Activity of Astrophysics in Hiroshima Group, led by T.Ohsugi - PowerPoint PPT Presentation

Activity of Astrophysics in Hiroshima Group, led by T.Ohsugi Yasushi Fukazawa Hiroshima Unversity Fermi/LAT X-ray satellite Suzaku Kanata Telescope 1

Observational Astrophysics Group in Hiroshima Univ. 2000- Gamma-ray and X-ray Observation Group T.Ohsugi, Y.Fukazawa(, T.Kamae) 2004- Hiroshima Astrophysical Science Center T.Ohsugi, K.Kawabata As of 2011 Gamma-ray,X-ray T.Ohsugi, Y.Fukazawa, T.Mizuno, H.Takahashi, M.Ohno Optical T.Ohsugi, M.Yoshida, K.Kawabata, M.Uemura, H.Akitaya Pos Doc 2 Graduate students D 8, M 12 Undergraduate students 7

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Persons with different backgrounds are collaborating. T.Ohsugi Particle Physics, Detector Y.Fukazawa X-ray observation, Detector K.Kawabata Optical observation, Detector Ohsugi-san said, You should not confine to a specific wavelength observation. A final goal is to understand astrophysical phenomena, so multi-wavelength observation is essential. We should utilize all the available observatory as much as possible. 4

Multi-wavelength Observation in Hiroshima Group Kanata Telescope Fermi/LAT X-ray satellite (2006-) (2008-) Suzaku (2005-) Unique in Japan High-energy astronomical phenomena

Crab Nebula Optical X-ray Multi-wavelength Spectra Multi- wavelength observation is important ! Radio Optical X-ray GeV TeV

High-energy objects are variable. Gamma-ray Sky with Fermi/LAT. 7

MISSION ELEMENTS m • Large Area Telescope sec GPS & GBM • - • Telemetry 1 kbps Fermi Spacecraft • TDRSS SN S & Ku DELTA • 7920H • S - - • GN • LAT Instrument White Sands Science Schedules Operations Center Mission Operations Science Center (MOC) Support Center HEASARC Schedules GRB GBM Instrument Coordinates Network Operations Center Alerts Data, Command Loads 8

Activity for Fermi/LAT  Development and Fabrication of Silicon Strip Sensors Balloon Flight Experiment Beam Test @CERN e – e Data Monitor (after launch) + Data Analysis (after launch) 9

Important contribution of Japan Development and Production of Silicon Strip Detectors By Hiroshima Univ. and HPK About 10,000 SSDs Supported by KEK US- J Collabo Fund, MEXT… Very High Quality Extremely low rate of dead strip 0.008% in 9500 SSD × 384 strips ＝ 3.7M strips Stable Performance Full-depletion voltage Leak Current ～ 65 V ～ 2.5 nA/cm ２  = 9 kWcm

Certificate of Appreciation from NASA to T.Ohsugi (2005)

Prof. T.Ohsugi retired from School of Science, Hiroshima University (2008 March), just before launch. T.Ohsugi continues his activity as a head of Higashi- Hiroshima Observatory. Final Lecture of T.Ohsugi 12

GLAST/Fermi launch 2008 June Press Conference 13

Fermi/LAT Collaboration Meeting in Hiroshima (2009 March) 14

Higashi-Hiroshima Observatory and Kanata Telescope T. Ohsugi T. Muta (President of Hiroshima U. in 2001-2006 ) 2000 Hiroshima University proposed to receive the optical telescope in NAOJ and utilize it to observe GLAST(Fermi) gamma-ray objects. 2002 Task force team of movement started the activity. Measurement of Observational Seeing Strong Support from Higashi-Hiroshima city 15 2004 Decision of movement

Higashi-Hiroshima Observatory （東広島天文台） • Found in 2006 • Only 20 min by car from campus (503m above sea level • Better weather condition and seeing relatively within Japan Red: Sunny >2000hr/yr Kyoto Okayama OAO Hiroshima Osaka HHO Hiroshima Univ. Higashi Hiroshima Observatory

Kanata Telescope 1.5m diameter Optical/Near Infrared （ the 4 th largest in Japan 、 2 nd among University ） • Very fast speed of pointing  Observe transient objects (gamma-ray bursts, AGNs,…) 2011/8/5 17

Kanata Telescope Originally constructed as a simulator of Subaru telescope in 1994 at Mitaka campus, NAOJ Before moved to Hiroshima, – Driving/control system replaced – Speed up of telescope pointing renewal （ 1deg/s ⇒ 5deg/s in azimuth ） 30 seconds in average to take to finish pointing to the next object – Automatic focus switching system – (New ceramic secondary mirror)  Capable of prompt observation of GRB, etc.

Subaru Telescope Kanata Telescope 2011/8/5 19

Telescope and Instruments Nasmyth#2 Nasmyth#1 High Speed-readout HOWPol 2009- spectrograph Imaging ： FoV 15′Φ ImagPol ： One-shot type FoV: 2.3’ × 2.3′ wide-f ： 7′(GRB -AG) Wavelength res.: R = λ/Δλ narrow- f: 1′ × 15′ = 9-70 （ 400-800nm ）、 Spec ： R~400(400-1050nm) 150 （ 430-690nm ） ~30 frames/sec Cassegrain TRISPEC: 2006-2011 HONIR : 2011- 1 Optical band + 2 Near-IR bands (simultaneously) Imaging ： FoV 7′ × 7′(T) 10′ × 10′(H) Spec ： R~150, 150, 360(T) ~300(H) ImagPol/SpecPol （ 3-4 shots necessary)

X-ray Observatory: Suzaku (ASTRO-E1,E2) satellite The 5 th Japanese X-ray Observatory Launch 2005 Well Unit Side Anti Unit Corner Passive Fine Collimator 60 Anti Unit GSO/BGO phoswich counter 4 25.5 25.5 BGO 60 40 8 10 57 320 60 57 380mm 340mm Diode GSO 40 2mmt Si-PIN 340mm Diode (HPK) Photomultiplier + pre-Amplifier HXD(Hard X-ray Detector) 340mm TOP VIEW CROSS-SECTION

The 6 th Japanese X-ray Observatory ASTRO-H (2014-) HXI DSSD APD (HPK) ΔE=4eV SGD Si-Pad APD (HPK) CCD(HPK) 22 Talk by Ohno, Hayashi, Saito in this conference

Active Galactic Nuclei with Jets Kanata monitored. IBL FSRQ PKS 0048-097 Mis V1436 S2 0109+224 PKS 0215+015 3C 66A QSO 0324+341 PKS0422+004 QSO 0454-234 S5 0716+714 OJ49 PKS 0754+100 QSO 1239+044 OJ 287 3C 279 ON 231 PKS 1502+106 PKS 1749+096 PKS 1510-089 3C371 3C 454.3 LBL 1ES 0323+022 AO 0235+164 1ES 0647+250 S5 1803+784 1ES 0806+524 BL Lac Mrk 421 HBL ON 325 Unknown PG 1553+113 PKS1222+216 H 1722+119 PX J1542.8+612 Mrk 501 S4 0954+65 1ES 1959+650 3EG 1052+571 PKS 2155-304 4C 14.23 1ES 2344+514

FSRQ 3C 279 Abdo et al. 2010. Nature Gamma-ray Flux Kanata found a rotation of Gamma-ray Index polarization vector, associated with Gamma-ray X-ray Flux flare. Optical Flux Suggested Bending Jet Polarization degree Polarization angle NIR flux Radio flux MJD -5400 [day]

Discovery of Giant gamma-ray lobe Abdo+10, Science ( One of Contact Authors: Y.Fukazawa ) Gamma-ray Image Moon 2M light year Centaurus A

Suzaku X-ray Spectra Radio Galaxy; 2009 Centaurus A 2005 Spectra became harder in 2009 than in 2005, suggesting an additional hard component. Abdo+10 Fukazawa+11 Suzaku COMPTEL (2009) (1991-1995) Jet? Fermi (2008-2009) Fermi Error circles

Gamma-ray Burst Constrain the Quantum Gravity Effect With Fermi/LAT, from the delay of high-energy gamma-ray Abdo+09, Nature ( One of contact authors: M.Ohno ) Gamma-ray Energy time GRB090510 Pulsar GRB AGN GRB AGN GRB080916C Planck mass min M QG (Kaaret 99) (Ellis 06) (Biller 98) (Boggs 04) (Albert 08) (GeV/c 2 ) 10 15 1.8x10 15 0.9x10 16 4x10 16 1.8x10 17 0.2x10 18 10 16 10 17 10 18 10 19 1.5x10 18 1.2x10 19 27 1.6x10 19

Suzaku, HXD-WAM Gamma-ray bursts (150/year) Solar Flares Transient Sources Ohno+06 HXD-WAM (Wide-band All-sky Monitor) Well Unit Side Anti Unit Corner Passive Fine Collimator 60 Anti Unit 4 25.5 25.5 BGO 40 60 8 10 57 320 60 57 380mm 340mm Diode GSO Swift 40 HXD-WAM 340mm Photomultiplier + pre-Amplifier 340mm CROSS-SECTION TOP VIEW

Uehara+11 Kanata observations of Gamma-ray burst afterglows Polarization 29

Kanata observations of Light curve SuperNovae Spectra 30 Yamanaka et al. 2009

Suzaku observations of black-hole, newtron star binaries Best-fit nuFnu spectral models determined with Suzaku Compton cloud i ~45 deg Accretion disk i ~75 deg H.Takahashi et al . PASJ 60 , S69 (2008) Makishima et al . PASJ 60 , in press

Multi-wavelength Observation in Hiroshima University was activated, led by T.Ohsugi, and is now nicely going on. We thanks T. Ohsugi, and we are going to continue and extend our activities. 32