重力波天体の光赤外線観測
諸隈 智貴 (東京大学)
on behalf of J-GEM collaboration

Morokuma et al. 2016, PASJ, 68, L9 (GW150914)
Yoshida et al. 2017, PASJ, 69, 9 (GW151226)
Utsumi et al. 2017a, PASJ, in press, arXiv:1710.00127 (GW151226)
Utsumi et al. 2017b, PASJ, in press, arXiv:1710.05848 (GW170817)
Tominaga et al. 2017, PASJ, submitted, arXiv:1710.05865 (GW170817)
Tanaka et al. 2017, PASJ, in press, arXiv:1710.05850 (GW170817)
天文月報2016年6号 (ASTRO NEWS)

天文月報2017年1号 (重力波特集)

天文月報2018年1,2号 (ASTRO NEWS)Contents
重力波源からの電磁波放射
電磁波フォローアップ観測網
光赤外+電波@日本 = J-GEM
LIGO-Virgo Collaboration (LVC)のルール
これまでの重力波源に対する電磁波観測
ブラックホール連星合体: GW150914
中性子星連星合体: GW170817
今後の観測方針まとめ

重力波天体の光赤外線観測

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LIGO x 2 (Hanford, Livingston)
https://www.ligo.caltech.edu/page/ligo-detectors

Virgo

KAGRA

http://public.virgo-gw.eu/index.php?gmedia=5vp4v&t=g

重力波天体の光赤外線観測

https://www.nao.ac.jp/contents/news/topics/2015/20151116-kagra-fig3-origin.jpg

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,223

https://www.ligo.caltech.edu/WA/image/ligo20160211c
重力波天体の光赤外線観測

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,22

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重力波

ligo.org
重力波天体の光赤外線観測

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,22

5

重力波 ==> rプロセス元素合成@中性子星連星合体

The Astrophysical Journal Letters, 789:

Wanajo+2014
重力波天体の光赤外線観測

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,22

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中性子星合体 ==> kilonova

material

radiation

Tanaka & Hotokezaka movies

Tanaka & Hotokezaka 2013
重力波天体の光赤外線観測

Hotokezaka+2013

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,22

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0

すぐに暗くなる
5

10

15

20

Days after the merger-20

i-band
18

20

22

24

-18
Type Ia SN
NS-NS
BH-NS
Wind

-16

-14

-12

Absolute magnitude

16

Observed magnitude (200 Mpc)
Observed magnitude (200 Mpc)

-10

26

-10

16
28
18

g

0

5

r

i

z

10

15

-18
SN 1998bw

z-band

22
18

NS-NS
1.5 days

24
20Type Ia SN
NS-NS
BH-NS
10.0 daysWind

5.0 days

26
22
28
24

-20

20

Days after the merger

16
20

暗い

Type Ia SN

-20

-16

-18

-14

-16

-14

4000

6000

8000

Wavelength (A)

10000
-12

-12

Absolute magnitude

26

-12

Absolute magnitude

-12

24

Absolut-14

中性子星合体: 超新星と比べて…
24

28

Observed magnitude (200 Mpc)

Observed ma

Absolut

Observed ma

-14

-10

赤い

EOS [95, 96]. It is however iemissionfrom BH-NS
merger
26
26
FIG.
3:
Expected
observed
spectra
of
the
NS-NS
merger
Type
Ia
SN
-10
-10
such an eﬀective
mass ejecti
withthe
21 model APR4-1215 (MNS-NS
ej = 0.01M⊙ ) comparedmass ratio and a highspecBH spi
z=0.3
28
tra of28
normal Type BH-NS
Ia SN 2005cf [79–81] Finally,and broad-line
although Typethe red
0
5
10
15
20
0
5
10
15
20
[82, 83].
shownaninearly
AB brightening
magni22 Ic SN 1998bw
Wind The spectra arenately,1
Days after the merger
Days after the merger 080503 at t ∼ 1−5 days can altudes(fν ) at 200 Mpc
distance. The corresponding absolute11[135]. Kasen et al. (2015) [118z=0.5
23 magnitudes
are indicated in the right axis.
tion
with
the diskwindmode
G. 2: Expected observed magnitudes of kilonova models at 200 Mpc distance [70, 71]. The red, blue,
and
green
lines
show
z=0.7
X-ray emission
was also
detec
5e models of NS-NS merger (APR4-1215), BH-NS merger(APR4Q3a75),
anda wind model, respectively.
The ejectamass
24days, and it may favor a comm
Mej = 0.01M⊙ for these models. For comparison, light curve models of Type Ia SN are shown in gray.
The
opticalandcorresponding
X-ray [130, 136].
5
solute magnitudes are indicated in the right axis.
25
5
i

20

is located at near-IR wavelengths [70, 77, 78].
10
Becauseoftheextremely high expansion
velocities,FO
IV. PROSPECTS
26
Tanaka 2016
OBSERVATIONS-1 NS-NS
0 mergers
1
2
3
show
feature-less
spectra (Figure3). This O
8
重力波天体の光赤外線観測
i - [48]).
z
al. 2013
adoptsa “soft”
B. NS-NS mergers 第7回光赤外線天文学大学間連携ワークショップ@京都大学,
2016/11/21,22
is et
a big
contrast
toThisthe model
spectraof SNe(blackEOS
andAPR4
grayfree neutron decay? (Metgzer+2015)
a small fraction of ejected neutron (~10-4 Msun)
expands rapidly. (Bauswein+2013)==> β-decay: n --> p + e- + ν
Neutronto
precursors
1117==> hour-scale “precursor” emission
kilonova
2.1 Shock break-out from NS collisions

Figure 2. Schematic illustration of the ejecta from a binary NS merger
leading to a neutron-powered precursor. Matter ejected from the shockheated interface between the merging NSs expands outwards with a range
of velocities
v(m) ∝ m−β (equation 4; Fig. 1) where β ≈ 3.第7回光赤外線天文学大学間連携ワークショップ@京都大学,
A small quantity
重力波天体の光赤外線観測
2016/11/21,22−0.17 0.62

Metzger+2015

Downloaded from http://mnras

Even if free neutrons are not abundant in the ejecta from standard
binary NS mergers, other related physical scenarios could produce
a small quantity of rapidly expanding ejecta. Alternatively, suchmatter could be present even in standard NS mergers even if it is notwell resolved by current simulations. One example is shock breakout following the collision in a standard NS–NS merger (Sekiguchi
et al. 2011; Paschalidis, Etienne & Shapiro 2012; Kyutoku, Ioka
& Shibata 2014) or as would be produced by the head-on collisionof two NSs. The latter could be physically realized if the binary
eccentricity is stochastically raised due to Kozai oscillations by atertiary companion (e.g. Katz, Dong & Malhotra 2011).
Two NSs that collide head-on at their escape velocity will dis2
/2Rns ≈ 3 × 1053 ergs, where
sipate an energy of Ecoll ≈ GMns
Mns ∼ 1.4 M⊙ and Rns ≈ 10 km are the NS masses and radii,
respectively. The collision drives dual shocks outwards through each
NS (e.g. Rosswog et al. 2009) which as they approach the surface
are accelerated to relativistic velocities by the decreasing density
profile ρ(r) ∝ (Rns − r)n (Johnson & McKee 1971), where n = 3.
According to the formalism outlined by Nakar & Sari (2012; theirsection 2.1 and equations 26), each shell of mass m = 10−4 m−4 M⊙will be accelerated to a four velocity

9Japanese collaboration for Gravitational wave
J-GEM = ElectroMagnetic follow-up
LIGO, Virgo, KAGRAからの重力波アラートを受けて突発天体の可視・近赤外、電波でのサーベイを行う
LSC-Virgo Collaboration (LVC)とのMoU (2014年4月)
PI: 吉田道利氏 (広島大学 ==> NAOJ/Subaru)
16望遠鏡: 多経度, 北天 + 南天

Development of the Kiso Extremely Wide-Field CMOS Camera: Tomo-e Gozen― Investigation of Space Debris with Wide-Field Movie Observations

広視野観測+ 近傍銀河ターゲット観測==>
GLADE)
木曽超広視野高速
CMOS カメラ(GWGC
Tomo-eGozenの開発― 広視野動画観測によるスペースデブリの観測的研究への貢観測体制強化: HinOTORI@チベット，岡山0.91m WFC, 京都3.8m/
KOOLS-IFU, 木曽/Tomo-e Gozen

色撮像カメラ HinOTORI プロジェクト
Operated Tibet Optical Robotic Imager

撮像光学系

良い
に入藏，仮設大澤亮, 酒向重行, 高橋英則, 一木真, 本原顕太郎, 宮田隆志, 諸隈智貴, 青木勉, 征矢野隆夫, 樽
猿楽祐樹, 森由貴, 三戸洋之, 中田好一, 小久保充, 満田和真, 谷口由貴, 土居守, 小林尚人 (東渡部潤一 (国立天文台), 浦川聖太郎, 奥村真一郎 (美星スペースガードセンター), 吉川真 (ISA
Tomo-e Gozen 開発

theTomo-e Gozen camera

2. OAOWFC S

The Tomo-e Gozen is the ﬁrst astronomical CMOS camera, which will be mounted on the 105cm Schmidt Telescope in Kiso Observatory of the University of Tokyo. The Tomo-e Gozen canmonitor a sky of about 20 sq-degree at 2 Hz, providing a great oppotunity to detect small and fastmoving objects. We present an overview of the Tomo-e Gozen project and describe theperformance of the Tomo-e Gozen camera in the context of observing space debris, along withthe observations with a prototype of the Tomo-e Gozen camera developed in 2015.

TelescopeEﬀective FOV†
祝 2016/9/8 FirstDetectors
light# of Detectors
重力波天体の光赤外線観測
Pixel Scale2(1 deg NIR cam

Kiso 105cm Schmidt
20 deg2 in Φ9 deg circle
2160×1200 CMOS sensor
84 chips
A 3D model of the Tomo-e Gozen camera
mounted on the105-cm Schmidt Telescope 10
第7回光赤外線天文学大学間連携ワークショップ@京都大学,
2016/11/21,22
1.2 arcsec/pix

4 deg2 ==> 20 deg2

1.8 deg2

2 deg2

重力波天体の光赤外線観測

電波

広視野望遠鏡

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,22

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Memorandum of Understanding (MoU)~ J-GEM & LIGO & VIRGO ~以下の3者の間で2014年4月締結
the Laser Interferometer Gravitational-Wave Observatory(LIGO) and LIGO Scientific Collaboration (LSC)
the European Gravitational Observatory and Virgo Collaboration(EGO/Virgo)
J-GEM
目的
to reference the parties involved and their relevant policies
define the appropriate data and information that is to beshared under this arrangement, and its permitted use
establish how any publications and presentations coming out of
this work will be handled
守秘義務
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

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守秘義務

analyses, and any publications or presentations using them are governed by the terms of this MOU
and its attachments indefinitely, unless all of J-GEM, LIGO and VIRGO mutually agree to a change.

D

Confidentiality and Appropriate Use of Data

1. All parties agree that any information or data products shared in the framework of the follow-up
program shall be used only for the purposes of the collaborative work covered by this agreement.
2. All information or data exchanged (by J-GEM, LIGO or VIRGO) related to this MOU will be treatedas confidential by all parties, unless it has already been made public as foreseen in Sec. F. Seniorscientists should ensure that all involved persons, including students and technical sta↵, understandand respect the sensitive nature of the data and information exchanged.
3. All J-GEM observations that have not been triggered by LIGO/VIRGO alerts, and all LIGO/VIRGO
analyses that do not make use of J-GEM observation data, are not a↵ected by this agreement. However,any information or data exchanged in connection with such observations or analyses must be kept
confidential by the recipient.
4. All parties are responsible for analyzing and interpreting their own data.
5. All parties will make certain that observations and data collected in the framework of this MOU
are compatible with the above rules of confidentiality. Specifically for J-GEM, this applies to public
facilities, which may not normally keep data confidential. In that case, J-GEM must impress on any
observers or sta↵ who are needed to assist that the observations and data must be kept confidential.

Epublicになるまで(=重力波の情報をLIGO/Virgoが発表するまで)は共有した情

Data and information sharing

報は秘密にすべし

1. All parties will share information with all PARTNERS in the follow-up program through a dedicatedcommunication network. LIGO and VIRGO will communicate the detected GW candidate events in
シニアは同様のことを学生・技術者に理解させるべし
the form of alerts. For each follow-up observation made by J-GEM, J-GEM will share the coordinates
共同利用望遠鏡では特に注意しなさい
of the observations that have been made as soon as practical and within 12 hours of the observing
time. For shared and space facilities, the intended coordinates should be shared as soon as practical
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

13

守秘義務

analyses, and any publications or presentations using them are governed by the terms of this MOU
and its attachments indefinitely, unless all of J-GEM, LIGO and VIRGO mutually agree to a change.

D

Confidentiality and Appropriate Use of Data

1. All parties agree that any information or data products shared in the framework of the follow-up
program shall be used only for the purposes of the collaborative work covered by this agreement.
2. All information or data exchanged (by J-GEM, LIGO or VIRGO) related to this MOU will be treatedas confidential by all parties, unless it has already been made public as foreseen in Sec. F. Seniorscientists should ensure that all involved persons, including students and technical sta↵, understandand respect the sensitive nature of the data and information exchanged.
3. All J-GEM observations that have not been triggered by LIGO/VIRGO alerts, and all LIGO/VIRGO
analyses that do not make use of J-GEM observation data, are not a↵ected by this agreement. However,any information or data exchanged in connection with such observations or analyses must be kept
confidential by the recipient.
4. All parties are responsible for analyzing and interpreting their own data.
5. All parties will make certain that observations and data collected in the framework of this MOU
are compatible with the above rules of confidentiality. Specifically for J-GEM, this applies to public
facilities, which may not normally keep data confidential. In that case, J-GEM must impress on any
observers or sta↵ who are needed to assist that the observations and data must be kept confidential.

Epublicになるまで(=重力波の情報をLIGO/Virgoが発表するまで)は共有した情

Data and information sharing

報は秘密にすべし

1. All parties will share information with all PARTNERS in the follow-up program through a dedicatedcommunication network. LIGO and VIRGO will communicate the detected GW candidate events in
シニアは同様のことを学生・技術者を理解させるべし
the form of alerts. For each follow-up observation made by J-GEM, J-GEM will share the coordinates
共同利用望遠鏡では特に注意しなさい
of the observations that have been made as soon as practical and within 12 hours of the observing
time. For shared and space facilities, the intended coordinates should be shared as soon as practical
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

14これまでの + これからの重力波電磁波対応天体フォローアップ観測(EM counterpart: ElectroMagnetic counterpart)

重力波天体の光赤外線観測

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重力波天体の光赤外線観測

http://ligo.org/detections/GW170817.php
第8回光赤外線天文学大学間連携ワークショップ@国立天文台,
2017/12/14,15

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Localization

LIGOx2: O(100) deg2
LIGOx2 + Virgo: O(10) deg2

http:/重力波天体の光赤外線観測/ligo.org/detections/GW170817.php
第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

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Abbott et al. 2016, ApJL, 826, L13

EM observations (GW150914 = 1st GW, BH-BH)
The Astrophysical Journal Letters, 826:L13 (8pp), 2016 July 20

Abbott et al.

0.1
The Astrophysical Journal Letters, 826:L13 (8pp), 2016 July 20

Abbott et al.

from detection/merger- Kiso/KWFC: 4.4 days
- B&C/Tripole5: 6.3-12 days

Figure 1. Timeline of observations of GW150914, separated by band and relative to the time of the GW trigger. The top row shows GW information releases. The
bottom four rows show high-energy, optical, near-infrared, and radio observations, respectively. Optical spectroscopy and narrow-ﬁeld radio observations areindicated with darker tick marks and boldface text. Table 1 reports more detailed information on the times of observations made with each instrument.

LIGO and Virgo detectors and several EM astronomy facilities
Multi-Band Template Analysis (MBTA; Adams et al. 2015)
in 2009 and 2010 (Abadie et al. 2012a, 2012b; Evans et al.
search speciﬁcally for NS binary mergers using matched2
2012; Aasi et al. 2014). In preparing for Advanced detector ~900
ﬁltering.
CBC waveforms can be precisely computed
degBecause
operations, the LIGO and Virgo collaborations worked with thefrom general relativity, GSTLAL and MBTA are more>~50%
LIBthanskymap
broader astronomy community to set up an evolved and greatly
sensitiveofto initial
CBC signals
the burst search pipelines are.
381
expanded EM follow-up program. Seventy-four groups withAll
four detection
pipelines
report candidates withina few
slightly
less:
final
LALInference
skymapaccess to ground- and space-based facilities joined, of which 63
minutes of data acquisition.
were operational during Advanced LIGOʼs ﬁrst observing run iPTF LIGO
(Kasliwal+2016)
conducted a series of engineering runs throughout(O1). Details of the 2009 to 2010 EM follow campaign andAdvanced LIGOʼs construction and commissioning to prepare
5collect
SNeand+ analyze
3 nucleartransients(w/
changes for O1 are given in Section 1 of the Supplement
todata in a stable
conﬁguration.
Thespec
eighth ID)(Abbott et al. 2016b).
engineering run (ER8)began on 2015 August 17 at 15:00 and
Pan-STARRS1(Smartt+2016)
After years of construction and commissioning, the Advanced
critical software was frozen by August 30.383 The rest of ER8
LIGO detectors at Livingston, Louisiana, and Hanford,
49toextragalactictransients(20
wasbe used to calibrate thedetectors, to carryout spec-ID
diagnostic SNe)
Washington, began observing in 2015 September with about
studies, to practice maintaining a high coincident duty cycle,
3.5 times the distance reach (<40 times the sensitive volume) of
and to train and tune the data analysis pipelines. Calibration
the earlier detectors. A strong GW event was identiﬁed shortly
was complete by September 12 and O1 was scheduled to begin
Figure 3. Footprints of observations in comparison with the 50% and 90% credible levels of the initially distributed GW localization maps. Radio ﬁelds are shaded in18
重力波天体の光赤外線観測
red, optical/infrared ﬁelds after
are in green,theand the pre-run
XRT ﬁelds are indicatedby the blue circles.
The all-sky 第7回光赤外線天文学大学間連携ワークショップ@京都大学,
Fermi
GBM, LAT,INTEGRAL SPI-ACS,Deepand MAXI
calibration
processwascompleted.
on September 18. On 2015 September 14,2016/11/21,22
cWB reported aGW170817: 1st NS-NS merger

http://ligo.org/detections/GW170817.php
week ending
VIEW
LETTERS
Abbott+2017
20 OCTOBER 2017

LIGO+Virgo

LIGO
2017/12/14,15
FIG. 1.重力波天体の光赤外線観測
Time-frequency representations [65]第8回光赤外線天文学大学間連携ワークショップ@国立天文台,
of data containing

19

GW170817 - GRB 170817A
Event rate (counts/s)

10

Fermi
Fermi+INTEGRALFrequency (Hz)Event rate (counts/s)

Event rate (counts/s)

9

Figure 1. The final localizations. The 90% contour for the final sky-localization map from LIGO-Virgo is shown in green(LIGO Scientific Collaboration & Virgo Collaboration 2017a,b,c). The 90% GBM targeted search localization is overlaid in
purple (Goldstein et al. 2017). The 90% annulus determined with Fermi and INTEGRAL timing information is shaded in gray
(Svinkin et al. 2017). The zoomed inset also shows the position of the optical transient marked as a yellow star (Coulter et al.
2017b,a; Abbott et al. 2017c). The axes are R.A. and Decl. in the Equatorial coordinate system.

mass 2–500 M . Signals are required to be coincident
n time and mass in the LIGO detectors, but Virgo data
are not used in the significance estimates of the all-skyo✏ine search (Abbott et al. 2017a).
We present the results of two o✏ine targeted searches
that coherently combine the data from the LIGO and
Virgo detectors and restrict the signal o↵set time and

2500

tart

ger
Bs
Mer
GR

Lightcurve from Fermi /GBM (1050 keV)

1750 Lightcurve from Fermi /GBM (50300 keV)

2250
2000
1750
1500
1250

1500
1250
1000
750
Lightcurve from INTEGRAL/SPI-ACS
120000 (> 100 keV)
117500115000112500400 Gravitational-wave time-frequency map
300
200
100

50
The first targeted search (Harry & Fairhurst 2011;
10
8
6
4
2
0
2
4
6
Williamson et al. 2014; Abbott et al. 2017d; Nitz et al.
2017a) assumes that the source is a BNS or NS–BH
Time from merger (s)binary merger and is located at the sky-position observed for the optical counterpart to GW170817 and2. The joint, multimessenger detection of GW170817 and GRB 170817A. Top: The summed GBM lig
GRB 170817A (Coulter et al. 2017b,a; Abbott etFigureal.
sodium iodide (NaI) detectors 1, 2, and 5 for GRB 170817A between 10 and 50 keV, matching the 100 ms time bins
2017c) and that there is a [ 1, +5] seconds time delay

重力波天体の光赤外線観測

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EM observations(GW170817)
Abbott et al. 2017, ApJL, 848, L12
EM counterpart: SSS17a
報告: Coulter+2017, GCN, 21529
1m望遠鏡(Swope)での発見
個別の銀河サーベイ
重力波検出の~11時間後
母銀河: NGC 4993@~40 Mpc
重力波: dL=40+8-14 Mpc
LIGO sensitivity: ~80 Mpc

重力波天体の光赤外線観測

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,22

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SSS17a (GW170817 EM counterpart) Discovery
w/ Swope 1m(!!!) telescope
1M2H collaboration (Swope+Nickel)

Figure 2 Sky region covering the 90th-percentile confidence region for the location of
GW170817. The 50th, 70th, and 90th-percentile contours are shown, with contours extracted
from the same probability map as Fig. 1. Grey circles represent
locations of galaxies in our
HDthe114098
Ψ byHydraegalaxy catalog and observed
the Swope telescope on 2017 August 17-18 to search for the
EM counterpart to GW170817. The size of the circle indicates the probability of a particulargalaxy being the host galaxy for GW170817. The square regions represent individual Swope
pointings with the solid squares specifically chosen to contain multiple galaxies (and labeledin the order that they were observed) and the dotted squares being pointings which contained
individual galaxies. The blue square labeled ’9’ contains NGC 4993, whose location is marked
by the blue circle, and SSS17a.

NGC 4993
p = 0.022

Coulter+2017, Science
重力波天体の光赤外線観測

30 arcmin10

ESO 508-G014
p = 0.009

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,22

22

8

August
Mon

2017

Tue

Wed

Thu

Thu

Fri

Sat

Sun

Mon

Tue

Wed

Thu

Fri

Sat

Sun

2
1
31

3
12

23

3

25

25
26

25
26
27

26
27
28

27
28
29

28
29
30

29
30
1

30
1

13 4

5
4

6
45

7
56

8
67

9
78

10
89

910

10 2

23

234

456

567

678

78

20
19

20 11

12
11

13
12
11

14
13
12

15
14
13

16
15
14

17
16
15

17
16

LIGO+PR
910
910
11

345

17 9

体育の日

体育の日

体育の日

10
11
12

11
12
13

12
13
14

13
14
15

14
15

26
27
25

27
26

27 18

19
18

20
19
18

21
20
19

22
21
20

23
22
21

24
23
22

24
23

24 16

16
17

16
17
18

17
18
19

18
19
20

19
20
21

20
21
22

21
22

123

23

3

25

26
25

27
26
25

28
27
26

29
28
27

30
29
28

1
30
29

1
30

1

23

23
24

23
24
25

24
25
26

25
26
27

26
27
28

27
28
29

28
29

30

30
31

234

345

45

11
910

15
16
14

16
17
15

17
18
16

18
19
17

19
20
18

22
23
21

23
24
22

24
25
23

25
26
24

29
30
28

30
31
29

31
1
30

12
31

GW170814

Wed

2017

1
31
30

8910
終戦記念日

Tue

October

31
30
29

789
終戦記念日

Mon

10

30
29
28

234

456

56

GW170817
11
12
13
12
13
10
11
12
山の日

Sun

2017

29
28

123

山の日

Sat

September

28

12
31
立秋

345

Fri

9

山の日

6

敬老の日

敬老の日

敬老の日

秋分の日

秋分の日

秋分の日

LIGO+PR
©

このカレンダーは、ちびむすドリル 検索

で無料ダウンロードできます。

©

このカレンダーは、ちびむすドリル 検索

で無料ダウンロードできます。

十五夜

十五夜

十五夜

J-GEM
PR 123
30
31
31
12
1

ハロウィン

ハロウィン

ハロウィン

©

衣がえ

衣がえ

このカレンダーは、ちびむすドリル 検索

で無料ダウンロードできます。

08/14 10:30 GW170814
08/14 11:01 GW170814 alert from LIGO
08/14 17:17 e-mail-based discussion in J-GEM started
08/16 12:32 Subaru/HSC (+Kiso) obs. for GW170814
08/17 12:41 GW170817
08/17 12:41 GRB 170817A detection with Fermi/GBM
08/17 13:08 GW170817 alert from LIGO
08/17 13:33 f2f/e-mail-based discussion in J-GEM started
08/17 20:00 GRB alert
08/17 IRSF obs. started
08/18 01:05 SSS17a@NGC 4993 discovery
08/18 05:08 Subaru/HSC (+IRSF, MOA-II, B&C) obs. for GW170817
09/18 Utsumi et al. submitted to PASJ
09/18 Utsumi et al. accepted
09/25 Tanaka et al. submitted to PASJ
09/27 GW170814 PR
09/29 Tanaka et al. accepted
10/16 Tominaga et al. submitted to PASJ
10/16 GW170817 PR (84 papers OUT including 3 J-GEM papers)
10/17 J-GEM PR
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

23

J-GEM Observations & Results (GW170817)

Publications of the Astronomical Society of Japan (2017), Vol. 00, No. 0

観測
NIR

Page 7 of 22

5

Utsumi+2017
Tominaga+2017

Subaru/HSC, MOIRCSIRSF/SIRIUS
MOA-II/MOA-cam3
Publicationsof the Astronomical Society of Japan
B&C/Tripole5
やけに明るい(intrinsic)

やけに青い(初期)
12 optical
3
4
300o
300o
5
6
7
8
9
Fig. 2.10
Light curves and color evolution of SSS17a. The face color is
Subaru/HSCでサーベイ(z-band)changed with the respective bands. The Galactic extinction has been
11
Fig. 4. Result of the photometry of SSS17a is plotted on !z and (i − z)1st
corrected by assuming E(B − V) = 0.1 mag (Schlafly & Finkbeiner 2011).
o
SSS17a以外にそれっぽい天体がいない
30kilonova
30o For SSS17a (red symbol),
12
plane withand supernova models.
!z is the magnitude difference between the two epochs, t = 1.7 and
13(CTIO/DECam,
Soares-Santos+2017)
7.7 d (!t = 6 d) after the detection of GW170817, and (i − z)1st is the
14color at the first epoch (t = 1.7 d). The models for kilonovae and super15
novae are shown by colored dots and gray dots, respectively. Each dot
corresponds to different starting epoch of2016/11/21,22!t with an increment of25
1 d.
16 重力波天体の光赤外線観測
第7回光赤外線天文学大学間連携ワークショップ@京都大学,

Interpretation (GW170817)

Publications of the Astronomical Society of Japan (2017), Vol.

0.03 Msun ejecta (思っていたより多い)
Lanthanide elementsを含む
今後の課題: 「中性子星合体での元素合成」
元素放出量はいつも同じなのか
Galacticなr-process elementの量, No. 0青い放射はいつもいるのか
見る角度でどう変わるのか5

Tanaka+2017
重力波天体の光赤外線観測
2016/11/21,22
Fig. 4. Schematic
picture of the ejecta of the第7回光赤外線天文学大学間連携ワークショップ@京都大学,
NS merger event GW170817.

26

detection==> release

重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

27

どうやって中性子星合体を観測するか??
1. 自分たちで発見する(少なくともそれを目指す)
広視野突発天体をサーベイする
近傍銀河を一つ一つ観測する
2. 発見は他グループに頼る ==> 追観測
全天に近い領域を常に監視観測している望遠鏡
ニュートリノ: IceCube
ガンマ線, X線: Fermi, INTEGRAL, MAXI
可視: MASTER
依然としてさらなるサーベイが必要な場合もGW170817
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

28

Server for Managing nearby galaxy observations
by 内海くん (広島大学 ==> Stanford/SLAC)

中性子星 = 超新星爆発の後に残る天体(の1種)
中性子星合体は星の集団に付随している確率が高いだろう
重力波で決まる位置(+距離)の近傍銀河で突発天体を探そう!!! GW170817の対応天体はこれで発見された !!!
銀河カタログ: GWGC (White+2011), GLADE (次ページ)
1つ1つの近傍銀河なら広視野望遠鏡でなくても観測可能
近傍銀河とはいえ，1つの望遠鏡で観測しきれない ==> 分担
全体で管理しないと重複が起こる“planner”, “supervisor”

重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

29

重力波望遠鏡
アラート発行Supervisor
アラート受取候補リスト作成
候補リスト更新
候補リスト更新

アラート更新アラート受取候補リスト追加
候補リスト更新

時系列

アラート更新時のフロー©Yousuke
Utsumi
重力波天体の光赤外線観測

観測所
Event list を監視

候補予約
観測実行
観測報告(予約取消)
Event list を監視
候補予約
観測実行

観測報告(予約取消)

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

30

観測所

Supervisor

Event list を監視

アラート受取候補リスト作成

候補予約
観測実行

候補リスト更新
候補リスト更新

観測報告(予約取消) 候補リスト更新

観測所
Event list を監視

候補予約
観測実行
観測報告(予約取消)

候補リスト更新

時系列

複数観測所を考慮した場合のフロー©Yousuke
Utsumi
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

31

©Yousuke Utsumi
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

32

Galaxy List for the Advanced Detector Era (GLADE)
higher completeness required than GWGC (White+2011)
2MASS
XSC and+ 2 comparison
MPZ + HyperLEDA
Summary
with other catalogs
aquarius.elte.hu/glade
B mag + redshift + IR magnitudes
No. of galaxies
Completeness % at 60 Mpc
Completeness% ofat galaxies
120 Mpc
DensityCompleteness % at 180 Mpc

GWGC [1]

CLU [2]

GLADE

53,255
60

?
100
80
40

2,068,841
104 ± 771 ± 565 ± 5~50 galaxies / deg2

90
350

Other advantages:
70

300

Declination [deg]50! Value-addedwith B mag and z data30
! We are working on associating stellar masses to each galaxy

250

10! We have a working pipeline to associate any other parameters200
relevant−10
for the Collaboration
150−30[1] White, D. J., Daw, E. J. & Dhillon, V. S., 2011, Class. Quantum Grav., 28 085016

100−50 J. K., Kanner, J. et al., 2015, submitted to ApJ[2] Gehrels, N., Cannizzo,
http://arxiv.org/abs/1508.03608
Gergely Dálya −70(ELTE)

dalyag@caesar.elte.hu

50

重力波天体の光赤外線観測

100

150

200

September 01, 2015

250

300

350

10 / 1150

02

ρ [1/deg 2017/12/14,15]
第8回光赤外線天文学大学間連携ワークショップ@国立天文台,
Right ascention [deg]33世界との熾烈な競争になる・・・
最初の中性子星合体: GW170817
発見(8/17) ==> 出版(10/16): 2ヶ月弱
重力波のプレスリリース(10/16)まで待った
84本の論文@arXiv, 10/16
極端な例: 後期のX線(Chandra)論文: 観測の翌日にsubmit(Ruan+2017)
O3からは「全世界にアラートが公開」(GRBと同じ)と思われる
重力波論文を待つ必要がない
重力波検出から(長くても)1ヶ月以内にsubmitまで
相当な準備が必要
自動観測, 自動解析, 自動測光, 自動執筆, …
テストアラートで練習しましょう“間に合った”データだけで論文出版
calibration済み(フィルター変換も)それが正しいことの実証 <== 逐一手作業でやるのは無理(GW170817では大変だった
by 内海くん)
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

34

O3でのJ-GEMの観測戦略
O3開始: 2018年後半
感度は不明, O2では80 Mpc (LIGO), 40 Mpc (Virgo)
アラートはおそらくpublicに==> いつでも論文を書ける(書けてしまう) ==> だとすると時間が命
望遠鏡3台 (LIGO x 2 + Virgo) ==> localization ~ O(10 deg2)「電磁波が出そうな天体」= NS+NS or NS+BHを優先的にサーベイ観測: すばる/HSC, 木曽シュミット望遠鏡, MOA-II
近傍銀河観測: それ以外で分担

重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

35

O3でのJ-GEMの観測戦略
発見 => 多バンド追観測(+できれば分光)までしないとサイエンスにならない
GWの性質とEMの性質の対応付け==> GW170817と比較して議論できる程度のデータは取りたい
距離40 Mpc級のイベントはおそらくレア (S/N~30)=> d~50-100 Mpcが重要だろう
100 Mpcなら世界中の1m級が活躍できる
地理的優位性を生かそうと思うと、とにかく1日以内の発見が重要先に発見されても，1日以内の進化は非常に早い．データはユニーク．
以下、戦略の議論にはGW170817と同じ性質を仮定(mass ratio, viewing angle => brightness, colorのvarietyに注意、特に可視の性質は非常にばらつき得る)

重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

36

reddening corrected E(B-V) = 0.1
16

g
r
i
z
J
H
K

17

Observed magnitude

18
19
20

-17
-16
-15
-14
-13

21

-12

22

-11

23

-10

24

-9

25

-8
15

0

©Masaomi
Tanaka重力波天体の光赤外線観測

510Days after GW170817

Absolute magnitude

40 Mpc~100倍

Utsumi+2017, Tanaka+2017

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

37

reddening corrected E(B-V) = 0.1
16

2 mag fainter

17

Observed magnitude

18
19
20
21

1m
optical

-17
-16

-14
-13

PS1 z
(3pi)

0

©Masaomi
Tanaka重力波天体の光赤外線観測

~100倍

-12

Subaru z(1 min)

24
25

-18

-15

22
23

g
r
i
z
J
H
K

-19

Absolute magnitude

100 Mpc-11

5
10
Days after GW170817-1015

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

38

reddening corrected E(B-V) = 0.1
16

3.5 mag fainter

17

Observed magnitude

18
19

g
r
i
z
J
H
K

-20
-19
-18
-17

20
-16
21
-15
22
23

-14

PS1 z
(3pi)

Absolute magnitude

200 Mpc~100倍-13Subaru z(1 min)24
250©Masaomi
Tanaka重力波天体の光赤外線観測

-12
5
10
Days after GW170817

15

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

39

GW150914
LVT151012
Both Spin
BH mass

NS mass
Expected
#
@
O3
(M )
(M )
distribution

2.1+4.1
3.6+6.90.130+0.084
0.21+0.14
1.7
2.9
0.051
0.08
+4.0
+6.8
+0.020+0.031
2.0 1.7 3.0 2.7 0.032 0.012 0.048 0.019
O3
NS-NS
+5.5
+9.2
3
3
1
et al. (Mpc)
pop syn
4.5 3.1hV T 7.4·Dominik· · Range· · · R90% (Gpc yr )i (Gpc5.1yr)
PyCBC

de Mink &PyCBC
Belczynski pop
syn
GstLAL
GstLAL

PyCBC

O1

3,270
2,820
2,490
1,660
2,800
1,270

BH-BH: O(10)-O(100)NS-NS: O(1-10)
NS-BH: O(1)Fong et al. GRB

103

O2

GstLAL4
et al. r-process5
Isotropic
7.01 ⇥ 10Astrophysical7.71 ⇥ 10 4Vangioni
110
112
3,600
Jin et al. kilonova
5
Aligned7.87 ⇥ 10 4 8.96 ⇥ 10 4
114
117
3,210
+0.060+0.096
3
0.093
10 Flat Isotropic
1.00⇥ 10 3 +7.9
1.01 ⇥ 10
123 et 0.150
122 0.0592,530
Petrilloal. GRB+4.9
0.036
3.2 2.4 4.8
3.8
3 +0.020
10 PowerAligned
1.36 ⇥ 10 3 1.52
⇥ 10
137 et0.0479
140 +0.031
1,850
Law
0.031
Cowardal. GRB
0.012
0.019
30
Isotropic
1.10 ⇥ 10 3 9.02 ⇥ 10 4
127
118
2,300
Siellez et al. GRB
30
Aligned1.98 ⇥ 10 3 1.99 ⇥ 10 3
155
153
1,280

1.4
1.4
1.4
1.4
1.4
1.4

13

Table 2. Sensitive space-time volume hV T i and 90% confidence upper limit RKim
NSBH systems with isotropic and aligned
90%etforal. pulsar
spin distributions.
The NS spin magnitudes are in the range [0, 0.04]
and the BH spin magnitudes are in the range [0, 1]. Values
BH-BH
aLIGO 2010 rate compendium
are shown for both the pycbc and gstlal pipelines. hV T i is calculated using a FAR threshold of 0.01 yr 1 . The rate upper
limit is calculatedusing a uniform prior on L = RhV T i and an 18% uncertainty in hV T i fromerrors.
100 calibration
101
102
103
104
2
10

BNS Rate (Gpc 3yr 1)⇤0

Figure 6.

101

100

O1
10

O2

O3

1

100

101

hV T i0 /hV T i0102

Abbott+2016 (arxiv:1602.03842)

A comparison of the O1 90% upper limit on the
NS-BH
O2
O1
BNS merger rate to other rates
discussed in the O3
text (Abadie
Dominik et al. pop syn
et al. 2010; Kim et al. 2015; Fong et al. 2015; Siellez et al.
de MinkCoward& Belczynski
pop2012;
syn Petrillo et al. 2013; Jin et al. 2015;2014;
et al.
Vangioniet etal.al. 2016;
Vangionir-processde Mink and Belczynski 2015; Dominik et al. 2015). The region excluded by the low-spin BNS
Jin et al. kilonova
rate limit is shaded in blue. Continued non-detection in O2
et al. GRB(slash) andPetrillo
O3 (dot)with higher sensitivities and longer operation time
would
Cowardet al.imply
GRB stronger upper limits. The O2 andO3 BNS ranges are assumed to be 1-1.9 and 1.9-2.7 times
Fong et al. GRB
larger than O1. The operation times are assumed to be 6 and2010(Aasi
rate compendium
9aLIGO
monthset al. 2016) with a duty cycle equal to that ofO1 (⇠ 40%).
10 2

10 1

100

101

102

NSBH Rate (Gpc 3yr 1)

103

104

6. Left panel: The median value and 90% credible interval for the expected number of highly significant40ev
重力波天体の光赤外線観測2010). We additionally include some more
recent estimates
第7回光赤外線天文学大学間連携ワークショップ@京都大学,
2016/11/21,22

Abbott+2016 (arxiv:1607.07456)

世界との競争
1-2m級望遠鏡
たくさんある。機動性も良い。
チリの望遠鏡は感度も良い。
銀河カタログを使うところが多い。
経度の差でユニークさを出すのが妥当か ==> 1日以内の勝負

O3でのJ-GEMの観測戦略(1-2m級望遠鏡)
100 Mpcのイベントで意味のある結果が出るようにする

1-2m級望遠鏡

1日以内に見つければユニーク (経度を生かす)

銀河カタログを使って探査 (100 Mpcならstellar massでcompleteness > 50%)
20 mag => 最初の1-2日で受ける必要 (21 mag => 最初の5日)
1-2m 広視野望遠鏡(木曽, MOA)
20-21 magで広視野探査 (20 mag => 2日、21 mag => 5日)
カタログ銀河の場所はすぐにチェックする
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

41

必要な準備: “1日以内に”見つけられるようにする
1-2m級望遠鏡の(半)自動観測、解析環境の整備は必須
1-2m望遠鏡:
銀河カタログの自動探査
自動解析
自動突発天体探査 (銀河カタログの画像で目視も??)1-2m 広視野望遠鏡（木曽, MOA）
自動tiling
自動解析
自動突発天体探査 ( + 銀河カタログとのクロスマッチ)「重力波のテストアラートで練習しましょう」
and/or 「BH-BHでも観測しましょう」
重力波天体の光赤外線観測

第8回光赤外線天文学大学間連携ワークショップ@国立天文台, 2017/12/14,15

42

OISTER

変光星

惑星

小惑星・彗星ニュートリノ

超新星

重力波

J-GEM

まとめ
重力波”天文学”が本当に始まった．
中性子星連星，中性子星ブラックホール連星からの電磁波を捉えたい．
r-process元素生成の場
暗く，赤く，早く減光する．
電磁波対応天体同定の試みは世界中のあらゆる波長の望遠鏡でJ-GEM = 日本@光赤外(+電波)
世界中に望遠鏡，すばる/HSCは特にユニーク．
J-GEM: GW150914 (TM+2016), GW151226 (Yoshida+2017, Utsumi+2017),
GW170817 (Utsumi+2017, Tominaga+2017, Tanaka+2017)
LIGO O3が1年以内(2018年後半)に始まる．
系統的な観測・解析環境(引き算処理含む)の準備(と練習)を!!!
天文学会2018春季年会(千葉大学)・特別セッション
天文月報AstroNews 2018年1号, 2号 (特集号 2017年1号, AstroNews 2016年6号)

重力波天体の光赤外線観測

第7回光赤外線天文学大学間連携ワークショップ@京都大学, 2016/11/21,22

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