1 / 35

Michitoshi YOSHIDA Hiroshima University

Optical-infrared telescope network for follow-up observation of gravitational wave transients in Japan. Michitoshi YOSHIDA Hiroshima University. Hiroshima Astrophysical Science Center. Founded in 2004 April Higashi-Hiroshima Observatory and the 1.5m optical – infrared telescope (Kanata)

duer
Download Presentation

Michitoshi YOSHIDA Hiroshima University

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Optical-infrared telescope network for follow-up observation of gravitational wave transients in Japan Michitoshi YOSHIDA Hiroshima University Japan-Korea WS on KAGRA

  2. 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.

  3. Kanata Telescope Diameter: 1.5m Ritchy – Cretien F/12 Foci: Cassegrain, 2 Nasmyths Originally constructed by Mitsubishi Electric Co. in 1996 for an instrumentation test bench of Subaru Telescope

  4. Searching for EM counter part is crucial for understanding the nature of GW sources Metzger & Berger 2012 The most promising GW sources  NS-NS merger Japan-Korea WS on KAGRA

  5. Optical, NIR and X-ray light curves of GRB130603B. NR Tanviret al.(2013) Kilonova models ejecta mass 10-1 M 10-2 M

  6. Kilonova model (Hotokezaka et al. 2013) NS-NS merger NS-BH merger Figure 3 from Progenitor Models of the Electromagnetic Transient Associated with the Short Gamma Ray Burst 130603B Kenta Hotokezaka et al. 2013 ApJ 778 L16 doi:10.1088/2041-8205/778/1/L16 Consistent with the models Mej～ 0.02 – 0.05 M Japan-Korea WS on KAGRA

  7. 2012 - 2016 PI : Takashi Nakamura (Kyoto Univ.) CoPI: Nobuyuki Kanda (Osaka City Univ.) Japan-Korea WS on KAGRA

  8. Overview of the project A01 A04 A02 A03 A05 Japan-Korea WS on KAGRA

  9. Goalsof the sub-project A02 PI: M.Yoshida • Develop an optical-infrared-radio observation network for GW transient follow-up • Kiso 6x6 deg2 Camera (optical imager) • OAO-WFC (wide-field infrared camera) • IFU for the spectrograph of 3.8m telescope • 50cm robotic telescope in Tibet(HinOTORI) • Establish a transient observation network by utilizing existing facilities: Mini-TAO, IRSF, Kanata, Yamaguchi 32m radio tel., etc. Japan-Korea WS on KAGRA

  10. 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 • KentaroMotohara (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 telescope Japan-Korea WS on KAGRA

  11. Schematic overview of the project Detection of EM counterpart of GW transient with wide-field observations Multi-mode observations  physics of EM counterpart The nature of GW transient GW alert （A04） alert Wide field obs. EM counterpart Rapid identification alert to other facilities X-γ obs. (A01) Coop. Kiso 6x6 deg2 Camera OAO IR WFC Neutrino obs. (A03) Multi-mode obs. detailed study redshift -> distance emission mechanism Multi-wavelen. detailed study identification emission mechanism Yamaguchi32m NRAO 45m Kyoto 3.8m World-wide obs. long term monitor event evolution IRSF Kanata Coop. miniTAO Subaru theory (A05) East Asia50cm

  12. Project schedule Construct the base of optical – radio follow-up observations of EM counterparts of GW transients until 2016 20122013201420152016 Regular obs. Development & preparation Test obs. Tel. contl system Kiso 6x6 deg2 camera GW transients follow-up 6x6 deg2 camera commissioning development OAOWFC Robotic obs. system Commissioning & operation development IFU of Kyoto 3.8m telescope design development commissioning operation complete Telescope design construction 50cm robotic telescope installation operation 3-color camera development Software system operation design commissioning Data analysis pipeline commissioning operation development Shift to GW transients follow-up Obs. with Kanata, Subaru, mini-TAO, IRSF, OAO-WFC, radio telescopes Transient object observation

  13. JapanCoordinated network for transients observation A part of the project “Multi-messenger Observations of GW sources” * collaborating with the KAGRA data analysis team * science cases: GRBs, supernovae, blazars, etc. • 1m KisoSchmidt telescope • 5 deg2camera  30 deg2 • 1.5m Kanata telescope • 50cm MITSuME • 91cm W-F NIR camera of NAOJ • 1 deg2 NIR camera • Yamaguchi 32m radio telescope Main features: 5 deg2 opt. imaging w/ 1m 1 deg2 NIR imaging w/ 1m opt-NIR spectroscopy w/ 1–8m opt-NIR polarimetry ★ 50cm telescope (Hiroshima Univ. 2014) 3.8m telescope (Kyoto Univ. 2015) Subaru @Hawaii ★ ★ IRSF (Nagoya Univ.) @ South Africa miniTAO (Tokyo Univ.) @ Chile Japan-Korea WS on KAGRA

  14. 1. Kiso 6x6 deg2 Camera(new instrument: 41 million Yen) Japan-Korea WS on KAGRA

  15. 1. 6x6 deg2 extremely wide field cameraKiso Observatory, the University of Tokyo Project plans 1. Development of 6deg x 6deg extremely wide field camera 2. Speeding-up and stabilizing Kiso 105cm Schmidt telescope system F.O.V 6deg x 6deg ・ 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. Results of simulation on estimation of an arrival direction of gravity wave. Hayama (NAOJ) 2012

  16. 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 • FY2012Evaluations of available CMOS sensors • Feasibility studies on cryogenics, optics, and electronics • FY2013-5Development of camera system with ~10 pcs. of available CMOS sensors. • Development of CMOS sensors with new designs. • FY2016Test observations Japan-Korea WS on KAGRA

  17. 2. OAO-WFC(install robotic observation function:15 million Yen) Japan-Korea WS on KAGRA

  18. 2. OAOWFCOkayama Astrophysical Observatory Wide Field Camera Japan-Korea WS on KAGRA

  19. 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) Japan-Korea WS on KAGRA

  20. Comparison of F.O.V.s WFCTII: 1.00 ×1.00 deg2 D=0.22m OAOWFC: 0.92 ×0.92 deg2 D=0.91m VISTA: 0.77 ×0.77 deg2 D=4.1m WFCAM: 0.46 ×0.46 deg2 D=3.8m IRIS: 0.22 ×0.22 deg2 D=0.8m D=1.4m SIRIUS: 0.13 ×0.13 deg2 OAOWFC has one of the world’s largest field of view. Japan-Korea WS on KAGRA

  21. 3. Integral Field Unit (IFU) for 3.8m telescope (new instrument: 29 million Yen) Japan-Korea WS on KAGRA

  22. prompt 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 Optical spectroscopy of possible optical counterparts of gravitational wave transients • Locations of large (>3m) optical/NIR telescopes. • No large telescopes around Japan • 3.8m telescope at Okayama is important to • make prompt optical follow-up spectroscopy Japan-Korea WS on KAGRA

  23. Integral Field Unit FoV ~ 30”x30” optical wavelength R~1000-3000 =>spectrograph Planned 3.8m telescope at Okayama Conceptual view of IFU

  24. 4. 50cm robotic telescope (new instrument: 83 million Yen) Japan-Korea WS on KAGRA

  25. 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 Japan-Korea WS on KAGRA

  26. Candidate site for the telescope West end of Tibet: ～60 degree west from Japan altitude: 5000m Japan-Korea WS on KAGRA

  27. Candidate site for the telescope West end of Tibet: ～60 degree west from Japan altitude: 5000m Gar Tibet Lhasa B1 B4 A2 A1 Japan-Korea WS on KAGRA

  28. Views of A1, A2 and B4 from B1 A1 A2 B4 Japan-Korea WS on KAGRA

  29. Telescope Alluna 50cm telescope (Germany: commercial product) Japan-Korea WS on KAGRA

  30. Optical Layout of the 3-color camera FOV: 24 arcmin^2 u’ band Ic band telescope dichroic mirror dichroic mirror Rc band Japan-Korea WS on KAGRA

  31. Operation • Fully robotic operation • Heritage of MITSuMEproject will be used. MITSuME @ OAO Japan-Korea WS on KAGRA

  32. 5. Other facilities and transients observation network Japan-Korea WS on KAGRA

  33. JapanCoordinated network for transients observation A part of the project “Multi-messenger Observations of GW sources” * collaborating with the KAGRA data analysis team * science cases: GRBs, supernovae, blazars, etc. • 1m KisoSchmidt telescope • 5 deg2camera  30 deg2 • 1.5m Kanata telescope • 50cm MITSuME • 91cm W-F NIR camera of NAOJ • 1 deg2 NIR camera • Yamaguchi 32m radio telescope Main features: 5 deg2 opt. imaging w/ 1m 1 deg2 NIR imaging w/ 1m opt-NIR spectroscopy w/ 1–8m opt-NIR polarimetry ★ 50cm telescope (Hiroshima Univ. 2014) 3.8m telescope (Kyoto Univ. 2015) Subaru @Hawaii ★ ★ IRSF (Nagoya Univ.) @ South Africa miniTAO (Tokyo Univ.) @ Chile

  34. GW detectors Wide-field imaging High-E satellites Optical Kiso 6x6 deg2 camera 50cm tel. (0.5x0.5 deg2) Near-Infrared OAO-WFC (1x1 deg2) Multi-band observation Multi-mode observation Near-infrared radio spectroscopy polarimetry miniTAO Yamaguchi 32m 3.8m telescope Kanata IRSF Nobeyama 45m Kanata IRSF Subaru Subaru Japan-Korea WS on KAGRA

  35. 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. Japan-Korea WS on KAGRA

More Related