COMMISSION J: Radio Astronomy (November 2013 – October 2016)
Edited by Kenta Fujisawa
J1. Introduction
This report presents a summary of Japanese contributions, including those ofinternational collaborations, in the field related to URSI Commission J during the last
three years. It is not intended to be an exhaustive survey of all relevant works. If
important contributions in some field are missing, it is due to the limited knowledge
and effort of the editor. The most important progress of this field is found in ALMA
project which is now operational and some scientific results have been obtained. In thefollowing sections, projects led by National Astronomical Observatory of Japan (NAOJ)
including NRO 45m, and VLBI (Mizusawa VLBI Onservatory), ALMA (Chile
Observatory) are shown. Most of this part is cited from “Annual Report of the National
Astronomical Observatory of Japan, Volume 18.”
J2. Nobeyama Radio Observatory(1) Scientific Studies
Nobeyama Radio Observatory are carrying out the (a) Star Formation Project, (b)Galactic Plane Survey, and (c) Nearby Galaxy Project as legacy projects with the 45-m
telescope. The star formation project and the Galactic plane survey project obtained
scientific data and their results are described below. Research results from open-use
observations are given separately.
(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), C18O (1-0), and N2H+ (1-0). Many cores and clumps have been identified

from structure analysis of these data. We succeeded in finding a protostellar molecular
outflow in the Orion Molecular Cloud data by using existing data taken by BEARS.
(b) Galactic Plane Survey Project (FUGIN: FOREST Ultra-wide Galactic plane survey
In Nobeyama)
We are conducting the highest resolution simultaneous survey to date 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 make maps of the inner Galaxy and the outer
Galaxy including the spiral arms and bar structure. In 2015, we covered areas with 46
and 28 square degrees for a total of 74 square degrees. In the last two years, 115 square1degrees have been mapped. As a result, we have revealed a wide range of molecular
clouds and their fine structures and also found a new cloud-cloud collision system andan interacting region with a supernova.
(c) Nearby Galaxy Project (COMING: CO Multi-line Imaging of Nearby Galaxies)
We started COMING (CO Multi-line Imaging of Nearby Galaxies) in April 2015 tomap more than 200 nearby galaxies in 12CO, 13CO, and C18O J=1-0 emission lines using
FOREST. As of now, mapping observations of more than 40 galaxies are complete.
Among our samples, the precise 13CO/12CO line ratio has been obtained for a barredgalaxy NGC 2903. Excitation analysis revealed that star formation efficiency isdetermined by molecular gas density. In addition, through comparison with archived
data of CO (J=3-2), it became clear that gas content depends on the surface gas density
in dwarf galaxy NGC 2976.
(2) Improvements and Developments
Maintenance of the 45-m telescope, the receiver systems, the cryogenics, etc. were
performed as follows:-

The replacement of the sub-reflector servo system was completed. A plan wasdeveloped for the millimeter wave calibration drive system repairs to be conducted
next year.

-

Surface measurements with the holography system and surface adjustment were
performed. Consequently the surface accuracy of the 45-m telescope was improved.

-Gold foil was put on the 2nd and 3rd mirrors to reduce the loss of the beamtransmission system and decreasing the antenna noise temperature by about 10 K
at 3 mm.

-

Some parts of the new multi-pixel receiver FOREST were replaced and the gainstability and linearity were improved.

-

New AD converters were installed in all the intermediate frequency lines and wereused in open use observations.

-

NRO supported user instruments including the Z45 receiver in the 45 GHz band,the digital spectrometer ROACH, and a 90/150 GHz continuum camera.

J3. Mizusawa VLBI Observatory
NAOJ

Mizusawa

VLBI

Observatory

operates

VLBI

(Very

Long

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 research2

institutes. In the meantime, astronomical research using these VLBI arrays is
conducted mainly on the Galactic structure, celestial masers, AGNs and so on. Using
the unique dual-beam system which is capable of phase referencing by observing twosources simultaneously, VERA conducts high accuracy astrometry of maser sources anddetermines the detailed structure of the Milky Way. In addition to the operation of
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 the East Asian VLBI Network, thelatter of which is a joint VLBI array between the People’s Republic of China, Japan, andthe Republic of Korea.
1. VERAIn FY 2015, the second part of the PASJ VERA special issue has been published as acontinuation from the one in FY 2014. The FY 2015 part included 6 papers, and in total
there have been 13 papers in the VERA special issues in 2014-2015. This has been thethird PASJ VERA special issue after the ones in FY 2008 and FY 2011. As the results ofthe project observations of VERA, the parallaxes and proper motions have beenreported for five galactic star-forming regions, namely, G48.99-0.30, G49.19-0.34, IRAS
20126+4104, IRAS 21379+5106, and IRAS 07427-2400. The last source is located in the
Perseus spiral-arm, and together with the previously published sources associated withthe arm, non-circular motion associated with the Perseus spiral-arm was successfully
detected, showing systematic inward motion toward the Galactic center and lagging
behind the Galactic rotation. It has been shown that the motions can be described wellby a density-wave-type spiral model. This is the first result on the Galactic non-circularmotion based on VERA astrometry, and thus it is one of the milestones of the Galactic
structure study with VERA. Simulation studies have been performed to evaluate theexpected accuracy with which future VLBI astrometry will be able to constrain the
Galactic parameters. It is demonstrated that astrometric measurements for ~300
sources will provide accuracies of a few % for the Galactic fundamental parameters andaccuracies of about 10 % for the parameters associated with the non-circular motion andasymmetric structure, such as spiral arms and/or bar. Astrometric results are also
published for a late-type star U Lyn, and the data are used to calibrate the
Period-Luminosity relation of Mira-type variables based on U Lyn and 8 other sources
for which accurate distances have been measured so far. Other than the Galactic
astrometry, astrometric observations of the core position of TeV blazar Mrk 501 have3

been used to constrain the Lorentz factor of the jet, demonstrating that accurate VLBI
astrometry has a wide range of possible applications other than Galactic structurestudies.
2. JVN (Japanese VLBI Network)
The Japanese VLBI Network (JVN) is operated as a joint research project of NAOJ
and seven universities. JVN consists of VERA and radio telescopes operated byuniversities and research institutes such as ISAS/JAXA, NICT, and GSI. VLBI
observations by JVN were done for 250 hours at 3 bands of 6.7, 8, and 22 GHz in FY
2015. Single Dish Observations related to JVN were also done about 2000 hours at eachtelescope. The major research topics are AGNs, masers, and star forming regions. The
main subjects of research are active galactic nuclei and masers in star-forming regions.
Scientific results obtained with JVN were published as four papers, while ten more
papers reported JVN related scientific studies. Fujinaga et al. (2016) reported theresultsofagamma-ray-emitting-AGN

surveythroughhigh-sensitivity

VLBI

observations. Sugiyama et al. (2016) reported the first results of internal motion in a 6.7
GHz methanol maser source obtained by EAVN (East-Asian VLBI Network) including
JVN. Yonekura et al. (2016) reported on the telescope and observing system of Ibaraki
station. Nine papers including the above four will be published as a special issue of
PASJ in FY 2016. Education is also one of the main aims of university collaboration in
VLBI. Twenty-nine students conducted undergraduate studies using JVN and related
research activities. Sixteen master-course students completed their master’s theses
using JVN, and two Ph.D. students finished their theses using JVN. Many university
students made presentations and talks in research meetings related to JVN.
3. Japan-Korea Joint VLBI (KaVA)
Following the successful opening of KaVA common-use observations and the firstpublications of KaVA papers in FY 2014, the science productivity of KaVA is growing
satisfactorily with the stable array operation throughout FY 2015. As for AGN science,the detailed motions of relativistic jets are now regularly monitored for a number ofsources; three refereed papers were published on several bright blazars including 3C345
during FY 2015. Moreover, our KaVA monitoring of the M87 jet made the first discovery
of a superluminal motion near the black hole. The talk on this result was selected for apress release at the ASJ meeting in March 2016 and was picked up by many media
outlets, returning scientific results from KaVA to the broad general public. Anotherrefereed paper reporting a detailed imaging of SiO masers around the late-type star WX

4

Psc was also accepted. The KaVA Large Program has finally started from late FY 2015,
which aims at performing ambitious, high-scientific impact studies with KaVA byspending a large amount (typically more than 100 hours per year) of the machine time.
Currently three large programs are ongoing, each of which is led by one of the three
KaVA science working groups (AGN, star-forming regions, and late-type stars). Not only
researchers in NAOJ/KASI but also many external researchers (universities inJapan/Korea, Australia, Italy, etc.) are joining these projects. Scientific outcomes basedon these programs will be expected to emerge from the next year.
4. East-Asian VLBI Network (EAVN)
Aiming at expanding the capability of international VLBI over East Asia, thedevelopment of the East-Asian VLBI Network (EAVN) is currently underway as acollaboration between Japan, South Korea, and China. Technical assessment of thearray and test observations are promoted by the Japan-Korea-China joint task force(the so-called Tiger Team), and in FY 2015 a report summarizing the successful
detections of fringes over the last few years was published in the proceedings of aninternational conference (Wajima et al. 2015). Following this success, in FY 2015
further test observations were conducted to evaluate the imaging performance of the
EAVN array at 8, 22, and 43 GHz. Detailed reports of these data will appear next year.
Meanwhile, recently there is a growing discussion toward the future construction of a
new VLBI facility in Thailand (Thailand VLBI Network; TVN). In these circumstances,in FY 2015 a KaVA science workshop was held in Thailand in collaboration with local
astronomers, and discussed the possibility and potential impact of the future extensionof TVN by joining the EAVN. In FY 2015 the annual EAVN workshop was held at
Hokkaido University, and the next meeting in FY 2016 will take place in China.
5. System Development
In 2015, the magnetic tape recorders were replaced with new hard disk drive
recorders, and the Mitaka FX correlator was also replaced with a newly developed
software correlator. The software correlator is located at Mizusawa Campus and is now
in regular operation. The modifications to the KJCC (Korea Japan Correlation Center)system were done based on the feedback from scientific evaluation of the KaVA
observations. Discussions on future development have been done in particular toward
high frequency VLBI and SKA as future extensions of VLBI activities. Basic design anddevelopment were done including a low power consumption optical transmitter,ultrawideband A/D convertors, high accuracy surface reflectors, and balloon-borne radio5interferometry.
J4. Chile Observatory
The ALMA Project is a global partnership of East Asia (led by Japan), Europe, andNorth America (led by the United States) in cooperation with other nations to constructand operate a gigantic millimeter/submillimeter radio telescope deploying 66
high-precision parabolic antennas in the 5000-m altitude Atacama highlands innorthern Chile. ALMA aims to achieve a spatial resolution nearly ten times higher thanthat of the Subaru Telescope or the Hubble Space Telescope. Early scientificobservations with ALMA began in FY 2011 with a limited number of antennas and fulloperation commenced in FY 2012. This report describes the progress of the ALMA
project, which includes the 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. It has been operated to make headway into
submillimeter observations toward the ALMA Era. This report also describes the
progress of the ASTE telescope.
1. ALMA Project Progress
Along with scientific observations, ALMA commissioning observations have been
underway, including polarization tests and solar observation tests. NAOJ staff members
played leading roles in the polarization tests and solar observation tests. As
demonstrated by Koichiro Nakanishi and Hiroshi Nagai for polarization, and Masumi
Shimojo for solar observation tests, East Asian researchers have been taking theinitiative in the international teams. Also Band 10 receivers, the highest observing
frequency band, became available for scientific operations starting from the fourthround of open-use observations of ALMA (Cycle 3) which started in FY 2015. The
sub-components developed by Japan, such as the antennas, correlators, and receivers(Bands 4, 8, and 10), are working properly for the operations.
2. ALMA Open-Use and Scientific Observations
The fourth round of open-use observations of ALMA commenced in October 2015 as
Cycle 3. The Cycle 3 main capabilities include: interferometric observations using
thirtysix 12-m parabolic antennas; Atacama Compact Array (ACA) observations(interferometric observation with ten 7-m antennas and single-dish observations withtwo 12-m antennas); seven frequency bands (Bands 3, 4, 6, 7, 8, 9, and newly-addedBand 10); maximum baselines greatly extended from 1.5 km to 10 km (for Bands 3 to 6),6

5 km (for Band 7) and 2 km (for Band 8 to 10); and polarization for continuum
observations. In response to the Cycle 3 call for proposals, 1578 observation proposals
were submitted from all over the world. This figure exceeded the world’s highest
number of proposals ever recorded, which was submitted to the Hubble Space Telescope.
Such a high submission rate to ALMA shows high expectations for “the global telescope
ALMA” with the potential to contribute to a wide-range of fields such as galaxy
formation, star and planet formation, the Solar System, astrobiology, and interstellar
chemistry. An open call for the fifth round of open-use observations was issued as Cycle
4. The anticipated capabilities of Cycle 4 include: interferometric observations using
forty 12-m antennas; ACA observations (interferometric observation 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), maximum baselines of 12.6 km (for Bands 3 to 6),
6.8 km (for Band 7), and 3.7 km (for Bands 8 to 10). Cycle 4 also provides newopportunities for large programs that require long observations exceeding 50 hours;
millimeter-wavelength VLBI observations; ACA stand-alone mode; solar observations;and polarization for spectral line and continuum observations. The public call for Cycle
4 proposals is set to close at 00:00 JST on April 22, 2016. Cycle 4 is scheduled to start in
October 2016. Open use of ALMA has already produced a number of scientificachievements. This section describes some of them, focusing mainly on East Asian
projects. A research group led by Yoichi Tamura at the University of Tokyo found several
dust clouds with a size of 500 light-years distributed inside SDP.81 through detailed
analyses of the image of the gravitationally lensed galaxy SDP.81 captured byhigh-resolution observations with ALMA and comparison of this image to its
gravitational lens model. The results of their study also indicate the existence of asupermassive black hole over 300 million times more massive than the Sun at thecenter of the foreground galaxy. A research group led by Kyoko Onishi at SOKENDAI(The Graduate University for Advanced Studies) observed the barred spiral galaxy NGC
1097 with ALMA and through a detailed study on the kinematics of molecular gas at thecenter of the galaxy found that this galaxy harbors a supermassive black hole 140
million times more massive than the Sun. This research result is based on the ALMA
observation data obtained within a two-hour observation, which demonstrates theoutstanding capability of ALMA in the mass measurement of supermassive black holes.
A research team led by Hideki Umehata successfully captured a cluster of nine
starburst galaxies in a cluster of young galaxies 11.5 billion light years away from the
Earth (at the center of a “proto-Great Wall” known as the largest structure in the
Universe). This result supports the idea that the proto-Great Wall is the matrix that7

supports the formation of galaxies. This could lead to unveiling the formation process of
starburst galaxies and their subsequent evolutionary process. A research team led by
Yusuke Aso at the University of Tokyo and Nagayoshi Ohashi at NAOJ observed aproto-star called TMC-1A and revealed the movements of the inner rotating gas disk
around the proto-star and the outer gas envelope with the highest accuracy everachieved. The high-sensitivity observations with ALMA made it possible to directly
observe the boundary between the disk surrounding the proto-star and the outerinfalling gas envelope. These results are very important in finding out when the
proto-planetary disk appears in the process of star formation and how it evolves.
3. ASTE Telescope
The ASTE telescope has been operated to promote fullfledged submillimeter
astronomical research in the southern hemisphere and to develop/verify observational
equipment and methods. With the ALMA telescope entering its operation phase in FY
2012, ASTE will be engaged mainly to provide observational evidence for strengthening
ALMA observation proposals and to pursue development for enhancing ALMA’s future
performance. Other than ALMA, there are only two large-scale submillimeter telescopeswith a 10-m-class antenna that can observe the southern sky in the world: one is ASTE
and the other is APEX operated by ESO. Therefore, having ASTE operated by Japan
will be a big advantage in strengthening ALMA proposals and in implementing ourstrategies for further extending the capabilities of observing equipment. Looking to the
future, ASTE is also important since it provides opportunities for nurturing young
researchers who will play key roles in the equipment 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 Radio Telescope. Three public calls
were made in FY 2015 for open-use observation proposals: the first call (2015a) for
spectroscopic observations in 345 and 460 GHz bands was from June to September, thesecond call (2015b) and an additional call for spectroscopic observations only in the 345
GHz band (2015c) from October to December. To render support for researchers
contributing to enhancing the observational performance of ASTE, the Guaranteed
Time Observation (GTO) scheme has been offered since FY 2013. This allows themexclusively to make proposals for the GTO slots. A total of 53 proposals for open-use
observations and GTO slots had been made including 25 for open use and one for GTO
in the first call; 12 for open use in the second call; and 15 for open use in the additionalcall. These proposals were reviewed by the NAOJ Chile Observatory programsubcommittee and 41 proposals were subsequently adopted, including 22 for open use

8and one for GTO in the first call; 11 for open use in the second call; and seven in the
additional call. Open-use observations were carried out from the ASTE Mitaka
operation room, other universities or research institutes between June 8 and December
18, 2015.
J5. 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 theseprojects are attached to the Division of Radio Astronomy, which promotes radio
astronomy research to harmonize these radio astronomy projects. The research themesof the Division of Radio Astronomy are represented by keywords such as Big Bang, early
Universe, galaxy formation, black holes, galactic dynamics, star formation, planetarysystem formation, planets and satellites, the Moon, the evolution of interstellar matter,and the origin of life in the context of the evolution of the Universe. Radio astronomy
unravels mysteries and phenomena in the Universe through radio waves, which areinvisible to human eyes. The detailed research results are reported in each project’s
section and in the research highlights. The Radio Astronomy Frequency Subcommittee
has been established within the division, engaging in discussions on protection against
artificial interference generated by electrical equipment, which causes major obstacles
in radio astronomical observations.
The mission of the Radio Astronomy Frequency Subcommittee is to protect theenvironment 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 the field 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 inwireless communication technologies in recent years, and wireless commercial products
such as mobile phones, wireless LANs, and automotive radars are widely used. The
areas of radio applications will further expand in the future owing to its ubiquitous
nature. But because of its unique capabilities, compatibility among various radio
services, including both active and passive ones, will become a serious issue. Frequency

9

is a finite resource and its sharing is an unavoidable issue. Therefore, further efforts
will be necessary for maintaining the sky free from artificial interference for betterradio astronomy observations.
Radio Astronomy Frequency Subcommittee is to ensure that radio astronomical
observations are free from artificial interference and to raise public awareness of theimportance of the protection activities. Radio astronomical observation does not emit
radio waves; thus, it does not interfere with other wireless communications. A proactive
approach is needed to widely raise awareness of the efforts to protect the environment
for radio observations. Regular explanatory sessions are provided at the Ministry ofInternal

AffairsandCommunications

(MIC)

and

regional

Bureausof

Telecommunications to solicit appreciation of the importance of protecting the field. The
coordination between the community of radio astronomy and commercial wirelessoperators is led by the MIC within Japan and internationally by the International
Telecommunication Union (ITU) Radiocommunication Sector (ITU-R) of the United
Nations. As part of the activities for FY 2015 the Subcommittee took an active role informulating the opinion of the Japanese radio astronomical community (on behalf of theJapanese radio astronomers) in these coordination efforts. The Subcommittee iscomposed of members from NAOJ and representatives of universities and research
institutes in Japan.
J6. Hokkaido University
The radio astronomy research group of Hokkaido University is led by Associate
Professor Kazuo Sorai. They use their own Tomakomai 11m radio telescope andNobeyama 45m radio telescope for the study of Galactic plane survey and the dynamics
of the extra galaxies with molecular lines.
J7. Ibaraki University
The radio astronomy research group of Hokkaido University is led by Professor
Munetake Momose and Associate Professor Yoshinori Yonekura. They use Nobeyama
45m radio telescope, ALMA for the study of star formation with molecular lines.
Moreover, two 32-m radio telescope (Hitachi and Takahagi) are operated by the group
under collaboration with NAOJ. These telescopes are used as elements of the Japanese
VLBI Network, and single telescope for methanol and water maser observations.
J8. Tsukuba University
The radio astronomy research group of Tsukuba University is led by Professor

10Naomasa Nakai. They use Nobeyama 45m radio telescope for the study of galaxies andactive galactic 5 nuclei (AGNs). Tsukuba 32-m antenna for geodetic VLBI owned by the
Geospatial Information Authority of Japan (GSI) is used by Tsukuba group as a radio
telescope.
J9. Institute for Astronomy of the University of Tokyo
The radio astronomy research group of Institute for Astronomy of the University ofTokyo is led by Professor Kotaro Kohno. They use ASTE 10m radio telescope and ALMAfor the study of Highest redshift (sub)millimeter galaxies.
J10. Astro-Chemistry
Professor Satoshi Yamamoto leads the Astro-Chemistry Group in the University ofTokyo. Their research subjects are: Submillimeter-wave and Terahertz Astronomy,
Chemical Evolution of Interstellar Molecular Clouds, Star and Planet Formation,
Development of Terahertz Detectors.
J11. Nagoya University
The radio astronomy research group of Nagoya University is led by Professor Yasuo
Fukui. They use their own NANTEN2 telescope located in the Atacama plateau in
Northern Chile, Nobeyama 45m radio telescope, and ALMA for the study of interstellar
matter and star formation.
J12. Osaka Prefecture University
The radio astronomy research group of Osaka Prefecture University is led byProfessor Hideo Ogawa, Kazutoshi Ohnishi, and Hiroyuki Maezawa. They use theirown 1.85m telescope and SPART 10m telescope at Nobeyama, and Small telescopes in
the Campus of Osaka Prefecture. Their research has wide variety, such as developmentof radio astronomical observation system, molecular clouds and star formation, andplanetary atmosphere.
J13. Yamaguchi University
The radio astronomy research group of Yamaguchi University is led by Professor
Kenta Fujisawa. They use Yamaguchi 32-m radio telescope under collaboration with
NAOJ. Their research focuses on star formation with masers, active galactic nuclei.
Yamaguchi University leads the Japanese VLBI Network.

11J14. Kagoshima University
The radio astronomy research group of Kagoshima University is led by Professor
Toshihiro Omodaka and Toshihiro Handa. They use one telescope of the VERA network,
Iriki 20-m, under collaboration with NAOJ. Their research focuses on the galactic
dynamics, star formation, evolved stars. They lead the SKA Japan consortium. Square
Kilometer Array (SKA) is the world largest radio telescope project planning to constructlarge interferometers in the decade of 2020.

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