Gamma-ray Observation in Space

Transcription

1 T.Takahashi

2 Gamma-ray Observation in Space Synergy between X-ray and Gamma-ray Observation present and future Tadayuki Takahashi Institute of Space and Astronautical Science (ISAS) Yasushi Fukazawa Hiroshima Univ. Makoto Tashiro Saitama Univ. Astro-E2/Swift/Glast Astro-E2/Glast Astro-E2/Swift

3 INTEGRAL 2002 Gamma-ray Mission in 21st Century GLAST 2006 Swift 2003 Chandra Newton AstroE II AstroE Astro-E AGILE 2003

4 X-ray/Gamm-ray Observation is Hot plasma High Temperature electron/ion crucial to access Black Hole X-ray Jet Non-Themal Emission from accelerated Particle Gamma-ray Non-Thermal Emission from the extremely high density/temperature plasma Toward the event horizon Black Hole (Makishima et al. 2002) Hard X-ray & Gamma-ray

5 To Probe Obscured Black Hole NGC4945 Done et al. 1996

6 Optical/HST Van der Marel et al.,2002 Binary BH in NGC 6240 N S X-ray/Chandra Komossa et al., 2002 Source of Gravitational Wave? from presentation by

7 Gamma-ray Black Hole (Blazars) surprise! PKS Mkn421 Kubo et al Synchrotron, peak at IR-X ray energies Inverse Compton, peak at GeV-TeV energies from the same electron distribution The relativistic jet points close to the observer. The nonthermal emission is Doppler boosted and greatly enhanced.

8 Blazar Variability & Internal Mrk kev Shocks Simulation Observation 4/25 4/26 4/27 4/28 4/29 4/ Time (hours since April :00 UT ) Takahashi et al EUVE 1keV 6.3keV 15keV R fo =0.7, T chr =40 ks D 0 =1x1013 cm s G =0.015, G =15 (assumed) Γ / σ Γ =1,000 from G. Madejski, 2001 L kin ~1,000 L jet Tanihata, Takahashi, Kataoka et al. 2002, Iwamoto, Takahara et al. 2003

9 Particle Accelerator in SNRs (1) The remnant of SN 1006 Discovery of synchrotron X-ray emission by ASCA (Koyama et al. 1995) X-ray image X-ray spectrum CANGAROO TeV Gamma-ray (Tanimori et al. 1998) I(ε) ε Γ Photon index =3.0 2 hν synch = 5.3 E 100TeV Log Power-law type spectrum = synchrotron radiation B 10µG [kev] Bamba et al Direct evidence of > 10 TeV particles (from presentation X-ray observation highest energy electrons by Uchiyama 2003)

10 Particle Accelerator in SNRs (2) GeV -ray TeV -ray Accelerator Target molecular cloud ASCA Emission due to electron/proton interaction in the dense molecular cloud Characteristic 1/ Spectrum (Uchiyama, Takahashi and Aharonian,2002) Filament Chandra

11 Annihilation Fountain in the Center of Milky Way CGRO-OSSE 511 kev Purcell et al. 1977

12 Deep Sky: Black holes are ubiquitous in the Universe

13 Gamma-ray Burst BASTE Afrerglow: X-ray Images from BeppoSax 6 hours 48 hours Optical discoveries of host galaxies and measurements of spectroscopic redshift distances HST Gamma Ray bursts are occuring in distant (z = 1-3) galaxies Most powerful and relativistic phenomena known ( ergs)

14 Present and Future X-ray/Gamma-ray Missions >10 16 AGASA, HiRes, A U G E R >PeV Milagro Whipple,Cangaroo1/2 CAT, HEGRA Cangaroo3, VERITAS H E S S MAGIC TeV Energy in ev EGRET OSSE CMPTL Celeste, STACEE RXTE, BeppoSAX HETE2 AGILE I N T E G R A L SWIFT X M M AstroE2 C h a n d r a G L A S T AstroE2 MAXI NeXT (Japan) Constellation X GeV MeV kev Year of Operation Compiled by Kamae (2002)

15 Electro-Magnetic Radiation and Electron Energy Electron Energy kev MeV GeV TeV Radio Synchrotron GLAST(Bremsstrahlung) GLAST(Inverse Compton) X-ray Brems. X-ray Inv.Compton X-ray Synch.

16 from Integral Homepage Integral Mission (2002-) Big Gamma-ray Mission After CGRO (15 kev 10 MeV) Imaging (Coded Mask) High Energy Resolution X-ray Detector (JEM-X)

17 from Integral Homepage High resolution Gamma-ray detector (SPI) 19 Cooled Ge detector (each 6x7 cm) FWHM : 1.3 MeV

18 from Integral Homepage Solar Flare Spectrum by SPI

19 from Homepage

20 INTEGRAL Integral Science High Energy and Spatial Resolution Line Gamma-ray from Nuclear Decay 511 kev Annihilation line from our galaxy by OSSE osi 44 Ti and 26 Al (and more) from past SN explosions Vela region 1.5 MeV 1.8 MeV INTEGRAL SPI (Tobs = 10 6 s) 44 Ti 26 Al by Comptel

21 from Integral Homepage Galactic Plane Scan Cen region with ISGR (CdTe Imager)

22 Rapid response satellite sec to slew within FOV of BAT Swift Mission (2003- ) autonomous operations factor 100 improved response time continue monitoring of fading afterglow Multi-wavelength observatory Burst Alert Telescope (BAT): kev detect ~ 300 gamma ray bursts per year onboard computation of positions arc-minute positional accuracy Dedicated telescopes for X-rays, UV, and optical afterglow follow up: kev X-ray Telescope (XRT) nm UV/Optical Telescope (UVOT) arc-second locations existing hardware from JET-X and XMM determine redshifts from X-ray absorption, lines, and Lyman-α cutoff

23 BAT Imager on Swift CdZnTe detectors 4x4 mm 2 x2mm t detector Japanese Contribution to Calibration/Software (ISAS/Saitama U./U. Tokyo)

24 Multiwavelength Cascade of Images Gamma Ray (arc-minute) X-ray (2.5 arc-second) HST, Keck, etc. UVOT (0.3 arc-second)

25 Swift Performance Location in host galaxies Probe the surrounding environment Use gamma-ray bursts as cosmological probes Sensitivity GRB980228

26 AstroE2 Multi-band Mission Recovery Mission of Astro-E Launch in 2005 Design almost identical to Astro-E AstroE2 Five thin-foil mirrors Four X-ray CCD cameras(xis) Microcalorimeter array(xrs) Launch 2005 Feb. ISAS Non-imaging Hard X-ray detector XRS CCD(XIS) Chandra Newton S(cm 2 ) ,000 E(e V) Fe 6.7KeV arcsec) E rage (kev) 0.3~10 0.3~12 HXD Astro-E 5, ~600

27 Hard X-ray Detector (HXD) passive fine collimator (FOV FWHM ~30 ) Narrow FOV by well type (phoswitch) active shield & passive fine collimator (<100keV) Wide energy band ( kev) w/ 64 Si-PIN (2mm thick) diodes Background rejection w/ LSI pulse shape discrimination anti-coincidence with 36 detector units & onboard CPU software Low Background & High sensitivity are expected Si-PIN diode GSO detection crystal BGO active shield/ Well type collimator (FOV~4deg)

28 Astro-E2 HXD & Integral Continuum Spectrum Continuum Sensitivities for HXD and INTEGRAL JEM-X HXD Tobs =10 5 s SIGMA OSSE IBIS HXD-II has much narrower FOV and thus Background is lower and the sensitivity is higher. CGRO/ INTEGRAL Tobs = 10 6 s SPI COMPTEL Simultaneous observation with highly sensitive X-ray instruments gives us very unique opportunities to study gamma-ray sources.

29 High Resolution Detector (XRS) on AstroE2 Bulk motions of ICM in cluster mergers will be detected for the first time Counts FWHM: ev Direct measure of gas temperature Energy [ev] eV kt (kev) (Inoue, 2002)

30 Glast Mission GLAST Large Area Telescope (LAT) Burst Monitor (GBM) SLAC Utilize Pair-production International Mission Japanese Contribution (Hiroshima, ISAS, RIKEN, Titech) Wide FOV, Survey Operatiom 20MeV GeV Large Area Silicon Strips.

31 Tracker Module Mechanical Design 16 Towers cm 4 4 array of Sistrip sensors (X) by Hiroshima Univ. Bias supply C-fiber face shee Hex cell core Al closeout C-fiber face sheet converter Carbon thermal panel Readout circuit 4 4 array of Si-strip sensors (Y)

32 New approach GLAST will bring forth -EGRET s3 rd Catalog in 2 days sec All 3EG sources + ~ 80 new in 2 days Time Variability Monitoring: Flares (Blazars, AGNs, Coronas), Precessions and Glitches (Pulsars), Lensing (AGNs) 1 orbit* - GRB (100sec) - PKS flare - 3C279 flare - Vela Pulsar -Crab Pulsar - 3EG (SNR g Cygni?) 1 day^ - 3EG C279 lowest 5s detection - 3EG (AGN) - Mrk Weakest 5s EGRET source *zenith-pointed, ^ rocking all-sky scan

33 Sensitvity of GLAST Cygnus Region 3C279 Vela Geminga Crab PKS Cosmic Ray Interactions With ISM PSR B PKS LMC

34 From presentaion by S.Ritz, 20 Unidentified Source 172 of the 271 sources in the EGRET 3 rd catalog are unidentified EGRET source position error circles are ~0.5, resulting in counterpart confusion. GLAST will provide much more accurate positions, with ~30 arcsec - ~5 arcmin localizations, depending on brightness. Cygnus region (15x15 deg)

35 Future Perspectives Sensitivity Gap

36 Future Mission -- Focusing Hard X-ray Experiments -- Key technology: Super Mirror & -ray Imager Extensible Optical Bench Focusing Telescope is not only for the equipment to take pictures but also for the key to achieve high sensitivity. Because, a mirror concentrates the incoming flux onto a small spot of the detector, greatly reduce background. ISAS, Japan Constellation X ISAS s NeXT mission ~800cm 2 at 40keV 80 kev NASA

37 NeXT Mission These sensitivities are calculated for the case of the propo based on a CdTe pixel detector (HXI detector team, 2003)

38 cosθ =1 m e c 2 + m c 2 e E 1 E 1 + E 2 Beyond COMPTEL θ Compton-Dominant Region

39 Next generation Compton Telescope in Japan Semiconductor Multi Compton Telescope (SMCT) (ISAS) with high Z semiconductor 25cm (CdTe) 80 layers Compact BUT Detection Efficiency at 1 MeV becomes 10 times higher than COMPTEL (weight 1 ton) on CGRO Takahashi et al. SPIE layers of 0.5 mm thick CdTe strip detectors 625 cm 2 4cm CdTe Detector: ISAS/SLAC/Osaka U. Hiroshima U./ U.Tokyo Compton telescope based on Micro Gas Pixel Chamber (Kyoto Univ.)

40 Polarization Polarization in X-ray/Gamma-ray is the only remaining parameter to be measured. Expected from Jet Sources/Pulsars/Accretion Disk/GRB Development of New and Sensitive Instruments are crucia Gamma-ray by Newly Desined Gamma-ray Polarimeter (Kamae et al. 2003) by Compton Telescope (INTEGRAL, SMCT, MEGA

41 Summary X-ray and Gamma-ray energy band in space are very important window to study high energy particles (cosmic rays) in the universe By combining information from X-ray and Gamma-ray observations, we can deepen our understandings of Accelerator in the universe