GeV-TeV Gamma-ray Astronomy Masaki Mori ICRR, Univ. Tokyo International Workshop on Extremely High Energy Cosmic Rays, March 22-23, 2001, Kashiwa

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Presentation transcript:

GeV-TeV Gamma-ray Astronomy Masaki Mori ICRR, Univ. Tokyo International Workshop on Extremely High Energy Cosmic Rays, March 22-23, 2001, Kashiwa

Gamma-ray astronomy: short history Prediction of nuclear gamma-rays Hayakawa 1952; Morrison 1958 Ground-based Cherenkov: Jelly (1953), Chudakov (1960-) Prediction of emission from the Crab nebula Cocconi 1959 [nuclear]; Gould 1965 [inverse Compton] Satellites: OSO-3 ( ), SAS-2 ( ), COS-B ( ) Compton Gamma Ray Observatory EGRET/COMPTEL/OSSE/BATSE ( ) Imaging Cherenkov: Whipple, CANGAROO, HEGRA (1980’s-1990’s)

Gamma-ray emission mechanisms  Gamma-rays are produced in inherently non-thermal processes! e  + B e  + matter e  + h p + matter

CGRO/EGRET Apr 1991 – Jun MeV – 30 GeV  67% =5.85  (100 MeV/E) 0.534

EGRET Allsky Map

EGRET: observed intensity Galactic longitude Galactic latitude

EGRET: diffuse emission model

EGRET: sources = observed - model

Diffuse gamma-ray spectrum Flatter than expected (E ): why? ⇒ Flatter proton/electron spectrum?? S. Hunter, Heidelberg WS, 2000 EGRET Nishimura et al. JACEE Whipple 00 Brems IC ————————————— ——— uniform

Third EGRET catalog R.C. Hartman et al., ApJS, 1999

EGRET point source summary Pulsars5 AGN (mostly blazars)66 27 (marginal) Radio galaxy (Cen A)1 (marginal) Unidentified (Some may be SNRs) 170 Large Magellanic Cloud1 Solar flare1 Total271 R.C. Hartman et al., ApJS, 1999

Pulsars GeV Thompson, Heidelberg WS, 2000 Radio Princeton catalog (706 pulsars), 1995 (GeV candidates: , , J ) MeV only

Pulsars : radio vs gamma-ray Thompson, Heidelberg WS, 2000

Gamma-ray pulsar light curves GLAST proposal

BL Lac ’ s and EGRET AGNs TeV Whipple, HEGRA, CAT, 7TA, Durham RED EGRET 3 rd catalog AGNs Green Padovani & Giommi MN 1995

Gamma-ray blazars Mostly FSRQ and BL Lac ’ s Lin et al. ApJ 1999 Mukherjee et al. ApJ 1997 H(igh freq. peaked) BL  X(-ray selected) BL L(ow-freq. peaked) BL  R(adio-selected) BL

Multiwavelength spectrum of AGNs Double-peaked structure = synchrotron + inverse Compton Kubo et al. ApJ 1998 PKS (z=2.1, FSRQ) Mrk 421 (z=0.03, XBL) Kataoka, Ph.D 2000 ↑ ν sync ↑ ν IC =γ 2 ν sync

EGRET unidentified sources Low vs High latitude Persistent vs Variable Geminga-like pulsars? SNRs? OB associations? Gould belt? I. Grenier, GeV-TeV WS, 1999

EGRET unIDs and SNRs GeV Esposito et al. ApJ 461, 1996 TeV CANGAROO RED EGRET 3 rd catalog unID Green D.A. Green’s catalog TeV HEGRA

Extragalactic diffuse gamma-rays Single power-law E –2.10  0.03 (30 MeV-100 GeV) Unresolved point sources (ex. Blazars etc.)? Upscattered CMB? P. Sreekumnar et al., ApJ 1998 E –2.10  0.03

Imaging Cherenkov technique

Image parameters ● D.J. Fegan, J.Phys.G, 1997 (Simulation)

Example of image cut analysis Hadron rejection power ～ 100 M. Punch et al., Nature, 1992T. Yoshikoshi et al., ApJ, 1997 CANGAROO (Vela) Whipple

TeV catalog 2000 ClassificationObjectGroupRemark Grade A (>5σ, multiple) Crab PSR Mrk 421 Mrk 501 Many CANGAROO, Durham Many Plerion AGN (BL Lac) Grade B (>5σ) SN1006 Vela RXJ PKS ES BL Lac CANGAROO Durham Utah7TA Crimea SNR Plerion SNR AGN (BL Lac) Grade C (strong but with some qualifications) Cas A Cen X-3 1ES C66A Geminga B HEGRA CT Durham Whipple Crimea CANGAROO SNR X-ray binary AGN (BL Lac) AGN (z=0.44) Pulsar Plerion T.C. Weekes, Heidelberg WS, 2000

TeV sky 2000

TeV observations of Plerions S. Fegan, astro-ph/

Crab nebula Unpulsed spectrum Aharonian & Atoyan, astro-ph/ / Heidelberg WS, 2000 synchrotron IC

Crab pulsar spectrum: where is the cutoff? Musquere, 26 th ICRC, 1999

TeV observations of shell-type SNRs S. Fegan, astro-ph/

Supernova remnant: SN1006 T. Naito

SNR: SN interpretation Synch+IC Only IC? No pro- tons? Naito et al. Astron. Nach. 320, 1999

TeV observations of AGNs Krennrich, astro-ph/ (Detection of 1ES (z=0.13) is claimed by Whipple but not published)

AGN: Mrk 421 variability Time scale < a few hours Correlation with X-ray flux Takahashi et al. ApJ 542, 2000Gaidos et al., Nature, 383, 1996

AGN: Mrk 421 spectrum Synchrotron + inverse Compton model works well ⇒ e  origin Proton model still possible Takahashi et al. ApJ 542, 2000 One-zone SSC model δ=14, B=0.14G synchrotroninverse Compton z=0.031

AGN: TeV gamma-ray absorption by IR background Protheroe et al. astro-ph/ IR Background Mean free path for e + e - pair production

AGN: Mrk 501 spectrum Protheroe et al. astro-ph/ Aharonian et al. A&Ap 349, 1999 Crisis? ↓ z=0.033

Next generation projects Satellites MeV: INTEGRAL 15keV-10MeV, ACT (Advanced Compton Telescope) 300keV-20MeV, 2008? GeV: AGILE 30MeV-50GeV, GLAST 20MeV-300GeV, 2005? Ground-based CANGAROO-III 4  10m, Australia, MAGIC 1  17m, Canary Island, HESS 4  12m, Namibia, VERITAS 7  10m, Arizona, 2004-

Sensitivity of future detectors

Summary Plerions (pulsar nebula) Inverse Compton? ⇔ synchrotron origin? Pulsars Cutoff in pulse component? ⇔ polar cap/outer gap SNRs π 0 contribution? ⇔ cosmic ray origin AGNs Gamma-ray source: e ± or p? Intergalactic IR ⇔ cosmology EGRET unIDs, Neutralinos, GRBs, QG, Galactic/extragalactic diffuse, …, and more? Gamma-ray observation maps the non-thermal Universe!