Michitoshi YOSHIDA Hiroshima University 2014/06/201Japan-Korea WS on KAGRA.
Michitoshi YOSHIDA Hiroshima University 2012/11/291Japan-Korea WS on KAGRA.
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Transcript of Michitoshi YOSHIDA Hiroshima University 2012/11/291Japan-Korea WS on KAGRA.
Optical-infrared telescope network for follow-up observation of gravitational
wave transients in Japan
Michitoshi YOSHIDAHiroshima University
2012/11/29 1Japan-Korea WS on KAGRA
Hiroshima Astrophysical Science Center
Founded in 2004 April Higashi-Hiroshima Observatory and the 1.5m
optical – infrared telescope (Kanata) Mission:
Observation of Targets of Opportunity (ToO) in collaboration with high-energy astronomical satellites (Fermi gamma-ray satellite, Suzaku X-ray satellite)
Reveal high-energy, dynamic activity in the universe Main targets:
Gamma-ray bursts, Supernovae, Novae, Cataclysmic variables, X-ray binaries, blazars, etc.
Kanata TelescopeDiameter: 1.5mRitchy – Cretien F/12Foci: Cassegrain, 2 NasmythsOriginally constructed by Mitsubishi Electric Co. in 1996for an instrumentation test bench of Subaru Telescope
Searching for EMcounter part is crucialfor understanding the nature of GW sources
The most promising GWsources NS-NS merger
Metzger & Berger 2012
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NR Tanvir et al. (2013)
Optical, NIR and X-ray light curves of GRB130603B.
Kilonova models
ejecta mass10-1 M
10-2 M
2012/11/29
Figure 3 from Progenitor Models of the Electromagnetic Transient Associated with the Short Gamma Ray Burst 130603BKenta Hotokezaka et al. 2013 ApJ 778 L16 doi:10.1088/2041-8205/778/1/L16
Kilonova model (Hotokezaka et al. 2013)
NS-NSmerger
NS-BHmerger
Consistent with the models Mej ~ 0.02 – 0.05 M
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2012 - 2016
PI : Takashi Nakamura (Kyoto Univ.)CoPI: Nobuyuki Kanda (Osaka City Univ.)
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Overview of the project
A01
A02
A03
A04
A05
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Goals of the sub-project A02
Develop an optical-infrared-radio observation network for GW transient follow-up
1. Kiso 6x6 deg2 Camera (optical imager)2. OAO-WFC (wide-field infrared camera)3. IFU for the spectrograph of 3.8m telescope4. 50cm robotic telescope in Tibet (HinOTORI)5. Establish a transient observation network
by utilizing existing facilities: Mini-TAO, IRSF, Kanata, Yamaguchi 32m radio tel., etc.
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PI: M.Yoshida
Japan-Korea WS on KAGRA
Members Michitoshi Yoshida (Hiroshima University)
Project chief, Development of a 60cm robotic telescope at Tibet Koji Ohta (Kyoto University)
Development of an IFU for spectrograph of a new 3.8m telescope, and coordinated observation with Subaru
Kentaro Motohara (Tokyo University) Development of a wide-field CMOS camera of the Kiso Schmidt
telescope, and mini-TAO (in Chile) observation Kenshi Yanagisawa (NAOJ)
Development of robotic observation system for the Okayama wide-field infrared telescope
Associate researchers Mamoru Doi (Tokyo Univ.) → Kiso observatory, mini-TAO Koji S. Kawabata (Hiroshima Univ.) → Kanata telescope Takahiro Nagayama (Nagoya Univ.) → IRSF in South Africa Kenta Fujisawa (Yamaguchi Univ.) → Yamaguchi radio telescope2012/11/29 10Japan-Korea WS on KAGRA
Schematic overview of the project
World-wide obs.long term monitorevent evolution
KanataIRSF
GW alert( A04 )
theory(A05)
X-γ obs.(A01)
Neutrino obs.(A03)
Kiso 6x6 deg2
CameraOAO IR WFC
Kyoto 3.8m
Yamaguchi32mNRAO 45m Multi-wavelen.
detailed study identification emission mechanism
Multi-mode obs.detailed study redshift -> distance emission mechanism
East Asia50cm
SubaruminiTAO
Wide field obs.EM counterpartRapid identification alert to other facilities
alert
Coop.
Coop.
Detection of EM counterpart of GW transientwith wide-field observationsMulti-mode observations physics of EM counterpart
The natureof GW transient
Project schedule
2012 2013 2014 2015 2016
Kiso 6x6 deg2
camera
OAOWFCRobotic obs.system
50cm robotictelescope
IFU of Kyoto3.8m telescope
Softwaresystem
Data analysispipeline
Transient objectobservation
Tel. contl system
6x6 deg2 camera development
development
development
design development commissioning
commissioning
Development & preparation Test obs.Regularobs.
installation
GW
transie
nts fo
llow
-up
commissioning
Commissioning & operation
Telescope design construction
3-color camera development
completeoperation
operation
operation
Obs. with Kanata, Subaru, mini-TAO,IRSF, OAO-WFC, radio telescopes
Shift to GW transients follow-up
operation
Construct the base of optical – radio follow-up observations of EM counterparts of GW transients until 2016
design
commissioning
12
IRSF (Nagoya Univ.) @ South Africa
• 1m Kiso Schmidt telescope
5 deg2 camera 30 deg2
• 1.5m Kanata telescope • 50cm MITSuME• 91cm W-F NIR camera of
NAOJ1 deg2 NIR camera
• Yamaguchi 32m radio telescope
★★
miniTAO (Tokyo Univ.) @ Chile
50cm telescope (Hiroshima Univ.
2014)
Japan Coordinated network for transients observation
Subaru @Hawaii
★
A part of the project “Multi-messenger Observations of GW sources” * collaborating with the KAGRA data analysis team * science cases: GRBs, supernovae, blazars, etc.
3.8m telescope (Kyoto Univ.
2015)
Main features: 5 deg2 opt. imaging w/ 1m 1 deg2 NIR imaging w/ 1m opt-NIR spectroscopy w/ 1–8m opt-NIR polarimetry
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1. Kiso 6x6 deg2 Camera(new instrument: 41 million Yen)
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1. 6x6 deg2 extremely wide field cameraKiso Observatory, the University of Tokyo
Results of simulation on estimation of an arrival direction of gravity wave. Hayama (NAOJ) 2012
・ 105cm Kiso Schmidt telescope・ F.O.V of 6deg x 6deg・ Since Apr. 2012, the KWFC (Kiso Wide
Field Camera) with a F.O.V of 2deg x 2deg has been operated.
F.O.V6deg x 6deg
Project plans1. Development of 6deg x 6deg extremely wide field camera2. Speeding-up and stabilizing Kiso 105cm Schmidt telescope system
15
1.1 Development of 6x6 deg2 Extremely Wide Field Camera
• The world’s widest survey camera- The current widest field came is Pan-STARRS with a F.O.V. of 3deg x
3deg.
• CMOS sensors adopted- 15-20 um/pixel, 20kx20k pixels camera (Data rate: ~800MB/frame)- Operation at -10 degrees of elevation - High-speed read-out (1-10 frames/sec) + Extremely wide field New scientific fields, in addition to follow-up of gravity wave.- Key components
• CMOS sensor : Collaborate with a domestic company.• Read-out system : Use read-out technologies developed for
infrared CMOS detectors by U-Tokyo.
• Time line- FY2012 Evaluations of available CMOS sensors Feasibility studies on cryogenics, optics, and electronics- FY2013-5 Development of camera system with ~10 pcs. of
available CMOS sensors. Development of CMOS sensors with new designs.- FY2016 Test observations
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2. OAO-WFC(install robotic observation function:
15 million Yen)
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2. OAOWFCOkayama Astrophysical Observatory Wide Field Camera
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OAOWFCOkayama Astrophysical Observatory Wide Field Camera
Wide Field NIR Camera Optics:
Effective Diameter: φ 0.91 m Forward Cassegrain + quasi Schmidt F/2.5 (the fastest optics in the NIR)
F.O.V. : 0.92 × 0.92 sq.deg. ( 1.62 arcsec/pix )
HAWAII2-RG, Teledyne 0.47 x 0.47 sq.deg. (1.67 arcsec/pix) HAWAII
Eng., Teledyne Wavelengths : 0.9 – 2.5 um (Y,J,H,Ks-band)
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WFCT II: 1.00 ×1.00 deg2D=0.22m
Comparison of F.O.V.s
D=0.91m OAOWFC: 0.92 ×0.92 deg2
D=4.1m VISTA: 0.77 ×0.77 deg2
D=3.8m WFCAM: 0.46 ×0.46 deg2
IRIS: 0.22 ×0.22 deg2D=0.8m
SIRIUS: 0.13 ×0.13 deg2D=1.4m
OAOWFC has one of the world’s largest field of view.2012/11/29 20Japan-Korea WS on KAGRA
3. Integral Field Unit (IFU) for 3.8m telescope
(new instrument: 29 million Yen)
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Optical spectroscopy of possible optical counterparts of gravitational
wave transientsprompt optical spectroscopy with Integral Field Unit for• short GRBs (+ long GRBs)• possible optical counterparts of the transients identified with imaging facilities (Kiso, Okayama, etc)• supernovae
Locations of large (>3m) optical/NIR telescopes. No large telescopes around Japan Þ3.8m telescope at Okayama is important to make prompt optical follow-up spectroscopy
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Planned3.8m telescopeat Okayama
Integral Field Unit FoV ~ 30”x30” optical wavelength R~1000-3000
=>spectrograph
Conceptual view of IFU2012/11/29
4. 50cm robotic telescope (new instrument: 83 million Yen)
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HinOTORI project Development of a 50cm robotic
telescope + 3-color camera system West China (Tibet area)
Expected limiting mag. (S/N=5 for 10 min exp.) 18.5 mag. u’-band 21.1 mag. Rc-band 20.8 mag. Ic-band
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Candidate site for the telescopeWest end of Tibet: ~ 60 degree west from Japan altitude: 5000m
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A1
A2
B4
B1
Lhasa
Gar
Candidate site for the telescope
Tibet
West end of Tibet: ~ 60 degree west from Japan altitude: 5000m
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A1A2
B4
Views of A1, A2 and B4 from B1
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Telescope
Alluna 50cm telescope(Germany: commercial product)
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Optical Layout of the 3-color camera
u’ band
Rc band
Ic bandtelescope
dichroic mirrordichroic mirror
FOV: 24 arcmin^2
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Operation Fully robotic operation
Heritage of MITSuME project will be used.
MITSuME @ OAO
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5. Other facilities and transients observation network
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IRSF (Nagoya Univ.) @ South Africa
• 1m Kiso Schmidt telescope
5 deg2 camera 30 deg2
• 1.5m Kanata telescope • 50cm MITSuME• 91cm W-F NIR camera of
NAOJ1 deg2 NIR camera
• Yamaguchi 32m radio telescope
★★
miniTAO (Tokyo Univ.) @ Chile
50cm telescope (Hiroshima Univ.
2014)
Japan Coordinated network for transients observation
Subaru @Hawaii
★
A part of the project “Multi-messenger Observations of GW sources” * collaborating with the KAGRA data analysis team * science cases: GRBs, supernovae, blazars, etc.
3.8m telescope (Kyoto Univ.
2015)
Main features: 5 deg2 opt. imaging w/ 1m 1 deg2 NIR imaging w/ 1m opt-NIR spectroscopy w/ 1–8m opt-NIR polarimetry
GW detectors
High-E satellitesWide-field imaging
Multi-mode observationMulti-band observation
OpticalKiso 6x6 deg2 camera50cm tel. (0.5x0.5 deg2)
Near-InfraredOAO-WFC(1x1 deg2)
3.8m telescope
spectroscopy polarimetry
Kanata
IRSFKanata
Near-infrared
miniTAO
IRSF
radio
Yamaguchi 32m
Nobeyama 45m
SubaruSubaru
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Summary We are developing a coordinated network of optical-
infrared-radio observations for follow-up of GW transients. This project is funded till March 2017 by Grant-in-Aid for Scientific Research on Innovative Area of MEXT (Monbu-Kagaku Sho).
The network contains several existing small optical-infrared telescopes in Japan, South-Africa, and Chile.
Two new telescopes are under construction (50cm in Tibet and 3.8m in Japan).
We plan to join the LIGO/Virgo collaboration for EM follow-up next year.
Collaboration with Korea is important and fruitful on this subject.
2012/11/29 Japan-Korea WS on KAGRA 35