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

Activity of Astrophysics in Hiroshima Group, led by T.Ohsugi

Hiroshima Unversity

Yasushi Fukazawa

1

Kanata Telescope Fermi/LAT X-ray satellite Suzaku

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

3

4

T.Ohsugi Particle Physics, Detector Y.Fukazawa X-ray observation, Detector K.Kawabata Optical observation, Detector Persons with different backgrounds are collaborating. Ohsugi-san said, You should not confine to a specific wavelength

• bservation. 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.

Kanata Telescope (2006-) Fermi/LAT (2008-) X-ray satellite Suzaku (2005-)

Multi-wavelength Observation in Hiroshima Group

High-energy astronomical phenomena

Unique in Japan

Radio Optical X-ray GeV TeV

Crab Nebula Optical X-ray

Multi-wavelength Spectra

Multi- wavelength

• bservation is

important !

High-energy objects are variable.

7

Gamma-ray Sky with Fermi/LAT.

GN

HEASARC

• DELTA

7920H

• White Sands

TDRSS SN S & Ku

LAT Instrument Science Operations Center GBM Instrument Operations Center GRB Coordinates Network

• Telemetry 1 kbps
• S

Alerts Data, Command Loads Schedules Schedules

Mission Operations Center (MOC) Science Support Center

• m

sec

• Fermi Spacecraft

Large Area Telescope & GBM GPS

MISSION ELEMENTS

8

9

e

+

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

in 9500 SSD×384 strips＝3.7M strips Extremely low rate of dead strip 0.008% Very High Quality Stable Performance Development and Production of Silicon Strip Detectors By Hiroshima Univ. and HPK About 10,000 SSDs

～2.5 nA/cm２ ～65 V = 9 kWcm

Important contribution of Japan Leak Current Full-depletion voltage

Supported by KEK US-J Collabo Fund, MEXT…

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

12

• 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

13

GLAST/Fermi launch 2008 June Press Conference

14

Fermi/LAT Collaboration Meeting in Hiroshima (2009 March)

15

Higashi-Hiroshima Observatory and Kanata Telescope

2000 Hiroshima University proposed to receive the optical telescope in NAOJ and utilize it to observe GLAST(Fermi) gamma-ray objects.

• T. Ohsugi
• T. Muta

(President of Hiroshima U. in 2001-2006)

2002 Task force team of movement started the activity. Measurement of Observational Seeing Strong Support from Higashi-Hiroshima city 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

Hiroshima Univ. Higashi Hiroshima Observatory

Osaka Kyoto Okayama OAO Hiroshima HHO

Red: Sunny >2000hr/yr

Kanata Telescope

1.5m diameter Optical/Near Infrared

（the 4th largest in Japan、2nd among University）

• Very fast speed of pointing

 Observe transient objects (gamma-ray bursts,

AGNs,…)

2011/8/5 17

– Driving/control system replaced – Speed up of telescope pointing （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. Originally constructed as a simulator of Subaru telescope in 1994 at Mitaka campus, NAOJ Before moved to Hiroshima,

renewal Kanata Telescope

2011/8/5 19

Subaru Telescope Kanata Telescope

Telescope and Instruments

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)

High Speed-readout spectrograph

FoV: 2.3’×2.3′ Wavelength res.: R = λ/Δλ = 9-70（400-800nm）、 150（430-690nm） ~30 frames/sec

Cassegrain Nasmyth#2 HOWPol 2009-

Imaging： FoV 15′Φ ImagPol： One-shot type wide-f： 7′(GRB-AG) narrow-f: 1′×15′ Spec： R~400(400-1050nm)

Nasmyth#1

X-ray Observatory: Suzaku (ASTRO-E1,E2) satellite The 5th Japanese X-ray Observatory

340mm 340mm BGO Diode GSO Photomultiplier + pre-Amplifier

TOP VIEW CROSS-SECTION

Well Unit Side Anti Unit Corner Anti Unit Passive Fine Collimator

320

340mm

380mm

2mmt Si-PIN Diode (HPK) GSO/BGO phoswich counter

HXD(Hard X-ray Detector) Launch 2005

22

The 6th Japanese X-ray Observatory

ASTRO-H (2014-) HXI SGD

Talk by Ohno, Hayashi, Saito in this conference

DSSD APD (HPK) Si-Pad APD (HPK) CCD(HPK) ΔE=4eV

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

Active Galactic Nuclei with Jets Kanata monitored.

FSRQ 3C 279

Abdo et al. 2010. Nature

MJD -5400 [day]

Gamma-ray Flux Gamma-ray Index X-ray Flux Optical Flux Polarization degree Polarization angle NIR flux Radio flux

Kanata found a rotation of polarization vector, associated with Gamma-ray flare. Suggested Bending Jet

Discovery of Giant gamma-ray lobe

2M light year

Moon

Centaurus A Gamma-ray Image

Abdo+10, Science (One of Contact Authors: Y.Fukazawa)

Abdo+10

Suzaku X-ray Spectra

Spectra became harder in 2009 than in 2005, suggesting an additional hard component.

2005 2009 Jet?

COMPTEL (1991-1995) Fermi (2008-2009)

Suzaku (2009)

Fukazawa+11

Fermi Error circles Radio Galaxy; Centaurus A

27

min MQG (GeV/c2) 1016 1017 1018 1015 1.8x1015

Pulsar (Kaaret 99)

0.9x1016 1.8x1017 0.2x1018 4x1016

GRB (Ellis 06) GRB (Boggs 04) AGN (Biller 98) AGN (Albert 08)

GRB080916C Planck mass 1019 1.5x1018 1.2x1019 GRB090510 1.6x1019

Gamma-ray Burst

Constrain the Quantum Gravity Effect With Fermi/LAT, from the delay of high-energy gamma-ray time

Gamma-ray Energy

Abdo+09, Nature (One of contact authors: M.Ohno)

Suzaku, HXD-WAM Swift HXD-WAM

340mm 340mm BGO Diode GSO Photomultiplier + pre-Amplifier

TOP VIEW CROSS-SECTION

Well Unit Side Anti Unit Corner Anti Unit Passive Fine Collimator

340mm

HXD-WAM

(Wide-band All-sky Monitor)

Gamma-ray bursts (150/year) Solar Flares Transient Sources

Ohno+06

29

Uehara+11

Kanata observations of Gamma-ray burst afterglows Polarization

30

Yamanaka et al. 2009

Light curve Spectra

Kanata observations of SuperNovae

i~45 deg i~75 deg

H.Takahashiet al. PASJ 60, S69 (2008) Makishima et al. PASJ 60, in press

Best-fit nuFnu spectral models determined with Suzaku

Compton cloud Accretion disk

Suzaku observations of black-hole, newtron star binaries

32

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.