gev-tev gamma-ray astronomy masaki mori icrr, univ. tokyo international workshop on extremely high...
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GeV-TeV Gamma-ray Astronomy
Masaki MoriICRR, Univ. Tokyo
International Workshop on Extremely High Energy Cosmic Rays, March 22-23, 2001, Kashiwa
http://icrhp9.icrr.u-tokyo.ac.jp
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Gamma-ray astronomy: short history
Prediction of nuclear gamma-rays Hayakawa 1952; Morrison 1958Ground-based Cherenkov: Jelly (1953), Chudakov (1960-)Prediction of emission from the Crab nebula Cocconi 1959 [nuclear]; Gould 1965 [inverse Compton]
Satellites: OSO-3 (1967-68), SAS-2 (1972-73), COS-B (1975-82)Compton Gamma Ray Observatory EGRET/COMPTEL/OSSE/BATSE (1991-2000)Imaging Cherenkov: Whipple, CANGAROO, HEGRA (1980’s-1990’s)
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Gamma-ray emission mechanisms
Gamma-rays are produced in inherently non-thermal processes!
e + B
e + matter
e + h
p + matter
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CGRO/EGRETApr 1991 – Jun 200030 MeV – 30 GeV67%=5.85(100 MeV/E)0.534
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EGRET Allsky Map
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EGRET: observed intensity
Galactic longitude
Galactic latitude
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EGRET: diffuse emission model
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EGRET: sources = observed - model
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Diffuse gamma-ray spectrum
Flatter than expected (E -2.75): why?⇒ Flatter proton/electron spectrum??
S. Hunter, Heidelberg WS, 2000
EGRET Nishimura et al.
JACEE
Whipple0
Brems
IC
————————————————
uniform
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Third EGRET catalog
R.C. Hartman et al., ApJS, 1999
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EGRET point source summary
Pulsars 5
AGN (mostly blazars) 6627 (marginal)
Radio galaxy (Cen A) 1 (marginal)
Unidentified(Some may be SNRs)
170
Large Magellanic Cloud 1
Solar flare 1
Total 271
R.C. Hartman et al., ApJS, 1999
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Pulsars
GeV Thompson, Heidelberg WS, 2000
Radio Princeton catalog (706 pulsars), 1995
(GeV candidates: 1046-58, 0656+14, J0218+4232)
MeV only
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Pulsars : radio vs gamma-ray
Thompson, Heidelberg WS, 2000
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Gamma-ray pulsar light curves
GLAST proposal
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BL Lac’s and EGRET AGNs
TeV Whipple, HEGRA, CAT, 7TA, Durham
RED EGRET 3rd catalog AGNs
Green Padovani & Giommi MN 1995
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Gamma-ray blazars
Mostly FSRQ and BL Lac’s
Lin et al. ApJ 1999Mukherjee et al. ApJ 1997
H(igh freq. peaked) BL X(-ray selected) BL
L(ow-freq. peaked) BL R(adio-selected) BL
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Multiwavelength spectrum of AGNs
Double-peaked structure= synchrotron + inverse Compton
Kubo et al. ApJ 1998
PKS0528+134 (z=2.1, FSRQ)
Mrk 421 (z=0.03, XBL)Kataoka, Ph.D 2000
↑
νsync
↑
νIC
=γ2νsync
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EGRET unidentified sources
Low vs High latitudePersistent vs Variable
Geminga-like pulsars?SNRs?OB associations?Gould belt?
I. Grenier, GeV-TeV WS, 1999
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EGRET unIDs and SNRs
GeV Esposito et al. ApJ 461, 1996
TeV CANGAROO
RED EGRET 3rd catalog unID
Green D.A. Green’s catalog
TeV HEGRA
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Extragalactic diffuse gamma-rays
Single power-law E –2.100.03 (30 MeV-100 GeV)
Unresolved point sources (ex. Blazars etc.)?Upscattered CMB?
P. Sreekumnar et al., ApJ 1998
E –2.100.03
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Imaging Cherenkov technique
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Image parameters
●
D.J. Fegan, J.Phys.G, 1997(Simulation)
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Example of image cut analysis
Hadron rejection power ~ 100
M. Punch et al., Nature, 1992 T. Yoshikoshi et al., ApJ, 1997
CANGAROO (Vela)
Whipple
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TeV catalog 2000Classification Object Group Remark
Grade A
(>5σ,multiple)
Crab
PSR1706-44
Mrk 421
Mrk 501
Many
CANGAROO, Durham
Many
Many
Plerion
Plerion
AGN (BL Lac)
AGN (BL Lac)
Grade B
(>5σ)
SN1006
Vela
RXJ1713.7-3946
PKS2155-304
1ES1959+650
BL Lac
CANGAROO
CANGAROO
CANGAROO
Durham
Utah7TA
Crimea
SNR
Plerion
SNR
AGN (BL Lac)
AGN (BL Lac)
AGN (BL Lac)
Grade C
(strong but with somequalifications)
Cas A
Cen X-3
1ES2344+514
3C66A
Geminga
B1509-58
HEGRA CT
Durham
Whipple
Crimea
Crimea
CANGAROO
SNR
X-ray binary
AGN (BL Lac)
AGN (z=0.44)
Pulsar
Plerion
T.C. Weekes, Heidelberg WS, 2000
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TeV sky 2000
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TeV observations of Plerions
S. Fegan, astro-ph/0102324
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Crab nebula
Unpulsed spectrumAharonian & Atoyan, astro-ph/9803091 /
Heidelberg WS, 2000
synchrotron
IC
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Crab pulsar spectrum: where is the cutoff?
Musquere, 26th ICRC, 1999
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TeV observations of shell-type SNRs
S. Fegan, astro-ph/0102324
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Supernova remnant: SN1006
T. Naito
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SNR: SN1006 - interpretation
Synch+ICOnly IC?No pro-tons?
Naito et al. Astron. Nach. 320, 1999
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TeV observations of AGNs
Krennrich, astro-ph/0101120
(Detection of 1ES1426+428 (z=0.13) is claimed by Whipple but not published)
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AGN: Mrk 421 variabilityTime scale < a few hoursCorrelation with X-ray flux
Takahashi et al. ApJ 542, 2000Gaidos et al., Nature, 383, 1996
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AGN: Mrk 421 spectrum
Synchrotron+ inverse Comptonmodel workswell⇒ e originProton modelstill possible
Takahashi et al. ApJ 542, 2000
One-zone SSC model
δ=14, B=0.14G
synchrotron
inverse Compton
z=0.031
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AGN: TeV gamma-ray absorption by IR background
Protheroe et al. astro-ph/0005349
IR BackgroundMean free path for e+e- pair production
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AGN: Mrk 501 spectrum
Protheroe et al. astro-ph/0005349
Aharonian et al. A&Ap 349, 1999
Crisis?↓
z=0.033
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Next generation projects
SatellitesMeV: INTEGRAL 15keV-10MeV, 2002-
ACT (Advanced Compton Telescope) 300keV-20MeV, 2008?
GeV: AGILE 30MeV-50GeV, 2003-
GLAST 20MeV-300GeV, 2005?
Ground-basedCANGAROO-III 410m, Australia, 2000-2004-
MAGIC 117m, Canary Island, 2001-
HESS 412m, Namibia, 2002-
VERITAS 710m, Arizona, 2004-
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Sensitivity of future detectors
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Summary
Plerions (pulsar nebula)Inverse Compton? ⇔ synchrotron origin?PulsarsCutoff in pulse component? ⇔ polar cap/outer gapSNRsπ0 contribution? ⇔ cosmic ray originAGNsGamma-ray source: e± or p?Intergalactic IR ⇔ cosmologyEGRET unIDs, Neutralinos, GRBs, QG,Galactic/extragalactic diffuse,…, and more?
Gamma-ray observation maps the non-thermal Universe!