1. Michitoshi YOSHIDA HASC, Hiroshima University 2014/01/14G.W. 2nd Symposium @ TITech1

2. Searching for EM counter part is crucial for understanding the nature of GW sources The most promising GW sources  NS-NS merger Metzger & Berger 2012 2 Nearly isotropic emission from ejecta of NS-NS coalescence = Kilo-nova is one of promising EW counterpart of GW sources

3. NR Tanvir et al. (2013) Optical, NIR and X-ray light curves of GRB130603B. Kilonova models ejecta mass 10 -1 M  10 -2 M  2014/01/143 z=0.356 ～ 20-21 mag @200Mpc

4.  Develop an optical-infrared-radio observation network for GW transient follow-up 1.Kiso 6x6 deg 2 Camera (optical imager) 2.OAO-WFC (wide-field infrared camera) 3.IFU for the spectrograph of Kyoto 3.8m telescope 4.50cm robotic telescope in Tibet 5.Establish a transient observation network by utilizing existing facilities: Mini-TAO, IRSF, Kanata, Yamaguchi 32m radio tel., etc. 2014/01/144 PI: M.Yoshida G.W. 2nd Symposium @ TITech

5.  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 telescope 2014/01/145G.W. 2nd Symposium @ TITech

6. World-wide obs.  long term monitor event evolution Kanata IRSF GW alert （ A04 ） theory (A05) X-γ obs. (A01) Neutrino obs. (A03) Kiso 6x6 deg 2 Camera OAO IR WFC Kyoto 3.8m Yamaguchi32m NRAO 45m Multi-wavelen.  detailed study identification emission mechanism Multi-mode obs.  detailed study redshift -> distance emission mechanism East Asia50cm Subaru miniTAO Wide field obs.  EM counterpart Rapid identification alert to other facilities alert Coop. Detection of EM counterpart of GW transient with wide-field observations Multi-mode observations  physics of EM counterpart The nature of GW transient 6 TAO 6.5m

7. 2012 2013 2014 2015 2016 Kiso 6x6 deg 2 camera OAOWFC Robotic obs. system 50cm robotic telescope IFU of Kyoto 3.8m telescope Software system Data analysis pipeline Transient object observation Tel. contl system 6x6 deg 2 camera development designdevelopmentcommissioning Development & preparationTest obs. Regular obs. installation GW transients follow-up commissioning Commissioning & operation Telescope designconstruction 3-color camera development complete 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 72014/01/14G.W. 2nd Symposium @ TITech

8. IRSF (Nagoya Univ.) @ South Africa 1m Kiso Schmidt telescope 5 deg 2 camera  30 deg 2 1.5m Kanata telescope 50cm MITSuME 91cm W-F NIR camera of NAOJ 1 deg 2 NIR camera Yamaguchi 32m radio telescope ★ ★ miniTAO (Tokyo Univ.) @ Chile 50cm telescope (Hiroshima Univ. 2014) A02 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 deg 2 opt. imaging w/ 1m 1 deg 2 NIR imaging w/ 1m opt-NIR spectroscopy w/ 1–8m opt-NIR polarimetry 2014/01/148

9. 9G.W. 2nd Symposium @ TITech

10. previous 105cn KISO Schmidt telescope improved Drive mechanics Cabling Controller Kiso is an old observatory (founded 1974) Clock-drive tracking-system with fast and slow gears Low-resolution encoders Old-fashioned electrical system Driving speed: 1.5  2.0 deg/sec Pointing-accuracy: ~ 100  ~ 10 arcsec Intelligent system Achieve Stable operation and Quick response to alerts of GW Events Direct driving system with servo motors Compact & stable control system upgrade

11.  Kiso Supernova Survey (KISS)  Shock-breakout survey  Carried out using KWFC (Wide Field CCD Camera)  Requires instantaneous alert system  Now a pipeline to identify outbreak objects is working  Data reduction  Image Subtraction  Identify variable objects  Create web page for screening by human-eyes  All done within 10 minutes  Possibly applicable to GW event identification ReferenceNew Subtracted 11

12.  2 runs in FY2013  Jun : Cancelled due to heavy snow  Oct-Nov :  Lightning damages found at the telescope and the dome  Power Generator Trouble ⇒ Both fixed in October  Successful ANIR observational run : 11/20-11/30  New building under construction at San Pedro de Atacama  With remote operation room for miniTAO  Will be completed within FY2013  Large laboratory, office, kitchen, bedrooms… 2014/01/14G.W. 2nd Symposium @ TITech12

13. 2014/01/1413G.W. 2nd Symposium @ TITech

14.  Primary work in 2013  Optical alignment 1. Primary mirror optical axis 2. Telescope tube center  Goal: Shift < 1.0mm & Tilt < 0.1 deg.  Measurements  Optical axis : Hartmann test  Tube center: Laser zenith plummet & pin-hole  During the measurements  Displacement(9mm) between the primary mirror center and the optical axis was found. It was fixed by shifting the mirror cell with respect to the telescope tube center.  Adjustment Status  Shift < 0.4 mm, Tilt < 0.02 deg.  Commissioning will start in next spring. 2014/01/14G.W. 2nd Symposium @ TITech14

15. A ： Telescope pointed toward zenith B: Laser zenith plummet C: Pin hole(φ1mm ） disk D ： The pin-hole located at the tube center is irradiated by the laser zenith plummet E: Diffraction image on the prime focus CCD. The center corresponds the tube center. ABC D E 2014/01/14G.W. 2nd Symposium @ TITech15

16. T ~ a( (x – x0) 2 + (y – y0) 2 ) + z0 T : Hartmann const[ arcsec ] x0, y0 : optical axis x0 = 1528 +/- 4.8 [pix] y0 = 782 +/- 5.6 [pix] z0 = 0.956 +/- 0.007 [arcsec] image scale : 0.58 [arcsec/pix] ＋ location of reference stars Distribution of Hartmann constants In 3D 2014/01/14G.W. 2nd Symposium @ TITech16

17. 2014/01/1417G.W. 2nd Symposium @ TITech

18. Optical follow-up spectroscopy of GW sources and sGRBs with IFU Case for 188 cm telescope Case for 3.8 m telescope fibre bundle KOOLS IFU in HIDES fibre-feed Movable IFU 182014/01/14G.W. 2nd Symposium @ TITech Opt spectrograph KOOLS

19. 19 Follow-up observation strategy for GW source GW alert from KAGRA + LIGO/VIRGO (position accuracy > several degrees) optical counterpart search with wide field cameras (position accuracy ~ a few arcsec) spectroscopy with KOOLS-IFU (field of view = 15”—30”) 2014/01/14G.W. 2nd Symposium @ TITech

20. 20 Tanaka & Hotokezaka (2013) i -band (~8000 Å) KOOLS-IFU with 3.8 m telescope exposure = 1800 sec x 9 frames best condition -> S/N = 9 at 20 Mpc 600 sec exposure -> S/N = 61 2014/01/14G.W. 2nd Symposium @ TITech Kilo nova

21. micro- lens array fibre bundle CCD Spectrograph ： KOOLS Kyoto Okayama Optical Low-resolution Spectrograph We will add a fibre bundle and micro-lens arrays. 2014/01/14G.W. 2nd Symposium @ TITech21

22. Expected observation parameters telescopeOAO 188 cmKyoto 3.8 m spatial sampling1.8” / fiber0.91” / fiber number of fibres127 field of view30”15” filling factor 58 % observable 4000—8500 Å spectral resolution R =  /  ~ 700 sensitivity (best) ※ 19.0 mag20.0 mag ※ obs = 6000 Å, exposure = 1800 sec, S/N = 10, combine 2 wavelength- pixels (= 7.6 Å), seeing = 1.0”

23. 23 Fibre bundle: tested and ordered core/cladding diameter: 100/125  m length: 24 m throughput: ~80 % Status of development Entrance side Microlens array: in hand Pre-optics:designed and ordered 2014 1 st half:Assemble and install in KOOLS(spectrograph) 2014 2 nd half: test obs w/ 188cm? 24m bundle 2014/01/14G.W. 2nd Symposium @ TITech

24. 2014/01/1424G.W. 2nd Symposium @ TITech

25.  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. R c -band  20.8 mag. I c -band 2014/01/1425G.W. 2nd Symposium @ TITech

26. West end of Tibet: ～ 60 degree west from Japan altitude: 5000m 2014/01/1426G.W. 2nd Symposium @ TITech

27. A1 A2 B4 B1 Lhasa Gar Tibet West end of Tibet: ～ 60 degree west from Japan altitude: 5000m 2014/01/1427G.W. 2nd Symposium @ TITech

28. A1 A2 B4 Views of A1, A2 and B4 from B1 2014/01/1428G.W. 2nd Symposium @ TITech

29. Telescope Alluna 50cm telescope (Germany: commercial product) 2014/01/1429G.W. 2nd Symposium @ TITech

30. Optical Layout of the 3-color camera u ’ band R c band I c band telescope dichroic mirror FOV: 24 arcmin^2 2014/01/1430G.W. 2nd Symposium @ TITech

31.  Fully robotic operation  Heritage of MITSuME project will be used. MITSuME @ OAO 2014/01/1431G.W. 2nd Symposium @ TITech

32. 2012 2013 2014 2015 2016 Kiso 6x6 deg 2 camera OAOWFC Robotic obs. system 50cm robotic telescope IFU of Kyoto 3.8m telescope Software system Data analysis pipeline Transient object observation Tel. contl system 6x6 deg 2 camera development designdevelopmentcommissioning Development & preparationTest obs. Regular obs. installation GW transients follow-up commissioning Commissioning & operation Telescope designconstruction 3-color camera development complete 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 322014/01/14G.W. 2nd Symposium @ TITech

33. 2012 2013 2014 2015 2016 Kiso 6x6 deg 2 camera OAOWFC Robotic obs. system 50cm robotic telescope IFU of Kyoto 3.8m telescope Software system Data analysis pipeline Transient object observation 6x6 deg 2 camera development designdevelopmentcommissioning development Development & preparationTest obs. Regular obs. installation GW transients follow-up SN search software Commissioning & operation Telescope designconstruction 3-color camera development complete 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 332014/01/14G.W. 2nd Symposium @ TITech Tel. contl system development Initial testing development complete

34. 2014/01/14G.W. 2nd Symposium @ TITech34 2013/7 Letter of Interest 2013/8 Collaboration meeting @Amsterdam 2013/12 Call for participation 2014/2 Deadline CfP We will join this collaboration

35. 352014/01/14G.W. 2nd Symposium @ TITech 2014 2015 2016 Kiso 6x6 deg 2 camera OAOWFC Robotic obs. system 50cm robotic telescope IFU of Kyoto 3.8m telescope Software system Data analysis pipeline Transient object observation 6x6 deg 2 camera development install commissioning development Development & preparation Test obs. Regular obs. Shipping & installation GW transients follow-up SN search software Commissioning & operation 3-color camera development Assemble & commissioning operation Obs. with Kanata, Subaru, mini-TAO, IRSF, OAO-WFC, radio telescopes operation design commissioning Training observation commissioning Training observation with GBM LIGO/Virgo EM follow-up

36.  Current status  Improvement of the control system of Kiso Schmidt telescope has been done  Development of OAO-WFC  by April 2014  Initial testing of IFU for Kyoto 3.8m telescope has been done  50cm telescope & three color camera  by May 2014  Future plans  Development of 6x6 deg2 CMOS camera (Sako’s talk)  Start test observation with OAO-WFC  Install IFU to KOOLS spectrograph of OAO  Commissioning of Tibet telescope system  shipping to China  Training observations using GBM (Fermi) alert 2014/01/14G.W. 2nd Symposium @ TITech36