michitoshi yoshida hiroshima university

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


NR Tanvir et al. (2013)Optical, NIR and X-ray light curves of GRB130603B.

Kilonova models

ejecta mass10-1 M10-2 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


2012 - 2016

PI : Takashi Nakamura (Kyoto Univ.)CoPI: Nobuyuki Kanda (Osaka City Univ.)


Overview of the project

A01

A02

A03

A04

A05


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.

2012/11/29 9

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

SoftwaresystemData analysispipelineTransient objectobservation

Tel. contl system6x6 deg2 camera development

development

development

design development commissioning

commissioning

Development & preparation Test obs. Regularobs.

installation

GW transients follow-up

commissioning

Commissioning & operation

Telescope design construction3-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


1. Kiso 6x6 deg2 Camera(new instrument: 41 million Yen)


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 observations2012/11/29 16Japan-Korea WS on KAGRA

2. OAO-WFC(install robotic observation function:

15 million Yen)


2. OAOWFCOkayama Astrophysical Observatory Wide Field Camera


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)


WFCT II: 1.00 ×1.00 deg2D=0.22m

Comparison of F.O.V.sD=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)


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 Þ 3.8m telescope at Okayama is important to make prompt optical follow-up spectroscopy


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)


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


Candidate site for the telescopeWest end of Tibet: ～ 60 degree west from Japan altitude: 5000m


A1A2

B4

B1

Lhasa

Gar

Candidate site for the telescope

Tibet

West end of Tibet: ～ 60 degree west from Japan altitude: 5000m


A1A2

B4

Views of A1, A2 and B4 from B1


TelescopeAlluna 50cm telescope(Germany: commercial product)


Optical Layout of the 3-color camera

u’ band

Rc band

Ic bandtelescope

dichroic mirror dichroic mirror

FOV: 24 arcmin^2


Operation Fully robotic operation

Heritage of MITSuME project will be used.

MITSuME @ OAO


5. Other facilities and transients observation network


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 detectorsHigh-E satellites

Wide-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

KanataIRSFKanata

Near-infrared

miniTAOIRSF

radio

Yamaguchi 32mNobeyama 45m

SubaruSubaru


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

michitoshi yoshida hiroshima university

Documents

yoshidajapankorea ws

m201211296japankorea

kiso schmidt telescope

radio observation network

kanata telescope diameter

transient observation

observation of targets

coordinated observation