. 19–23, 2017).
Kambe, E.: 2016, High Resolution Spectrographs for Okayama
Telescopes, I2 and Astro-Comb, and HIDES FITS Header, Softwareand Observational Strategy for Precise Radial Velocity Work with
Medium Size Telescopes, (Munchen, Germany, Dec. 1–3, 2016).
Kameya, O.: 2016, Twenty Five Years of the Mizusawa 10m Radio
Telescope, East Asia VLBI Workshop 2016, (Guiyang, Guizhou,
China, Nov. 7–11, 2016).
Kano, R., et al. including Ishikawa, R., Narukage, N., Bando, T.,
Katsukawa, Y., Kubo, M., Giono, G., Hara, H., Suematsu, Y.:
2016, Spectro-polarimetric Observations in UV with CLASP to Probe
the Transition Region, 47th Solar Physics Division meeting, (Boulder,
USA, May 31–Jun. 3, 2016).
Kano, R., et al. including Ishikawa, R., Narukage, N., Bando, T.,
Katsukawa, Y., Kubo, M., Giono, G., Hara, H., Suematsu, Y.:
2016, Initial Results of Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP), Theoretical and observational approaches tothe solar magnetic field, (Tokyo, Japan, May 27, 2016).
Kano, R., Trujillo Bueno, J., Winebarger, A., Auchere, F., Ishikawa,
R., Kobayashi, K., CLASP team: 2016, Lyman-alpha Scattering
Polarization Observed with the Chromospheric Lyman-Alpha
Spectro-Polarimeter, 8th Solar Polarization Workshop, (Firenze, Italy,
Sep. 12–16, 2016).

198

XIII Publications, Presentations

Karino, S., Agata, H., Canas, L.: 2016, An Analysis of the Syllabi of
Astronomy in Japanese Universities, 10th East-Asia Meeting on
Astronomy (EAMA), (Seoul, Korea, Sep. 26–30, 2016).
Kashikawa, N.: 2017, Wide Survey for Early Universe by Subaru/HSC,
Dawn of Galaxies 2017, (Obergurgl, Austria, Jan. 14–18, 2017).
Katsukawa, Y., Kamata, Y., Anan, T., Hara, H., Suematsu, Y., Bando,
T., Ichimoto, K., Shimizu, T.: 2016, Development of a Nearinfrared Detector and a Ber-optic Integral Field Unit for a Space
Solar Observatory SOLAR-C, SPIE Astronomical Telescopes +Instrumentatio, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Katsukawa, Y., Kimura, Y., Okamoto, T. J.: 2016, Penumbral Microjets: Rapid Heating Driven by Magnetic Reonnection in The
Chromosphere, AOGS 2016, (Beijing, China, Jul. 31–Aug. 5, 2016).
Katsukawa, Y.: 2016, High-Precision Spectro-Polarimetry in the Visible
and Infrared on the SUNRISE Balloon-Borne Solar Observatory, 10th
Hinode Science Meeting, (Nagoya, Japan, Sep. 5–8, 2016).
Kawaguchi, T., et al. including Ozaki, S.: 2017, Current Status of Our
AO-Assisted Optical IFU Study on Galaxy-BH Coevolution, Subaru
Users’ Meeting FY2016, (Tokyo, Japan, Jan. 10–12, 2017).
Kawaguchi, T., Ozaki, S., Sugai, H., Matsubayashi, K., Hattori, T.,
Shimono, A., Minowa, Y., Hayano, Y., Aoki, K., Mitsuda, K.,
Hashiba, Y.: 2016, An AO-Assisted Optical IFU Study on GalaxyBH Coevolution, Australia-Japan workshop on collaborative science,(North Ryde, Australia, Dec. 15, 2016).
Kawakita, H., Shinnaka, H.: 2016, Survey for Ortho-to-Para AbunanceRatios (OPRS) of NH2 in Comets: Revisit to the Meaning of OPRs of
Cometary Volatiles, DPS48/EPSC11 meeting, (Pasadena, CA, USA,
Oct. 16–21, 2016).
Kawamura, T., Ishihara, Y., Ogawa, K., Tsuji, T., Kobayashi, T.,
Yamada, R., Araya, A., Tanaka, S., Takeuchi, N.: 2017, Conceptual
Study of Small Active Seismic Exploration Package on Moons andSmall Bodies, 48th Lunar and Planetary Science Conference , (theWoodlands TX, USA, Mar. 20–24, 2017).
Kawamura, T., Yamada, R., Tanaka, S., Ishihara, Y., Murakami, H.,
Shiraishi, H., Shirai, K., Hayakawa, M., Goto, K.: 2016, Scientificsignificance of internal structure of the Moon and objectives of
APPROACH, Joint ISAS_LPL Workshop on Planetary Sceince Enabled
by Epsilon Class Missions, (Tucson, AZ, USA, Nov. 15, 2016).
Kawamura, T.: 2016, Dynamics of Deep/Shallow Moonquakes andImpacts, ISSI-BJ Forum on Lunar and Planetary Seismology, (Beijing,
China, Jan. 11, 2017).
Kim, J. S.: 2016, Rapid Change of Outflow Morphology in Massive
Star-Forming Region Cepheus A, East Asia VLBI Workshop 2016,(Guiyang, Guizhou, China, Nov. 7–11, 2016).
Kim, J. S.: 2016, KaVA Observations of Cyg X-3 in 2016, East Asia
VLBI Workshop 2016, (Guiyang, Guizhou, China, Nov. 7–11, 2016).
Kitagawa, Y., Yamagata, Y., Morita, S., Motohara, K., Ozaki, S.,
Takahashi, H., Konishi, M., Kato, N. M., Kobayakawa, Y., Terao, Y.,
Ohashi, H.: 2016, Fabrication of a Wide-field NIR Integral Field Unit
for SWIMS Using Ultra-precision Cutting, SPIE Advances in Opticaland Mechanical Technologies for Telescopes and Instrumentation II,(Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Kiuchi, H., Hills, R., Whyborn, N. D., Asayama, S., Sakamoto, S.,
Iguchi, S., Corder, S. A.: 2016, An Artificial Calibration Source
Based on the Photonic THz Technique for High-frequency Radio
Astronomy, Energy Materials Nanotechnology meeting on Terahertz,

(San Sebastian, Spain, May 14–18, 2016).
Kiuchi, H., Hills, R., Whyborn, N. D., Asayama, S., Sakamoto, S.,
Iguchi, S., Corder, S. A.: 2016, Artificial Calibration Source for
ALMA Radio Interferometer, SPIE Astronomical Telescopes +Instrumentatio, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Kobayashi, H.: 2016, Future of EAVN, East Asia VLBI Workshop 2016,(Guiyang, Guizhou, China, Nov. 7–11, 2016).
Kodama, T.: 2016, The Nature of Star-forming Disc Galaxies in Protoclusters, Discs in Galaxies, (Garching, Germany, Jul. 11–15, 2016).
Kodama, T.: 2016, The Changing Face of Proto-clusters, The Changing
Face of Galaxies: uncovering transformational physics, (Hobart,
Tasmania, Australia, Sep. 19–23, 2016).
Kodama, T.: 2016, ULTIMATE-Subaru and PFS Overview, The galaxy
life cycle, (Venice, Italy, Oct. 24–28, 2016).
Kodama, T.: 2016, Star Formation Histories across the Cosmic Noonand Environments, In Situ View of Galaxy Formation, (Ringberg
Castle, Bavaria, Germany, Oct. 30–Nov. 5, 2016).
Kodama, T.: 2016, Panoramic Mapping of Star Formation Activities
across Environments since z~3, Panoramas of the Evolving Cosmos,
The 6th Subaru Int. Conf., (Hiroshima, Japan, Nov. 28–Dec. 2, 2016).
Kojima, K., Takahashi, H., Kroug, M., Uzawa, Y.: 2017, Performanceand characterization of an SIS-mixer-amplifier module with wideband
IF for submillimeter-wave receivers, 28th Int. Symp. on Space
Terahertz Technology, (Cologne, Germany, Mar. 13-15, 2017)
Kojima, T., Gonzalez, A., Asayama, S., Uzawa, Y.: 2016, Developmentof an RF Waveguide Frequency Multiplexer for a Multiband
Heterodyne System, 27th Int. Symp. on Space Terahertz Technology,(Nanjing, China, Apr. 12–15, 2016).
Kojima, T., Gonzalez, A., Kroug, M., Fujii, Y., Kaneko, K., Shan,
W., Asayama, S., Uzawa, Y., Makise, K., Terai, H., Wang, Z.: 2016,
Superconducting Receivers for ALMA Radio Telescope and Future
Development, 29th Int. Symp. on Superconductivity, (Tokyo, Japan,
Dec. 13–15, 2016).
Kojima, T., Kroug, M., Sato, K., Sakai, T., Uzawa, Y.: 2016, Capacitance
Measurement of High Current Density Nb/AlN/Nb Junctions with
a 4-K Probe Station, Applied Superconductivity Conference 2016,(Denver, CO, USA, Sep. 4–6, 2016).
Kojima, T.: 2016, Development of SIS Mixers for Future Receivers at
NAOJ, ALMA Developer’s workshop, (Gothenburg, Sweden, May
25–27, 2016).
Kojima, T.: 2016, Feasibility Studies of a Wideband IF Receiver, NROALMA Joint Science/Development Workshop 2016, (Nagano, Japan,
Jul. 20–21, 2016).
Kokubo, E.: 2016, Orbital Architecture of Planetary Systems Formed by
Giant Impacts, Japan-Germany Planet and Disk Workshop, (Ishigaki,
Japan, Sep. 25–30, 2016).
Kokubo, E.: 2017, Formation of Terrestrial Planets, Formation of the
Solar System and the Origin of Life, (Leiden, The Netherlands, Feb.
20–24, 2017).
Kokubo, T., Mori, T., Kurokawa, T., Kashiwagi, K., Tanaka, Y.,
Kotani, T., Nishikawa, J., Tamura, M.: 2016, 12.5-GHz-spaced
Laser Frequency Comb Covering Y,J, and H Bands for Infrared
Doppler Instrument, SPIE Astronomical Telescopes + Instrumentatio,(Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Komiyama, Y.: 2016, Subaru Hyper Suprime-Cam Survey for Local
Group Dwarf Galaxies, Panoramas of the Evolving Cosmos, The 6th

Subaru Int. Conf., (Hiroshima, Japan, Nov. 28–Dec. 2, 2016).
Koyama, Y.: 2016, Unveiling the Environmental Effects on Internal
Star/gas/dust Properties in Galaxies Across Cosmic Time, ALMA
workshop “Extensive CO survey of nearby galaxies”, (Mitaka,
Tokyo, Japan, Dec. 7–9, 2016).
Koyama, Y.: 2016, From Panoramic to Microscopic: Probing the Natureof cluster galaxy population Across Cosmic Time with Subaru,
Panoramas of the Evolving Cosmos, The 6th Subaru Int. Conf.,(Hiroshima, Japan, Nov. 28–Dec. 2, 2016).
Koyama, Y.: 2016, Environmental Impacts on Various Galaxy Properties
across Cosmic Time, In Situ View of Galaxy Formation, (Ringberg
Castle, Bavaria, Germany, Oct. 30–Nov. 5, 2016).
Koyama, Y.: 2016, From MAHALO-Subaru to the New World:
Environmental Impacts on Various Properties of Galaxies AcrossCosmic Time, ALMA workshop "Extensive CO survey of nearby
galaxies", (Mitaka, Tokyo, Japan, Dec. 7–9, 2016).
Koyama, Y.: 2017, An Overview of Galaxy Cluster and Environment
Science with Subaru, Subaru International Partnership Science andInstrumentation Workshop, (Tokyo, Japan, Mar. 22–24, 2017).
Kroug, M., Ezaki, S., Kojima, T., Noguchi, T.: 2016, High Current
Density SIS Junctions Based on Nb / Al,AlN / Al / Nb Multi Layers,
Applied Superconductivity Conference 2016, (Denver, CO, USA,
Sep. 4–6, 2016).
Kroug, M., Ikeya, M., Kojima, T., Noguchi, T.: 2016, Niobium SIS
Junction Technology for Sub-mm Wave Mixers, 29th Int. Symp. on
Superconductivity, (Tokyo, Japan, Dec. 13–15, 2016).
Kroug, M., Kojima, T., Makise, K., Uzawa, Y.: 2017, Material Study
for a THz SIS Mixer, 28th Int. Symp. on Space Terahertz Technology,(Cologne, Germany, Mar. 13–15, 2017)
Kroug, M., Uemizu, K., Ezaki, S., Niizeki, Y., Kojima, T.: 2016, High
Current Density SIS Mixers for the 400–500 GHz Band, 2016 URSI
Asia-Pacific Radio Science Conference, (Seoul, South Korea, Aug.
21–25, 2016).
Kubo, M., et al. including Kano, R., Ishikawa, R., Narukage, N., Bando,
T., Katsukawa, Y., Giono, G., Hara, H., Suematsu, Y., Yoshida, M.:
2017, Results & Future of CLASP Project - From CLASP1 to CLASP2-, Solarnet IV Meeting, (Lanzarote, Spain, Jan. 16–20, 2017).
Kubo, M., Katsukawa, Y., Suematsu, Y., Kano, R., Bando, T.,
Narukage, N., Ishikawa, R., Hara, H., Giono, G., Tsuneta, S.,
Ishikawa, S., Winebarger, A., Kobayashi, K., Trujillo Bueno,J., Auchere, F.: 2016, Ubiquitous Fast Propagating Intensity
Disturbances in Solar Chromosphere, 10th Hinode Science Meeting,(Nagoya, Japan, Sep. 5–8, 2016).
Kubo, M., Katsukawa, Y., Suematsu, Y., Kano, R., Bando, T.,
Narukage, N., Ishikawa, R., Hara, H., Giono, G., Tsuneta, S.,
Ishikawa, S., Winebarger, A., Kobayashi, K., Trujillo Bueno, J.,
Auchere, F.: 2017, Discovery of Ubiquitous Fast Propagating
Intensity Disturbances by CLASP/SJ, Solarnet IV Meeting,(Lanzarote, Spain, Jan. 16–20, 2017).
Kusakabe, M., Koh, S., Kim, K. S., Cheoun, M.-K., Kajino, T., Mathews,
G. J.: 2016, Effects of the f(R) and f(G) Gravities and the Exotic
Particle on Primordial Nucleosynthesis, 14th Int. Symp. on Nuclei in
the Cosmos (NIC2016), (Niigata, Japan, Jun. 19–24, 2016).
Kusakabe, N., Tamura, M.: 2016, SEEDS Direct Imaging Survey of
Exoplanet and Disks, and Next Steps (I), 10th East-Asia Meeting on
Astronomy (EAMA), (Seoul, Korea, Sep. 26–30, 2016).

XIII Publications, Presentations

199

Kusakabe, N.: 2016, Exoplanet to Lives in the Universe, Asian
Astronomical Forum, (Chiang Mai, Thai, Nov. 11, 2016).
Kuzanyan, K., Otsuji, K., Sakurai, T., Hagino, M., Yokoi, N.: 2016,
Current Helicity in the Solar Cycle, the Properties of Turbulent
Magnetic Field from Mosaic SOT/SP Raster Scans and Messages for
Dynamo Theory, 10th Hinode Science Meeting, (Nagoya, Japan, Sep.
5–8, 2016).
Kuzuhara, M.: 2017, Exploring Exoplanet and Disk with Subaru
Telescope, from SEEDS to Next, Subaru International Partnership
Science and Instrumentation Workshop, (Tokyo, Japan, Mar. 22–24,
2017).
Kwon, Y. G., Ishiguro, M., Kuroda, D., Hanayama, H., Kawabata, K.
S., Akitaya, H., Itoh, R., Nakaoka, T., Toda, H., Yoshida, M., Kawai,N., Watanabe, J.: 2016, A Study of Polarimetric Properties of Comet
C/2013 US10 (Catalina) in Optical and Near-Infrared Wavelength
Regions, 2015 KAS FALL MEETING, (Daejeon, Korea, Oct. 13–14,
2016).
Kwon, Y. G., Ishiguro, M., Kuroda, D., Hanayama, H., Kawabata, K.
S., Akitaya, H., Itoh, R., Nakaoka, T.: 2016, A Polarimetric Study ofLong-Period Comet C/2013 US10 (Catalina) and Estimation of Its
Gas Contamination in Optical and Near-Infrared Wavelengths, 2016
KAS FALL MEETING, (Daejeon, Korea, Oct. 13–14, 2016).
Kwon, Y. G., Ishiguro, M., Kuroda, D., Hanayama, H., Kawabata, K.
S., Akitaya, H., Itoh, R., Nakaoka, T.: 2016, An Optical and Infrared
Polarimetric Study of Non-Periodic Comet C/2013 US 10, Catalina,
AOGS 2016, (Beijing, China, Jul. 31–Aug. 5, 2016).
Labadie, L., Berger, J.-P., Cvetojevic, N., Haynes, R., Harris, R.,
Jovanovic, N., Lacour, S., Martin, G., Minardi, S., Perrin, G., Roth,M., Thomson, R. R.: 2016, Astronomical Photonics in the Context
of Infrared Interferometry and High-resolution Spectroscopy, SPIE
Optical and Infrared Interferometry and Imaging V, (Edinburgh, UK,
Jun. 26, 2016).
Lee, J.-W., Je, D.-H., Lee, B., Kang, H., Kim, J., Wagner, J., Asayama, S.,
Gonzalez, A., Kroug, M., Kojima, T., Shan, W., Iguchi, S., Iono, D.:
2016, ASTE Focal Plane Array as Prototype FPA for ALMA TP Array,
2016 URSI Asia-Pacific Radio Science Conference, (Seoul, South
Korea, Aug. 21–25, 2016).
Lee, K.-S.: 2016, Quantitative Estimation of the Energy Flux During
Evaporation in a White Light Flare Kernel Observed by Hinode,
IRIS, SDO, and RHESSI, 10th Hinode Science Meeting, (Nagoya,Japan, Sep. 5–8, 2016).
Lozi, J., Guyon, O., Jovanovic, N., Singh, G., Goebel, S., Norris,
B., Okita, H.: 2016, Characterizing and Mitigating Vibrations for
SCExAO, SPIE Adaptive Optics Systems V, (Edinburgh, UK, Jun.
26, 2016).
Lu, X., Zhang, Q., Liu, H. B.: 2016, High-mass Star Formation in
Filamentary Molecular Clouds, TOPSCOPE workshop, (Beijing,
China, Dec. 13–15, 2016).
Lu, X.: 2017, SMA/JVLA Synergetic Study of Onset of Star Formationin the Central Molecular Zone, East-Asian ALMA Science Workshop
2016, (Hsinchu, Taiwan, Mar. 10–12, 2017).
Maehara, H.: 2016, Starspot Activity and Superflares on Solar-type
Stars, IAUS 328: Living Around Active Stars, (Maresias, Brazil, Oct.
17–21, 2016).
Maehara, H.: 2016, Solar /Stellar Flares on K-M Dwarfs, Impact of
Exoplanetary Space Weather On Climate and Habitability, (New200

XIII Publications, Presentations

Orleans, LA, USA., Nov. 29–Dec. 2, 2016).
Maehara, H.: 2017, Starspot Activity and Superflares on Solar-type Stars,
2nd PSTEP International Symposium, (Kyoto, Japan, Mar. 23–24,
2017).
Males, J., Close, L., Guyon, O., Morzinski, K., Hinz, P., Esposito, S.,
Pinna, E., Xompero, M., Briguglio, R., Riccardi, A., Puglisi, A.,
Mazin, B., Ireland, M., Weinberger, A., Conrad, A., Kenworthy, M.,
Snik, F., Otten, G., Jovanovic, N., Lozi, J.: 2016, The Path to Visible
Extreme Adaptive Optics with MagAO-2K and MagAO-X, SPIE
Astronomical Telescopes + Instrumentatio, (Edinburgh, UK, Jun. 26–
Jul. 1, 2016).
Marchio, M., Flaminio, R., Forest, D., Pinard, L., Tatsumi, D., Sakai,
K.: 2017, Development of an Absorption Bench and Some Results
about Crystalline Coatings, KAGRA F2F Meeting, (Niigata, Japan,
Mar. 28–30, 2017).
Martinache, F., Jovanovic, N., Guyon, O.: 2016, Subaru Coronagraphic
eXtreme Adaptive Optics: On-sky Performance of the Asymmetric
Pupil Fourier Wavefront Sensor, SPIE Adaptive Optics Systems V,(Edinburgh, UK, Jun. 26, 2016).
Maruyama, T., Cheoun, M.-K., Kajino, T., Mathews, G. J.: 2016, Pion
Production from Proton Synchrotron Radiation in Strong Magnetic
Fields, 14th Int. Symp. on Nuclei in the Cosmos (NIC2016), (Niigata,Japan, Jun. 19–24, 2016).
Mathews, G. J., Shibagaki, S., Kajino, T.: 2016, Origin of r-Process
Elements and Galactic Chemodynamical Evolution, 14th Int. Symp. on
Nuclei in the Cosmos (NIC2016), (Niigata, Japan, Jun. 19–24, 2016).
Matsuda, Y., et al. including Hatsukade, B., Iono, D., Kawabe,R., Kubo, M., Nakanishi, K.: 2016, ALMA 860 μm Continuum
Observations of Lyman-alpha Blobs at z=3.1, Half a Decade of
ALMA: Cosmic Dawns Transformed, (Indian Wells, CA, USA, Sep.
20–23, 2016).
Matsumoto, K., Ikeda, H.: 2016, Moments of Inertia of Phobos with
Inhomogeneous Internal Structure, ISLPS2016, (Wuhan, China, Jun.
9–10, 2016).
Matsumoto, K., Ikeda, H.: 2016, Moments of Inertia of Phobos with
Inhomogeneous Internal Structure, Japan Geoscience Union Meeting
2016, (Chiba, Japan, May 22–26, 2016).
Matsumoto, K., Ikeda, H.: 2016, Moments of Inertia of Phobos with
Inhomogeneous Internal Structure, AOGS 2016, (Beijing, China, Jul.
31–Aug. 5, 2016).
Matsuo, H., Ezawa, H., Honma, M., Kiuchi, H., Murata, Y.: 2016,
Terahertz Intensity Interferometry for Very High Angular Resolution
Observations, The 27th Internatiional Symposium on Space Terahertz
Technoloty, (Kurume, Fukuoka, Jul. 17–21, 2016).
Matsuo, H., Ezawa, H., Honma, M., Kiuchi, H., Murata, Y.: 2016,
Terahertz Intensity Interferometry for Milli-arcsecond Resolution,
SPIE Astronomical Telescopes + Instrumentatio, (Edinburgh, UK,
Jun. 26–Jul. 1, 2016).
Matsuo, H., Ezawa, H., Honma, M., Kiuchi, H., Murata, Y.: 2017,
Feasibility Studies on Photon Counting Terahertz Interferometry,
The 28th Internatiional Symposium on Space Terahertz Technoloty,(Cologne, Germany, Mar. 13–15, 2017).
Matsuo, H., Inoue, A., Tamura, Y.: 2016, ALMA observation of star
forming galaxies in the early Universe, Dark Ages and White Nights,(Saint Petersburg, Russia, Jun. 20–24, 2016).
Matsuo, H.: 2016, CMB Photon Statistics, Dark Ages and White Nights,

(Saint Petersburg, Russia, Jun. 20–24, 2016).
Matsuo, H.: 2017, Study on Exoplanet Imaging using Intensity VLBI,Black Hole Astrophysics with VLBI - Past, Present and Future,(Mitaka, Japan, Mar. 27–29, 2017).
Matsuo, K., Otsubo, T.: 2016, Interannual Geocenter Motion withRelation to El Nino Southern Oscillation, 20th Int. Workshop on
Laser Ranging, (Potsdam, Germany, Oct. 10–Oct. 14, 2016).
McKenzie, D. E., et al. including Ishikawa, R., Narukage, N., Kano,R., Yoshida, M.: 2016, CLASP2: The Chromospheric LAyer SpectroPolarimeter, 8th Solar Polarization Workshop, (Firenze, Italy, Sep.
12–16, 2016).
Mitsuda, K., Hashiba, Y., Minowa, Y., Hayano, Y., Sugai, H., Shimono,A., Matsubayashi, K., Hattori, T., Kamata, Y., Ozaki, S., Doi,
M., Sako, S.: 2016, CCD System Upgrading of the Kyoto3DII and
Integral Field Spectroscopic Observation with the New System,
SPIE Ground-based and Airborne Instrumentation for Astronomy VI,(Edinburgh, UK, Jun. 26–30, 2016).
Miyamoto, H., Araya, A., Matsumoto, K., Terada, N., Nishibori, T.,
Kikuchi, H., Hemmi, R., Niihara, T., Tanaka, H., Ogawa, K.: 2016,
Key Observations to Understand the Internal Structure of Phobos,
Japan Geoscience Union Meeting 2016, (Chiba, Japan, May 22–26,
2016).
Miyamoto, Y., Yamauchi, A., Nakai, N., Okumura, T., Zhou, B.,
Isami, K., China, K., Taniguchi, K., Kaneko, H., Matsumoto, N.,
Salak, D., Nishimura, A.: 2016, H2O Maser Survey of Obscured
AGNs, NRO-ALMA Joint Science/Development Workshop 2016,(Nagano, Japan, Jul. 20–21, 2016).
Miyazaki, S.: 2016, Subaru Contribution to Euclid Photo-Z, Uclid
Consortium Meeting, (Lisbon, Poltogal Jun. 1, 2016).
Miyazaki, S.: 2016, Hyper Suprime-Cam, Subaru International
Conference, (Hiroshima, Japan, Dec. 2, 2016).
Mizuno, T., et al. including Noda, H., Namiki, N.: 2016, Development
and Initial Operation of Hayabusa2 LIDAR, ISLPS2016, (Wuhan,
China, Jun. 9–10, 2016).
Momose, M.: 2016, Sintering-Induced Dust Ring Formation In
Protoplanetary Disks: Application To The Hl Tau Disk, Resolving
planet formation in the era of ALMA and extreme AO, (Santiago,
Chile, May 16–20, 2016).
Mori, K., Famiano, M. A., Kajino, T., Suzuki, T., Hidaka, J., Honma, M.,
Iwamoto, K., Nomoto, K., Otsuka, T.: 2016, Impact of New GamowTeller Strengths on Explosive Type Ia Supernova Nucleosynthesis,
14th Int. Symp. on Nuclei in the Cosmos (NIC2016), (Niigata, Japan,
Jun. 19–24, 2016).
Moriya, T.: 2016, Superluminous Supernovae and Their Origins, 2nd
NAOJ-ECT Workshop on Many Riddles About Core-Collapse
Supernovae: Bethe and Beyond, (Mitaka, Japan, Jun. 27–Jul. 1, 2016).
Moriya, T.: 2016, Type Ic Superluminous Supernovae and Possible
Signatures of Their Progenitor Binary Companions, ISSI Workshop
on Supernovae, (Bern, Switzerland, Oct. 3–7, 2016).
Moriya, T.: 2016, Signatures of a Progenitor Binary Companion in TypeIc Superluminous Supernovae, The Mysterious Connection Between
Superluminous Supernovae and Gamma-Ray Bursts, (Baltimore,
MD, USA, May 23–25, 2016).
Moriya, T.: 2016, Rapidly-evolving Faint Transients from Strippedenvelope Electron-capture Supernovae, European Week of Astronomy
and Space Science 2016, (Athens, Greece, Jul. 4–8, 2016).

Moriya, T.: 2016, Light-curve and Spectral Properties of Ultra-stripped
Core-collapse Supernovae, European Week of Astronomy and Space
Science 2016, (Athens, Greece, Jul. 4–8, 2016).
Moriya, T.: 2016, Light-curve and Spectral Properties of Ultra-stripped
Core-collapse Supernovae, Supernovae Through the Ages, (Easterisland, Chile, Aug. 8–13, 2016).
Moriya, T.: 2016, Light-curve and Spectral Properties of Ultra-stripped
Core-collapse Supernovae, IAUS 329: The Lives and Death-throes ofMassive Stars, (Auckland, New Zealand, Nov. 28–Dec. 2, 2016).
Moriya, T.: 2016, Constraining the Ellipticity of Magnetars Powering
Superluminous Supernovae, 4th DTA Symp., (Mitaka, Japan, May
13–14, 2016).
Moriya, T.: 2017, Light-curve and Spectral Properties of Ultra-stripped
Core-collapse Supernovae, Transient Universe in the Big Survey Era:
Understanding the Nature of Astrophysical Explosive Phenomena,(Kyoto, Japan, Jan. 23–24, 2017).
Nagai, H.: 2017, 3C 84: Past, Present, and Future, Black Hole Astrophysics
with VLBI - Past, Present and Future, (Mitaka, Japan, Mar. 27–29, 2017).
Nagai, H.: 2017, Latest Results from ALMA Polarimetry, Cosmic
Polarimetry from Micro to Macro Scales, (Hiroshima, Japan, Feb.
17–18, 2017).
Nakanishi, K., Sorai, K., Nakai, N., Kuno, N., Matsubayashi, K., Sugai,
H., Ando, R., Kohno, K.: 2016, Dense Ionized Gas Embedded with
Infant Massive Stellar Clusters in the NGC 253 Nuclear Starburst,
Half a Decade of ALMA: Cosmic Dawns Transformed, (Indian Wells,
CA, USA, Sep. 20–23, 2016).
Nakanishi, K.: 2016, ALMA polarization calibration, NRO-ALMA Joint
Science/Development Workshop 2016, (Nagano, Japan, Jul. 20–21,
2016).
Narita, N.: 2016, Introduction of Subaru IRD and Okayama MuSCAT,TESS Science Team Meeting, (Cambridge, MA, USA, May, 19,2016).
Narita, N.: 2016, MuSCAT and MuSCAT2 / IRD, TESS Science Team
Meeting/TFOP splinter session, (Cambridge, MA, USA, Dec. 8–9,
2016).
Narita, N.: 2017, MuSCAT and MuSCAT2 for Detection andCharacterization of Transiting Exoplanets, Formation and Dynamical
Evolution of Exoplanets, (Aspen, CO, USA, Mar. 26–Apr. 1, 2017).
Narita, N.: 2017, TRAPPIST-1 and Future Surveys of Habitable
Transiting Earth-like Planets, Astrobiology Center Internatioal
Workshop, (Hiroshima, Japan, Mar. 22–24, 2017).
Narita, N.: 2017, Subaru-TESS Synergy, Subaru Users’ Meeting
FY2016, (Tokyo, Japan, Jan. 10–12, 2017).
Narukage, N., et al. including Ishikawa, R., Kubo, M., Kano,
R., Suematsu, Y., Yoshida, M.: 2016, Chromospheric LAyer
SpectroPolarimeter (CLASP2), SPIE Astronomical Telescopes +Instrumentatio, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Narukage, N., Kano, R., Ishikawa, R., Kubo, M., Katsukawa, Y.,
Giono, G., Bando, T., Hara, H., Suematsu, Y., Ishikawa, S., Shimizu,
T., Sakao, T., Tsuneta, S., Winebarger, A., Kobayashi, K., Trujillo
Bueno, J., Auchere, F., Stepan, J., CLASP team: 2016, Temporal
Variation in the Ly-alpha Linear Polarization Observed with the
CLASP sounding Rocket, 10th Hinode Science Meeting, (Nagoya,Japan, Sep. 5–8, 2016).
Narukage, N., Kano, R., Ishikawa, R., Winebarger, A., Kobayashi, K.,
Trujillo Bueno, J., CLASP team: 2016, Temporal Variation in the

XIII Publications, Presentations

201

Ly-alpha Linear Polarization Observed with the CLASP Sounding
Rocket (poster), 8th Solar Polarization Workshop, (Firenze, Italy,
Sep. 12–16, 2016).
Nemoto, S.: 2017, Dynamic preservation of Tangible Cultural Properties
in NAOJ, Symposium: Is the Collaboration between the Natural
Science and the Human Sciences Possible?, (Osaka, Japan, Mar. 10,2017).
Niino, Y., Totani, T., Okumura, J. E.: 2017, Separating an FRB Optical
Counterpart from Contaminating Supernovae, Fast Radio Bursts:
New Probes of Fundamental Physics and Cosmology, (Aspen, CO,
USA, Feb. 12–17, 2017).
Niino, Y., Aoki, K., Hashimoto, T., Hattori, T., Ishikawa, S.,
Kashikawa, N., Kosugi, G., Onoue, M., Toshikawa, J., Yabe, K.:
2016, The Redshift Selected Sample of Long Gamma-Ray Busrt Host
Galaxies: The Complete Metallicity Measurements at z ≤ 0.41, The
Eighth Huntsville Gamma-Ray Burst Symposium, (Huntsville, AL,
USA, Oct, 24–28. 2016).
Noda, H., Kunimori, H., Mizuno, T., Senshu, H., Ogawa, N., Takeuchi,
H., Moore, C., Pollard, A., Yamaguchi, T., Namiki, N., Kase,
T., Saiki, T., Tsuda, Y.: 2016, Laser Link Experiment between
Hayabusa2 Laser Altimeter and SLR Stations, 20th Int. Workshop on
Laser Ranging, (Potsdam, Germany, Oct. 10–Oct. 14, 2016).
Nozawa, T.: 2016, On Properties of Interstellar Dust Responsible for
Steep Extinction Curves Measured toward Type Ia Supernovae,
International Molecule-type Workshop “Transient Universe in the Big
Survey Era: Understanding the Nature of Astrophysical Explosive
Phenomena”, (Kyoto, Japan, Jan. 23–24, 2017).
Nozawa, T.: 2016, Physical Conditions of Supernova Ejecta as Viewed
from the Measured Sizes of Presolar Al2O3 Grains, The 9th meetingon Cosmic Dust, (Sendai, Japan, Aug. 15–19, 2016).
Nozawa, T.: 2016, Properties of Interstellar Dust as Probed by Extinction
Laws toward Type Ia Supernovae, Multiple Faces of Interstellar Dust,(Garching, Germany, Sep. 15–19, 2016).
Nozawa, T.: 2016, Mass of Dust in Core-collapse Supernovae as Viewed
from Energy Balance in the Ejecta, IAUS 329: The Lives and Deaththroes of Massive Stars, (Auckland, New Zealand, Nov. 28–Dec. 2,2016).
Nozawa, T.: 2017, Properties of Dust Accounting for Extinction Laws
toward Type Ia Supernovae, International Molecule-type Workshop“Transient Universe in the Big Survey Era: Understanding the Natureof Astrophysical Explosive Phenomena”, (Kyoto, Japan, Jan. 23–24,
2017).
Nozawa, T.: 2017, Overall Dust Input from Core-collapse Supernovae
in the Galaxy, The AGB-Supernovae Mass Transition, (Rome, Italy,
Mar. 27–31, 2017).
Oe, M.: 2016, The Introduce of Network Research Topics in the Fieldof Astronomy, 20th Anniversary of AI3 & 15th Anniversary of SOI
Asia, (Bangdung, Indonesia, Sep. 4–6, 2016).
Ogawa, K., et al. including Yamada, R.: 2016, Geophysical Experiments
on Phobos Proposed for JAXA Mars Moon Exploration Mission,
Japan Geoscience Union Meeting 2016, (Chiba, Japan, May 22–26,
2016).
Ogihara, M.: 2016, Terrestrial Planet Formation in Disks Evolving
via Disk Winds, New Directions in Planet Formation, (Leiden, The
Netherlands, Jul. 11–15, 2016).
Ogihara, M.: 2016, Formation of Terrestrial Planets in Disks Evolving

202

XIII Publications, Presentations

via Disk Winds, Japan-Germany Planet and Disk Workshop, (Ishigaki,
Japan, Sep. 25–30, 2016).
Ohashi, N., Kobayashi, K., Fujitake, M.: 2016, IAM(-LIKE) Tunneling
Matrix Formalism for One- and Two-Methyl-Top Molecules Based on
the Extended Permutation-Inversion Group Idea and Its Application
to the Analyses of The Methyl-Torsional Rotational Spectra, 71st
International Symposium on Molecular Spectroscopy, (UrbanaChampagne, IL, USA, Jun. 20–24, 2016).
Ohishi, M.: 2016, Sensitive Observations on CH2NH and CH3NH2 —Precursors to Glycine, Space Talk, (Hanoi, Vietnam, Dec. 6, 2016).
Ohishi, M.: 2016, Sensitive Observations on CH2NH and CH3NH2 —Precursors to Glycine, Seminar, (Buon Ma Thout, Vietnam, Dec. 7,2016).
Ohishi, M.: 2016, Astrochemistry, Training School on Basics ofAstrobiology, (Quy Nhon, Vietnam, Dec. 9, 2016).
Ohishi, M.: 2016, ALMAWebQL, IVOA Interoperability meeting,(Stellenbach, South Africa, May 5–13, 2016).
Ohishi, M.: 2016, ALMA WebQL2 via JVO, NRO-ALMA Joint Science/
Development Workshop 2016, (Nagano, Japan, Jul. 20–21, 2016).
Ohsuga, K.: 2016, Theory of Ultra Luminous X-ray Sources, Breaking
the Limits: Super-Eddington Accretion on Compact Objects,(Sardinia, Italy, Sep. 19–23, 2016).
Ohtani, Y., Suzuki, A., Shigeyama, T.: 2016, Scattered X-ray Photons
due to Axisymmetric Shock Breakout in a Circumstellar Medium,
14th Int. Symp. on Nuclei in the Cosmos (NIC2016), (Niigata, Japan,
Jun. 19–24, 2016).
Ohtani, Y., Suzuki, A., Shigeyama, T.: 2016, Influence of ShockAsymmetry on Observable Features of Shock Breakout, 2nd NAOJECT Workshop on Many Riddles About Core-Collapse Supernovae:
Bethe and Beyond, (Mitaka, Japan, Jun. 27–Jul. 1, 2016).
Ohtani, Y., Suzuki, A., Shigeyama, T.: 2017, Properties of X-ray
Emission of an Aspherical Shock Breakout, IAU focus meeting 331,
(Reunion Island, France, Feb. 20–24, 2017).
Ohtawara, K., et al. including Ishii, S., Oshima, T., Takekoshi, T., Izumi,
N., Uemizu, K., Ito, T., Fujii, Y., Arai, H., Hirota, A., Minamidani,T., Iwashita, H., Maekawa, J., Saito, T., Miyamoto, Y., Kaneko,
H., Morokuma, K., Matsuo, H., Kawabe, R.: 2016, On-site
Measurement of TES bolometer Camera for the ASTE Telescope: (3)Calibration, ALMA/45m/ASTE Users Meeting 2016, (Mitaka, Japan,
Dec. 19–20, 2016).
Oi, Y., Yokoyama, T., Toriumi, S.: 2016, Flux Rope Formation and
Eruption in a Quadrupolar Active Region Holding a Delta-spot,
Hinode-10 Science Meeting, (Nagoya, Japan, Sep. 5–8, 2016).
Oka, T., Geballe, T. R., Goto, M., Usuda, T., Indriolo, N.: 2016, Central
300 PC of the Galaxy Probed by the Infrared Spectra of H3+ and Co:
I. Predominance of Warm and Diffuse Gas and High H2 Ionization
Rate, 71st International Symposium on Molecular Spectroscopy,(Urbana-Champagne, IL, USA, Jun. 20–24, 2016).
Okamoto, J., Liu, W., Tsuneta, S.: 2016, High Resolution Observationsof Prominence Rotation by Hinode and IRIS, AGU Fall Meeting
2016, (San Francisco, CA, USA, Dec. 12–16, 2016).
Okamoto, J., Liu, W., Tsuneta, S.: 2016, Rotation of Helical Prominence
Threads Observed by Hinode and IRIS, Hinode-10 Science Meeting,(Nagoya, Japan, Sep. 5–8, 2016).
Okamoto, J., Liu, W., Tsuneta, S.: 2016, 3D Motion of Active-region
Prominences: Rotation, IAU Symp. 327, (Cartagena, Colombia, Oct.

9–13, 2016).
Okamoto, J., Liu, W., Tsuneta, S.: 2016, Helical Motions of Finestructure Prominence Threads Observed by Hinode and IRIS, IRIS-6:
The Chromosphere, (Stockholm, Sweden, Jun. 20–23, 2016).
Okamoto, J.: 2016, Waves in Prominences and Approaching to theCoronal Heating, AOGS 2016, (Beijing, China, Jul. 31-Aug. 5, 2016).
Okamoto, T. J.: 2016, Introduction to the operation of HINODE, IRIS-7
Workshop, (Weihai, China, Apr. 11–15, 2016).
Okutomi, K., et al. including Takahashi, R., Shoda, A., Fujii, Y.,
Sekiguchi, T., Peña Arellano, F. E., Barton, M., Hirata, N.,
Ishizaki, H., Akutsu, T., Ohishi, N., Aso, Y., Flaminio, R.: 2016,
Vibration Isolation System for KAGRA: Overview and Results in theFirst Operation, GWADW2016, (Elba, Italy, May 22–28, 2016).
Onishi, T., Kawabe, R., Oshima, T., Takekoshi, T., Kohno, K., Tamura,Y., Ishii, S. and LST Working Group: 2016, Large Submillimeter
Telescope (LST), Metrology and Control of Large Telescopes, (Green
Bank, WV, USA, Sep. 19–24, 2016).
Onishi, T.: 2016, Science Review of Nearby Galaxy and Star Formation,
ALMA/45m/ASTE Users Meeting 2016, (Mitaka, Japan, Dec. 19–20,
2016).
Onishi, T.: 2016, Physical Properties and Evolution of Giant Molecular
Clouds in the MagellanicClouds, Star Formation in Different
Environments, (Quy Nhon, Vietnam, Jul. 25–29, 2016).
Onodera, M., Carollo, C. M., Lilly, S., Renzini, A., Arimoto, N., Capak,
P., Daddi, E., Scoville, N., Tacchella, S., Tatehora, S., Zamorani, G.:2016, ISM Excitation and Metallicity of Star-forming Galaxies at z~3.3
from Near-IR Spectroscopy, Panoramas of the Evolving Cosmos, The
6th Subaru Int. Conf., (Hiroshima, Japan, Nov. 28–Dec. 2, 2016).
Onodera, M.: 2016, PFS Operation from the Observatory Perspectives,
PFS software collaboration meeting, (Princeton, USA, Sep. 5–6,
2016).
Onodera, M.: 2016, Stellar Populations as a Key Diagnostics in the Size
Evolution of Passive Galaxies, Deconstructing Galaxies at Cosmic
Noon: The Present and Future of Deep Spectroscopic Surveys at HighRedshift, (Leiden, The Netherlands, Aug. 1–5, 2016).
Oshigami, S., Hirata, N., Kimura, J., Namiki, N.: 2016, Slope andRoughness Characteristics Derived from High-resolution Images ofGalilean Satellites, Japan Geoscience Union Meeting 2016, (Chiba,
Japan, May 22–26, 2016).
Oshigami, S., Hirata, N., Kimura, J., Namiki, N.: 2016, Slope andRoughness Characteristics of Galilean Moons Derived from HighResolution Images, AOGS 2016, (Beijing, China, Jul. 31–Aug. 5,2016).
Oshima, T., et al. including Takekoshi, T., Ohtawara, K., Izumi,
N., Ishii, S., Arai, H., Hirota, A., Minamidani, T., Iwashita, H.,
Maekawa, J., Uemizu, K., Ito, T., Fujii, Y., Saito, T., Miyamoto, Y.,
Kaneko, H., Morokuma, K., Matsuo, H., Kawabe, R., TESCAM
commissioning team: 2016, On-site Measurement of TES Bolometer
Camera for the ASTE Telescope: (1) Project Overview, ALMA/45m/
ASTE Users Meeting 2016, (Mitaka, Japan, Dec. 19–20, 2016).
Ozaki, S., Miyazaki, S., Tsuzuki, T., Tanaka, Y.: 2016, Polishing Testof a Poly-crystal Calcium Fluoride Lens: toward the Development of
TMT WFOS, SPIE Ground-based and Airborne Instrumentation for
Astronomy VI, (Edinburgh, UK, Jun. 26–30, 2016).
Ozeki, H., Miyahara, R., Ihara, H., Todaka, S., Kobayashi, K., Ohishi, M.:
2016, The Millimeter-Wave Spectroscopy of Hydantoin, A Potential

Precursor of Glycine, 71st International Symposium on Molecular
Spectroscopy, (Urbana-Champagne, IL, USA, Jun. 20–24, 2016).
Pathak, P., Guyon, O., Jovanovic, N., Lozi, J., Martinache, F., Minowa,
Y., Kudo, T., Takami, H., Hayano, Y., Narita, N.: 2016, First On-sky
Closed Loop Measurement and Correction of Atmospheric Dispersion,
SPIE Astronomical Telescopes + Instrumentatio, (Edinburgh, UK, Jun.
26–Jul. 1, 2016).
Phillips, A. C., Suzuki, R., Larkin, J. E., Moore, A. M. Hayano, Y.,
Tsuzuki, T., Wright, S. A.: 2016, The Infrared Imaging Spectrograph(IRIS) for TMT: the ADC optical design, SPIE Astronomical
Telescopes + Instrumentatio, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Rains, A., Ireland, M., Jovanovic, N., Feger, T., Bento, J., Schwab, C.,
Coutts, D., Guyon, O., Arriola, A., Gross, S.: 2016, Precision Single
Mode Fibre Integral Field Spectroscopy with the RHEA Spectrograph,
SPIE Ground-based and Airborne Instrumentation for Astronomy VI,(Edinburgh, UK, Jun. 26–30, 2016).
Sagawa, H.: 2016, Planetary & Solar System Science in the Era of ALMA,
NRO-ALMA Joint Science/Development Workshop 2016, (Nagano,
Japan, Jul. 20–21, 2016).
Sakai, N.: 2016, Current Status of KaVA Galactic Astrometry Sub-WG,
East Asia VLBI Workshop 2016, (Guiyang, Guizhou, China, Nov.
7–11, 2016).
Sasaki, H., Takiwaki, T., Kajino, T., Hidaka, J., Maruyama, T., Pehlivan,
Y., Balantekin, B.: 2016, Collective Neutrino-Flavor Oscillations andApplication to Supernova Nucleosynthesis, 14th Int. Symp. on Nuclei
in the Cosmos (NIC2016), (Niigata, Japan, Jun. 19–24, 2016).
Sato, K., Kojima, T., Kroug, M., Sakai T., Uzawa, Y.: 2016, Capacitance
Measurements of Niobium SIS Junctions at Microwave Frequencies,
29th Int. Symp. on Superconductivity, (Tokyo, Japan, Dec. 13–15,
2016).
Sawada, T., Hasegawa, T., Koda, J.: 2016, Internal Structures of
Molecular Clouds in the LMC Revealed by High-Fidelity Imaging
with ALMA, Half a Decade of ALMA: Cosmic Dawns Transformed,(Indian Wells, CA, USA, Sep. 20–23, 2016).
Schwab, C., Jovanovic, N., Feger, T., Bakovic, M., Gurevich, Y. V.,
Stürmer, J., Apodaca, R., Vanzi, L., Rukdee, S., Lawrence, J. S.,
Coutts, D. W., Cvetojevic, N., Mahadevan, S., Stefánsson, G. K.,
Halverson, S. P., Guyon, O.: 2016, Adaptive Optics Fed Single-mode
Spectrograph for High-precision Doppler Measurements in the Nearinfrared, SPIE Advances in Optical and Mechanical Technologies forTelescopes and Instrumentation II, (Edinburgh, UK, Jun. 26, 2016).
Sekine, Y., Tabata, H.: 2016, Runaway Acidification of Surface Water
on Early Mars in Response to Atmospheric Evolution, AOGS 2016,(Beijing, China, Jul. 31–Aug. 5, 2016).
Shan, W., Ezaki, S., Kaneko, K., Kroug, M., Gonzalez, A., Kojima, T.,
Fujii, Y., Asayama, S., Noguchi, T.: 2017, Design and Fabricationof a Dual-Polarization, Balanced SIS Mixer Integrated Circuit, 28th
Int. Symp. on Space Terahertz Technology, (Cologne, Germany, Mar.
13–15, 2017)
Shibagaki, S., Takiwaki, T., Kajino, T.: 2016, 1.5D GRMHD Simulationof Core-Collapse Supernova, 14th Int. Symp. on Nuclei in the
Cosmos (NIC2016), (Niigata, Japan, Jun. 19–24, 2016).
Shibata, Y., Agata, H., Usuda-Satoh, K., Cheung, S., Canas, L.: 2016,
To Overcome the Language Barrier – Case Study in Japan, CAP2016,(Medellín, Colombia, May 16–20, 2016).
Shibata, Y.: 2016, To Overcome the Language Barrier — Casestudy in

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Japan, Communicating Astronomy with the Public 2016, (Medellin,
Colombia, May 16–20, 2016).
Shimojo, M., ALMA Solar Development Team: 2016, Solar Observations
in Cycle 4 of ALMA, Cool Star 19, (Uppsala, Sweden, Jun. 6–10,
2016).
Shimojo, M., ALMA Solar Development Team: 2016, What Solar Data
will ALMA Provide to Us in Cycle 4 and Beyond?, Hinode-11,(Nagoya Japan, Sep. 5–8, 2016).
Shimojo, M., ALMA Solar Development Team: 2016, What Solar Data
will ALMA Provide to Us in Cycle 4 and Beyond?, Solar Physics
with Radio Observations 2016, (Nagoya Japan, Sep. 9–10, 2016).
Shimojo, M., ALMA Solar Development Team: 2016, Solar Observations
in Cycle 4 of ALMA, 2016 URSI Asia-Pacific Radio Science
Conference, (Seoul, South Korea, Aug. 21–25, 2016).
Shimojo, M., ALMA Solar Development Team: 2017, New window ofsolar physics: Solar observations with ALMA, East-Asian ALMA
Science Workshop 2016, (Hsinchu, Taiwan, Mar. 10–12, 2017).
Shin, J. W., Park, T.-S., Kajino, T., Cheoun, M.-K.: 2016, Neutrino
Interactions with Matter by a New Neutrino Source From the Isotope
Radioactive Decay Produced by the Proton Accelerator, 14th Int.
Symp. on Nuclei in the Cosmos (NIC2016), (Niigata, Japan, Jun.
19–24, 2016).
Shinnaka, H.: 2016, Ortho-to-Para Abundance Ratios of Water from
High-resolution Spectra of Water Ion in the Optical Wavelength
Region, Water in the Universe: From Clouds to Oceans, (Noordwijk,
Netherland, Apr. 12–15, 2016).
Shinnaka, H.: 2016, Imaging Observations of Hydrogen Coma of 67P/
Churyumov-Gerasimenko by PROCYON/LAICA, Cometary science
after Rosetta, (London, UK, Jun. 14–15, 2016).
Shinnaka, H.: 2016, Lyman-alpha Imaging of Whole Coma for 67P/
Churyumov-Gerasimenko by PROCYON/LAICA, Cometary Science
After Rosetta: Future Directions, (London, UK, Jun. 16–17, 2016).
Shinnaka, H.: 2016, Spectroscopic Observations of 14N/15N Ratios inboth NH2 and CN in Comet C/2013 US10 (Catalina), DPS48/EPSC11
meeting, (Pasadena, CA, USA, Oct. 16–21, 2016).
Shinnaka, H.: 2017, Ortho-to-Para Abundance Ratios (OPRs) of NH2 in
Comets: The Meaning of OPRs of Cometary Volatiles, Subaru Users'
Meeting FY2016, (Tokyo, Japan, Jan. 10–12, 2017).
Shinnaka, H.: 2017, Nitrogen Isotopic Ratios of NH2 and CN in Comet
C/2013 US10 (Catalina) based on high-resolution optical spectra
taken by the HDS/Subaru, Subaru Users’ Meeting FY2016, (Tokyo,
Japan, Jan. 10–12, 2017).
Shirasaki, Y., Hiramatsu, M.: 2017, JVO ALMA FITS Data Archive,
Data to Dome Workshop, (Tokyo, Japan, Mar. 2–3, 2017).
Shirasaki, Y., Zapart, C., Ohishi, M., Mizumoto Y.: 2016, Updateof the JVO Subaru Suprime-Cam Mosaic Image Archive, ADASSXXVI, (Trieste, Italy, Oct. 16–20, 2016).
Shirasaki, Y.: 2016, Properties of Galaxies around z=0.6–3.0 QSOs
Revealed by Clustering Analysis Using Data from HSC-SSP Wide
Survey, HSC-AGN meeting, (Chiba, Japan, Aug. 26–27, 2016).
Shirasaki, Y.: 2016, Delivery of Gaia Source Catalog from NAOJ, GaiaJASMINE joint meeting, (Mitaka, Japan, Dec. 6–9, 2016).
Shoda, A.: 2016, GWADW 2016: Environment at the Underground GW
Detector KAGRA, GWADW2016, (Elba, Italy, May 22–28, 2016).
Singh, G., Lozi, J., Choquet, E., Serabyn, E., Guyon, O.: 2016, PSF

204

XIII Publications, Presentations

Calibration Using the Lyot-based Low Order Wavefront Sensor
Telemetry: First Simulations, SPIE Astronomical Telescopes +Instrumentatio, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Sôma, M.: 2016, Derivation of the Inclination of Mars’ Orbit in the
Almagest, The 9th International Conference on Oriental Astronomy(ICOA-9), (Pune, India, Nov. 14–19, 2016).
Sôma, M.: 2017, Results from Recent Lunar Graze Observations, 7thInternational Workshop on Occultation and Eclipse, (Shahr-e kord,
Iran, Mar. 8–10, 2017).
Sotani, H.: 2016, Nuclear Symmetry Energy and Crustal Torsional
Oscillations in Neutron Stars, 6th International Symposium on Nuclear
Symmetry Energy (NuSYM16), (Beijing, China, Jun. 13–17, 2016).
Sotani, H.: 2016, Crustal Torsional Oscillations and Nuclear Symmetry
Energy, 14th Int. Symp. on Nuclei in the Cosmos (NIC2016), (Niigata,Japan, Jun. 19–24, 2016).
Sotani, H.: 2016, Gravitational Waves of Core-collapse Supernova at Postbounce Phase, 21st Int. Conf. on General Relativity and Gravitation(GR21), (New York, USA, Jul. 10–25, 2016).
Sotani, H.: 2016, Scalar-gravitational Waves from Relativistic Stars in
Scalar-tensor Gravity, Gravitational Waves from modified gravity
theories, (Athens, Greece, Sep. 15–17, 2016).
Sotani, H.: 2016, Gravitational Wave Asteroseismology in ProtoneutronStars, NEB 17 - Recent Developments in Gravity, (Mykonos, Greece,
Sep. 19–22, 2016).
Sotani, H.: 2016, Probing the Nuclear Symmetry Energy via NeutronStar Asteroseismology, International Symposium on Neutron Star
Matter (NSMAT2016), (Sendai, Japan, Nov. 21–24, 2016).
Sotani, H.: 2017, Gravitational Waves from Protoneutron Stars, Testing
Gravity 2017, (Vancouver, BC, Canada, Jan. 26–28, 2017).
Sotani, H.: 2017, Protoneutron Star Properties via Gravitational Wave
Asteroseismology, Quarks and Compact Stars 2017 (QCS2017),(Kyoto, Japan, Feb. 20–23, 2017).
Srikanth, S., Gonzalez, A.: 2016, ALMA Band 2 Optics: Design,
Constraints, Implementation and Measurements, 2016 URSI AsiaPacific Radio Science Conference, (Seoul, South Korea, Aug. 21–25,
2016).
Suematsu, Y., Saito, K., Koyama, M., Enokida, Y., Okura, Y., Nakayasu,
T., Sukegawa, T.: 2016, Compact Integral Field Unit for Optical
Telescope of the SOLAR-C Mission, International Conference onSpace Optics 2016, (Biarritz, France, Oct. 18–21, 2016).
Suematsu, Y.: 2016, On the Roots of Solar Spicules revealed with
Hinode/SOT-NFI Observations in Na I D and Mg I b Lines, 10th
Hinode Science Meeting, (Nagoya, Japan, Sep. 5–8, 2016).
Suzuki, T., Honma, M., Mori, K., Famiano, M. A., Kajino, T., Hidakai, J.,
Otsuka, T.: 2016, Electron-capture Rates for pf-shell Nuclei in Stellar
Environments and Nucleosynthesis, 14th Int. Symp. on Nuclei in the
Cosmos (NIC2016), (Niigata, Japan, Jun. 19–24, 2016).
Suzuki, T., Yoshida, T., Shibagaki, S., Kajino, T., Otsuka, T.: 2016, BetaDecay Rates for Exotic Nuclei and R-Process Nucleosynthesis up
to Th and U, 14th Int. Symp. on Nuclei in the Cosmos (NIC2016),(Niigata, Japan, Jun. 19–24, 2016).
Takahashi, H. R., Ohsuga, K.: 2016, Accretion and Outflows Observedin GRRMHD Simulations, ULXs and their environments, (Strasbourg,
France, Jun. 13–16, 2016).
Takahashi, H. R.: 2016, Relativistic Radiation Magnetohydrodynamics

of Accretion Disks, International Congress on Plasma Physics(ICPP)-2016, (Kaohsiung, Taiwan, Jun. 27–Jul. 1, 2016).
Takahashi, H. R.: 2017, General Relativistic Radiation Magnetohydrodynamic Simulations of Disk Accretion onto a Black Holeor a Neutron Star, US Japan Workshop and School on Magnetic
Reconnection (MR2017), (Matsuyama, Ehime, Japan, Mar. 19–23,
2017).
Takahashi, H. R.: 2017, Black Hole and Neutron Star Accretion Disk,
Ultra-Luminous X-ray Source, (Sagamihara, Japan, March. 3–4,
2017).
Takahashi, H. R.: 2017, Radiation Magnetohydrodynamic Simulationsof Accretion Disks, East Asian Numerical Astrophysics Meeting,(Beijing, China, Oct. 24–16, 2016).
Takahashi, R.: 2016, Vibration Isolation System for KAGRA, The 1st
International Meeting on KAGRA, (Daejon, Korea, Jun. 23–25,
2016).
Takahashi, R.: 2016, Installation Plan of Vibration Isolation System
for KAGRA, The 2nd International Meeting on KAGRA, (Beijing,
China, Nov. 10–12, 2016).
Takekoshi, T., et al. including Oshima, T., Ohtawara, K., Izumi,
N., Ishii, S., Arai, H., Hirota, A., Minamidani, T., Iwashita, H.,
Maekawa, J., Uemizu, K., Ito, T., Fujii, Y., Saito, T., Miyamoto, Y.,
Kaneko, H., Morokuma, K., Matsuo, H., Kawabe, R., Izumi, T.,
TESCAM commissioning team: 2016, On-site Measurement of TES
Bolometer Camera for the ASTE Telescope: (2) Optics Evaluation,
ALMA/45m/ASTE Users Meeting 2016, (Mitaka, Japan, Dec. 19–20,
2016).
Taki, T., Okuzumi, S., Fujimoto, M., Ida, S.: 2016, Dust and Gas Density
Evolution at a Radial Pressure Bump, Japan-Germany Planet andDisk Workshop, (Ishigaki, Japan, Sep. 25–30, 2016).
Takiwaki, T.: 2016, Gravitational Signals from Core-collapase
Supernovae: Cutting-edge samples, 4th DTA Symp., (Mitaka, Japan,
May 13–14, 2016).
Takiwaki, T.: 2016, Supernova Simulations with Updated Microphysics,
14th Int. Symp. on Nuclei in the Cosmos (NIC2016), (Niigata, Japan,
Jun. 19–24, 2016).
Takiwaki, T.: 2016, Supernova Neutrinos, The First Workshop on theSecond Hyper-Kamiokande Detector in Korea, (Seoul, Korea, Nov.
22, 2016).
Takiwaki, T.: 2016, Intensive and Extensive Studies of Core-collapse
Supernovae: Status Reports of Japanese Group, 2nd NAOJ-ECTWorkshop on Many Riddles About Core-Collapse Supernovae: Bethe
and Beyond, (Mitaka, Japan, Jun. 27–Jul. 1, 2016).
Takiwaki, T.: 2016, Toward Multi-messenger Observation of Corecollapse Supernovae from Simulations of the Central Engine,
Supernovae Though the Ages, (Ester Island, Chile, Aug. 9–13, 2016).
Takiwaki, T.: 2016, A Clockwork Supernova: Precision Numerical
Experiments and Their Applications, DTA colloquium, (Mitaka,
Japan, Apr. 13, 2016).
Tamura, M.: 2016, Astrobiology Center (ABC) of NINS, EANA,(Athens, Greece, Sep. 27–30, 2016).
Tamura, N., et al. including Takato, N., Ueda, A., Kamata, Y., Minowa,
Y.: 2016, Prime Focus Spectrograph (PFS) for the Subaru Telescope:
Overview, Recent Progress, and Future Perspectives, SPIE
Astronomical Telescopes + Instrumentatio, (Edinburgh, UK, Jun. 26–
Jul. 1, 2016).

Tanaka, M.: 2016, Galaxy Evolution Science with Hyper SuprimeCam, Prime Focus Spectrograph, and ULTIMATE, Ultimate Subaru
Science Workshop 2016, (Tokyo, Japan, Jun. 16–17, 2016).
Tanaka, M.: 2016, Deep Near-IR Spectroscopy of Massive Galaxies inProto-clusters, Deconstructing Galaxies at Cosmic Noon: The Present
and Future of Deep Spectroscopic Surveys at High Redshift, (Leiden,
The Netherlands, Aug. 1–5, 2016).
Tanaka, M.: 2016, Hyper Suprime-Cam Subaru Strategic Program,
Cosmology and Structure Formation, (Seul, South Korea, Nov. 1–4,
2016).
Tanaka, M.: 2016, Science Database: NAOJ’s perspectives and plansforward, PFS collaboration meeting 2016, (Baltimore, USA, Dec.
12–16, 2016).
Tanaka, M.: 2016, Kilonova/Macronova Emission from Compact Binary
Mergers, Gravitational-Wave Astrophysics in the High Event Rate
Regime, (Tokyo, Japan, Dec. 5–6, 2016).
Tanaka, M.: 2016, Kilonova/Macronova Emission from Compact Binary
Mergers, Compact stars and gravitational waves, (Kyoto, Japan, Oct.
31–Nov. 4, 2016).
Tanaka, M.: 2016, Time-Domain Science with ULTIMATE-Subaru,
Ultimate Subaru Science Workshop 2016, (Tokyo, Japan, Jun. 16-17,
2016).
Tanaka, M.: 2016, Three-dimensional Geometry of Core-collapse
Supernovae: Observations and Modelling, Bridging the gap: frommassive stars to supernovae, (Buckinghamshire, UK, Jun. 1–2, 2016).
Tanaka, M.: 2016, TMT and Gravitational Wave Astronomy, TMT
Science Forum 2016, (Kyoto, Japan, May 24–26, 2016).
Tanaka, M.: 2016, Transient Surveys with Subaru/Hyper SuprimeCam, The Ninth Harvard-Smithsonian Conference on Theoretical
Astrophysics “The transient sky”, (Boston, USA, May 16–19, 2016).
Tanaka, M.: 2016, Kilonova Emission from Compact Binary Mergers,
Supernovae Through the Ages, (Easter island, Chile, Aug. 8–13,
2016).
Tanaka, M.: 2016, Electromagnetic Counterparts of Gravitational Wave
Sources, 4th DTA Symp., (Mitaka, Japan, May 13–14, 2016).
Tanaka, M.: 2017, Deep Near-IR Spectroscopy of Massive Galaxies inProto-clusters, Subaru Users’ Meeting FY2016, (Tokyo, Japan, Jan.
10–12, 2017).
Tanaka, M.: 2017, First Data Release of the Hyper Suprime-Cam Subaru
Strategic Program, “Accelerated Universe” Symposium, (Tsukuba,
Japan, Mar. 8–10, 2017).
Tanaka, M.: 2017, HSC+Huntsman: a Search for Dwarf Galaxies
around Nearby Galaxies, Subaru International Partnership Scienceand Instrumentation Workshop, (Tokyo, Japan, Mar. 22–24, 2017).
Tanaka, M.: 2017, Time-Domain Science with Subaru/HSC, Subaru
International Partnership Science and Instrumentation Workshop,(Tokyo, Japan, Mar. 22–24, 2017).
Tanaka, M.: 2017, Multi-Messenger from Supernovae, Workshop on
Supernova at Hyper-Kamiokande, (Tokyo, Japan, Feb. 12–13, 2017).
Tanaka, M.: 2017, Rapid Transients from Subaru/HSC Transient Survey,
International Molecule-type Workshop “Transient Universe in the Big
Survey Era: Understanding the Nature of Astrophysical Explosive
Phenomena”, (Kyoto, Japan, Jan. 23–24, 2017).
Tanaka, S., Shiraishi, H., Shirai, K., Ishihara, Y., Goto, K., Hayakawa,
M., Ozaki, M., Mizuno, T., Yamada, K., Murakami, H., Yamada, R.:
2016, Development of a Penetrator Probe Dropping from a UAV for

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Disaster Prevention, Japan Geoscience Union Meeting 2016, (Chiba,
Japan, May 22–26, 2016).
Tanaka, Y., Heling, C., Suzuki, T. K., Inutsuka, S.: 2016, AtmosphericEscape from Close-in Gaseous Planets Driven by Magnetohydrodynamic
Waves, Japan-Germany Planet and Disk Workshop, (Ishigaki, Japan,
Sep. 25–30, 2016).
Tanikawa, K., Sôma, M., Shylaja, B., Vahia, M. N.: 2016, Reliabilityof the Records of Observed Solar Eclipses in India and Comparison
with Contemporaneous Eclipse Data of Other Countries, The 9thInternational Conference on Oriental Astronomy (ICOA-9), (Pune,
India, Nov. 14–19, 2016).
Tapia, V., Nesti, R., Gonzalez, A., Barrueta, I., Mena, F.P., Reyes, N.,
Villa, F., Cuttaia, F., Yagoubov, P.: 2016, An Ultra-broadband Optical
System for ALMA Band 2+3, SPIE Conference on Astronomical
Telescopes + Instrumentation 2016, (Edinburgh, UK, Jun. 10–15, 2016).
Tei, A., Sakaue, T., Asai, A., Ueno, S., Ichimoto, K., Shibata, K., Kawate,
T., Okamoto, T. J.: 2016, Dynamic Response of the Chromospherein a Solar Flare Based on Spectroscopic Observations, Hinode-10
Science Meeting, (Nagoya, Japan, Sep. 5–8, 2016).
Terada, H.: 2016, Observations of Ices in Protoplanetary Disks, Ice Age- The Era of JWST, (Leiden, The Netherlands, Oct. 4–7, 2016).
Terai, T., Yoshida, F.: 2017, Jupiter Trojan Survey with Hyper SuprimeCam, Subaru Users’ Meeting FY2016, (Tokyo, Japan, Jan. 10–12,
2017).
Toirumi, S.: 2016, Flux Emergence Studies: Past, Present and Future,
10th Hinode Science Meeting, (Nagoya, Japan, Sep. 5–8, 2016).
Toriumi, S., Katsukawa, Y., Cheung, M. C. M.: 2016, Hinode-IRIS
Observation and MHD Modeling of Sunspot Light Bridges, IRIS-7
Workshop, (Weihai, China, Apr. 11–15, 2016).
Toriumi, S., Katsukawa, Y., Cheung, M. C. M.: 2016, Hinode-IRIS
Analysis of Various Chromospheric Heatings in Emerging Flux
Regions, IRIS-6: The Chromosphere, (Stockholm, Sweden, Jun.
20–23, 2016).
Toriumi, S., Schrijver, C. J., Harra, L. K., Hudson, H., Nagashima, K.:
2016, Properties and Developments of Flaring Active Regions, SDO
2016: Unraveling the Sun’s Complexity, (Burlington, VT, USA, Oct.
17–21, 2016).
Toriumi, S., Schrijver, C. J., Harra, L. K., Hudson, H., Nagashima, K.:
2017, Flare-productive Active Regions: Magnetic Properties andEvolutions, Solarnet IV Meeting, (Lanzarote, Spain, Jan. 16–20,
2017).
Toriumi, S.: 2016, Flux Emergence Studies: Past, Present and Future,
Hinode-10 Science Meeting, (Nagoya, Japan, Sep. 5–8, 2016).
Toriumi, S.: 2017, Review on Recent Publications of Light Bridge
Studies, ISSI UV Bursts Meeting, (Bern, Switzerland, Mar. 6–10,
2017).
Toriumi, S.: 2017, Various Local Heating Events in the Earliest Phase ofFlux Emergence, ISSI UV Bursts Meeting, (Bern, Switzerland, Mar.
6–10, 2017).
Toriumi, S.: 2017, Observation and Modeling of Flare-productive Solar
Active Regions, 2nd PSTEP International Symposium, (Kyoto, Japan,
Mar. 23–24, 2017).
Tsujimoto, T.: 2016, Observational Constraints on r-process Site &Nucleosynthesis from Dwarf Galaxies, the Milky Way, and the Solar
System, The r-process nucleosynthesis: connecting FRIB with thecosmos, (Lansing, MI, USA, Jun. 6–17, 2016).

206

XIII Publications, Presentations

Tsujimoto, T.: 2016, Origina and Evolution of r-process Nuclides in Local
Universe, Goldschmidt, (Yokohama, Japan, Jun. 27–Jul. 1, 2016).
Tsujimoto, T.: 2016, r-process Enrichment in the Milky Way and Nearby
Dwarf Galaxies, The Milky Way and its environment, (Paris, France,
Sep. 19–23, 2016).
Tsuzuki, T., Suzuki, R., Harakawa, H., Ikenoue, B., Larkin, J. Moore,
A., Obuchi, Y., Phillips, A. C., Saito, S., Uraguchi, F., Wincentsen,J., Wright, S., Hayano, Y.: The Infrared Imaging Spectrograph (IRIS)
for TMT: Optical Design of IRIS Imager with “Co-axis Double
TMA”, SPIE Astronomical Telescopes + Instrumentatio, (Edinburgh,
UK, Jun. 26–Jul. 1, 2016).
Uraguchi, F., Obuchi, Y., Ikenoue, B., Saito, S., Suzuki, R., Hayano,
Y.: The Infrared Imaging Spectrograph (IRIS) for TMT: Prototypingof Cryogenic Compatible Stage for the Imager, SPIE Astronomical
Telescopes + Instrumentatio, (Edinburgh, UK, Jun. 26–Jul. 1, 2016).
Usuda, T.: 2016, Thirty Meter Telescope (TMT) Project Status, 10th
East-Asia Meeting on Astronomy (EAMA), (Seoul, Korea, Sep.
26–30, 2016).
Usuda, T.: 2017, Direct Detection of Cosmic Acceleration by TMT &High Dispersion Spectrograph B04 Overview & Current Status of
TMT, “Accelerated Universe” Symposium, (Tsukuba, Japan, Mar.
8–10, 2017).
Usuda-Sato, K., Canas, L.: 2016, Universal Design Symposium
in Japan - International Collaboration -, Astronomy beyond theCommon Senses, (Cartagena de Indias, Colombia, Oct. 8, 2016).
Usuda-Sato, K., Mineshige, S., Canas, L.: 2016, Sharing Japanese
Resources of “Universal Design” for Astronomy, Astronomy beyond
the Common Senses, (Cartagena de Indias, Colombia, Oct. 8, 2016).
Usuda-Sato, K., Shibata, Y., Canas, L.: 2016, Exploring the Universe
Using Mitaka Software, Communicating Astronomy with the Public
2016, (Medellin, Colombia, May 16–20, 2016).
Usuda-Sato, K.: 2016, Participation by non-English Speakers in theWorldwide NameExoWorlds Contest, Communicating Astronomy
with the Public 2016, (Medellin, Colombia, May 16–20, 2016).
Usuda-Sato, K.: 2017, Inclusivity at NAOJ Miaka Visitors’ Area,
Symposium: Is the Collaboration between the Natural Science andthe Human Sciences Possible?, (Osaka, Japan, Mar. 10, 2017).
Uzawa, Y., Fujii, Y., Kroug, M., Makise, K., Gonzalez, A., Kaneko,
K., Kojima, T., Miyachi, A., Saito, S., Terai, H., Wang, Z.: 2016,
Development of Superconducting THz Receivers for Radio
Astronomy, 41st International Conference on Infrared, Millimeter,
and Terahertz Waves (IRMMW-THz 2016), (Copenhagen, Denmark,Sep. 25–30, 2016).
Uzawa, Y., Kroug, M., Kojima, T., Makise, K., Gonzalez, A., Saito,
S., Fujii, Y., Kaneko, K., Terai, H., Wang, Z.: 2016, Development of
Terahertz SIS Mixers Using Nb/AlN/Nb Tunnel Junctions Integrated
with All NbTiN Tuning Circuits, 27th Int. Symp. on Space Terahertz
Technology, (Nanjing, China, Apr. 12–15, 2016).
Uzawa, Y., Kroug, M., Kojima, T., Makise, K., Gonzalez, A., Saito,
S., Fujii, Y., Kaneko, K., Terai, H., Wang, Z.: 2016, Developmentof Terahertz SIS Mixers Using Nb/AlN/NbTunnel junctions
Integrated with All NbTiNTuning Circuit, Applied Superconductivity
Conference 2016, (Denver, CO, USA, Sept. 4–6, 2016).
Uzawa, Y., Makise, K., Saito, S., Terai, H., Wang, Z., Kojima, T.,
Kroug, M., Fujii, Y., Gonzalez, A., Kaneko, K.: 2016, Developmentof Highly Sensitive Superconducting Receivers for ALMA Band

10 and Future Prospects, 2016 URSI Asia-Pacific Radio Science
Conference, (Seoul, South Korea, Aug. 21–25, 2016).
Uzawa, Y., Shan, W., Kojima, T., Gonzalez, A., Kroug, M.: 2017,
Theoretical Consideration of SIS Up-converters for Frequency Division
Multiplexing, 28th Int. Symp. on Space Terahertz Technology,(Cologne, Germany, Mar. 13–15, 2017)
Wakita, S., Nozawa, T., Hasegawa, Y.: 2017, Diffusion Process in
Thermally Evolving Planetesimals for Presolar Silicate Grains, 48th
Lunar and Planetary Science Conference , (the Woodlands TX, USA,
Mar. 20–24, 2017).
Wenlei, S., Gonzalez, A., Kroug, M., Kojima, T., Fujii, Y., Asayama, S.,
Noguchi, T.: 2016, Concept Design of a Dual-Polarization SidebandSeparating Multi-Pixel SIS Receiver, 27th Int. Symp. on Space
Terahertz Technology, (Nanjing, China, Apr. 12–15, 2016).
Wong, K. C.: 2016, Cosmology from Gravitational Lens Time Delays,
10th East-Asia Meeting on Astronomy (EAMA), (Seoul, Korea, Sep.
26–30, 2016).
Wong, K. C.: 2016, A Spectroscopically Confirmed Double Source
Plane Lens System in the Hyper Suprime-Cam Subaru Strategic
Program, Panoramas of the Evolving Cosmos, The 6th Subaru Int.
Conf., (Hiroshima, Japan, Nov. 28–Dec. 2, 2016).
Wu, Y. W.: 2016, Maser Survey towards Sgr Stellar Stream, East Asia
VLBI Workshop 2016, (Guiyang, Guizhou, China, Nov. 7–11, 2016).
Yagoubov, P., Gonzalez, A., Tapia, V., Reyes, N., Mena, F. P., Nesti,R., Cuttaia, F., Ricciardi, S., Villa, F.: 2016, 67–116 GHz Optics
Development for ALMA band 2–3 Receivers, 41st International
Conference on Infrared, Millimeter, and Terahertz Waves (IRMMWTHz 2016), (Copenhagen, Denmark, Sep. 25–30, 2016).
Yaji, K.: 2016, EPO Coordinated Observations for High School Students- Let's observe the sun with Hinode!, 10th Hinode Science Meeting,(Nagoya, Japan, Sep. 5–8, 2016).
Yaji, K.: 2016, How do you communicate the sun?, Communicating
Astronomy with the Public 2016, (Medellin, Colombia, May 16–20,
2016).
Yaji, K.: 2016, Let’s Cook Solar Data/Images for Your Classroom!,
Global Hands on Universe 2016, (Stord, Norway, Aug. 22–27, 2016).
Yamada, R., Ishihara, Y., Kobayashi, N., Murakami, H. Tanaka, S.:
2016, Scientific Results Expected from the APPROACH Mission,
ISLPS2016, (Wuhan, China, Jun. 9–10, 2016).
Yamada, R., Ishihara, Y., Kobayashi, N., Murakami, H., Tanaka, S.,
Takeuchi, N., Shiraishi, H., Hayakawa, M., Goto, K., Kikuchi, F.,
Nishida, K.: 2016, Expected Results on the Lunar Science from
Scientific Observations in Approach Mission, Japan Geoscience
Union Meeting 2016, (Chiba, Japan, May 22–26, 2016).
Yamada, R., Senshu, H., Namiki, N., Mizuno, T., Abe, S., Yoshida, F.,
Asari, K., Noda, H., Hirata, N., Oshigami, S., Araki, H., Ishihara, Y.,
Matsumoto, K.: 2016, The Instrument Error on Estimation of Normal
Albedo of Ryugu Using the Laser Altimeter On-board Hayabusa2 andthe Reflectance Measurement of the Carbonaceous Chondrite at zero
Phase Angle, Japan Geoscience Union Meeting 2016, (Chiba, Japan,
May 22–26, 2016).
Yamada, R., Shiraishi, H., Asari, K., Nébut, T., Lognonné, P., Hanada, H.,
Tanaka, S.: 2016, Development of the New Broadband Seismometersfor Moonquake Observation, AOGS 2016, (Beijing, China, Jul. 31–
Aug. 5, 2016).
Yamada., R. Senshu, H., Namiki, N., Mizuno, T., Noda, H., Asari, K.,

Araki, H., Yoshida, F., Abe, S., Oshigami, S., Hirata, N., Ishihara,Y., Matsumoto, K.: 2017, Albedo observation of near Earth C-type
asteroid by Hayabusa2 LIDAR, AGU Fall Meeting 2016, (SanFrancisco, CA, USA, Dec. 12–16, 2016).
Yamamoto, Y., Yamada, R.: 2016, Current Status of Data Restoration of
the Seismometer Onboard Viking Lander 2, Japan Geoscience Union
Meeting 2016, (Chiba, Japan, May 22–26, 2016).
Yamaoka, H., Agata, H.: 2016, NAOJ Public Relations Center, TMTWEPOC meeting, (Shinagawa, Japan, May 27–28, 2016).
Yamaoka, H.: 2016, Scientist Talk: National Astronomical Observatoryof Japan (NAOJ) ~From East to Worldwide~, New Scientist Live2016, (London, UK. Sep. 22–25, 2016).
Yamazaki, D. G., Kusakabe, M., Kajino, T., Mathews, G. J., Cheoun,
M.-K.: 2016, The New BBN Model with the Photon Cooling, X
Particle, and the Primordial Magnetic Field, 14th Int. Symp. on
Nuclei in the Cosmos (NIC2016), (Niigata, Japan, Jun. 19–24, 2016).
Yano, T.: 2016 , Number of Stars Observable with Small-JASMINE andCalibration with Gaia Data, Gaia-JASMINE joint meeting, (Mitaka,
Japan, Dec. 6–9, 2016).
Yoshida, M., Hara, H., Katsukawa, Y., Suematsu, Y.: 2016, Structuresof Turbulent Plasma Motions in the Cusp Region of the 2015 Mar
7 Flare, 10th Hinode Science Meeting, (Nagoya, Japan, Sep. 5–8,
2016).
Zeidler, S., Akutsu, T.: 2016, Wide-Angle Baffles and Length-Sensing
OpLevs for bKAGRA, KAGRA F2F Meeting, (Toyama, Japan, Aug.
25–27, 2016).
Zeidler, S., Akutsu, T.: 2017, Scattering of the ITM and ETM mirrors
and Constraints for the Wide-Angle Baffles in bKAGRA, KAGRA
F2F Meeting, (Niigata, Japan, Mar. 28–30, 2017).
Zenitani, S.: 2016, The Structure of the Diffusion Region in Collisionless
Magnetic Reconnection: Theory, Simulation, and Observation,
Dynamical Processes in Space Plasmas (Isradynamics 2016), (Deadsea, Israel, Apr. 3-10, 2016).
Zenitani, S.: 2016, Dissipation in relativistic Pair-plasma Reconnection:
Revisited, Workshop on Relativistic Plasma Astrophysics, (Purdue
University, IN, USA, May 9–11, 2016).
Zenitani, S.: 2016, Particle Dynamics in the Electron Current Layer
in Collisionless Magnetic Reconnection, Japan Geoscience Union
Meeting 2016, (Chiba, Japan, May 22–26, 2016).
Zenitani, S.: 2016, Nongyrotropic Electron Orbits in Collisionless
Magnetic Reconnection, AGU Fall Meeting 2016, (San Francisco,
CA, USA, Dec. 12–16, 2016).
Zenitani, S.: 2017, Electron Particle Dynamics in Collisionless Magnetic
Reconnection, US Japan Workshop and School on Magnetic
Reconnection (MR2017), (Matsuyama, Ehime, Japan, Mar. 19–23,
2017).

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