Current status and future plans of TeV gamma-ray observations
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Current status and future plans of TeV gamma-ray observations
Hidetoshi Kubo (Kyoto University)
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Outline
• TeV gamma-ray telescopes
• Observations Results– Galactic
• HESS plane survey• G.C., Diffuse emission• PWN, SNR, etc.
– Extragalactic sources• AGN, Starburst galaxy
• Future plans
• Summary
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TeV gamma-ray observation• Cherenkov shower pool
• Better angular resolution=0.20.07/
• Better energy resolution E/E=30%15%
• E>100GeV at present
• Higher E threshold at larger zenith angle
• 1%Crab for 25hrs(HESS)
• FOV < 5, < 3 (FWHM)
Altitude 10 ~ 20km
~300m
+Water Cherenkov telescope, Air Shower Array
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CANGAROO-III
T2 T4 T3 T1
T2
114 80cm FRP mirrors
427ch (4 FOV)
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STACEE
MILAGRO
TIBETARGO-YBJ
PACT
GRAPES
TACTIC
VERITAS
MAGIC
HESS CANGAROO
TIBETMILAGRO
STACEE
TACTIC
TeV gamma-ray telescopes
R.Ong (2005)
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HESS Galactic Plane Survey in 2004
Survey Region
PSR B1259HESS J1303
MSH 15-52RXJ 1713
GC
RXJ 0852
Vela X
• 30°in longitude, 3° in latitude• 230hrs(95 hrs scanning + follow-up observations)• E > 200GeV• Flux > 2%Crab Aharonian et al. (2005)
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Detections with CANGAROOBefore the HESS survey Gal. Centre
330°
30° 0°
RX J1713.7-3946
359° 330°
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HESS Survey: New sources
HESS J1804-216 Gal. Centre HESS J1837-069
330°
G0.9+0.1 HESS J1813-178 HESS J1825-137
HESS J1834-087
30° 0°
RX J1713.7-3946 HESS J1640-485HESS J1616-508
HESS J1614-518
359° 330°
Sources > 6 sigma (10 new, 12 total)
Aharonian et al. (2005)
LS 5039
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HESS Survey: New Sources
HESS J1702-420HESS J1713-381 HESS 1632-478
330°
RX J1713.7-3946 HESS J1640-465HESS J1616-508
HESS J1614-518
359°
HESS J1708-410 HESS J1634-472HESS J1745-303
LS 5039
HESS J1804-216 Gal. Centre HESS J1837-069
G0.9+0.1 HESS J1813-178 HESS J1825-137
HESS J1834-087
30° 0°
Sources > 6 sigma (10 new, 12 total)Sources > 4 sigma (6 new)
Aharonian et al. (2005)
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HESS GP Source Associations
PWN
PWN
PWN/UID
XRB/SNRSNR/UID
SNRSNR
XRB
SNR
SNRUID
UIDSNR/BH
SNR/PWN
J1826-148 LS5039 XRB
○
○○○
○○◎
◎
◎
◎
◎◎◎◎◎◎
◎
◎ >6 ○ >4
Aharonian et al. (2005)
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The VHE Sky - 1995
Mrk421
Mrk501
Crab
R.A.OngAug 2005
Pulsar Nebula
SNR
AGN
Other, UNID
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The VHE Sky - 2003
Mrk421 H1426
Mrk501
1ES1959
1ES 2344
PKS 2155
Cas A
RXJ 1713
CrabTeV 2032
M87
GC
R.A.OngAug 2005
Pulsar Nebula
SNR
AGN
Other, UNID
12 sources
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The VHE Sky - 2005
Mrk421 H1426
Mrk501
1ES1959
1ES 2344
PKS 2155
Cas A
RXJ 1713
CrabTeV 2032
M87
PKS 2005
PSR B1259
RXJ 0852
MSH 15-52
SNR G0.9
HessJ1303
GC
R.A.OngAug 2005
Pulsar Nebula
SNR
AGN
Other, UNID
H2356
1ES 1218
1ES 1101
LS 5039Vela X
+ 8-15 add. sourcesin galactic plane.
CygnusDiffuse
33 sources
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TeV gamma-ray sources
Source Type* 2003 2005
Pulsar Wind Nebula (e.g. Crab, MSH 15-52 …) 1 6
Supernova Remnants (e.g. Cas-A, RXJ 1713 …) 2 6
Binary Pulsar (B1259-63) 0 1
Microquasar (LS 5039) 0 1
Diffuse (Cygnus region) 0 1
AGN (e.g. Mkn 421, PKS 2155 …)
Starburst galaxy (NGC253)
7
0
11
1
Unidentified 2 6
TOTAL 12 33
Based on R.A.Ong ICRC2005
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SGR A
Galactic Center
CANGAROO(E>300GeV)
EGRET(E>500MeV) r<0.2
Tsuchiya et al.(2004)
Mayer-Hasselwander et al.(1998)
VLA@5GHz
HESS (E>125GeV)
Contour: Radio
Consistent with SGR A* to 6’’±10”stat±20”sysPoint like core + slightly extended tail
Aharonian et al.(2004),Rolland et al.(2005)
Yusef-Zadeh & Morris(1987)
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Galactic Center– Unbroken power-law.– Hard spectrum = 2.2
(HESS).– No evidence for
variability
π0→2γ
CANGAROO-III(stereo)under analysis
HESS
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Galactic Center Region
CS
gamma rays(subtracted)
HESS
2.29±0.07±0.20
CS
gamma rays
Harder than Diffuse model
Hinton et al.(2005)
CS
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Galactic Diffuse emission
E-2.51±0.05
EGRET longitude latitude R1 40-100°±5° R2 140-200°±5°
Milagro (2000 ~ 2002)
Sinnis et al.(2005)
Milagro4.5
-1.3
x1/100
CANGAROO-II ULl=+13,b=0, l=-19.5,b=-3,0,+3Ohishi et al.(2005)
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Cygnus region
+20
+40
+60
+100
+80
Milagro (2000 ~ 2005)
Excess >5°(1.55Crab for E>2TeV) from Cygnus region
PSF
Contour: 1420MHz
HEGRA unIDTeV 2032+4130
Smith et al.(2005)
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HESS (440GeV<E<10TeV)Consistent with point source(PSF σ ~ 0.14°)Error 5”(stat)±20”(sys)
Crab ー standard candle in VHE ー PWN(1/5)
Gravity of the X-ray emissionWeisskopf et al.(2000)
Masterson et al.(2005)
UL for pulse
Continuum
Aharonian et al.(2004)
=2.6
E>100GeV
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SNR MSH-52(PSR B1509-58) PWN(2/5)
Aharonian et al.(2005)
Contours: X-ray(ROSAT)
HESS
PSF
Photon index2.27 ± 0.03 ± 0.20
Gray:RadioContours:ROSAT
Chandra
B ~ 17GDust=2.3eV/cm3
Major axis 6.4’±0.7’Minor 2.3’±0.5’
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Vela pulsar
ROSATcontours
Khelifi et al.(2005)
Preliminary
HESSNo emission from Vela pulsar position, butExtented hard spectrum ≈1.9 or ≈1.5 cutoffextends to50 TeV
Vela PWN(3/5)
HESS
CANGAROO-IIalso detected
Enomoto et al.(2005)
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HESS J1825-137(4/5)
TeV
17%Crab(E>200GeV)
Aharonian et al.(2005)
Offset by 11’ south to PSR B1823-13(101ms) in PWN G18.0-0.7
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SNRG0.9+0.1
Radio
Radio (90 cm)
HESS・ Consistent with point source at core, not SN shell・ 2% Crab flux(E>200GeV)
PWN in SNR G0.9+0.1(5/5)
HESS
Aharonian et al.(2005)
G.C.
6G
=2.40±0.11±0.20
Chandra Gaensler et al.(2001)Hard spectrum Point Src(No pulsed emission)Newton Porquet al.(2003)Softening of spectrum with increasing distance from the center
GLAST 1yr
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Berge et al.(2005)
Shell structureclearly resolved.Morphology does not change with energy.
RXJ 1713.7-3946 SNR(1/4)From the NW rim, non-thermal X-ray emission detected with ASCA (Koyama et al.1997) TeV - detectionE>1TeV CANGAROO-I in 1998E>400GeV CANGAROO-II in 2000+1Enomoto et al.(2002)
HESS
Spectral index:little variation across SNR
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RXJ 0852.0-4622 “Vela Jr.” SNR(2/4)
Katagiri et al.(2005)
CANGAROO-II
4850MHz
ASCA
HESS Aharonian et al.(2005)
Contour: ROSAT
TeV flux ~ Crab
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SNR RXJ 0852.0-4622 “Vela Junior”
Bremsstrahlung
Synchrotron
IC
0 decay
Katagiri et al.(2005)
0 decay? Brems.? IC?
GLAST 1yr
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Cas A SNR(3/4)
Chandra image
HEGRACenter of TeV excess
Aharonian et al.(2001)IC+Bremsstrahlung?
0 decay?
GLAST 1yr
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Earlier detection by CANGAROO-I from NE rim.& HEGRA CT1.
CANGAROO-III
2 U.L.
HESS & CANGAROO-III
SN1006 not detected at previous levels.
SN1006 SNR(4/4)Upper limit
ASCA
Tanimori et al.(2005)
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PSR B1259-63/SS2883
331 R*
Aharonian et al. (2005)
PSR B1259-63 (P=48ms)
around Be star SS2883 in
a highly eccentric 3.4yr orbit
1.4GHz
HESSperia
stro
n
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Aharonian et al. (2005)
PSR B1259-63/SS2883
electron origin? Hadronic origin?
Kawachi et al.(2004)
GLAST?
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Paredes et al. (2002)
RA (mas)
compact 4 (?) M object in eccentric 4 day orbit around 20-30 M starclosest approach ~1012 cm or ~2 stellar radii
Aharonian et al.(2005)
Microquasar LS 5039first detection of TeV emission from a microquasar
European VLBI@5GHz
Jets
HESS
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2.12 ± 0.15
Flux (E>250GeV)(5.1±0.8stat±1.3sys)x10-12
ph cm-2s-1
2003 XMM
1998 RXTE
L ~ 1033 erg/s at 3kpc
Microquasar LS 5039
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Aharonian et al. (2005)
Extented with radius 6.2’(±1.2’stat±0.9’sys)
HEGRA observations 1999 ~ 2002
Hard spectrum Γ=1.9±0.1’stat±0.3’sys
Flux (6.2±1.5stat±1.3sys)x10-13
ph cm-2s-1TeV-1@1TeV
unID TEV J2032+4130
3EGJ2033+4118
Higher angular resolution of GLAST canresolve it
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Source Redshift Type First Detection Confimation
M87 0.004 FR I HEGRA HESS
Mkn 421 0.031 BL Lac Whipple Many
Mkn 501 0.034 BL Lac Whipple Many
1ES2344+514 0.044 BL Lac Whipple HEGRA
1ES1959+650 0.047 BL Lac Tel. Array Many
PKS 2005-489 0.071 BL Lac HESS
PKS 2155-304 0.116 BL Lac Mark VI HESS
H1426+428 0.129 BL Lac Whipple Many
H2356-309 0.165 BL Lac HESS
1ES1218+304 0.182 BL Lac MAGIC
1ES 1101-232 0.186 BL Lac HESS
TeV –ray detected AGNs
R.Ong (2005)
5014212155
23441426
Costamante & Ghisellini(2002)
2005
1101
2356
HB
LLB
L
Total :11 sources
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Extragalactic Background Light
Aharonian et al.(2005)
TeV
HESS limits Reference shape
TeV photon + EBL → e+ + e-
More transparent than previously thought
If we assume (electron index>2)for intrinsic spectrum
GLAST
GLAST
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Mrk 421 & Mrk 501
Light Curve: 2 min time bins.Mazin et al.(2005)
STACEE
Carson et al.(2005)
Mrk 501 Big Flare in Jul 2005
Rapid variation
Mirzoyan et al.(2005)
4CrabMAGIC
Wide range:300GeV – 30TeV
GLAST
Simulataneous obs. with GLAST is needed
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Radio galaxy M87(16Mpc)
Beilicke et al.(2005)
Georganopoulos et al.(2005)
HESS(2003+2004)
5.8
HEGRA
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Starburst galaxy NGC253
Multi-band spectrum Itoh et al. A&AL 2002
Crab(65%)
DSS2
CANGAROO
CANGAROO-II
E-1.5e-√E/(0.25±0.01)
• Nearby(2.5Mpc) spiral galaxy
• Radio Halo extending to ~9kpc
First TeV gamma-ray detection from anormal spiral galaxy other than our own
Detected with CANGAROO-II in 2000 and 2001 with 11 (E>0.5TeV)
GLAST 1yr
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Future plans of TeV ray observations
Project Site Current Plan From E>
VERITAS USA 12m x 1 12m x 4 2006 50GeV
CANGAROO Australia 10m x 3 10m x 4 100GeV
HAGAR India(4.2km) 0.9m x 1 0.9m x 7 2006 60GeV
MACE India(4.2km) 21m x 2 15GeV MAGIC Canary is. 17m x 1 17m x 2 2007 20GeV
HESS Namibia 12m x 4 +28m x 1 2008 20GeV
Ashra Hawaii
HAWC 300mx300m pondLower Energy Threshold at higher altitude
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Future plans of TeV ray observations
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Cherenkov telescope network
・ Continuous monitoring of time variable objects such as blazars・ Simultaneous observations with GLAST
+
HAGAR,Mace
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Summary
• 33 sources detected in TeV ray region, including newcomers (Pulsar Binary, Microquasar, Starburst Galaxy, unID). Candidates for GLAST detection.
• Improved resolution of TeV(< 0.1/) + GLAST enable us to investigate detail morphology of SNRs, PWNs, etc.
• TeV + GLAST reveal electron or proton origin of ray emission in SNR etc., the intrinsic spectrum of blazars, and the EBL spectrum.
• Simultaneous monitoring with Cherenkov telescope network and GLAST for variable sources.
• New telescopes are under construction in order to lower the energy threshold to <100GeV, overlapped with GLAST region.