PROGRAM

7 years of MAXI : monitoring X-ray transients / Programme

Monday 05 December 2016

7 years of MAXI : monitoring X-ray transients
Monday 05 December 2016
Registration - (09:30-10:00)
Opening remarks - (10:00-10:10)- Presenters: Prof. MATSUOKA, Masaru

Session 1 : Highlights - (10:10-11:30)
Chair : Prof. KAWAI, Nobuyuki

time title

presenter

10:10 MAXI 7 years highlights

Dr. MIHARA, Tatehiro

10:40 MAXI-SSC results in 7 years

Prof. TSUNEMI, Hiroshi

11:00 Discovery of 17 X-ray transients with MAXI/GSC and their nature

Prof. NEGORO, Hitoshi

Lunch & Poster - (11:30-13:30)

Session 2 : Stellar Mass Black Hole - (13:30-15:00)
Chair : Prof. UEDA, Yoshihiro

time title

presenter

13:30 Progress Galactic black hole binaries over the past 7 years: a selection ofrecent results

Dr. RODRIGUEZ, Jerome

14:00 Violent optical variations and correlation with X-ray variability in the 2015
outbursts in V404 Cygni

Ms. KIMURA, Mariko

14:15 Two optical emission components with different variability in V404 Cygni

Mr. TACHIBANA, Yutaro

14:30 Observation of the long-term variability of Cygnus X-1 with MAXI

Ms. SUGIMOTO, Juri

14:45 Accretion flow properties of three MAXI Black Hole candiadtes: analysis with
TCAF solution

Dr. DEBNATH, Dipak

Coffee & Poster - (15:00-15:30)

Session 3 : Low Mass X-ray Binaries - (15:30-17:05)
Chair : Prof. MATSUOKA, Masaru

time title

presenter

15:30 Black holes and neutron stars in Low Mass X-ray binaries

Prof. DONE, Chris

16:00 Spectral states in NS-LMXBs observed with MAXI/GSC and Swift/BAT

Dr. ASAI, Kazumi

Page 1

7 years of MAXI : monitoring X-ray transients / Programme

Monday 05 December 2016

16:20 Overview of spectral change in NS-LMXB

Dr. TAKAHASHI, Hiromitsu

16:50 Unveiling the spectral transition of Aql X-1 from the hard to soft state

Mr. ONO, Ko

Session 4 : GRB - (17:05-18:10)
Chair : Dr. SAKAMOTO, Takanoritime title

presenter

17:05 Short-GRB rate from Yonetoku relation for SGRB and the detectability of GW in Prof. NAKAMURA, Takashi
O2 of aLIGO/aVirgo
17:20 GRB radio view from all angles

Dr. VAN DER HORST,
Alexander

17:40 GRBs with MAXI and CALET

Dr. NAKAHIRA, Satoshi

17:55 POLAR - The gamma-ray burst polarimetry experiment onboard China's TG-2
spacelabProf. ZHANG, Shuang-Nan

Note : 30 min talk = 25 + 5 min discussion / 25 min talk = 20 + 5 min discussion/ 20 min talk = 15 + 5 min discussion / 15 min talk = 12 + 3 min discussion

Page 2

7 years of MAXI : monitoring X-ray transients / Programme

Tuesday 06 December 2016

Tuesday 06 December 2016
Session 5 : MAXI Transients - (09:00-10:35)
Chair : Prof. NEGORO, Hitoshi

time title

presenter

09:00 Quick review of X-ray transientsProf. NEGORO, Hitoshi

09:05 Swift/MAXI transient collaboration: 7 years of success

Dr. KENNEA, Jamie

09:35 On the orbital period of MAXI J1305-704

Dr. SHAW, Aarran

09:50 A multi-wavelength view of jets in accreting binaries

Prof. CORBEL, Stephane

10:20 Novae with super-Eddington luminosities

Prof. SHIGEYAMA, Toshikazu

Session 6 : Superbursts - (10:35-11:25)
Chair : Dr. IWAKIRI, Wataru

time title

presenter

10:35 Understanding superbursts

Dr. IN 'T ZAND, Jean

11:05 MAXI detections of superbursts

Dr. SERINO, Motoko

Session 7 : MAXI Archive - (11:25-11:40)
Chair : Dr. IWAKIRI, Wataru

time title

presenter

11:25 MAXI data archive plan

Prof. EBISAWA, Ken

Lunch & Poster - (11:40-13:30)

Session 8 : Steller Flares - (13:30-14:40)
Chair : Dr. SUGAWARA, Yasuharu

time title

presenter

13:30 X-ray study of stellar flaresProf. TSUBOI, Yohko

13:55 Superflares on Sun-like stars

Prof. SHIBATA, Kazunari

14:25 Transient magnetars and magnetic field evolution of neutron stars

Dr. ENOTO, Teruaki

Coffee & Poster - (14:40-15:10)

Session 9 : AGN - (15:10-16:30)

Page 3

7 years of MAXI : monitoring X-ray transients / Programme

Tuesday 06 December 2016

Chair : Dr. ISOBE, Naokitime title

presenter

15:10 Hard X-ray luminosity function of tidal disruption events: first results from MAXI Mr. KAWAMURO, Taiki
extragalactic survey
15:25 First statistical tests for clumpy-torus models: constraints from RXTE monitoring Dr. MARKOWITZ, Alexof Seyfert AGN
15:55 A Novel view of AGN accretion flows revealed by X-ray and optical monitoring

Prof. MAKISHIMA, Kazuo

16:15 An X-ray spectral variability of fast disk winds in AGN

Dr. HAGINO, Kouichi

Session 10 : Science from Hitomi - (16:30-18:00)
Chair : Prof. MAKISHIMA, Kazuo

time title

presenter

16:30 Science from Hitomi: Introduction

Prof. OHASHI, Takaya

16:35 Hitomi observation of the Perseus cluster - gas motions and resonant scattering Dr. SATO, Kosuke
16:59 Hitomi observation of the Perseus cluster - temperature and elemental
abundances -Dr. NAKASHIMA, Shinya

17:23 Hitomi results of NGC 1275: the origin of Fe-K alpha Line

Dr. NODA, Hirofumi

17:41 Hitomi observation of the supernova remnant N132D in the Large Magellanic
Cloud

Dr. KATSUDA, Satoru

Banquet - Hirosawa Club (18:15-20:30)

Note : 30 min talk = 25 + 5 min discussion / 25 min talk = 20 + 5 min discussion/ 20 min talk = 15 + 5 min discussion / 15 min talk = 12 + 3 min discussion

Page 4

7 years of MAXI : monitoring X-ray transients / Programme

Wednesday 07 December 2016

Wednesday 07 December 2016
Session 11 : Binary X-ray pulsars - (09:00-11:55)
Chair : Dr. MIHARA, Tatehiro

time title

presenter

09:00 Monitoring activities of X-ray binary pulsars with Fermi/GBM

Dr. JENKE, Peter

09:30 Luminosity and spin-up relation in X-ray binary pulsars with MAXI/GSC andFermi/GBM

Dr. SUGIZAKI, Mutsumi

10:00 Monitoring Supergiant Fast X-ray Transients with Swift and XMM-Newton

Dr. BOZZO, Enrico

10:15 MAXI/GSC observation of X-ray outbursts from Be/X-ray binary pulsars

Dr. NAKAJIMA, Motoki

10:40 Cyclotron absorption lines in the era of Suzaku and NuSTAR

Mr. GAURAVA K., Jaisawal

10:55 Indian Astro-sat : results in the first year

Prof. PAUL, Biswajit

11:25 The Hard X-ray Modulation Telescope mission

Prof. ZHANG, Shuang-Nan

11:40 X-ray polarimetry mission PRAXyS

Dr. TORU, Tamagawa

Lunch & Poster Session - (11:55-13:50)
Session 12 : Gravitational wave sources - (13:50-15:40)
Chair : Dr. SERINO, Motoko

time title

presenter

13:50 Advanced LIGO first light: multimessenger astrophysics at the birth ofgravitational-wave observatory

Dr. SINGER, Leo

14:20 Binary black hole remnants of first stars for the gravitational wave source

Dr. KINUGAWA,, Tomoya

14:35 Search for X-ray counterparts of gravitational wave events

Prof. KAWAI, Nobuyuki

14:55 X-ray Transient Localization Experiment aboard a micro-satellite formulti-messenger counterpart search

Mr. SAWANO, Tatsuya

15:10 Einstein Probe -- a small mission to explore the transient X-ray sky

Dr. YUAN, Weimin

Closing remarks - (15:40-15:50)- Presenters: Prof. MAKISHIMA, Kazuo

Note : 30 min talk = 25 + 5 min discussion / 25 min talk = 20 + 5 min discussion/ 20 min talk = 15 + 5 min discussion / 15 min talk = 12 + 3 min discussion

Page 5ORAL
PAPERSOct. 5, 10:10MIHARA, Tatehiro (RIKEN)MAXI 7 Years highlights
MAXI started observation on August 15, 2009. Since then MAXI is monitoring the
X-ray sky for more than 7 years. The light curves of about 350 sources are updated inevery 4 hours or 1 day and open through MAXI homepage (http://maxi.riken.jp).
MAXI s alert on new X-ray transients are sent to subscribers in the MAXI alert mailinglists in 12 seconds as the earliest case. Most of them were followed up by the Swift/XRT
revealing the nature of the source. Seventeen new sources were found by MAXI. Sixof them were new black holes. Soft X-ray flash at an ignition of a nova was detected
for the first time in November 11, 2011. Tidal disruption events have formed a new
category after the discovery of Swift J1644+57.
MAXI catalogs of both GSC and SSC were issued revealing new members of X-ray
emitters in the 21st century. Fluxes of X-ray binaries are monitored continuously recording histories of activities of the neutron stars. Monitoring is used for detailed observations with Suzaku, Chandra and XMM-Newton. Data with uniform quality are used
for power-spectrum-density analysis in AGNs and study of accretion disk instabilities
in NS-LMXB and black hole binaries. Normal and giant outbursts of Be X-ray binaries
are monitored enabling a detailed discussion on the Be stellar disk together with opticalemission-line profile. MAXI detected large flares from blazars as well as those from
active stars, and one-hour lasting superbursts from NS-LMXB. Gamma-ray bursts havebeen detected steadily, whose number reached 85. Still, we have 7 MAXI unidentified
short soft transients (MUSST).
Last year LIGO started operation and found the gravitational wave sources. NICER,an X-ray telescope on the ISS, will be mounted in several months. Together with these
new instruments, MAXI will open new windows to understand the universe further.

Oct. 5, 10:40TSUNEMI, Hiroshi (Osaka university)
MAXI-SSC results in 7 years
MAXI-SSC consists of two sets of CCD camera having a fan-beam collimator to scan
the sky. Its eﬀective energy range is 0.7–7 keV that covers the lower energy band thanthat of MAXI-GSC. So far, we discovered the novae, flares and GRBs. The SSC source
catalog in 2016 contains 170 point-sources. Other than them, we detected extended
sources and a large scale structure in the sky. The North Polar Spur is one of themost prominent soft X-ray features in the sky. This seems to be a part of a large
scale structure in the northern sky in galactic coordinate. We confirmed its spectrum
originated from a thin thermal emission. Although we cannot measure the distance tothe plasma, we measure its intensity, structure and temperature. We will report thesummary of the MAXI-SSC results in this 7 years.

Oct. 5, 11:00NEGORO, Hitoshi (Nihon University)
Discovery of 17 X-ray Transients with MAXI/GSC and their Nature
MAXI newly discovered 15 uncatalogued, and 2 unidentified X-ray novae since 2009in terms of the MAXI/GSC nova-alert system (Negoro et al. 2016). By MAXI and followup observations, especially thanks to rapid Swift/XRT followup observations, thosetransients are found to be 6 black hole candidates, 6 neutron stars including 1 pulsar,
and 1 white dwarf. The nature of 4 transients is still unclear.
In this talk, I review the characteristics and statistics of these X-ray novae by comparison with transients discovered by other all-sky-monitors or X-ray detectors with a wide
field of view. For instance, except for MAXI J1659−152 and MAXI J1910−057, peak
fluxes of the MAXI novae are relatively low and about 100 mCrab. Does this indicatethat MAXI observes distant area in our Galaxy as is expected before the launch? I try
to estimate the distance to the sources using various methods, and answer the above
question.
Possible nature of the unknown/unidentified 4 sources are also discussed. Finally, I
summarize what we have learnt from 7 years transient search by MAXI, and future
expectation.

Oct. 5, 13:30RODRIGUEZ, Jerome (CEA - Astrophysics division)
Progress on Galactic black hole binaries over the past 7 years: a selection ofrecent results
The RXTE era have revolutionized our understanding of X-ray Binaries and Galactic accreting black holes in general by providing systematics survey and monitoringof sources during outbursts. Generic patterns, and global phenomenology of outburst
evolution, coupled with multi-wavelength approach and study of the fast temporal variability have allowed us to discover tight connections between accretion, ejection, andthe presence of variable features with quasi periodicities.
After the end of the RXTE mission, one could have feared a dark age for microquasars.
In particular since 2010, and thanks to survey of the X-ray sky with Maxi, Swift, andsome specific programs with INTEGRAL, black hole binaries have continued to befollowed in a rather systematic way. By pointing these sources in specific states withmore sensitive instrument such as XMM-Newton, Chandra and more recently Nustar,several new results of high importance have been obtained over the past 6–7 years.
In this review I will present a selection of some of these results and will in particularfocus on those that have implied multi-instrumental and/or multi-wavelength observations, and campaigns that usually started with alerts given by large fields of view X-ray
telescopes.

Oct. 5, 14:00KIMURA, Mariko (Kyoto University)
Violent Optical Variations and Correlation with X-ray Variability in the2015 Outbursts in V404 Cygni
V404 Cyg is one of transient black-hole (BH) low-mass X-ray binaries (LMXBs). Thissystem underwent outbursts in June and December in 2015 and showed large-amplitude
and short-term variations in optical wavelengths and X-rays. We performed the optical photometry of the two outbursts and compared them with the X-ray light curves
from Swift/XRT, Swift/BAT and INTEGRAL IBIS/ISGRI. Analyzing the simultaneous optical and X-ray data, we found large-amplitude optical variations with repetitive
patterns (the period: 30 min – 2.5 hours, the amplitude: about 2 mag) at low luminosity (even at one hundredth of the Eddington luminosity) in the June outburst for
the first time among BH LMXBs. Although repetitive variations in BH LMXBs had
been observed only at high luminosity (e.g., GRS 1915+105) and the existing theories
were developing to explain these observations before the outburst, they overturned theconventional idea. The correlation between them and the X-ray variations was good.
With the time lag between them and our multi-wavelengths SED analysis, we demonstrated that the repetitive optical variability was mainly dominated by reprocessing of
X-ray irradiation in the disk (Kimura et al. 2016). Also in the December outburst, therepetitive optical variations were detected in one term. In addition, we found that the
optical variability was positively correlated with the X-ray one in another two terms.
The time lag between them was very small and the relation between the optical and
X-ray luminosity was inconsistent with canonical disk reprocessing. The results suggestthat there is a possibility that the origin of the optical variations was diﬀerent fromthat of the repetitive optical variations (Kimura et al. submitted). In this presentation,
I report the analysis of the simultaneous optical and X-ray light curves and discuss thevarious origins of the optical variations in outbursts in V404 Cyg.

Oct. 5, 14:15TACHIBANA, Yutaro (Tokyo Institute of Technology)
Two optical emission components with diﬀerent variability in V404 Cygni
The nearest black hole binary V404 Cygni (=GS 2023+338) went into an outburst
again on June 15, 2015 after 26 years of quietness. Soon after the notifications by
MAXI and Swift, we started intense observation campaign of this source using the
MITSuME 50cm telescope in Akeno, Yamanashi, and MURIKABUSHI 1.0m Telescopein Ishigakijima Astronomical Observatory.
The spectral variation in the optical band was quite mysterious. The spectral index
between Rc -band and Ic -band was stable over the outburst, whereas that between g′ band and Rc -band varied violently. With the time domain analysis of the multi-color
optical light curves, however, we successfully decomposed optical variations into threecomponents: highly-variable component (HVC), little-variable component (LVC), andstable component. The loci of the LVC in the color-color diagram is consistent with thatof a multi-color blackbody radiation from a standard accretion disk, while those of the
HVC trace that of power-law spectra, possibly represents synchrotron emission from thejet. The observed spectral energy distribution (SED) from NIR to UV is also naturally
well reproduced by a model consisting of a power-law component with a spectral index
α ∼ 0.5 and a multi-color standard accretion disk emission.
Additionally, we found the correlated flux decay in optical and X-ray bands at a highlyvariable phase in MJD 57193. At that time, the extrapolation of the SED of the optical
HVC is roughly agrees with the observed X-ray flux. In the variation, the amplitude in
optical and X-ray was quite diﬀerent; ∼ 10 times in optical and ∼ 1000 times in X-ray,
as reported by previous works (e.g., Kimura et al. 2016). The result of our analysis
naturally explains this situation, since only the HVC is strongly correlating with the
X-ray emission while the LVC and the stable component provide uncorrelated baseline.

Oct. 5, 14:30SUGIMOTO, Juri (RIKEN / Rikkyo university)
Observation of the long-term variability of Cygnus X-1 with MAXI
We studied the long-term X-ray variability of the black hole binary, Cygnus X-1,
using about 6 years of MAXI data from 2009 to 2016, in a high/soft state (HSS) and a
low/hard state (LHS).
We analyzed an aperiodic long-term variation, using Normalized Power Spectrum
Densities (NPSDs), in the frequency range from 10−7 to 10−4 Hz, with 2–4 keV, 4–10
keV and 10–20 keV data. From the comparison with previous works in the frequency
region above 10−3 Hz, it was shown that the NPSD extends with a single index from10−3 to 10−7 Hz in both the LHS and HSS. Such the long-term variation is mostly
caused by power-law component in the energy spectrum. In the LHS, the variability
slightly decreased towards higher energies, and in the HSS, it was found to increasesignificantly with energy.
We also studied the 5.6-day orbital modulation in the LHS and HSS. In both states,
the orbital modulations were seen in the light curves with roughly 4%, except for the 2–4
keV band in the LHS. It is interpreted as the modulation of the power-law component
and can be explained by a scattering by the stellar wind, implying that the stellar windis almost ionized in both states. In 2–4 keV of the LHS, the modulation was larger
than those in other bands. At the superior conjunction of the black hole, we see thegas, which is not fully ionized. These conditions can be explained by an inhomogeneous
stellar wind.
From our results, we propose a new large-scale disk structure, which can explain
the long-term aperiodic variation. In our model, an optically-thin and geometricallythick accretion flow coexists with an optically-thick and geometrically-thin, standard
accretion disk, which is extending up to a large radius of sim 1012 cm, in both states.

Oct. 5, 14:45DEBNATH, Dipak (Indian Centre for Space Physics)
Accretion Flow Properties of Three MAXI Black Hole Candidates: Analysis
with TCAF Solution
Recently after the implementation of Chakrabarti and his collaborators Twocomponent advective flow (TCAF) model into HEASARC’s spectral analysis software
package XSPEC as an additive table model, we found that it is quite capable todescribe the underlying accretion flow dynamics around BHs with spectral fitted
physical parameters. Properties of diﬀerent spectral states and their transitions during
an outburst of a transient BHC are more clear. One can even predict frequencyof the dominating quasi-periodic oscillation (QPO) from TCAF model fitted shock
parameters and even predict the most probable mass range of an unknown BHC from
TCAF fits. This gives us a confidence that the description of accretion process ismore clear than ever before. Recently we studied three Galactic transient black holecandidates (BHCs), such as, MAXI J1659−152, MAXI J1836−194, MAXI J1543−564
with the TCAF solution to study accretion flow properties of these compact objects
during their very first outbursts. We classified entire outbursts of these sources into
diﬀerent spectral states on the basis of nature of variations of TCAF model fitted
physical flow parameters and observed QPOs. Probable mass ranges of these BHCs arealso estimated from our study. Estimation of X-ray jet fluxes during the 2011 outburstof MAXI J1836−194 are also done.

Oct. 5, 15:30DONE, Chris (ISAS/JAXA and University of Durham, UK)
Black holes and Neutron stars in Low Mass X-ray binaries
Black holes and neutron stars both show dramatic spectral and timing evolution as
a function of mass accretion rate. This is seen most clearly in the transient outburstsof these systems, which can be followed with MAXI and other all sky monitors. I
will discuss the similarities and diﬀerences between the neutron stars and black holes,
showing how to fit this together in a picture of a very similar accretion flow with avery diﬀerent boundary condition - an event horizon in black holes, versus a surface inneutron stars.

Oct. 5, 16:00ASAI, Kazumi (RIKEN)
Spectral states in NS-LMXBs observed with MAXI/GSC and Swift/BATThe NS-LMXBs show two kinds of X-ray spectra depending on their X-ray luminosities. In the high luminosity(1037 erg/s) it is dominated by blackbody components, andcalled the soft state. On the other hand, in the low luminosity(5 × 1036 erg/s) it isdominated by a Comptonized component, and called the hard state. The transitions
between the two states were seen in the NS-LMXB transients. This was caused by the
instability in a standard accretion disk.
We define the spectral state with MAXI/GSC (2–10 keV) and Swift/BAT (15–50 keV).
Sensitive observations with GSC-BAT showed outbursts even with small peak luminosities and shorter durations. Such ”mini-outburst” were observed in four sources;
4U 1636−536, 4U 1705−44, 4U 1608−52, and GS 1826−238 (Asai+ 2015). We understand it as a ”purr-type” of disk instability predicted by Mineshige and Osaki (1985).
(The large normal outburst is named as a roar-type.)
There are several atoll NS-LMXBs which are persistent and always in the soft state.
Although the hardness ratio (HR) in GSC-BAT observations is always low, the HR
distributed in two (higher/lower) groups. The higher group contains 4U 1820−30 and
4U 1735−44, while the lower group contains GX 3+1, GX 9+1, GX 13+1, and GX 9+9.
We interpreted the diﬀerence to come from the size of the Comptonized cloud. The highHR was resulted from a large Comptonized cloud, which might be dammed at the Alfven
radius by rather high magnetic fields (Asai+ 2016).
In the brightest NS-LMXB (Z sources), there are three branches; Horizontal Branch(HB), Normal Branch (NB) and Flaring Branch (FB). Although the diﬀerences of HB
and NB in the spectral and timing properties indicated some changes in the geometricalstructure, the physical understanding is still controversial. We suggest that the diﬀerence of HB and NB might be explained by the disk evaporation (Asai+ in preparation).

Oct. 5, 16:20TAKAHASHI, Hiromitsu (Hiroshima University)
Overview of spectral change in NS-LMXB
Neutron Star (NS)-Low Mass X-ray Binaries (LMXBs) are historically divided into twoclasses called Z and atoll sources, according to the shape of their color-color diagrams.
Z sources (including Sco X-1, Cyg X-2, etc.) are always very bright close to Eddington
luminosity, and show three distinct states named as Horizontal, Normal and Flaring
branches (HB, NB and FB). Atoll sources are transient and sometimes switch the states
between low/hard and high/soft states. After the discovery of the bright transient NSLMXB XTE J1701−462, which followed the spectral states of both Z and atoll sources,
it is clear these two types of NS-LMXBs are determined mainly by the mass accretion
rate. However, the physical origins are still unclear how Z sources change the threebranches. In this presentation, I review the current observational results of NS-LMXB
high/soft state, including Z and atoll sources, and explain the detail behaviors of physicalparameters obtained from the spectral analyses.

Oct. 5, 16:50ONO, Ko (The University of Tokyo)
Unveiling the spectral transition of Aql X-1 from the hard to soft state
A ToO observation of the recurrent transient Aquila X-1 was carried out during an
initial rising phase of an outburst on 2011 October 21. It fortunately captured a clear
spectral transition from the hard to the soft state, on a time scale of only 30 ks. During
the transition, spectrum changed from a power-low like shape with a high-energy cutoﬀ,
to that typical in the soft state with more convex shape, resulting in an increase of the
0.8–10 keV XIS 0 count rate by a factor of 3 and an decrease of the 15–60 keV HXD
count rate by about the same factor. All the wide-band spectra during the transition
were successfully reproduced with a model consisting of a multi-color blackbody and aComptonized blackbody, which increased and decreased during the transition, respectively. The model parameters changed continuously from those typical in the hard state
to those typical in the soft state. In particular, the inner disk radius and the blackbody
radius decreased from ∼ 31 km to 18 km and 12 km to 7 km, respectively, accompanied
by a decrease in the coronal temperature from 10 keV to 3 keV. This implies that thecorona shrank towards a closer vicinity of the neutron star. Indeed, by utilizing themeasured coronal optical depth, the corona was confirmed to shrink toward the soft
state, and/or its motion becomes more Keplerian. These results establish the unified
view of LMXBs in the soft and hard states.

Oct. 5, 17:05NAKAMURA, Takashi (Kyoto Univ.)
SGRB rate from Yonetoku relation for SGRB and the detectability of GW
in O2 of aLIGO/aVirgo
Using 8 SGRB with Ep, z and Lp, Tsutsui et al. (2013) obtained Yonetoku relationfor SGRB. Applying this relation to bright BATSE SGRBs, the minimum event rate of−10 events/Mpc3 /yr. Under the assumption of beaming factor of
SGRB is 6.3(+3.1−3.9 ) × 10
100 and 4 times dimmer SGRBs, if 10% of SGRB is NS-BH or 100% is NS-NS, there
is a good chance to observe a few GW events in O2 of aLIGO/aVirgo so that MAXI
might see something at the same time.

Oct. 5, 17:20VAN DER HORST, Alexander (George Washington University)
GRB radio view from all angles
Gamma-ray bursts are among the most extreme objects in the Universe in terms of
the energetics and the physics needed to describe the observed phenomena. They aredetected across the entire electromagnetic spectrum, from low-frequency radio waves tohigh-energy gamma rays. Our current understanding of gamma-ray bursts is based on
multi-wavelength and multi-timescale observations. In this talk I will show the role thatradio observations have played, and will play in the future, in putting together a pictureof the physics behind the observed emission, the progenitors, and their environment. I
will highlight the unique role that radio observations can play in detecting gamma-ray
bursts for which the initial high-energy emission is beamed away from us, so-called orphan afterglows, and the possibilities that several new and upgraded radio observatories
oﬀer to obtain a better understanding of these enigmatic phenomena.

Oct. 5, 17:40NAKAHIRA, Satoshi (Japan Aerospace eXploration Agency)
GRBs with MAXI and CALETMAXI and CALET (CALorimetric Electron Telescope) are wide-field monitors currently operated in the exposed facility of ISS/Japanese Experiment Module (Kibo).
About one-third of the MAXI field of view is simultaneously covered by both HXM(Hard X-ray monitor) and SGM (Soft Gamma-ray monitor) scintillation detectors of the
CALET Gamma-ray Burst monitor (CGBM). They have overlapped energy range withfive scientific instruments; MAXI/SSC (0.7–7 keV), GSC(2–30 keV), CALET/HXM (7–1000 MeV), SGM (50 keV–20 MeV) and CAL (CALorimeter; 1 GeV–10 TeV). Therefore,
MAXI and CALET has a unique capability to observe GRBs with wide energy range
from sub-keV to TeV.
So far, MAXI observed more than 90 GRBs or short X-ray transients in the sevenyears. CGBM detected 38 GRBs in the first year, six GRBs (151225A, 160307A,
160408A, 160709A, 160726A and 160804B) were short burst and another four (160101A,
160107A, 160625B and 160814A) were also detected by MAXI/GSC. In this paper, we
will report systematic analysis of CGBM GRB samples and highlight several events
including simultaneously detected GRBs and a Soft Gamma-ray repeater.

Oct. 5, 17:55ZHANG, Shuang-Nan (Institute of High Energy Physics, China)
POLAR - The gamma-ray burst polarimetry experiment onboard China’s
TG-2 spacelab
On 2016-09-15, the gamma-ray burst polarimetry experiment, POLAR, onboard
China’s Tiangong-2 spacelab has been launched. The main scientific goal of theexperiment is to measure the polarization of gamma-rays from gamma-ray bursts
between 50–200 keV. POLAR will be able to detect about 50 gamma-ray bursts per
year and can measure the polarization with precision of about 10% for the brightest
gamma-ray bursts. POLAR can also detect solar flares and the Crab pulsar andmeasurement their polarization. In this talk I will describe the POLAR instrument
and report some early results.

Oct. 6, 9:05KENNEA, Jamie (Penn State)
Swift/MAXI transient collaboration: 7 years of success
JAXA’s ”Monitor of All-sky X-ray Image” (MAXI) part of the Japanese Experiment
Module on the International Space Station, provides a powerful tool for the discoveryof new X-ray transients in our Galaxy. The localization accuracy of MAXI does not
however allow for identification of sources in crowded fields, or for optical counterparts.
NASA’s Swift is uniquely capable of performing rapid (within hours) observations of
newly reported MAXI transients. In addition Swift’s X-ray Telescope provides a wellmatched field of view of ∼0.2 degrees, similar to that of the localization accuracy of
MAXI in most cases, allowing for easy localization of bright transients. The UV/Opticaltelescope provides both detection of optical counterparts of these transients, and reduces
the astrometry error on XRT positions to as little as 1.5 arc-seconds. Swift’s low overhead observations also allow for short (1 ks) high cadency (every 1–2 days) observationsof these transients in order to sensitively monitor outburst light-curves and spectral
evolution of these transients. We report on 7 years of successful collaboration between
the Swift and MAXI teams on Galactic Transient discovery, and discuss new initiatives
underway at Swift that will improve transient discovery both independently by Swift,
and in collaboration with MAXI.

Oct. 6, 9:35SHAW, Aarran (University of Alberta)
On the orbital period of MAXI J1305−704
MAXI J1305−704 is a candidate black hole X-ray binary discovered by MAXI in
2012. The system parameters are relatively unknown, with no dynamical determinationof the mass of the compact object measured. There have also been several conflicting
measurements of the source’s orbital period, the most recent of which is P=9.74 hours,
based on the observation of deep X-ray dips in the X-ray light curve. We reanalysea 40 ks Suzaku observation of MAXI J1305−704 in order to disentangle the multiple
periodicities previously reported. Using a number of timing analysis techniques, wesuggest that the orbital period is instead ∼5 hours. We also present optical spectroscopyof the source in outburst and attempt to place a limit on the mass of the compact object.

Oct. 6, 9:50CORBEL, Stephane (Univ. Paris Diderot & CEA Saclay & Observatoire de Paris)
A panchromatic overview of accreting binary systems and their associatedrelativistic jets
In the past decade, several considerable achievements have been reached in the fieldof Galactic accreting binary systems, especially in light of the extreme variability of
their relativistic jets. These jets have moved from being considered exotic and rare
abnormalities to being recognized as integral and vital components in the transfer ofenergy and angular momentum.
Although their phenomenology is now rather well established, their emission andcontribution to the total energy budget of microquasars at large (and connexion to
the supermassive black holes) is still the subject of active debates. I will present themost relevant observations concerning our understanding of relativistic jets in accretingsystems, discussing in particular some open issues.

Oct. 6, 10:20SHIGEYAMA, Toshikazu (University of Tokyo)
Novae with super-Eddington luminosities
We are trying to construct a theoretical model describing novae with super-Eddington
luminosities in the context of a steady wind model emanating from the surface of a whitedwarf. The motivation of this work originates from the discovery of a bright transient
event MAXI J0158−744 in the Small Magellanic Cloud by MAXI. We succeeded in
reproducing the peculiar spectrum showing a strong Ne IX emission line at 0.92 keV witha large equivalent width We are trying to construct a theoretical model describing novae
with super-Eddington luminosities in the context of a steady wind model emanatingfrom the surface of a white dwarf. The motivation of this work originates from thediscovery of a bright transient event MAXI J0158−744 in the Small Magellanic Cloudby MAXI. We succeeded in reproducing the peculiar spectrum showing a strong Ne IX
emission line at 0.92 keV with a large equivalent width and the absence of Ne X line at
1.02 keV by assuming a very fast wind accelerated out side the photosphere by a given
luminosity estimated by the MAXI observations (Ohtani et al. 2014). This is in contrast
with the existing nova wind model which assumes acceleration in the photosphere. Thus
we have extended the previous model to include the optically thin region by utilizing aflux-limited diﬀusion approximation (Wada & Shigeyama 2016). Though we can obtainsolutions in which the wind is accelerated outside the photosphere and the resultant
luminosities significantly exceed the Eddington limit, the luminosity cannot be so highas observed. We will discuss possibilities to obtain more luminous solutions compatible
with observed bright events including MAXI J0158−744.

Oct. 6, 10:35IN ’T ZAND, Jean (SRON)
Understanding superbursts
Superbursts were discovered in 2000 with the BeppoSAX Wide Field Cameras. Since
then, several tens of cases have been detected, for instance with MAXI. Superbursts
are carbon copies of ordinary thermonuclear (′ type-′ ) 1-min long X-ray bursts that arefound in many low-mass X-ray binaries, representing unstable thermonuclear burningof accreted hydrogen and helium on neutron stars, except that they are thousand times
longer, more energetic and deeper into the neutron star. Several questions are unresolved
regarding superbursts, for instance: 1) where does the carbon come from that is thought
to fuel them (and related to that: could it not be another fuel?); 2) why are they seen
at low mass accretion rates; 3) what constraint can be inferred about the neutronstar crust? Observational and theoretical studies will be discussed, as well as future
observational requirements and prospects.

Oct. 6, 11:05SERINO, Motoko (RIKEN)MAXI detections of Superbursts
MAXI observed eleven long X-ray bursts, which were observed at least two consecutive
scans, in seven years. We divided them into two classes according to their e-folding decay
time: the bursts with longer e-folding time (> 1 hour) are superbursts, and the others
are intermediate duration bursts. We found possible anti-correlation between the decay
time and the peak flux. Superbursts have low peak fluxes (10–50% of the Eddington
limit) and intermediate duration bursts have the peak fluxes of about the Eddington
limit. MAXI detected superbursts from 1) a bright persistent source (Ser X-1), 2) a
dim persistent source (4U 0614+091), and 3) four transient sources (Aql X-1, SAX
J1747.0−2853, EXO 1745−248, and SAX J1828.5−1037). Two of the superbursts fromtransient sources occurred at the time of very low accretion rate, which may be before theoutbursts. Four out of five intermediate duration bursts had low (< 2% of the Eddington
limit) persistent flux. Four intermediate duration bursts are from ultracompact X-ray
binary. These characteristics are common to the intermediate duration bursts whichwere observed before the MAXI era.

Oct. 6, 11:25EBISAWA, Ken (JAXA/ISAS)MAXI data archive plan
We will describe the MAXI data archive plan.
Currently, daily light curves are created for major known sources, and released fromRIKEN (http://maxi.riken.jp). In addition, the web-based ”on-demand” analysis
tool is available at RIKEN (http://maxi.riken.jp/mxondem), with which MAXI users
can retrieve images, light-curves, spectra and responses for a given region and timeperiod.
At DARTS (http://darts.isas.jaxa.jp), interactive all-sky images will be available in the JUDO2 system (http://darts.isas.jaxa.jp/astro/judo2), not only forthe entire MAXI mission period, but also, yearly, monthly, weekly and daily periods.
Users can superpose MAXI images with other astronomical images and catalogs, andalso easily jump from JUDO2 to the RIKEN on-demand system.
Also, we are developing the full MAXI data archive system, where all the MAXI events
are stored in the standard FITS formats commonly used in high energy astrophysics.
The sky is divided into 768 HEALPIX regions, and daily events from each region is kept
in a single event FITS file. Data analysis can be carried out MAXI specific ftool-liketools, with which users will have full access to the entire MAXI data. We will provide
simple user-friendly scripts which enable users to easily download only the required
event and auxiliary data from DARTS for a given position and time-period, and tohandle the data-sets to extract the data products for further analysis.
The full archive system will be made available from DARTS by the end of 2016. It isalso planned that the full archive system be released from HEASARC, and the MAXI
analysis tools included in HEAsoft.
After the MAXI project is over, the daily light-curves and the on-demand system will
be ported to DARTS. At DARTS, the MAXI data will be permanently archived as well
as JAXA’s other science satellite data.

Oct. 6, 13:30TSUBOI, Yohko (Chuo University)
X-ray study of stellar flares
Since the launch in 2009 August, with the unprecedentedly high sensitivity as anall-sky X-ray monitor, MAXI have caught more than a hundred of huge flares fromstars. Most of them are from cool, active stars (RS CVn systems, an Algol system,dMe systems, a dKe system, Young Stellar Objects). With the total radiative energyof 1034−39 ergs, the MAXI detections have broken the record of the largest flaring
magnitudes in each stellar categories (e.g. ”RS CVn” and so on). The enlarged sample
of intense flares have enabled us to do systematic studies in various viewpoints. One of
the studies is our discovery of a universal correlation between the flare duration and the
intrinsic X-ray luminosity, which holds for 5 and 12 orders of magnitude in the durationand LX , respectively. In this talk, we will review recent studies for flares we obtainedwith MAXI and/or the other X-ray astronomical satellites.
The talk also includes the topic of the MAXI detection of a historically brightest X-ray
flares on the massive star system, Eta Carinae.

Oct. 6, 13:55SHIBATA, Kazunari (Kwasan and Hida Observatories)
superflares on Sun-like stars
Many stars show flares similar to solar flares, and often such stellar flares are much
more energetic than solar flares. The total energy of a solar flare is typically 1029 –1032
erg. There are much more energetic flares (1033 –1038 erg) in stars, especially in youngstars with rapid rotation. These are called superflares. We propose that these stellar
superflares can be understood in a unified way based on the reconnection mechanism
which has been developed to explain solar flares. Recently, it has been revealed thatsuperflares with energy of 1034 –1035 erg (100–1000 times of the largest solar flares) occur
with frequency of once in 800–5000 years on Sun-like stars with slow rotation, which
are similar to our Sun. These superflares are usually associated with large spots witharea A = 103 –105 in unit of one millionth of solar hemisphere, much larger than normal
sunspots (with area A = 100–1000) on the Sun. It has become clear that superflares canoccur on slowly rotating Sun-like stars because very large star spots can be generated
in these slowly rotating stars, though frequency is very small. Hence, the problem
of superflare occurrence becomes dynamo problem; why can a very large star spot be
generated in slowly rotating stars like our Sun?

Oct. 6, 14:25ENOTO, Teruaki (Kyoto University)
Transient Magnetars and Magnetic Field Evolution of Neutron Stars
An increasing number of X-ray outbursts from transient magnetars has changed our
perception about the magnetic field evolution of highly magnetised isolated neutronstars. Magnetar activities, such as short bursts and activated persistent X-ray emission
during outbursts, have been also discovered from high-B rotation powered pulsars (e.g.,
PSR J1119−6127), low-field magnetars (e.g., SGR 0418+5729), and a Compact Central
Object (CCO) 1E 161348−5055 at the centre of the supernova remnant RCW 103. All
these sources exhibited not only a soft-thermal surface emission but also a hard powerlaw component extending above 10 keV, suggesting an unified view of the magnetar (andrelated) classes. Recent observational review will be presented from Swift, INTEGRAL,
Suzaku, and NuSTAR observations with future prospects of the NICER project launchedin 2017.

Oct. 6, 15:10KAWAMURO, Taiki (KyotoUniversity)
Hard X-ray Luminosity Function of Tidal Disruption Events: First Resultsfrom MAXI Extragalactic Survey
We derive the first hard X-ray luminosity function (XLF) of stellar tidal disruption
events (TDEs) by supermassive black holes (SMBHs), which gives an occurrence rateof TDEs per unit volume as a function of peak luminosity and redshift, utilizing an
unbiased sample observed by the Monitor of All-sky X-ray Image (MAXI). On thebasis of the light curves characterized by a power-law decay with an index of −5/3, asystematic search using the MAXI data in the first 37 months detected four TDEs, allof which have been found in the literature. To formulate the TDE XLF, we consider themass function of SMBHs, that of disrupted stars, the specific TDE rate as a function of
SMBH mass, and the fraction of TDEs with relativistic jets. We perform an unbinned
maximum likelihood fit to the MAXI TDE list and check the consistency with theobserved TDE rate in the ROSAT all sky survey. The results suggest that the intrinsic
fraction of the jet-accompanying events is 0.0007%–34%. We confirm that at z ! 1.5
the contamination by TDEs to the hard X-ray luminosity functions of active galactic
nuclei is not significant and hence that their contribution to the growth of SMBHs isnegligible at the redshifts.

Oct. 6, 15:25MARKOWITZ, Alex (Univ. of California, San Diego, Center for Astrophysics and Space Sciences)
First Statistical Tests for Clumpy-Torus Models: Constraints from RXTE
monitoring of Seyfert AGN
We present an analysis of multi-timescale variability in line-of-sight X-ray absorbing
gas as a function of optical classification in AGN to derive the first statistical constraints
for recent clumpy absorbing torus models. Such models represent the paradigm shift
away from the classical ”solid donut” morphology.
Such advances come courtesy of sustained long-term X-ray monitoring; we use the vastarchive of Rossi X-ray Timing Explorer multi-timescale monitoring of dozens of type I
and Compton-thin type II Seyfert AGN. We search for discrete absorption events due
to clouds transiting the line of sight; most of our twelve detected clouds are Comptonthin and are located in the outer BLR or inner dusty torus. We discuss the resulting
implications for cloud distributions in the context of the clumpy-torus models. We
discuss cloud sizes, stability, and radial distribution across a wide range of distances,and explore the exhibited range in density profiles for the highest-quality eclipse events.
We discuss possible connections to the mechanisms that form and launch clouds (e.g.
disk fragmentation). In addition, all observed clouds are sub-critical with respect to tidal
disruption; self-gravity alone cannot contain them. External forces, such as magnetic
fields or ambient pressure, are needed to contain them. Otherwise, clouds must be shortlived. Finally, we infer that the radial cloud density distribution behaves as ∼1/r0.7 ,compatible with VLTI observations.
Our results apply to both dusty and non-dusty clumpy media, and probe model parameter space complementary to that for short-term eclipses observed with XMM-Newton,
Suzaku, and Chandra.

Oct. 6, 15:55MAKISHIMA, Kazuo (RIKEN, Global Research Cluster)
A Novel View of AGN Accretion Flows Revealed by X-ray and Optical
Monitoring
In spite of long studies, the accrete flows in AGNs are not yet well understood, evenin the simplest Type I objects. Big debates continues whether they are similar to theHigh/Soft state of BHBs, where the accretion disk continuing to ISCO is illuminatedby a ”lamppost”-type corona (e.g., Uttely+ 2014), or they are closer to the Low/Hardstate of BHBs wherein the disk is truncated and transforms into a hot coronal flow (e.g.,
Yuan & Narayan 2014).
To settle the above controversy, we performed 1-year X-ray/optical monitoring of
the Seyfert NGC 3516, using Suzaku and 5 Japanese telescopes (Pirka, Kiso Schmidt,
MITSuME, Nayuta, Kanata). The source was in a very faint phase with the Eddington
ratio of < 0.01, and showed tight X-ray vs. optical correlation. Furthermore, X-rays
preceded the optical by ∼2 days, implying that the optical variation is produced when
the X-rays illuminate the accretion disk at a distance of ∼2-light days. This rules out
the High/Soft-state analogy, because an accretion disk with such a low Eddington ratio
would be too cool to emit optical at such a large distance. In contrast, the Low/hardstate analogy can successfully explain the results (Noda et al. 2016, ApJ, 828, 78),
More generally, we have shown, for the first time, that Type I Seyferts have two
distinct X-ray continua (Noda, Makishima+ 14, 13a, 13b, 11). One is a slowly-varying
absorbed hard (photon index∼1.5) power-law, which carried the tight correlation to theoptical in NGC 3516. The other is a fast-varying softer (index ∼2.2) power-law withlow absorption, which emerges at higher Eddington ratios and does not correlate with
optical signals.
Thus, X-ray and optical reverberation can be one of the most powerful methods toclarify the long-sought nature of the AGN engine. This encourages the promotion of ahigh-sensitivity X-ray all-sky monitor.

Oct. 6, 16:15HAGINO, Kouichi (ISAS/JAXA)An X-ray spectral variability of fast disk winds in AGN
Recent X-ray observations of blue-shifted absorption lines revealed an existence ofthe extremely fast disk winds with outflow velocities of ∼0.1-0.3c. Such fast outflows
would have a large impact on the coevolution of black holes and host galaxies since
they are expected to carry a large amount of kinetic energy. One of the common
characteristics of these fast winds is a strong time variability of the absorption feature.
To investigate this variability, we have developed a new X-ray spectral model of the disk
winds, which is generated by 3-dimensional Monte Carlo radiation transfer simulations
on the assumption of the realistic wind geometry. By applying our wind model to themulti-epoch X-ray data of an archetypal wind source PDS 456, we find the variability
in the absorption line is explained by a change of the wind outflowing angle without
any large variability in the mass outflow rate of the wind. This result indicates thatthe fast disk winds are stable and that local hydrodynamic instabilities produce a large
time variability of the absorption line.

Oct. 6, 16:30OHASHI, Takaya (Tokyo Metropolitan University)
Science from Hitomi: Introduction
I will give a short introduction of the science from Hitomi. Overview of results obtained
from 6 targets observed in the orbit will be presented, and detailed reports on individual
sources will follow this presentation.

Oct. 6, 16:35SATO, Kosuke (Tokyo university of Science)
Hitomi observation of the Perseus cluster - gas motions and resonant scattering Hitomi (ASTRO-H) SXS first allow us to investigate fine structures of emission lines
from highly ionized ions with its high energy resolution of ∼5 eV at 6 keV. The line
diagnostics make it possible to measure streaming and turbulent gas motions, which play
key roles for understanding the basic physical properties of the intra-cluster medium(ICM) in galaxy clusters, such as the thermal conductivity and viscosity. Particularlyin the cluster core, resonance scattering should be taken into account when inferring
physical properties from line intensities.
Hitomi SXS finds a extremely quiescent atmosphere in the ICM of the Perseus cluster
core where the gas has a line-of-sight velocity dispersion below 200 km/sec (Hitomi
collaboration, Nature, 2016). Also, the line-of-sight velocity map across the 60 kpc
image of the cluster core shows a relative gradient of 150 ± 70 km/sec. These suggestthat the cluster mass measurement under the assumption of hydrostatic equilibrium
would be little aﬀected by turbulent pressure. On the other hand, the observed line
flux ratio of Fe XXV He alpha resonant to forbidden lines is found to be lower in thecluster core when compared to the outer region, consistent with resonant scattering of
the resonant line and also in support of the low turbulent velocity.

Oct. 6, 16:59NAKASHIMA, Shinya (JAXA/ISAS)
Hitomi observation of the Perseus cluster - Temperature and Elemental
Abundances The unprecedented energy resolution of the Soft X-ray Spectrometer (SXS) aboard
Hitomi has opened up a new frontier for temperature and abundance measurements of
the intracluster medium. We successfully resolve emission lines which are degeneratein CCD spectra, including Ni XXVII Kα and Fe XXV Kβ lines, from the spectrum of
the Perseus cluster. We also detect Cr Kα, Mn Kα, and Fe K-shell lines from quantum
numbers of n > 3. These emission lines provide new insights as follows: (1) We find thatthe abundance ratio of Ni/Fe is ∼1 solar and is significantly smaller than previous results(∼2 solar). The abundance ratios of Cr/Fe and Mn/Fe are also found to be ∼1 solar.
This measurement suggests that both single-degenerate and double-degenerate channels
have contributed to past Type Ia supernovae in this cluster. (2) The observed fluxesof Fe XXV K-shell and Fe XXVI K-shell lines are inconsistent with single-temperaturecollisional ionization equilibrium plasma, suggesting a multi-temperature structure. We
find no prominent features of radiative recombination edges or high-n transition lines,
indicating little contribution of out-of-equilibrium atomic processes (including charge
exchange) to the observed Fe emission. The detailed analysis method and discussion
will be presented.

Oct. 6, 17:23NODA, Hirofumi (Tohoku University)
Hitomi Results of NGC 1275: The Origin of Fe-Kα? LineNGC 1275 is a bright radio galaxy at a center of the Perseus cluster of galaxies, andits radio lobes formed by past jet activity are known to deeply aﬀect the intracluster
medium. Hence, the AGN has been regarded as a promising candidate to study important topics such as the cooling flow problem and how AGN feedback influences clustersof galaxies. In 2016 February and March, Hitomi observed the AGN with the Soft X-ray
Spectrometer (SXS) and Soft X-ray Imager (SXI). We are analyzing the Hitomi data
and archival data of other X-ray satellites, aiming to understand the X-ray emission
mechanism and the structure of the central region in NGC 1275. One of the most important topics related to NGC 1275 is the source of the Fe-Kα? emission line at 6.4
keV. Possible sites of origin include the broad line region, dusty torus, and molecular
clouds outside the AGN. Thanks to the unprecedented energy resolution of ∼5 eV at 6
keV achieved by the SXS, we significantly detected the Fe-Kα? line with an equivalent
width of ∼10 eV, limiting its velocity width to ∼500-1400 km/s (FWHM) for the firsttime ever. Because the velocity width is too narrow to be emitted by the inner part of
the AGN, we can exclude a large contribution of the broad line region. Furthermore,
we performed Monte Carlo simulations calculating the Fe-Kα? intensity from molecular clouds, and found that their contribution is also too small. Thus, the origin of the
Fe-Kα? line from NGC 1275 is likely the dusty torus, possibly showing that the AGN
structure in NGC 1275 is diﬀerent from those in typical Seyfert galaxies, which have
Fe-Kα? velocity widths of ∼2000 km/s.

Oct. 6, 17:41KATSUDA, Satoru (Chuo University)
Hitomi Observation of the Supernova Remnant N132D in the Large Magellanic Cloud
N132D is one of the brightest supernova remnants (SNRs) in the Large Magellanic
Cloud, and has been served as a standard calibration source for modern X-ray astronomy
satellites. Like other satellites, Hitomi observed this SNR to calibrate the soft X-ray
spectrometer (SXS) and the soft X-ray imager (SXI). Unfortunately, just after pointing
to this remnant, an STT anomaly happened, causing an unstable satellite attitude.
Therefore, the SXS was able to catch it in its field of view for only an hour, allowing
us to detect only about 250 counts in the entire energy range. Of these, 16 photons are
identified as Fe He-α lines. After a careful data reduction and calibration, the energiesof the Fe He-α lines are found to be shifted redward by roughly 2000 km/s, suggesting
an asymmetric SN explosion. This result clearly demonstrates the power of the SXS,
and provides us with a good pathfinder for future high-resolution X-ray spectroscopyof extra-galactic and low-surface-brightness SNe with Athena. On the other hand, the
SXI succeeded in observing N132D even after the STT anomaly, thanks to its large fieldof view. Therefore, we obtained a statistically-rich SXI spectrum, from which we see
several emission lines including Fe He-α and Ly-α. The SXI spectrum can be used toconstrain the plasma state of the X-ray emitting gas. We will present the current statusof our analyses and interpretations of the Hitomi observation of N132D.

Oct. 7, 9:00JENKE, Peter (University of Alabama in Huntsville)
Monitoring activities of X-ray binary pulsars with Fermi/GBM
The Fermi Gamma ray Burst Monitor (GBM) is a unique instrument that oﬀers thelargest instantaneous field of view of any hard X-ray instrument currently in operation.
This capability along with excellent timing resolution, makes it very successful at detecting rare transient events as well as providing long integration times for pulsed signal
extraction. Even though GBM has a relatively modest size, we are able to observe a
typical accreting pulsar for over 40,000 seconds each day allowing us to make precise
measurements of the source frequency and pulsed flux for sources with a spin frequency
between 0.001 and 2 Hz. These frequency measurements along with GBM’s excellent
timing capabilities have given us the capability to determine/update orbital ephemerides
for many sources as well as monitor rare torque reversals in persistent (semi-persistent)
sources such as EXO 2030+375. Continuous Time Tagged Event data, available sinceNovember 2012, allows the GBM pulsar monitor to track the frequency of even higher
frequency sources and we plan to make these histories available later this year.
The GBM pulsar monitor consists of two parts: A daily blind search which looks
for excess power in the Fourier spectrum from 15 equally spaced directions along the
Galactic plane plus the directions to the SMC and LMC and a dedicated monitoring
program for 39 sources, in which 36 have been detected including SMC X-3. The
results of the dedicated monitoring program are available online (http://gammaray.
msfc.nasa.gov/gbm/science/pulsars.html) and updated twice a week.
We will present 8 years of accreting pulsar monitoring with Fermi/GBM and show
how Maxi has been an invaluable tool in making the GBM pulsar monitoring programand its sister programs (i.e. the XRB monitoring program) a success.

Oct. 7, 9:30SUGIZAKI, Mutsumi (RIKEN)
Luminosity and spin-up relation in X-ray binary pulsars with MAXI/GSC
and Fermi/GBM
To observationally study spin-period changes of accreting pulsars caused by the accretion torque, X-ray light curves of 12 Be binary pulsars obtained by the MAXI/GSC
all-sky survey and pulse periods measured by the Fermi/GBM pulsar project, both covering 6 years from 2009 to 2015, were analyzed. For this purpose, we selected 12 Be
binary pulsars whose stellar companion is certainly identified by optical observations
and surface magnetic field is determined from the cyclotron resonance scattering feature in X-ray spectra. The obtained luminosity, L, and the spin-frequency derivatives,fdot, during the large outbursts, clearly shows the positive correlation following thetheoretical relation represented by f˙ = KL6/7 , in all the 12 sources. The relative factor
K, derived for each target, is found to agree with that of the disk-accretion model proposed by Ghosh & Lamb (1979) within a factor of ∼3 if the typical neutron-star massof 1.4 solar mass and radius of 10 km are assumed. The dispersion of the ratios of thecoeﬃcient K to the model, which range from ∼0.3 to ∼3, is largely explained by theerrors on the distance estimate. We discuss the implication of the discrepancy in thecoeﬃcient K between the number observationally determined and that calculated fromthe canonical neutron-star parameter.

Oct. 7, 10:00BOZZO, Enrico (ISDC - University of Geneva)
Monitoring Supergiant Fast X-ray Transients with Swift and XMM-Newton
In this contribution, I will present the current status of our long term monitoring program of the Supergiant Fast X-ray transients with Swift/XRT, including an exhaustive
summary of the main findings on this class of extremely variable sources in the X-ray
domain. I will also report on the most recent results obtained through a combined XMM
and NuSTAR long observational campaign on the SFXT prototype IGRJ17544−2619,
highlighting all challenges that do not currently allow us to theoretically interpret the
SFXT phenomenology in a satisfiable way.

Oct. 7, 10:15NAKAJIMA, Motoki (Nihon University)
MAXI/GSC observation of X-ray outbursts from Be/X-ray binary pulsars
MAXI/GSC has been monitoring the X-ray activities of Be/X-ray binary pulsars for 7
years since the MAXI operation started. During this period, over the hundred outbursts
were observed, and ∼50 Atels were issued based on the MAXI/GSC observation data.
So far, two types of the X-ray outbursts (normal and giant) have been observed. The
reports of the onset of the giant outbursts from two sources (GX 304−1 and GRO
J1008−57) led the discovery of the cyclotron resonance features by the Suzaku ToO
observations. The observations of the consecutive X-ray outbursts from A 0535+26 andGX 304−1 found the systematic shift of the outburst peaks. This systematic shift canbe explained by the precessed Be disk model. Comparing with the previous results, wefind that these outburst phase shift rate might depend on the orbital parameters.

Oct. 7, 10:40JAISAWAL, Gaurava Kumar (Physical Research Laboratory)
Cyclotron absorption lines in the era of Suzaku and NuSTAR
Cyclotron resonance scattering features or cyclotron absorption lines are unique features observed in hard X-ray spectra of accretion powered X-ray pulsars with magnetic
field of the order of 1012 G. Detection of these features is a powerful tool and the only
direct method to estimate the magnetic field strength close to the surface of neutronstars. Corresponding to magnetic field of ∼1012 G, the fundamental lines are expected
in 10–100 keV energy range with harmonics expected at multiples of fundamental line
energy. However, we detected first harmonics of cyclotron line at less than twice of thefundamental line energy (∼1.7 times the fundamental line energy) in Be/X-ray binary
pulsar Cep X-4. With the broadband spectral capability of Suzaku and NuSTAR observatories, we have investigated several X-ray pulsars to understand line shape, width,
magnetic field mapping, anharmonicity in the line energies, and luminosity-dependent
properties of cyclotron lines. The results obtained from these works and new detectionof cyclotron line in unknown/ poorly studied sources will be discussed in detail.

Oct. 7, 10:55PAUL, Biswajit (Raman Research Institute)Some early results from Astrosat
Astrosat covers a wide energy band in X-rays from 0.2–150.0 keV and it also has two
UV telescopes. We will show some early results from Astrosat on a variety of objects
and discuss further science prospects with Astrosat and a small satellite mission with aThomson X-ray polarimeter POLIX.

Oct. 7, 11:25ZHANG, Shuang-Nan (Institute of High Energy Physics, China)
The Hard X-ray Modulation Telescope Mission
A dedicated X-ray astronomy satellite, the Hard X-ray Modulation Telescope (HXMT)
will be launched in the spring 2017. HXMT is composed of three sets of collimatedinstruments in 1–10 keV (about 400 cm2 ), 5–30 keV (about 1000 cm2 ) and 20–250 keV(about 5000 cm2 ) respectively. The anti-coincidence detector of HXMT can also be used
as a sensitive gamma-ray burst detector between 300 keV to 3 MeV. In this talk, I will
describe the instrumentation and scientific program of HXMT, including the Galactic
plane scanning survey and monitoring as well as pointed observations of X-ray binaries
and pulsars.

Oct. 7, 11:40TAMAGAWA, Toru (RIKEN)
X-ray polarimetry mission PRAXyS
Polarimeter for Relativistic Astrophysical X-ray Sources (PRAXyS) led by NASA’s
Goddard Space Flight Center is the highly sensitive X-ray polarimetry satellite, recently proposed as a NASA’s small explorer mission. NASA selected the PRAXyS
project for the Phase A study in July, 2015, together with another polarimetry mission Imaging X-ray Polarimetry Explorer (IXPE) led by NASA’s Marshall Space Flight
Center. PRAXyS will observe about 30 stellar objects such as stellar or massive black
holes, highly magnetized neutron stars, supernova remnants, etc. in the first 9 months
after launch with a detectable polarization of down to 1% for a 2 mCrab source with
3.4×106 seconds observation in the 2–10 keV energy band. Japanese contribution to the
PRAXyS mission was approved as a JAXA’s small project in 2016, and NASA’s final
decision will be made in February 2017 for a launch in 2020. At the conference we arepresenting the science cases explored by the PRAXyS mission and readiness of flight
instrumentations, as well as how all-sky X-ray monitoring missions impact to PRAXyS.

Oct. 7, 13:50SINGER, Leo (NASA Goddard Space Flight Center)
Advanced LIGO First Light: Multimessenger Astrophysics at the Birth ofGravitational-Wave Observatory
Advanced LIGO’s direct observation of gravitational radiation from a binary blackhole merger has sent quakes through the physics and astronomy community. In a few
short years, the search for gravitational waves will complete its transformation from anexperimental eﬀort into a new discipline of observational astronomy as we rapidly build
a sample of merging compact binaries. A particularly tantalizing goal is to combine
our new GW observatories with existing electromagnetic ones—uncovering the hostenvironments and formation channels of compact binaries, exposing the mechanism
behind short GRBs, explaining the cosmic inventory of r-process elements, and eventesting if stellar-mass black hole binaries are truly barren of matter and magnetic fields.
I will describe results from LIGO’s first observing run with a special focus on theelectromagnetic follow-up program, which brings together real-time GW data analysis
and 63 groups who are searching for counterparts of LIGO so urces using groundand space-based partner facilities spanning gamma ray, x-ray, optical, infrared, andradio wavelengths, as well as neutrinos. I will discuss the anticipated trajectory of theworldwide GW detector network from the standpoint of multimessenger observations,and I will conclude with some ideas for the future.

Oct. 7, 14:20KINUGAWA, Tomoya (Institute for Cosmic Ray Research)
Binary black hole remnants of First stars for the gravitational wave source
Using our population synthesis code, we found that the typical chirp mass of binary
black holes (BH-BHs) whose origin is the first star (Pop III) is ∼30 M⊙ with the total
mass of ∼60 Msun so that the inspiral chirp signal as well as quasi normal mode (QNM)
of the merging black hole are interesting targets of LIGO,VIRGO and KAGRA (Kinugawa et al. 2014 and 2016). The detection rate of the coalescing Pop III BH-BHs is ∼180 events/yr (SFRp /(10−2.5 M⊙ /yr/Mpc3 ))*([fb /(1+fb )]/0.33)*Errsys in our standard
model where SFRp , fb and Errsys are the peak value of the Pop III star formation rate,
the binary fraction and the systematic error with Errsys =1 for our standard model, respectively. Furthermore, We found that the chirp mass has a peak at ∼30 M⊙ in mostof parameters and distribution functions (Kinugawa et al. 2016). This result predicted
the gravitational wave events like GW150914 and LIGO paper said ’recently predicted
BBH total masses agree astonishingly well with GW150914 and can have suﬃciently
long merger times to occur in the nearby universe (Kinugawa et al. 2014)’ (Abbot et al.
ApJL 818, 22 (2016)). Nakano, Tanaka & Nakamura 2015 show that if S/N of QNM
is larger than 35, we can confirm or refute the General Relativity more than 5 sigma
level. In our standard model, the detection rate of Pop III BH-BHs whose S/N is larger
than 35 is 3.2 events/yr (SFRp /(10−2.5 M⊙ /yr/Mpc3 ))*([fb /(1+fb )]/0.33)* Errsys . Thus,
there is a good chance to confirm the existence of Pop III stars and to check whether
GR is correct or not in the strong gravity region.

Oct. 7, 14:35KAWAI, Nobuyuki (Tokyo Institute of Technology)
Search for X-ray Counterparts of Gravitational Wave Events
The Gas Slit Camera (GSC) of Monitor of All-sky X-ray Image (MAXI) on the ISS
scans most of the sky in the 2–20 keV X-ray band every 92 minutes with the orbital
revolution of the ISS. Thus it can be used to search for an X-ray counterpart without prompt precise location of the GW event if the emission lasts for tens of minutes.
We examined the MAXI/GSC all-sky X-ray images (2–20 keV) obtained in the orbits
preceding and following the gravitational wave event GW150914. In each of the 92min orbits, MAXI/GSC scanned more than 90% of the localization (90% confidence)
regions of the GW skymap. No significant new source was found in these scans withtypical upper limit of about 1 × 10−9 erg/s/cm2 in 2–20 keV. Based on this sensitivity, we argue that MAXI may be able to detect afterglows of short GRBs within the
LIGO/Virgo/KAGRA range for neutron star merger.

Oct. 7, 14:55SAWANO, Tatsuya (Kanazawa University)
X-ray Transient Localization Experiment aboard a micro-satellite for multimessenger counterpart search
Short gamma-ray bursts (SGRBs) are likely caused by the coalescence of double neutron star binary and/or neutron star and black hole binary, and therefore they are
expected to be promising electromagnetic counterparts of GW sources. The joint observation of SGRB and GW, and the identification of the host galaxy and distance ofsuch events will provide not only the definitive observational evidence for the origins
of SGRBs but also the insights to the compact object merger model and the explosion mechanism. However, GW sky location is uncertain by tens or hundreds of square
degrees, which is not well constrained for the eﬃcient follow-up observation with optical/NIR telescopes. Thus, we are developing X-ray imaging detector that has both fine
localization accuracy and wide field-of-view, named Transient Localization Experiment(T-LEX). The energy range, field-of-view, localization accuracy of T-LEX are designed
to be 1 – 20 keV, 1 steradian, and 15 arcminutes, respectively. To achieve such capability, we adopted two sets of 1-dimensional coded aperture imaging system, which
consists of tungsten mask with random pattern of 1-dimensional strip-like apertures andsilicon strip detector with an active area of 50 cm2 for each dimension. T-LEX is plan
to be launched onboard a microsatellite in 2018 – 2019, which are being developed at
Kanazawa University named as Kanazawa-SAT3 , with a designed mission life of morethan 1 year. The objective of the satellite mission is to localize X-ray transients including GW sources and to send real time alerts of X-ray transient information about theposition and the burst trigger time. In this talk, we report the objective, design, andcurrent performance of an engineering model of T-LEX.

Oct. 7, 15:10YUAN, Weimin (National Astronomical Observatories, CAS)
Einstein Probe – a small mission to explore the transient X-ray sky
The Einstein Probe is a small satellite dedicated to time-domain astronomy to monitor
the sky in the soft X-ray band, pursued within the space science programme of theChinese Academy of Sciences. It will enable systematic survey and characterisationof high-energy transients at unprecedented sensitivity, spatial resolution, Grasp andmonitoring cadence. Its wide-field imaging capability is achieved by using establishedtechnology of micro-pore lobster-eye X-ray focusing optics. Complementary to this is
deep X-ray followup capability enabled by a narrow-field X-ray telescope. It is also
capable of fast transient alerts triggering and downlink, aiming at multi-wavelength
followup observations by world-wide community. Its scientific goals are concerned withdiscovering new or rare types of transients, including tidal disruption events, supernova
shock breakouts, high-redshift GRBs, and of particular interest, electromagnetic sourcesof gravitational wave events.

POSTER
PAPERSPoster List
P-01

AXELSSON, Magnus

The broad-band X-ray power spectrum in black hole binaries:
from months to milliseconds

P-02

YAMAOKA, Kazutaka

X-ray monitering of the Galactic microquasar V4641 Sgr

P-03

JANA, ARGHA JIT

Inflow-Outflow Properties of Accretion Disk around MAXI

P-04

KAWASE, Tomofumi

J1836−194 with TCAF Solution during its 2011 Outburst
Improvements of power spectrum analysis of short-term X-ray
variability using MAXI/GSC data
P-05

MASUMITSU, Takahiro

Reinvestigation of the relation between the state transition andthe mass accretion rate in the black hole candidates.

P-06

QIAO, Erlin

The Coupling of a disk corona and a jet for the radio/X-ray
correlation in black hole X-ray binaries

P-07

UCHIYAMA, Hideki

Suzaku Observation of a Diﬀuse X-ray Lobe in the East Sideof SS433

P-08

EBISAWA, Ken

P-09

KITAOKA, Yoshiki

Classification of Hard X-ray Light Curves of Black Hole Binary
Transients
Optical monitoring of the MAXI sources by the optical telescope AROMA-N

P-10

SAKAMOTO, Takanori

The MAXI/GSC X-ray Burst Catalog

P-11

OKADA, Chiho

Hard X-ray study of low mass X-ray binary Sco X-1 with
SuzakuP-12

TANAKA, Koji

Localization of Gamma-ray Bursts with BGO Active Shield of
the Soft Gamma-ray Detector and Hard X-ray Imager onboard
Hitomi

P-13

OHNO, Masanori

Suzaku Wide-band All-sky Monitor view of soft gamma-raytransients

P-14

YAMADA, Yusuke

Energy response function of CALET Gamma ray Burst Monitor

P-15

KAWAKUBO, Yuta

Overview and the first year observation of CALET Gamma-ray
Burst Monitor

P-16

URATA, Yuji

Extremely Soft X-ray Flash as the indicator of oﬀ-axis orphan
GRB afterglow

P-17

FUJIWARA, Taichi

P-18

OHMORI, Norisuke

The first Suzaku/WAM Gamma-ray Burst catalog

P-19

IWAKIRI, Wataru

MAXI/GSC observation of new superburst from Ser X-1

P-20

YABE, Seiya

Suzaku/WAM Hard X-ray Observations of Solar Flares —from

Gamma-ray burst observation for eight and half year by Akeno
MITSuME telescope2005 to 2014

P-21

YABUKI, Ken

An investigation of the X-ray luminosity in quiescent phase forsuperflare stars.

P-22

SASAKI, Ryo

Statistical research of hyper X-ray flares detected with MAXI:a correlation between the quiescent luminosity and the largest
flare luminosity.

P-23

NAKAMURA, YumikoSuperflare star candidates detected by XMM-Newton

P-24

TODA, Koyo

Revisiting the cosmological evolution of X-ray selected blazars
with the Swift/BAT 70-month all sky survey data

P-25

CONNOLLY, Sam

P-26

FATIMA, Siti

Testing Accretion Disc Theory in AGN - X-Ray/Optical Interband Lags in NGC 4395
Variability Analysis of X-ray spectrum of Blazar OJ 287 from
Suzaku/XIS and Swift/XRT (2005–2016)

P-27

MATSUMOTO, Jin

P-28

ITOH, Ryosuke

Synergetic Growth of the Rayleigh-Taylor and RichtmyerMeshkov Instabilities in the Relativistic Jet
Mulit-wavelength observation of blazar Mrk 421 in extreme
X-ray flare

P-29

ISOBE, Naoki

MAXI and AKARI investigation of nearby active galactic nuclei

P-30

SHIKI, Kensei

Kanata optical monitoring of radio galaxy NGC 1275

P-31

SEINO, Manami

X-Ray Spectral Variability of the Narrow-Line Seyfert 1

P-32

MIYAKE, Katsuma

Galaxy NGC 4051 Observed with Suzaku
The new primary X-ray spectral component of IC4329A confirmed with Suzaku and NuSTAR
P-33

SAWADA, Makoto

Atomic data and spectral modeling constraints from highresolution X-ray spectroscopic observations of the Perseus cluster with Hitomi

P-34

NAKAJIMA, Hiroshi

Hitomi Observation of the Highly Obscured High-Mass X-ray

P-35

ISHIDA, Manabu

Calibration status of Hitomi with the Crab

P-36

NAKAZAWA, Kazuhiro

In-flight performance of the Hard X-ray Imager onboard Hit-

Binary IGR J16318−4848

omi
P-37

FUKAZAWA, Yasushi

In-flight performance of the Soft Gamma-ray Detector (SGD)
onboard Hitomi

P-38

OHNO, Masanori

Development and in-orbit performance of all-sky monitoring
function of BGO active shield of the soft gamma-ray detector
onboard Hitomi

P-39

HORI, Takafumi

The MAXI/GSC catalog in the low Galactic-latitude sky

P-40

SHIDATSU, Megumi

MAXI/GSC 7-year all-sky map and studies of large-scale dif-

P-41

SUGIZAKI, Mutsumi

fuse structures
Operation and calibration of MAXI Gas Slit Camera (GSC)
on the International Space Station for over 7 years
P-42

TOMIDA, Hiroshi

The current status of Solid-state Slit Camera aboard MAXI

P-43

FURUSHO, Tae

Energy spectra of bright clusters of galaxies obtained from the
MAXI data archive

P-44

KAWAI, Nobuyuki

iWF-MAXI: Soft X-ray Transient Monitor on the ISS

P-45

SUGITA, Satoshi

Development of the Hard X-ray Monitor onboard WF-MAXI

P-46

NAKANO, Toshio

End-to-End test of the mirror and polarimeter of PRAXyS

P-47

SANTANGELO, Andrea

The enhanced X-ray Timing and Polarimetry mission

P-48

MORI, Koji

A broadband X-ray imaging spectroscopy with high-angularresolution: the FORCE mission

P-49

HAYASHI, Hideki

P-50

HARITA, Shohei

Development of X-ray SOI pixel sensors for future X-ray wide
filed cameras
Micro-satellite for astrometry and photometry of gravitational
wave sources

P-51

YAMAOKA, Kazutaka

P-52

UCHIDA, Nagomi

Development of the Solar Neutron Monitor on the ChubuSat-2
Satellite
Development of an in-orbit radiation environment monitor
CUBES onboard a small satellite MIST

P-53

ONO, Yuki

X-ray emission of the Be star/pulsar system PSR B1259−63
at non-periastron phase

P-54

RODES ROCA, Jose JoaquinLong term variability of Cen X-3 with MAXI

P-55

ISLAM, Nazma

Orbital phase resolved spectroscopy of GX 301−2 with MAXI

P-56

PRADHAN, Pragati

A COMPARATIVE STUDY OF SG-HMXBS AND SFXTSUSING IRON K-ALPHA LINE AS A TRACER

P-57

INOUE, Hajime

Precessions of accretion rings and super-orbital periods

P-58

LAPLACE, Eva

Possible regular phenomena in EXO 2030+375

P-59

SAKAMAKI, Ai

MAXI Observations of Supergiant Fast X-ray Transients

P-60

OHUCHI, Haruka

Gamma-ray observation for PSR J2022+3842

P-61

YONEYAMA, Tomokage

Discovery of keV excess emission in the isolated neutron star

P-62

MORII, Mikio

RX J1856.5−3754
Search for soft X-ray flashes at the ignition phase of opticalnovae using GSC data
P-63

SUGAWARA, Yasuharu

X-ray spectral variability of the colliding wind binary WR140:
the origin of the cool plasma component

P-01
AXELSSON, Magnus (Tokyo Metropolitan University)
The broad-band X-ray power spectrum in black hole binaries: from months
to milliseconds
The X-ray emission from black hole binaries shows variability on timescales frommilliseconds to years. While the power spectrum has been well characterised above∼0.01 Hz for a number of sources, the frequency range below 10−5 Hz is much lessstudied. The monitoring capabilities of MAXI make it a unique tool in such studies.
Combined with RXTE observations, we compare the low and high frequency power
spectrum in hard and soft states of bright sources such as GX 339−4 and Cygnus X-1.
We find the broad-band variability to be more stable across states at low frequencies,and discuss our results in the context of propagating fluctuation models.

P-02
YAMAOKA, Kazutaka (Nagoya University)
X-ray monitering of the Galactic microquasar V4641 Sgr
V4641 Sgr is the black hole (BH) candidate which exhibits a giant outburst with an
X-ray intensity up to 12 Crab on September 1999. Since then, several small outbursts
with 1–100 mCrab level have been observed almost every year. However, it remains
unclear whether this source has typical spectral states such low/hard and high/soft
states seen in BH candidates and what X-ray emission mechanisms are. Large-scale
radio jets have also been observed from this source, hence it is very important source
to study the relation between jets and accretion flows. Since 2008, we have monitored
this source in an outburst with MAXI/GSC and Swift/XRT, and carried out detailed
observations with Suzaku and NuSTAR in 2014. The observed X-ray flux ranges up
to 40 mCrab. The spectra of this source look like high/soft state, and can be well
explained by multi-color disk model with an innermost temperature of 1.0–1.5 keV, but
the innermost radii, 8–21% of Schwarzchild radii, are too small to explain its emission
region and does not keep constant. We also detected iron emission lines at 6.8 keV
due to highly ionized irons from Swift/XRT, NuSTAR, and Suzaku spectra, and firstrevealed the presence of photo-ionized plasma in this source. In this paper, we will
discuss the origin of X-ray continuum and iron emission lines, and similarity to thepeculiar microquasar V404 Cyg.

P-03
JANA, ARGHA JIT (INDIAN CENTRE FOR SPACE PHYSICS)
Inflow-Outflow Properties of Accretion Disk around MAXI J1836−194 with
TCAF Solution during its 2011 Outburst
Galactic black hole candidate (BHC) MAXI J1836−194 was discovered by MAXI/GSC
on 29th August, 2011 at the sky location RA= 18h 35m 43s, DEC= −19deg 19m 12.1s.
We study this BHC during its 2011 outburst using 2.5-25 keV RXTE/PCA archival
data with Two Component Advective Flow (TCAF) solution. From spectral fit with the
TCAF solution, we extracted physical accretion flow parameters, such as, Keplerian diskrate, sub-Keplerian halo rate, shock location, and compression ratio, etc. Low frequency
quasi-periodic oscillations (QPOs) are observed sporadically during entire phase of theoutburst. TCAF model normalization values throughout the outburst are not observedwith in a constant narrow range, a higher values are required to fit spectra, specially inobservations when prominent jets are present. From our spectral study, we estimated
X-ray fluxes from jets. From the nature of variations of accretion rate ratio (ratio of halo
to disk rates) and QPOs (if observed), we have been able to classify entire epoch of theoutburst into two harder spectral state, such as, hard (HS), hard-intermediate (HIMS).
These states are observed in the sequence of HS (Ris.) → HIMS (Ris.) → HIMS (Dec.)→ HS (Dec.). This particular outburst of MAXI J1836−194 could be termed as ‘failed’
outburst, since no observation of soft (SS) and soft-intermediate (SIMS) spectral state
are found during the entire outburst. The reason for that could be the accretion disk isimmersed in the excretion disk of the companion which is a B[e] star.

P-04
KAWASE, Tomofumi (Nihon University)
Improvements of power spectrum analysis of short-term X-ray variability
using MAXI/GSC data
We performed a feasibility study for the detection of short-term X-ray variabilityof black hole candidates using MAXI/GSC data. Power spectrum densities (PSDs)
of bright black hole candidates and neutron star X-ray binaries must provide the information about, for instance, state transitions and quasi-periodic oscillations. There
are two reasons for using MAXI/GSC data. Firstly, MAXI scans the whole sky every
92 minutes, so the probability that GSC can observe new bright transients is higher
than other observatories. Secondly, in case extremely bright sources appear, MAXI canobserve these sources because GSC doesn’t have mirrors to focus X-rays. In contrast
other observatories having mirrors can’t do that for detector saturation. Therefore, thepreparations to analyze short-term variability using MAXI data are needed for upcoming new bright transients as well as black hole candidates. Light curves of individual
sources are, however, much aﬀected by a triangular window function of the eﬀective area
due to the scanning observation. Suzuki (2015) established the method of evaluating
resultant PSDs correctly, and showed its usefulness for short-term X-ray variability of
black hole candidates. We packaged those programs to analyze data more eﬃciently
and improved those to evaluate PSDs more correctly. Although scan duration in theprevious method was fixed to 40 seconds to analyze the minimum duration, we modified
those programs to use data as long as possible (!200 s). In addition, we also modified
those to adapt to not so bright sources by cutting the edges of window function toremove low S/N ratio data, and evaluated its eﬀects in the PSDs analytically. Since theprograms are improved, we must confirm the credibility of these again. Here we present
results of some simulations to verify this improved method, and some examples of the
PSDs observed with GSC.

P-05
MASUMITSU, Takahiro (Nihon University)
Reinvestigation of the relation between the state transition and the massaccretion rate in the black hole candidates.
The state transitions observed in the black hole candidates (BHCs) are thought toresult from changes in the mass accretion rate. Yu et al. (2007) showed that the peak flux
during the low/hard state (LHS) at the beginning of an outburst and the time since theflux peak of the LHS in the decay phase in the previous outburst were linearly related,
and that the peak luminosities of the LHS and those of the following high/soft state(HSS) were also linearly related. Maccarone (2003) demonstrated that the HSS-to-LHS
transition luminosities were 1–4% of the Eddington luminosities.
To verify these relations and to estimate the distance to 6 BHCs discovered by MAXI,
we analyzed MAXI/GSC, RXTE/ASM, and Swift/BAT data of the BHCs GX339−4
and H1743−322 which often exhibited outbursts previously. For MAXI/GSC data, wereevaluated light curves by using the image fit method that takes into account the point
spread function of the detectors (Morii et al. 2016). As a result, we obtained more
continuous and more reliable light curves, especially for the data of H1743−322 near
the Galactic center, influenced by X-ray emission from the Galactic plane.
We could confirm the relation in the HSS-to-LHS transition, but the flux and timeinterval relation and the relation between the peak fluxes in the LHS and the HSS were
not confirmed in both BHCs.

P-06
QIAO, Erlin (National Astronomical Observatories,CAS)
The Coupling of a disk corona and a jet for the radio/X-ray correlation inblack hole X-ray binaries
We interpret the radio/X-ray correlation of LR ∝ L∼1.4
for LX /LEdd ! 10−3 withinX
the framework of a disk corona-jet model, in which the matter in the accretion flow andthe matter in the jet are connected by a parameter, ‘η’, describing the fraction of thematter in the accretion flow ejected outward to form the jet. We calculate LR and LX
for diﬀerent Ṁ , adjusting η to fit the observed radio/X-ray correlation of the black hole
X-ray transient H1743−322 for LX /LEdd > 10−3 . It is found that the value of η forthis radio/X-ray correlation for LX /LEdd > 10−3 , is systematically less than that of thecase for LX /LEdd < 10−3 , which is consistent with the general idea that the jet is often
relatively suppressed at the high luminosity phase in black hole X-ray binaries.

P-07
UCHIYAMA, Hideki (Shizuoka University)
Suzaku Observation of a Diﬀuse X-ray Lobe in the East Side of SS433
Using Suzaku, we observed of a diﬀuse X-ray lobe in the east side of SS433. The
pointing is far away from SS433 by about 35 arcmin and the eﬀective exposure time is
107 ks.
Thanks to the low and stable non-X-ray background of XIS, we obtained a good
spectrum in the 0.5–10 keV band. The spectrum consists of thermal and non-thermal
components. We found that the non-thermal component is not a simple power-law as
it was reported before but it has a cutoﬀ around 8 keV. In addition, the cutoﬀ energy
becomes smaller with the distance from SS433. Probably, this shows synchrotron-coolingprocess of relativistic electrons that were accelerated by the SS433 jet.
From the spatial change of the cutoﬀ energy, we limited that the magnetic filed aroundthe lobe is less than 20 µG assuming the synchrotron cooling. If the magnetic field is
10 µG, our result indicated that the relativistic electrons move with the bulk velocity
of 5% of the light speed.
The details of the analysis and discussion will be shown in our poster.

P-08
EBISAWA, Ken (JAXA/ISAS)Classification of Hard X-ray Light Curves of Black Hole Binary Transients
Black hole binaries emit strong X-rays by releasing gravitational energies throughmass accretion from companions to the black holes. When the mass accretion increases
abruptly, they are observed as black hole transients, which exhibit varieties of durations, amplitudes and time-variations etc., presumably reflecting various aspects of theaccretion processes. However, our understanding of the physical mechanisms behindsuch X-ray light-curve morphology is very limited.
Today, MAXI and Swift, two hard X-ray all sky monitors are operational, and a large
amount of high quality X-ray light-curve data of bright sources are being accumulated.
We have systematically analyzed these hard X-ray light curves of transient black holebinaries taken by Swift/BAT (15–50 keV) and MAXI (3–20 keV), searching for common properties among diﬀerent outbursts. To that end, we have applied a techniquecommonly used in the data analysis, such that “distance” between two light-curves
is defined to quantify their similarities, “tree diagram” is made to classify all the observed light-curves. Consequently, we found the light-curves in 15–50 keV are classified
into major four groups based on their morphologies, while such a classification is notclear in the 3–20 keV light curves. This suggests that the hard X-ray light-curves are
more likely to reflect distinct mechanisms of the accretion processes than the soft X-ray
light-curves. In particular, we have found several intriguing, statistically significant resemblances among in hard X-ray light-curves of two or more outbursts from the same
sources or diﬀerent sources. This suggests that common accretion processes are taking
place in diﬀerent out-bursts even from diﬀerent sources.

P-09
KITAOKA, Yoshiki (Aoyama Gakuinn University)
Optical monitoring of the MAXI sources by the optical telescope AROMA-NMAXI is constantly monitoring variable X-ray sources and measuring the fluxes in
the X-ray bands. Aoyama Gakuin University(AGU) has a small optical telescope
called AROMA-N(AGU robotic monitor for astrophysical objects-narrow field) which
is detected to perform follow-up and coordinated observations of high energy source.
AROMA-N is located on the roof of the building of AGU. This telescope is SchmidtCassegrain type and 30cm in diameter. The German-type equatorial mount, the autofocuser and the filter wheel with the Johnson UBVRI filters are equipped. The typicallimiting magnitude of AROMA-N is 16–17 mag in 60 second exposures. The operation of AROMA-N is fully automated. Since AROMA-N constantly observes the MAXI
sources, we can track the flux variations of the sources both in X-ray and optical bands.
In this paper, we will introduce the importance of simultaneous observations with Xray and optical using the MAXI and the AROMA-N data. We will report the analysis
results and consider the prospects for the future.

P-10
SAKAMOTO, Takanori (Aoyama Gakuin University)
The MAXI/GSC X-ray Burst Catalog
We present the X-ray burst (XRB) catalog based on the MAXI/GSC observations.
Between August 15, 2009 and November 30, 2015 (six years and three months), we
identified 329 XRBs from 24 sources. The majorities of XRBs were detected from H
1636−536 (79 XRBs) and GS 1826−238 (139 XRBs). We compared burst durations,radiation energies and burst frequencies of those XRBs with the persistent fluxes near
the burst, and found relationships among them. We discuss the general picture of XRBs
based on the MAXI/GSC observations.

P-11
OKADA, Chiho (Hiroshima university)
Hard X-ray study of low mass X-ray binary Sco X-1 with Suzaku
Low-mass X-ray binaries, whose luminosity is close to Eddington limit (1038 erg/s),
are called a Z source. It is known that Z sources transit among three states on thecolor-color diagram; Horizontal branch (HB), Normal branch (NB), and Flaring branch(FB). Apart from the thermal emission, the hard X-ray tail in >50 keV from Sco X-1
has been reported by BoppoSAX, RXTE, INTEGRAL satellites. However, detection of
the hard emission relies on the time variability and instrument calibration uncertainties,
and thus the origin of the hard tail is not understood well. We think that clarifying
this phenomenon leads to understanding a physical picture of neutron stars and theirneighboring accretion disk. Since Sco X-1 is the most brightest object in the X-ray band,
it is suitable to examine time variation of the hard tail with three state transitions.
Therefore we performed an observation of Sco X-1 by Suzaku and on March 9–12,
2015. We confirmed that Sco X-1 transited among three states (HB, NB, FB) of Z
sources during the Suzaku observation by making a color-color diagram using XIS andPIN data. Reproducibility of the background model of PIN is not good because thebackground observation was limited due to the electricity shortage of Suzaku aroundthe observation epoch of Sco X-1. Therefore we studied and corrected the backgroundmodel carefully by ourselves. As a result, we found that inverse Compton scatteringof black body seed photons from the neutron star surface can reproduce only less than
50 keV. The hard-tail was more likely to exist above 50 keV with a flux of ∼ 10−10
erg/cm2 /s in 20–200 keV at average. In this paper, we will report the relation between
each state and strength of the hard tail.

P-12
TANAKA, Koji (Hiroshima University)
Localization of Gamma-ray Bursts with BGO Active Shield of the Soft
Gamma-ray Detector and Hard X-ray Imager onboard Hitomi
Gamma-ray bursts (GRBs) are the brightest explosions in the universe. The origin andemission mechanism of bursts whose duration of shorter than 2 seconds are not known
well. The merger of compact objects such as neutron star and black hole is the candidateof the origin of those short GRBs and such compact mergers are known to be a sourceof gravitational waves. Therefore, it is important to observe short GRBs in gammaray energy band and localize it to investigate the association between short GRBs andgravitational waves. Soft Gamma-ray Detector (SGD) and Hard X-ray Imager (HXI)
onboard Hitomi are surrounded by large and thick Bi4 Ge3 O12 (BGO) crystal scintillators
to reduce background. These BGO scintillators act as not only active shield but also allsky monitor, especially for GRBs. Therefore, we estimated the capability of localizationof GRBs with SGD and HXI BGO active shield by using geant4 based Monte Carlosimulation. We developed simulator of SGD and HXI BGO active shield including
mass model of Hitomi and detector parameters which are obtained ground calibration
test using flight model sensors. We made database of detection eﬃciency of GRBs forall 68 BGO units utilizing this simulator. Utilizing this database, we established two
localization methods. One is by utilizing photon counts ratio using only brightest 4
units from diﬀerent shape of crystal, and the other is finding best fit incident angle bycomparing observed photon counts of all 68 units and calculated database. By applying
these methods to actually observed by HXI/SGD BGO active shield, GRB 160324A,
we successfully constrained incident photon direction within 10 degrees uncertainty.

P-13
OHNO, Masanori (Hiroshima University)
Suzaku Wide-band All-sky Monitor view of soft gamma-ray transients
We review results of soft gamma-ray transients observed by the Wide-band All-sky
Monitor (WAM) onboard Suzaku satellite. The WAM had been operated for about 10
years from 2005 to 2015, and observed various types of transients and bright gamma-ray
sources, such as gamma-ray bursts (GRBs), solar flares, soft gamma repeaters (SGRs),
gamma-ray emission from Crab nebula ..etc. Thanks to its very large eﬀective area up to
soft gamma-ray energy band (∼400 cm2 even at 1 MeV), we can detect soft gamma-ray
photons from many objects with good statistics. Especially, detected number of GRBs
is more than 1400, which is comparable detection rate to other GRB instruments. With
those large number of samples, we can discuss many kinds of science topics. For example,
the duration distribution of observed GRBs, timing and spectral properties for short
GRBs, weak GRBs with high redshifts, time-resolved pulses for long GRBs, spectral
properties of solar flares in hard X-ray energy band, and emission mechanism of brightbursts from SGRs. In addition to transient observations, the WAM has the capability
to monitor the bright gamma-ray sources utilizing earth occultation technique. We
successfully monitored some sources such as Crab, Cyg X-1 from 150 to 500 keV energy
band and we can trace the broad-band spectral variability.

P-14
YAMADA, Yusuke (Aoyama Gakuin University)
Energy response function of CALET Gamma ray Burst Monitor
CALorimetric Electron Telescope (CALET) was successfully launched and attachedto the exposed facility of the Japanese Experimental Module called Kibo at the International Space Station (ISS) on August, 2015. CALET started its regular operation
on October 2015. CALET has two scientific instruments: CALorimetor (CAL) and
CALET Gamma-ray Burst Monitor (CGBM). CGBM is specifically designed to observe gamma-ray bursts (GRBs). CGBM has two kinds of scintillation detectors: Hard
X-ray Monitor (HXM) and Soft Gamma-ray Monitor (SGM). The HXM which utilizes
LaBr3(Ce) crystal has the energy range of 7 keV–1 MeV. The SGM uses BGO crystal
and covers 50 keV–20 MeV. We calibrate the energy response function of the CGBM
using the ground and the flight data. The well calibrated energy response function is
crucial for the spectral analysis of GRBs. We constructed the mass model of CALET
using the GEANT4 simulation package. This mass module is used to construct theenergy response function of CGBM. In this paper, we present the current status of theenergy response function of the CGBM. We will explain the development of the CGBM
energy response function. We will also show the spectral analysis results of CGBM
for simultaneously detected bright GRBs by other GRB detectors using our developedenergy response function.

P-15
KAWAKUBO, Yuta (Aoyama Gakuin University)
Overview and the first year observation of CALET Gamma-ray Burst Monitor
CALorimetric Electron Telescope (CALET) was launched by H-IIB/HTV-5 in August19, 2015. CALET Gamma-ray Burst Monitor (CGBM) is the scientific instrument anddesigned to observe a prompt emission of a gamma-ray burst (GRB). CGBM has two
kinds of scintillation detectors; Hard X-ray Monitor (HXM; 7 keV–1 MeV) and Soft
Gamma ray Monitor (SGM; 40 keV–20 MeV).
So far, CGBM has been detected 44 GRBs since October 2015. The GRB detection
rate of CGBM is about 4 GRBs per month. CGBM can detect both long and short
GRBs. Since MAXI and CALET are located at the same platform of International
Space Station, 4 CGBM-detected GRBs were also observed by MAXI (GRB 160101A,
GRB 160107A, GRB 160509A and GRB 160814A). For those GRBs, the MAXI data
provide the X-ray part of the emission. Whereas, the CGBM data cover the hard X-ray
and the soft gamma-ray range of the spectrum. We will report the overview of CGBM
and systematic analysis including temporal and spectral characteristics of the GRBs
detected by CGBM.

P-16
URATA, Yuji (IANCU)
Extremely Soft X-ray Flash as the indicator of oﬀ-axis orphan GRB afterglow
We verified the oﬀ-axis jet model of X-ray flashes (XRFs) and examined a discovery ofoﬀ-axis orphan gamma-ray burst (GRBs) afterglows. The XRF sample was selected on
the basis of the following three factors: (1) a constraint on the lower peak energy of theprompt spectrum Esrc , (2) redshift measurements, obs and (3) multi-color observationsof an earlier (or brightening) phase. XRF020903 was the only sample selected basisof these criteria. A complete optical multi-color afterglow light curve of XRF020903
obtained from archived data and photometric results in literature showed an achromaticbrightening around 0.7 days. An oﬀ-axis jet model with a large observing angle (0.21rad, which is twice the jet opening half-angle, θjet ) can naturally describe the achromaticbrightening and the prompt X-ray spectral properties. This result indicates the existenceof oﬀ-axis orphan GRB afterglow light curves. Events with a larger viewing angle(! 2θjet ) could be discovered using an 8-m class telescope with wide field imagers suchas Subaru Hyper-Suprime-Cam and the Large Synoptic Survey Telescope.

P-17
FUJIWARA, Taichi (Tokyo institute of technology)
Gamma-ray burst observation for eight and half year by Akeno MITSuME
telescope
We report on the observations of early GRB afterglows at Akeno MITSuME Telescopein 2008–2016. We had 29 detections and about 120 upper limits in this period. For
discuss their timing properties and correlations with gamma/X-ray light curves.

P-18
OHMORI, Norisuke (University of Miyazaki)
The first Suzaku/WAM Gamma-ray Burst catalog
The gamma-ray bursts (GRBs) are one of the most powerful explosion phenomena.
Many GRB catalogs have been published to study the origin of the prompt emission sofar, but the physical mechanisms remain unresolved. In order to investigate systematic
properties of GRBs, we are constructing the GRB catalog for GRBs observed by thewide-band all-sky monitor (WAM) onboard the Suzaku satellite. The WAM energy
range is 50–5000 keV, and its on-axis eﬀective area is large in comparison with other
GRB instruments: 800 cm2 at 100 keV and 400 cm2 at 1 MeV. In the first catalog, we
will summarize results from 1464 GRBs detected between August 4, 2005 and December
29, 2010. Ohmori et al. (2016) already reported the duration distributions with two
distinct peaks at 0.38 sec and 19 sec, which confirms the presence of short/hard andlong/soft GRBs. As a next step, we are performing spectral analysis with the threemodels (power-law, power-law with an exponential cutoﬀ, and the Band function) using
412 GRBs localized by Swift/BAT, Fermi/GBM and interplanetary network (IPN).
In this paper, we report on the status of the catalog project, focusing on distributionsof spectral parameters, fluence, and 1-s peak flux.

P-19
IWAKIRI, Wataru (RIKEN)MAXI/GSC observation of new superburst from Ser X-1
A new candidate of superburst was detected by MAXI/GSC data of Ser X-1. Three
superbursts have been observed from this source previously (Cornelisse et al. 2002,
Kuulkers 2009). The new long duration burst occurred on 2011 Dec 6 (MJD 55901).
It rose from persistent flux of 0.15 Crab in 2–10 keV to the observed peak flux of 0.33
Crab. The burst lightcurve shows that the e-folding decay time is 2.3 hours. Since theduration is consistent with superbursts previously observed, we concluded that this is
the fourth superburst from Ser X-1. The recurrence time between the third burst (MJD
54753) and fourth burst is 1148 day. We estimate the alpha of these superbursts (whichis ratio of average persistent flux times recurrence time and burst fluence) and theresult is 1000–10000. From fits of cooling models to superburst lightcurve (Cumming &Macbeth 2004), we found the energy release per unit mass is (1.4–6.5) × 1017 erg/g andthe ignition column depth is (1.7–2.5) ×1012 g/cm2 . These results are consistent withthe the results from the first superburst studied in Cumming et al. 2006. Comparing
these results with previous superbursts from Ser X-1, it suggests that the e-folding timeis negatively correlated with the superburst alpha although there is possibility of missing
superbursts.

P-20
YABE, Seiya (Sitama university)
Suzaku/WAM Hard X-ray Observations of Solar Flares —from 2005 to 2014
Solar flare is the largest explosive phenomenon in the solar system, which suddenly
releases magnetic energy built up in the solar atmosphere through reconnection. The
rate of solar flare is correlated with the solar activity whose 11-year period is wellknown. Solar flare is observed in entire band that we observe. In particular, hard
X-ray radiation is produced by non-thermal electrons accelerated at the magnetic fieldreconnection, although the detailed mechanism of particle acceleration is still in debate.
The Suzaku Wideband All-sky Monitor (WAM) had observed over 700 solar flares in 50
keV to over MeV band through the life of the hard X-ray detector (HXD) from 2005 to
2015. The first catalog was published by Endo et al. (2010). They showed the hard Xray properties of flares in the solar minimum from 2005 to 2009. Following their study,
we carried out systematic spectral analysis of solar flares observed with WAM during
the solar maximum from 2010 to 2014. We recognized no significant diﬀerence between
the solar maximum and minimum in the hard X-ray spectrum, and found following”common” characteristics. First, the hard X-ray flux of each event is well correlatedwith the thermal soft X-ray flux. Second, the spectral slope of the non-thermal hard
X-ray component shows clear correlation neither with event duration nor hard X-ray
flux of each event. In this presentation, we discuss hard X-ray emission mechanism
suggested by these observed properties.

P-21
YABUKI, Ken (Chuo university)
An investigation of the X-ray luminosity in quiescent phase for superflarestars.
Flares which occur on stellar surfaces are caused by the release of magnetic energy.
There are flares with more than 1033 ergs of energy, i.e. at least 10 times larger thanthe maximum solar flare. These flares are called ”superflare”. Maehara et al. (2012)
has searched for superflares on G-type dwarfs using Keplar data in optical band. They
found that slowly rotating stars, with spin period of about 20 days, like the Sun, canshow superflares. They also derived total bolometric energy of superflares and found thelargest values of those for each objects do not show any clear correlation with the periodof stellar rotation. These results indicate diﬀerent trend from that obtained in X-ray
band; Pizzolato et al. (2003) indicates the X-ray luminosity in quiescent phase declines
with increasing rotation periods for the stars with rotation periods of more than 7 days.
With the above background, we have searched for Lxq of superflare stars, using available
X-ray archived data. As the result, we found that 11 stars are in the fields of view of
XMM-Newton and 7 of them are detected. In addition, we confirmed that each of 3 stars
is identified with a source in the ROSAT All-Sky Survey catalog. In consequence, for thestars of which the rotational periods are more than 10 days, each Lxq is larger than thepredicted value from the relation by about an order of magnitude. This is consistent
with the result in optical band (Maehara et al. 2012). We further investigated thecorrelation between Lxq and Emax , and found positive correlation (Emax ∝ L1.2
xq ). This
relation is roughly consistent with that between Lxq and the largest flare luminosity
for each objects in X-ray band (see the poster by Sasaki et al. at this international
conference).

P-22
SASAKI, Ryo (Chuo University)
Statistical research of hyper X-ray flares detected with MAXI: a correlation
between the quiescent luminosity and the largest flare luminosity.
Stellar flares are unpredictable phenomena. It is adequate to survey all-sky for detection of large stellar flares. MAXI is mounted on the Japanese Experiment Module
Exposed Facility of International Space Station. It is designed for monitoring all-sky in
the X-ray band. It observes an area in the sky once per 92 min orbital cycle. MAXI
employs two types of X-ray camera. These are Gas Slit Camera and Solid-state Slit
Camera which cover the 2–30 keV and the 0.5–12 keV energy band, respectively. MAXI
started its operation in 2009 August. Owing to its unprecedentedly high sensitivity as
an all-sky X-ray monitor and its capability of real-time data transfer, we have detected
105 strong flares from 27 active stars (fourteen RS CVn systems, one Algol system, ninedMe systems, one dKe system, one Young Stellar Object, one T-Tauri Star). Theseflares have large X-ray luminosity of 2e30–7e33 erg s−1 in the 2–20 keV band, which canbe high ends of among their own categories. We compared the largest X-ray luminosity for each objects (Lx,f ) and quiescent state X-ray luminosity (Lx,q ). Each Lx,q was
extracted from the ROSAT all-sky survey bright source catalogue (Voges et al. 1999).
Such a statistical study has never been done. As a result, we obtained the correlation of
Lx,f ∝ L0.7
x,q . With the correlation, we can predict the largest luminosity for each stars
from the Lx,q . In this poster, we will report the interpretation of this statistical result.

P-23
NAKAMURA, Yumiko (Department of Physics, Chuo University, )Superflare star candidates detected by XMM-Newton
While superflare surveys on main-sequence stars have been well performed with Kepler
satellite in the optical band (e.g. Maehara et al. 2012), there are few reports in the Xray band. Hence necessity of statistical study in the X-ray band has been enhanced
recently.
We found 23 objects in 2XMMi-DR3 catalog (Dacheng et al. 2012) have the light
curves which resemble those of stellar flares. Among them, we have identified 22 objects
with the stars listed in available optical and infrared catalogs. We made SEDs from theoptical and infrared data, and derived temperatures and spectral types (M type:18, K
type:3, F type:1).
One of the 22 objects is concluded to be a new member of AB Dor moving group, fromthe coordinate and proper motion. The young age of AB Dor (50–120 Myr; Malo et al.
2013) also supports the membership, with the fact that YSOs originate flares frequently(e.g. Imanishi et al. 2003). Assuming that it is in the main sequence phase, we derived
the lower limit of the distance to the star as 77 pc from the apparent magnitude andthe color. With the lower limit and the estimation by Malo et al. (2013) of 7–77 pc,
distance to the star is determined to be 77 pc, and then LX is derived as 1029 ergs s−1 ,well in the range of superflare class.
The lower limits of the distance and Lx for the other 21 objects are also derived withthe same assumption, 10–500 pc and 1026 –1031 ergs s−1 , respectively. Among them, 15
objects have the lower limit of LX of 1028 ergs s−1 , well in the superflare class. Since a
detection of a superflare originated on the main sequence phase is quite rare, at least in
the X-ray band, our sample gives valuable candidates for them.

P-24
TODA, Koyo (Hiroshima University)
Revisiting the cosmological evolution of X-ray selected blazars with theSwift/BAT 70-month all sky survey data
Blazars constitute the most extreme class of active galactic nuclei. Recent multiwavelength observations allow us to understand the emission processes in blazars. In
contrast, the cosmic history of blazars is still veiled in mystery. The keys to understandtheir evolution is the cumulative source count distribution and the luminosity function
with which we are able to obtain the trend of evolution and the peak of blazar formation
epoch in the universe. In this talk, we report our study on the cosmological evolution of
blazars utilizing the 70-month data from the Swift/Burst Alert Telescope (BAT) survey.
Our sample comprises 41 flat-spectrum radio quasars (FSRQs) and 27 BL Lacertae (BLLac) objects. Our sample size is a factor of ∼2 bigger than that of the previous study
with the 22-month Swift/BAT survey data (Ajello et al. 2009). Although Ajello et al.
2009 reported the peak of the FSRQ density at z∼5, we find that the FSRQ density hasa peak around z∼2–3 which is nearly consistent with the study based on gamma-ray
selected FSRQs (Ajello et al. 2012). Furthermore, we will discuss prospects for blazar
detectability by future X-ray survey missions such as iWF-MAXI.

P-25
CONNOLLY, Sam (University of Southampton)
Testing Accretion Disc Theory in AGN - X-Ray/Optical Interband Lags in
NGC 4395
Measuring time lags between the X-ray and UV/optical variations in AGN is a powerful tool in determining both the emission mechanisms in these bands and the geometry of
the environment close to the black hole. Previous observations suggest that UV/opticalvariability usually lags X-ray variability, implying that the UV/optical variations result from reprocessing of the X-rays by the accretion disc. Recent Swift observationsof the 4 × 107 M⊙ AGN NGC 5548 confirm definite UV/optical lags which are consistent with reprocessing in a disc, however the lag is larger than expected from a standard
Shakura-Sunyaev disc model. In order to properly test our understanding of disc models,
it is vital to make similar lag observations of AGN of diﬀerent masses. Here, we report
XMM-Newton and ground-based optical observations of the low mass (3×105 M⊙ ) AGN
NGC 4395. We find UVW1 and g-band lags with respect to the X-rays of ∼450 s and800 s. We report the results of physical modelling of the lags according to the standard
Shakura-Sunyaev disc model, which imply that, unlike NGC 5548, the reprocessing in
NGC 4395 appears to be consistent with this model.

P-26
FATIMA, Siti (Department of Astronomy, Institut Teknologi Bandung)
Variability Analysis of X-ray spectrum of Blazar OJ 287 from Suzaku/XIS
and Swift/XRT (2005–2016)
Blazar OJ 287 is known to exhibit periodic outburst from optical observations. A
model of Binary Supermassive Black Holes (SMBHs) in the center of OJ 287 is used to
explain the phenomenon of 12 years periodic optic outburst. X-ray observations also
confirmed outbursts of OJ 287 in the X-ray band. X-ray spectra of OJ 287 from X-ray
observation in 2005 to 2016 were analyzed to determine the variability in X-ray. Spectral
data are obtained from X-ray Imaging Spectrometers (XIS) from Suzaku mission in
observation years of 2007 and 2015. Also obtained from X-ray Telescope (XRT) mission
from Swift in observation period since May 2005 to March 2016. Energy interval of
the X-ray spectrum is 0.4 – 10 keV for Suzaku/XIS and 0.3 – 7 keV for Swift/XRT.
The data are divided into several non-outburst and outburst data groups. In general
power law model is the best model and it is also confirmed that the X-ray spectra of
OJ 287 during that period exhibit fluctuation in photon index value, Γ. Variability ofthe value of Γ indicates that there is evolution of the X-ray spectrum of OJ 287 during
non-outbursts time and also during transition between non-outburst and outburst phaseand vice versa. Diﬀerent values of Γ are also found during diﬀerent outburst phases.
In general the derived values of Γ are in agreement with the inverse compton model(Γ ∼1 – 2) in contrast with the synchrotron model (Γ ∼2 – 3). We also found that Γ
increases as the flux increases as opposed to that of synchrotron model. In addition,
X-ray luminosity of OJ 287 shows fluctuation within ∼ 1 × 1011 ≤ L⊙ ≤ 1 × 1012 .

P-27
MATSUMOTO, Jin (RIKEN)
Synergetic Growth of the Rayleigh-Taylor and Richtmyer-Meshkov Instabilities in the Relativistic Jet
The relativistic jet is ubiquitous phenomenon among astrophysical systems consistingof a compact object surrounded by an accretion disk, e.g., active galactic nuclei, microquasars, and the central engine of gamma-ray bursts. The dynamics and stabilityof the relativistic jet is important in order to understand the emission properties of thejet. The radial oscillating motion of the jet is naturally excited due to the pressuremismatch between the jet and surrounding medium, that is, cocoon when the jet propagates through an ambient medium. In the rest frame of the decelerating jet interface
that expands radially, an eﬀective inertia force acts on the interface and is directed outward. Therefore the jet medium is on top of the cocoon medium in the eﬀective gravity
in this frame and the Rayleigh-Taylor instability is expected to grow at the interface.
We investigate the growth of the Rayleigh-Taylor instability at the interface of the jet
using three-dimensional hydrodynamic simulations. The propagation of the relativistic
jet that is continuously injected from the boundary of the calculation domain into a
uniform ambient medium is solved. We find that the interface of the jet is deformed bya synergetic growth of the Rayleigh-Taylor and Richtmyer-Meshkov instabilities regardless of the launching condition, such as the specific enthalpy of the jet or the eﬀective
inertia ratio between the jet and ambient medium. The material mixing between the
jet and external medium due to these instabilities causes the deceleration of the jet.

P-28
ITOH, Ryosuke (Tokyo Institute of technology)
Mulit-wavelength observation of blazar Mrk 421 in extreme X-ray flare
Blazars are highly variable active galactic nuclei that can be detected for all wavelengths and thought to have relativistic jets. Blazar Mrk 421 exhibited extreme X-ray
flares in 2010. We performed optical photopolarimetric follow-up observations using
the Kanata telescope. In 2010, the variability in the X-ray band was significant, while
the optical and ultraviolet (UV) flux decreased gradually. Polarization properties also
exhibited unique variability in 2010, suggesting the presence of systematic component ofpolarization and magnetic field alignment for the emergence of a new polarized emission
region. The results revealed diﬀerent behaviors in terms of spectral evolution and suggested diﬀerent variability mechanisms between 2010 and 2011. In 2010, the radiation
was likely the result of energy injection into the emitting regions with an aligned magnetic field. In contrast, in 2011 the superposition of diﬀerent emission regions may havecontributed to the low degree of observed polarization. It also implies that high-energy
electron which were not accelerated to ultra-relativistic velocities were injected in 2011.

P-29
ISOBE, Naoki (Tokyo Institute of Technology)
MAXI and AKARI investigation of nearby active galactic nuclei
X-ray and infrared properties of nearby active galactic nuclei were studied with MAXI
and the Japanese infrared observatory AKARI, respectively. In the second release of
the MAXI all-sky X-ray source catalog, 100 non-blazar-type active galactic nuclei, including 95 Seyfert galaxies and 5 quasars, are listed. They are composed of 73 type-1
and 27 type-2 objects. The AKARI all-sky survey point source catalog was searched fortheir mid- and far-infrared counterparts at 9, 18, and 90 micron. As a result, 69 Seyfert
galaxies in the MAXI catalog (48 type-1 and 21 type-2 ones) were found to be detectedwith AKARI. The X-ray and infrared luminosities of these objects and their color information were investigated. When the canonical photon index, 1.9, of the intrinsic
X-ray spectrum of the Seyfert galaxies was adopted, the absorption column density wasestimated from the X-ray hardness ratio between the 3–4 and 4–10 keV ranges obtainedwith MAXI. After the absorption correction based on the estimated column density, thewell-known X-ray-to-infrared luminosity correlation was confirmed in the Compton-thinregime. In contrast, NGC 1365, only one Compton-thick object in the MAXI catalog,
was found not to follow the correlation in the sense that this object exhibits a significantly lower X-ray luminosity by nearly an order of magnitude. It was verified that
Compton-thick objects are eﬀectively picked up by using the relation between the X-ray
hardness below 10 keV and X-ray-to-infrared color. The diﬀerence in the infrared colors
between the type-1 and type-2 Seyfert galaxies were briefly investigated from the pointof view of the unified picture of active galactic nuclei.

P-30
SHIKI, Kensei (Hiroshima University)
Kanata optical monitoring of radio galaxy NGC 1275
NGC 1275 is a radio galaxy, located at the center of Perseus cluster. The multiwavelength spectrum from radio to gamma-ray of NGC 1275 is similar to that of blazars,
and it shows a variable gamma-ray activity. NGC 1275 showed broad emission lines
in optical band and a Fe-K line in X-ray band which are similar to Seyfert galaxies.
Therefore emission of accretion disk dominates in optical and X-ray bands. In previous
works (e.g., Yamazaki et al. 2013), there was no evidence about time variability in the
optical bands from 2010 to 2011, and X-ray bands from 2006 to 2011. On the other
hand, Aleksic et al. (2014) showed a variability in gamma-ray and optical bands by
the data of MAGIC between October 2009 and February 2010, Fermi-LAT and KVA in
between and August 2010 and February 2011. In their paper, optical variability was also
reported. Fukazawa et al. 2016 (astrp-ph) has reported gradually brightening of NGC
1275 in X-ray correlated with gamma-ray activity from 2013 to 2014. Based on theseresults, we expect a jet origin brightening in optical band during the same time period.
We performed optical and near-infrared photometry using HONIR installed on the 1.5
m Kanata telescope since February 2015. Furthermore, we analyzed X-ray archival
public data of XRT onboard the Swift satellite, and also investigated time variability
correlation between X-ray and optical bands.

P-31
SEINO, Manami (the University of Tokyo)
X-Ray Spectral Variability of the Narrow-Line Seyfert 1 Galaxy NGC 4051
Observed with Suzaku
Time resolved X-ray spectra study of Seyfert 1 galaxies have shown that it consists ofa highly time variable (∼10 ks) soft (photon index Γ ∼ 2.2) power-law (PL) component,a less variable (∼months) reflection component with Iron K-line and Compton hump,
and another hard PL component, presumably originating from another hot corona (e.g.
Noda+ 2013). In this work, we investigated if the three-components view can be appliedalso to narrow-line Sayfert 1 galaxies (NLS1s), whose black holes (BHs) are less massive,and have higher Eddington ratio and fast (∼100 s) time variability.
NGC 4051 is a near-by (redshift of 0.0024; Brinkmann+ 1995) NLS1. It has a 1.7 ×
106 M⊙ BH (Denney+ 2009) and high X-ray flux of ∼ 2 × 10−11 erg cm−2 s−1 at 2–10
keV, and the intensity varied by a factor of 2 within 500 s. Therefore, it is one of
the best targets for our study. we observed the source two times with Suzaku in 2008
November, with a two-weeks interval.
Based on 500 s bin light curve at 2–10 keV made from the XIS, we obtained two
spectra of higher-/lower-than-average count rate periods, and generated a diﬀerence
spectrum representing the fast-time-variable component. Both observations show soft
PL-like spectra with Γ ∼ 2.2. On the other hand, a diﬀerence spectrum between thetwo observations, which are 2 weeks apart, shows a hard X-ray hump in addition to the
PL continuum below 10 keV.
These properties can be understood well in the three-spectral-components view. We
investigated three candidates as the additional hard component: another primary component, partial covering absorption of the Γ ∼ 2.2 primary component, and relativistically smeared reflection. While all three models explained the time-averaged spectra
well, lack/existence of the hard X-ray hump in diﬀerence spectra of 500 s / 2 weeks,
respectively, suggests that the idea of slowly variable another PL is preferable.

P-32
MIYAKE, Katsuma (The University of Tokyo)
The new primary X-ray spectral component of IC4329A confirmed with
Suzaku and NuSTAR
X-ray spectra of active galactic nuclei (AGNs) were so far considered to consist of asingle power-law (PL) like primary continuum, and its reflection component accompanied by an FeKα line. However, this assumption was model-dependent, and was subject
to ambiguities of how to model their relatively featureless spectra. Noda et al. (2011,2013, 2014) developed a method that can decompose AGN spectra model-independently
using time-variability, and discovered that two diiferent primary components coexist inspectra of some Seyfert 1 AGNs. We applied the spectral decomposition method to thebright and highly-variable Seyfert 1 AGN, IC4329A. This AGN was observed in 2012
August simultaneously with Suzaku and NuSTAR. The source was detected in 2–70 keVwith 2–10 keV flux of 1e−10 erg cm−2 s−1 , and the source intensity changed by a factorof 1.5 within the observation. Using the Noda’s method, the time-averaged Suzaku and
NuSTAR spectra (3–70 keV) were consistently decomposed into a fast variable continuum and another slowly-varying component. While the former can be modeled as a PL
with photon index Γ = 2.1, the latter was reproduced only when a strongly-absorbed
hard (Γ = 1.4) PL was added to the reflection.
In terms of its variability and spectral shape, the harder PL cannot be a partiallyabsorbed part of the Γ = 2.1 PL, nor relativistic reflection. Instead, it is considered
as an additional primary X-ray component from this AGN. By combining Suzaku and
NuSTAR, the presence of this new PL component and its interpretation as a new primaryemission have been reinforced than in the case of using only the Suzaku data (Miyake etal. 2016). Considering similar results on other Seyfert 1 AGNs (Noda et al. 2011, 2013,2014), we conclude that Seyfert 1 AGNs have multiple Comptonized X-ray radiation,in contrast to the previous popular view.

P-33
SAWADA, Makoto (Aoyama Gakuin University)
Atomic data and spectral modeling constraints from high-resolution X-ray
spectroscopic observations of the Perseus cluster with Hitomi
High-resolution X-ray spectroscopy is a key to understand nature of cosmic plasmas, as
it provides direct measurements of temperature and velocity structures, chemical abundances, and charge-state distributions. It also opens a window for new spectral featuresthat reflect non-equilibrium phenomena or interactions with environments. Plasma
codes are indispensable to carry out high-resolution spectroscopy as any spectral analysis uses a plasma code to derive physical parameters. Thus, accurate atomic databaseand emission models, and appropriate numerical and statistical treatments are needed
to minimize systematic errors originating from plasma codes. The first high-resolution
X-ray spectrum of the Perseus cluster has been obtained with the Soft X-ray Spectrometer on the Hitomi X-ray satellite. It covers major spectral features in 2–9 keV, including
K-shell emission lines of abundant elements Si through Ni. The Hitomi spectrum canbe used for the first practical benchmark of plasma codes.
The atomic team in the Hitomi science working group is working on this with aclose collaboration with other teams analyzing the Perseus data. One of our purposes
is to evaluate systematic uncertainties in calculations of spectra and their impacts onderiving physical parameters. Even with the relatively simple plasma condition of the
Perseus cluster, roughly a 4-keV plasma at collisional ionization equilibrium, many
diﬀerences have been identified between codes developed by diﬀerent groups. This
clearly shows the need of further developments on plasma codes, including feedbacks
from ground plasma experiments, for existing Hitomi data and future high-resolution
X-ray spectroscopy missions. Another purpose is to investigate possibilities to detect
new spectral features, for instance charge-exchange emissions or characteristic emission
line ratios due to interactions with non-thermal electrons. In this presentation, a current
status of our activity will be reported.

P-34
NAKAJIMA, Hiroshi (Osaka University)
Hitomi Observation of the Highly Obscured High-Mass X-ray Binary IGR
J16318−4848
IGR J16318−4848 is a highly absorbed X-ray source discovered by INTEGRAL. The
X-ray spectrum is characterized by a strong Fe absorption edge and is dominated by
Fe Kα, Kβ, and Ni Kα fluorescence emission lines. The lines as well as the continuum
vary on time scales of thousands of seconds, corresponding to an emitting region of
about 1013 cm. The optical/near-infrared (NIR) counterpart exhibits less absorption
than that measured in the X-ray band, which implies that the absorbing material isconcentrated around the compact object. The NIR spectrum also suggests the counterpart is a supergiant B[e] star. The source is thus classified as a high-mass X-ray binary
system. It was observed by Hitomi from March 10th to 14th, just after the startup of
the Soft X-ray Spectrometer (SXS), the Soft X-ray Imager (SXI), and the Hard X-ray
Imager (HXI). Because the observation was performed before optimizing the attitude
matrices of the star trackers, the source was outside of the field of view (FoV) of the
SXS for most of the observation and only the outskirts of the point spread functionof the Hard X-ray Telescopes were within the FoV of the HXI. On the other hand,
thanks to the large FoV of the SXI, we successfully obtained a CCD spectrum with aneﬀective exposure time of 147 ks. The X-ray emission exhibits time variability in termsof flux and spectral shape as seen in the previous observations by XMM-Newton andSuzaku. We report the characteristics of the long-term variability of this source since
its discovery. We also show the possible X-ray events from this source detected by the
SXS and HXI.

P-35
ISHIDA, Manabu (Institute of Space and Astronautical Science)
Calibration status of Hitomi with the Crab
The X-ray astronomy satellite Hitomi observed the Crab on March 26, 2016. All thescientific instruments had been started up, and we successfully carried out a wide band
observation in the band 0.5–300 keV. We present results from this observation primarily
focusing on instrument calibration.

P-36
NAKAZAWA, Kazuhiro (the University of Tokyo)
In-flight performance of the Hard X-ray Imager onboard Hitomi
The Hitomi (ASTRO-H) mission is the sixth Japanese X-ray astronomy satellite developed by a large international collaboration. Its one month of operation in orbit
demonstrated that many of the new technologies introduced to the Hitomi mission
worked well. The hard X-ray imaging spectroscopy system of Hitomi composed of 2
sets of hard X-ray telescopes (HXT, a super-mirror with a focal length of 12 m) andhard X-ray imagers (HXI). It provides 1.7–1.9 arcmin (HPD) imaging in 5–80 keVband with 9×9 arcmin2 field of view. The HXI is designed to provide low background,utilizing the deep-well shaped BGO active shield, made of 9 BGO units read-out via
avalanche photo diode. In the bottom of the well, a camera made of 4 layers of 32×32
mm2 double-sided Si strip detectors and 1 CdTe double-sided strip detector beneathare located. The HXI saw 13 days of successful operation in orbit. We observed two
pulsar wind nebula, and some blank sky fields. No malfunction nor degradation wasseen after launch, and temperature control also worked well. The imaging spectroscopy
was performed well. Energy resolution was 1.0 keV (FWHM) at 14 keV. After proper
screening, in-orbit background was about (1 − 3) × 10−4 cts/s/cm2 and relatively stable
thanks to tight active shielding as well as comprehensive CXB baﬄing.

P-37
FUKAZAWA, Yasushi (Hiroshima University)
In-flight performance of the Soft Gamma-ray Detector (SGD) onboard Hitomi
The Soft Gamma-ray Detector (SGD) is one of observational instruments onboard
the Hitomi (ASTRO-H), and will provide better sensitivity in 60–600 keV than the pastobservatories. The SGD utilizes similar technologies to the Hard X-ray Imager (HXI)
onboard the ASTRO-H. The SGD achieves low background by constraining gammaray events within a narrow field-of-view by Compton kinematics, in addition to the
BGO active shield. SGD was successfully turned on and observed the Crab nebula.
All the instrumental components, including 6 Compton cameras and 50 BGO active
shields, were worked well without significant problems. Noise performance was <2 keV(FWHM) at 100 keV, as well as expected, and the pulse profle from the Crab neutronstar was obtained. Polarization studies of the Crab nebula is going on. In this paper,
we will report the in-flight operation, calibration, and performance of SGD.

P-38
OHNO, Masanori (Hiroshima University)
Development and in-orbit performance of all-sky monitoring function of
BGO active shield of the soft gamma-ray detector onboard Hitomi
BGO active shields of the Soft Gamma-ray Detector (SGD) onboard Hitomi satellite
can also act as an all-sky monitor with very large eﬀective area up to soft gamma-ray
energy band. We have developed the hardware and signal processing system of BGO
active shield so that we can perform eﬀective all-sky observations with limited resources.
The data processing system accumulates high-time resolution (16 ms) spectral data
(32 channels) once the onboard hardware trigger is activated for 5.376 sec duration.
Therefore, this trigger data is dedicated to short transients such as short gamma-ray
bursts or terrestrial gamma-ray flashes. We also added the autonomous data accumulation system with moderate time resolution (4 s) spectral data (128 channels) during
about 512 seconds after the trigger to cover the long-duration transients such as long
gamma-ray bursts and solar flares. The recorded data is transferred to the digital electronics soon after the data accumulation is finished and make ready for the next trigger
so that we can maximize the trigger eﬃciency.
We confirmed that above data accumulation system of BGO active shield works wellat on-ground calibration tests. After the launch, we activated the all-sky monitoring
function after the commissioning phase of SGD finished. Unfortunately, we could not
optimize the trigger judgement parameters during the observation and we had no trigger data from astronomical origin. However, we confirmed that our developed signal
processing system itself worked well in the orbit. We will present about the detail ofdevelopment and in-orbit performance of all-sky monitoring function of SGD and discuss possible synergy with MAXI and such large area all-sky monitor as the future
perspective.

P-39
HORI, Takafumi (Kyoto University)
The MAXI/GSC catalog in the low Galactic-latitude sky
Complete X-ray source catalogs in our Galaxy are the basis to study the demographyof Galactic X-ray populations. Since MAXI/Gas Slit Camera (GSC) covers the 2–10
keV band with the highest sensitivity as an all-sky mission, its Galactic source catalog
will be complementary to those of hard X-ray (>10 keV) missions. Here we present thelatest X-ray source catalog of MAXI/GSC in the low Galactic-latitude sky (|b| < 10
degrees) based on the first 74 month data. We utilize the same image fitting method
as that in Hiroi et al. (2013), who constructed the 37-month MAXI/GSC catalog athigh Galactic latitudes (|b| < 10 degrees). To overcome source confusion in crowded
regions, we have accurately calibrated the position-dependent shape of the point spreadfunction of MAXI/GSC by utilizing the onboard data. We also take into account the
Galactic ridge X-ray emission in the background, utilizing the model by Revnivtsev etal. (2006). With a preliminary analysis, we detect at least 150 sources with significanceabove 8 sigma, among which about 70% have counterparts in the Swift/BAT 70-monthcatalog. Updated results will be presented.

P-40
SHIDATSU, Megumi (RIKEN)MAXI/GSC 7-year all-sky map and studies of large-scale diﬀuse structures
We present MAXI/GSC all-sky maps in the soft (3–4 keV), medium (4–10 keV), andhard (10–20 keV) X-ray bands constructed from the whole 7-year data. To realize
maximum sensitivity, we have developed a model of the non X-ray background (NXB)
with high accuracy, by using the rate of the coincident events between a signal anodeand a veto anode, as a tracer of the intensity and energy distribution of the NXB.
The model has enabled us to obtain the high-quality all-sky maps and to analyse Xray sources all over the sky. We report our studies of extended structures, including
the spatial distribution of the Galactic ridge X-ray background and constraints on thestrength of the Fermi bubbles in the X-ray band.

P-41
SUGIZAKI, Mutsumi (RIKEN)
Operation and calibration of MAXI Gas Slit Camera (GSC) on the International Space Station for over 7 years
GSC (Gas Slit Camera) is the main X-ray instrument of the MAXI mission carriedout on the International Space Station (ISS). Utilizing 6 identical camera units, each ofwhich consists of two Xe-gas counters and a slit mask with one-dimensional field of view,it scans the almost entire sky every ISS orbital cycle of 92 minutes. The Xe-gas counters
employ resistive carbon anodes to archive the position sensitivity. Passing through thein-orbit operation for over 7 years since 2009, some gas counters are now found to expose
significant performance degradation. Three out of the 12 counters are considered tohave a broken anode wires, which is thought to be caused by repeated heavy particle
irradiation and discharge. We operate these counters carefully by activating only theiralive segments. Another counter showed a sudden gain increase on 2013 June. From
the diagnostic data analysis, it is suggested that the gas pressure began to decrease atthat time with the exponential decay time of ∼1.5 year. We operate the counter bytuning the anode voltage so that the gas gain keep constant. The paper summarizes thein-orbit performance of the GSC for over 7 years and the response calibration.

P-42
TOMIDA, Hiroshi (ISAS/JAXA)The current status of Solid-state Slit Camera aboard MAXI
We will report the current performance-status of the CCD camera aboard MAXI
(Solid-state Slit Camera: SSC). After the 7-years operation in orbit, the performanceof the MAXI/SSC has been guradually decreasing. The incrasing dark current andthe charge transfer ineﬃciency led to the degradation of the energy resolution. In theposter, we will summarize the history of the SSC perfomances.

P-43
FURUSHO, Tae (ISAS/JAXA)
Energy spectra of bright clusters of galaxies obtained from the MAXI dataarchive
In order to enhance use of the MAXI data by scientists all over the world, we aredeveloping the MAXI data archive. The archival data and tools will be released fromDARTS at ISAS/JAXA by the end of 2016. Also, it is planned that the data andtools be available from HEASARC at NASA/GSFC. Although MAXI data analysis
procedure is complicated, we oﬀer simple analysis tools that enable end-users to easily
create standard images, energy spectra and responses, and light curves. We describe
design of the MAXI data archive system and how to use the analysis tools for endusers. To demonstrate performance of the MAXI archive, we present energy spectraof the Perseus cluster and other clusters of galaxies accumulated over the seven-year
MAXI life-period. Thanks to MAXI’s sensitivity to largely extended emission and wide
energy band, we are able to create high-quality spectra in 0.7–30 keV from the entire
clusters of galaxies.

P-44
KAWAI, Nobuyuki (Tokyo Institute of Technology)
iWF-MAXI: Soft X-ray Transient Monitor on the ISS
iWF-MAXI is an X-ray transient monitor mission proposed as an experiment payloadon the JEM/EF (Japanese Experiment Module Exposed Facility) of the International
Space Station. Its main scientific goals are monitor the large part of the sky in X-ray
band to find and localize astrophysical transient events. Prompt X-ray emission associated with gravitational wave events is its prime target. Other targets include gamma-ray
bursts, tidal disruption events, stellar flares, nova ignitions, supernova shock breakouts,
black hole/neutron star binaries, and active galactic nuclei (AGN). Its main scientific instrument is the Soft X-ray Large Solid Angle Camera (SLC) with a localization accuracyof 0.1 degrees.
Its overview and current status are presented.

P-45
SUGITA, Satoshi (Tokyo Institute of Technology)
Development of the Hard X-ray Monitor onboard WF-MAXI
Wide-Field MAXI (WF-MAXI) is a mission to detect and localize X-ray transientswith short-term variability including EM counterparts of gravitational-wave events suchas gamma-ray bursts and supernovae etc. WF-MAXI consists of two main instruments,
Soft X-ray Large Solid Angle Camera (SLC) for localization of the events with few
arc-minutes error in soft X-ray band and Hard X-ray Monitor (HXM) to measure thespectrum and the lightcurves in hard X-ray band. The field of view of WF-MAXI is
20% of all sky at any given time and the energy band is covered from 0.7 keV to 1
MeV. We have developed the HXM components which consists of 24 channel arrays of
Ce:GAGG scintillators coupled with APDs covering the hard X-ray band with eﬀective
area of above 120 cm2 . To read out signals from the censor arrays, we designed a new
LSI dedicated with the readout of 32 APDs’ signals using 0.35 µm CMOS technology.
We will report the integration and the end-to-end test of the components of HXM BBM.

P-46
NAKANO, Toshio (RIKEN)
End-to-End test of the mirror and polarimeter of PRAXySThe Polarimeter for Relativistic Astrophysical X-ray Sources (PRAXyS), NASA’s
small explore mission, will allow us to measure the polarization of the X-ray in the 2–10
keV energy band. We carried out an end-to-end test of the X-ray optics combining a
grazing incident X-ray mirror and a Time Projection Chamber Polarimeter for PRAXyS
at the NASA Goddard Spacecraft Center 100m X-ray beamline in June and July 2016.
To simulate the spacecraft rotation canceling out instrumental fake polarizations, the
X-ray tube, mirror and polarimeter in the test were designed to rotate around beamline
axis independently. The optics was tested with 2.7 keV, 4.5 keV and 6.4 keV X-rays(and bremsstrahlung X-rays) at several combinations of angles. We verified uniformityof the mirror and performance of the polarimetry.

P-47
SANTANGELO, Andrea (University of Tübingen)
The enhanced X-ray Timing and Polarimetry mission
I present here the enhanced X-ray Timing and Polarimetry (eXTP) mission concept,
currently developed by an international Consortium led by the IHEP of CAS. The
science goals aim at studying matter under the extreme conditions of density (equationof state and QCD), gravity (strong field gravity and GR) and magnetism (strong andextreme magnetic fields and QED). The mission will also monitor the X-ray sky in the
2–50 keV range. The scientific payload includes a suite of instruments devoted to largearea and high-sensitivity spectral, timing and polarimetric studies:- The Spectroscopy Focusing Array (SFA, 0.5–10 keV)
- The Large Area Detector (LAD, 2–30 keV)
- The Polarimetry Focusing Array (PFA, 2–10 keV)
- The Wide Field Monitor (WFM, 2–50 keV)
After presenting the science case of the mission, I will then describe the current mission
configuration, and its capability as All sky monitor.

P-48
MORI, Koji (University of Miyazaki)
A broadband X-ray imaging spectroscopy with high-angular resolution: the
FORCE mission
We present our concept of future Japan-lead medium-class mission, FORCE (Focusing On Relativistic universe and Cosmic Evolution), to be launched in the mid 2020s.
FORCE is the direct successor to the broadband X-ray imaging spectroscopy aspectof Hitomi (ASTRO-H) with significantly higher angular resolution. The current designof FORCE defines energy band pass of 1–80 keV with angular resolution of < 15” inhalf-power diameter, achieving a 10 times higher sensitivity above 10 keV compared toany previous missions with simultaneous soft X-ray coverage. Our primary scientificobjective is to trace the cosmic formation history by searching for “missing black holes”
in various mass-scales: “buried supermassive black holes (SMBHs)” residing in the center of galaxies in a cosmological distance, “intermediate-mass black holes” acting as thepossible seeds from which SMBHs grow, and “orphan stellar-mass black holes” without
companion in our Galaxy. In addition to these missing BHs, hunting for the nature of
relativistic particles at various astrophysical shocks is also in our scope, utilizing thebroadband X-ray coverage with high angular-resolution. FORCE are going to open a
new era in these fields. The satellite is proposed to be launched with the Epsilon vehicle that is a Japanese current solid-fuel rocket. FORCE carries three identical pairs ofSuper-mirror and wide-band X-ray detector. The focal length is currently planned tobe 10 m. The silicon mirror with multi-layer coating is our primary choice to achieve
lightweight, good angular optics. The detector is a descendant of hard X-ray imager
onboard Hitomi (ASTRO-H) replacing its silicon strip detector with SOI-CMOS silicon
pixel detector, allowing an extension of the low energy threshold down to 1 keV or even
less.

P-49
HAYASHI, Hideki (Kyoto University)
Development of X-ray SOI pixel sensors for future X-ray wide filed cameras
MAXI has opened up the all-sky monitor and time-domain astronomy in the soft
X-ray band below 10 keV. In order to push out the frontiers, we develop X-ray wide
field cameras using two-dimensional coded masks with XRPIX. XRPIX is a monolithic
active pixel sensor based on the silicon-on-insulator (SOI) pixel technology. XRPIX
contains a comparator circuit in each pixel for hit trigger (timing) and two-dimensional
hit-pattern (position) outputs in addition to the imaging and spectroscopic capabilities
comparable to those of an X-ray CCD. The function allows us to read out analog signalsof only hit pixels, which is referred to as the event-driven readout mode. Thus, XRPIX
oﬀers a good time resolution better than 10 microsecond and a high throughput reaching>1 kHz in the event-driven readout mode. The pixel size of XRPIX is 36 micron × 36
micron. Thus, the angular resolution reaches 2.5 arcmin in principle by adopting thesame pitch size for the coded mask and the distance between XRPIX and the mask of
10 cm. We can also reduce the non-X-ray background by applying the anti-coincidence
technique because XRPIX has the high time resolution. In our previous studies, we havesuccessfully demonstrated the X-ray detection by the event-driven readout. Recently,
we successfully processed XRPIX with an imaging area of 24.6 mm × 15.3 mm and theformat of 608 × 384 pixels. In this poster, we report the evaluation results of the newdevice together with the concept of the wide field camera using XRPIX.

P-50
HARITA, Shohei (TokyoTech)
Micro-satellite for astrometry and photometry of gravitational wave sources
We are planning a micro-satellite for astrometry and UV photometry of gravitational
wave sources. Humankind had detected three gravitational waves arise from BH-BH
mergers that were totally unexpected. Another candidates of gravitational wave source
are NS-NS or NS-BH mergers. Short Gamma-ray Bursts (sGRB) have been believed tobe related to the NS mergers. If it is the case, gravitational waves may be accompanied
by sGRBs and their optical afterglows. Furthermore, recent theoretical study predicts
that the NS merger may radiate strong UV light caused by free neutron beta-decay. To
detect these phenomena we propose a wide-field UV surveying observation mission in
space utilizing micro-satellite.
In the strictly limited mission payload we packed an UV telescope, two wide field
optical monitors, and gamma-ray scintillation detectors to detect and localize sGRBs.
The diameter of the UV telescope is 200mm to achieve the limiting magnitude of 22
mag in u’-band for 1000s exposure. In the current design the FoV of the UV telescopeamounts to 4◦ ×4◦ . While the optical wide field monitor have 10◦ ×10◦ FoV and achieve
the limiting magnitude of 20 mag at optical band for 1000s exposure.
Based on a brief estimation, these detector system can detect several supernovae permonth. Therefore this may be capable with detecting not only the GW sources but also
the other transient sources, like supernova shock breakouts.
Those telescope system mounted on 50 kg class micro-satellite with brand-new attitudecontrol system, namely ”variable shape attitude control (VSAC)” system which satisfies
both maneuver speed and stability. We plans tiling observation utilizing for surveying
GW sources by using the agile satellite bus and follow-up observation based on the GW
alert sent by LIGO/Virgo/KAGRA. This project is just started but we aim to launchwithin 2020.

P-51
YAMAOKA, Kazutaka (ISEE, Nagoya University)
Development of the Solar Neutron Monitor on the ChubuSat-2 Satellite
The solar neutron observation is a key in understanding of the ion acceleration mechanisms at the Sun surface since neutrons are not aﬀected by the magnetic field around the
Sun and interstellar mediums. However, there have only been a few tens of detection so
far since its discovery in 1982. ChubuSat is a series of 50-kg class microsatellites jointly
developed by Nagoya university, Daido university, and aerospace industrial companies
in the Chubu area of central Japan. ChubuSat-2 was selected as one of the four piggyback payloads of the X-ray astronomy satellite ASTRO-H in 2014 summer, and was
successfully launched by the H-IIA launch vehicles from the JAXA Tanegashima Space
Center (TNSC) on February 17, 2016. ChubuSat-2 carries two mission instruments, theradiation detector (RD) and the infrared camera. The main mission of ChubuSat-2 isdevoted to monitoring neutrons and gamma-rays which can be background sources for
ASTRO-H celestial observations. The mission also involves solar neutron observations
which were originally proposed by graduate students who join the leadership development program for space exploration and research, a program for the leading graduate
schools (LGS) at Nagoya University. The RD has a similar detection area and eﬃciency
to those of the neuron detector, SEDA-AP FIB on the International Space Station (ISS),but is expected to have a lower background than the SEDA-AP FIB thanks to a muchsmaller mass of the micro-satellite. In this paper, we will describe development of the
ChubuSat-2 satellite and the RD, and the current status in orbit.

P-52
UCHIDA, Nagomi (Hiroshima University)
Development of an in-orbit radiation environment monitor CUBES onboard
a small satellite MIST
Gamma-ray Bursts (GRBs) are the brightest explosions in the universe, and someof GRBs could be a candidate of gravitational wave sources. However, the emission
mechanism and physical environment of GRBs are not understood well. To investigate
them, we are planning to observe gamma-ray polarization of GRBs, using the Segmented
Polarimeter for High eNergy X-rays (SPHiNX) launched in 2020. Since the gamma-ray
polarization information has been measured from a few sources, SPHiNX will observe
polarization properties of 30 GRBs in 2 years and accumulate the statistics. If theemission is produced in photospheric through the thermal process, polarization degree
is expected to be weaker. On the other hand, if the emission is produced far from theprogenitor through the synchrotron process, the polarization degree is expected to behigher.
The main detector of SPHiNX is the Compton-based hard X-ray polarimeter which
consists of plastic scintillators as the scatterer, and Bi4 Ge3 O12 (BGO) or Gd3 Al2 Ga3 O12(GAGG) as the absorber. Compared to BGO, GAGG is a new material with high lightyield and good energy resolution, however it has not been used much in space. We areinvestigating which scintillators are suitable for SPHiNX. This satellite will move aroundthe low earth orbit and thus will be exposed to primary cosmic rays, and secondary
charged particles, gamma-rays, and neutrons which are sources of background.
CUBES is a detector jointly developed by Hiroshima University and KTH in Sweden
and launched by the MIST satellite in 2018. The aims of CUBES are to study the behavior of these scintillators and radiation environment in the SPHiNX orbit. CUBES loads
the three candidates of scintillators for SPHiNX which are read by Si-Phtomultiplier.
We present sciences of SPHiNX, current development of the analog readout circuit for
CUBES and test of radiation tolerance of GAGG against 60 Co gamma-rays.

P-53
ONO, Yuki (Tokyo Tech)
X-ray emission of the Be star/pulsar system PSR B1259−63 at nonperiastron phase
PSR B1259−63/SS 2883 is a binary system in which a pulsar orbits around a Be starwith a long orbital period of about 3.4 yr. It is argued that the system is non-accreting
and a shock is formed between the pulsar wind and the Be star wind, resulting inparticle acceleration and non-thermal emission near periastron up to TeV gamma-ray
bands. In the five years MAXI observation of the field of PSR B1259−63, X-ray flares
have been observed at orbital phases far from the periastron. The resolution of MAXI
GSC is typically on the order of 1.5◦ , while a nearly transient source IGR J13020−6359
is located at 0.16◦ from PSR B1259−63, making it diﬃcult to identify the sources ofthe flares. In this study, we fit the X-ray images with the Point Spread Function of
MAXI GSC to determine the position of the X-ray flares accurately. As a result, we candistinguish the flares of PSR B1259−63 from those of IGR J13020−6359; three flaresout of five flares are likely to be from PSR B1259−63. We suggest that the Be star
temporarily releases the large amount of gas in a direction other than the circumstellar
disk, resulting in increases of the stellar wind density around the pulsar at phases far
from the periastron.

P-54
RODES ROCA, Jose Joaquin (University of Alicante)Long term variability of Cen X-3 with MAXI
Cen X-3 is an O-type donor Supergiant X-ray Binary with a neutron star as a compact
object and a prime benchmark to study disk fed accreting systems. The aim of this work
is to study both the light curve and orbital phase spectroscopy of this system in thelong term. Here we estimate the orbital period from the light curve and then we derive
the good time interval to extract the spectrum from diﬀerent orbital phases. We obtainorbital phase-averaged and phase-resolved spectra and we analyse the variability of themodel parameters to infer properties of the circumstellar environment of Cen X-3 andpossible dependences of the spectral parameters. The MAXI spectra in the 2–20 keVenergy range were fitted with typical models used in X-ray accreting systems. Then weused the best one to discuss the orbital phase variability of the parameters.

P-55
ISLAM, Nazma (Raman Research Institute)
Orbital phase resolved spectroscopy of GX 301−2 with MAXI
GX 301−2, a bright high-mass X-ray binary with an orbital period of 41.5 d, exhibits
stable periodic orbital intensity modulations with a strong pre-periastron X-ray flare.
Several models have been proposed to explain the accretion at diﬀerent orbital phases,
invoking accretion via stellar wind, equatorial disc, and accretion stream from the companion star. We present results from exhaustive orbital phase resolved spectroscopic
measurements of GX 301−2 using data from the Gas Slit Camera onboard MAXI. Using spectroscopic analysis of the MAXI data with unprecedented orbital coverage formany orbits continuously, we have found a strong orbital dependence of the absorption
column density and equivalent width of the iron emission line. A very large equivalent
width of the iron line along with a small value of the column density in the orbital
phase range 0.10–0.30 after the periastron passage indicates the presence of high density absorbing matter behind the neutron star in this orbital phase range. A low energy
excess is also found in the spectrum at orbital phases around the pre-periastron X-ray
flare. The orbital dependence of these parameters are then used to examine the various
models about mode of accretion on to the neutron star in GX 301−2.

P-56
PRADHAN, Pragati (University Of North Bengal & Raman ResearchInstitute)
A COMPARATIVE STUDY OF SG-HMXBS AND SFXTS USING IRON
K-ALPHA LINE AS A TRACER
We present a comparative study of classical supergiant HMXB and SFXT systems
by making a detailed study of the variation of the equivalent width of iron K-alphaline with the absorption column density using out-of-eclipse observations from Suzaku,
XMM, and Chandra (and taking care not to mix observations in diﬀerent spectral
states). Analysis of the entire archival Suzaku observations of these systems show thatthe equivalent width of SFXTs is significantly smaller compared to those of classicalsupergiant HMXBs even when the hydrogen column density of both are comparable.
We discuss the results of the analysis in the light of two theories on SFXTS: the clumpy
wind and the magnetic gating model. The findings are also used to make a comparison
between these two systems as a class.

P-57
INOUE, Hajime (Meisei University)
Precessions of accretion rings and super-orbital periods
I show that X-ray light curves of three X-ray pulsars, Her X-1, LMC X-4 and SMC
X-1, folded with their respective super-orbital periods, can well be reproduced by amodel that X-rays from a compact object towards us are periodically obscured by aprecessing ring at the outermost part of an accretion disk around the central object.

P-58
LAPLACE, Eva (University of Tübingen)Possible regular phenomena in EXO 2030+375
The X-ray source EXO 2030+375 (spin period: 42 s; orbital period: 46.021 d) is
known for being the Be X-ray binary system showing the largest number of recurring
low-luminosity X-ray outbursts (type I) every orbital period. Recently, however, its
behaviour started to change: the X-ray flux decreased significantly and some expected
type I outbursts were not detected, while the spin frequency reached a plateau (Fuerst
et al. 2016). We report a striking similarity with events which occurred 20 years
ago, just before the source showed a sudden shift of the orbital phase of the outburst
peak (orbital phase jump) in 1995 (Wilson et al. 2002). Moreover, we investigate therelation between these events and the long high-luminosity outbursts (type II), whichwere observed in 1985 (Parmar et al. 1985) and 2006 (Corbet & Levine 2006). The
existence of an underlying periodicity between an orbital phase jump and/or type II
outbursts is considered. We discuss possible models explaining the observed changes
such as Kozai-Lidov oscillations of the circumstellar disk. If our view is correct, weshould experience another orbital phase jump in December 2016/January 2017.

P-59
SAKAMAKI, Ai (Nihon University)
MAXI Observations of Supergiant Fast X-ray Transients
MAXI has often detected short X-ray flares or outbursts possibly from supergiant fast
X-ray transients (SFXTs), for instance, IGR J18483−0311, AX J1841.0−0536, and IGR
J08408−4503. Peak X-ray fluxes from those sources are just around the detection limit
in a single (80∼100 mCrab) or a few (30–50 mCrab) scanning observations. Here, we
briefly summarize MAXI observations of SFXTs: detection frequencies, (peak) fluxes,
and average orbital X-ray light curves.

P-60
OHUCHI, Haruka (Tokyo Institute of Technology)
Gamma-ray observation for PSR J2022+3842
The Fermi Gamma-ray Space Telescope has observed more than 200 pulsars and about
half of them are young pulsars (http://tinyurl.com/fermipulsars). About 1/3 ofthem are also known as radio pulsars. On the other hand, there some pulsars whichhave not been detected in the gamma-rays in spite of radio observations. It is important
to investigate how many pulsars can be observed in radio and/or gamma-ray (Romani
et al. 1995).
PSR J2022+3842 was discovered in SNR G76.9+1.0 as an energetic rotation-poweredyoung pulsar and has period of 48 ms (Arzoumanian et al. 2011, Arumugasamy et al.
2014). It is a Vela-like pulsar due to its spin down energy rate of 3.0 × 1037 erg/s andthe characteristic age of 8.9 kyr. Though radio and X-ray pulse emission were observed,
the pulsar has not been detected in gamma-rays due to its location on the galactic plane
resulting in high background levels.
We report that we observed the gamma-ray pulsation of PSR J2022+3842 and its
anomalous behavior.

P-61
YONEYAMA, Tomokage (Osaka University Graduate School of Science)
Discovery of keV excess emission in the isolated neutron star RX
J1856.5−3754
RX J1856.5−3754 is the brightest and nearest (∼120 pc) thermally emitting isolated
neutron star, a prototype of X-ray dim neutron stars (XDINS). After its discovery withROSAT, the source was observed many times with various X-ray satellites. Observations
with XMM-Newton and Chandra satellites indicate that the X-ray spectrum is well
reproduced with a combination of blackbody models, one with kT ∼ 32 eV and theother with kT ∼ 63 eV. In addition, the X-ray spectrum and intensity are found tobe fairly stable over the time. Therefore, the source was employed as a calibration
target of the soft X-ray detectors, which are sensitive to contamination of material
onto detectors or filters inside the satellites. Suzaku observed this source 10 times
during its lifetime primarily for the calibration purpose. The X-ray spectra below 0.8
keV are well fitted with the two blackbody model determined with XMM-Newton andChandra. Nevertheless, we notice systematic excess of the observed spectra over thetwo blackbody model. The excess is about 20% in the integrated counts in 0.8–1.2 keVband, and is found both in the spectra of BI-CCD (XIS1) and FI-CCD(XIS0+XIS3).
We further analyze the XMM-Newton EPIC-PN spectra of this source and find similar
excess. We call this keV excess, discovered 1st time for this source and for the XDINS
class. We examine possible causes of this excess, including uncertainty in backgroundsubtraction, pileup of photons below 0.8 keV, and contamination of other sources. We
show qualitative diﬃculties in explaining the keV excess with these causes. We thenconclude the keV excess is originated in the source RX J1856.5−3754, or its neighborwithin the radius of 0.2 arcmin. The keV excess component is fitted either with ablackbody model ( kT ∼ 140 eV) or a power law model (Γ ∼ 4.5), though it is hard toconstrain considering the systematic uncertainty. We shortly discuss possible origin of
this keV excess.

P-62
MORII, Mikio (Institute of Statistical Mathematics)
Search for soft X-ray flashes at the ignition phase of optical novae using GSC
data
We searched for soft X-ray flashes associated with optically discovered classical orrecurrent novae in 5-yr MAXI/GSC data in 2–4 keV band. For this purpose, we developed a tool to make the light curves of a point source by fitting the event distribution
with point spread functions (PSF-fit tool). We applied the PSF-fit tool to 40 classical/recurrent novae that were discovered in optical observations from 2009 August to2014 August. We found no precursive soft X-ray flashes with significance above the3-sigma level between T − 10 day and T (T = discovery date). We obtained the upper
limits for the bolometric luminosity of soft X-ray flashes, and compared them with thetheoretical prediction and that observed for MAXI J0158−744.

P-63
SUGAWARA, Yasuharu (JAXA/ISAS)
X-ray spectral variability of the colliding wind binary WR140: the origin of
the cool plasma component
We present the results from the X-ray spectral analysis of the colliding wind binary
WR140 (WC7pd+O5.5fc) using archival XMM-Newton, Suzaku and Chandra data.
The long period binary WR140 (P=7.94 yr) is considered as the textbook example ofan episodic dust-making colliding wind binary and a good natural laboratory for the
study of shock physics, because the orbital parameters have well determined. Recently
we reported that a cool plasma component in a recombining phase was discovered fromthe WR140 X-ray spectrum at near periastron (Sugawara et al. 2015). In order to
uncover the origin of the cool plasma component, we performed the spectral analysis
using XMM-Newton, Suzaku and Chandra data at near periastron. These observations
cover four diﬀerent epochs from 2008 December 26 to 2009 January 25 for a total
exposure of about 184 ks. The spectra of the cool plasma component were well-fitted
by a single-absorbed non-equilibrium ionization collisional plasma model. It is found
for the first time that the emission measure of the cool plasma component decreased
at approximately fifty percent per month. This variation indicates that the plasma
was cooled down by radiation and/or was expanded. As one interpretation, the coolcomponent may be a relic of the wind-wind collision plasma, and may represent atransitional phase from the compressed hot gas to dust formation.

Sponsored by :RIKENSociety for Promotion of Space Science