Current status and future plans of TeV gamma-ray observations
Hidetoshi Kubo (Kyoto University)
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
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
CANGAROO-III
T2 T4 T3 T1
T2
114 80cm FRP mirrors
427ch (4 FOV)
STACEE
MILAGRO
TIBETARGO-YBJ
PACT
GRAPES
TACTIC
VERITAS
MAGIC
HESS CANGAROO
TIBETMILAGRO
STACEE
TACTIC
TeV gamma-ray telescopes
R.Ong (2005)
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)
Detections with CANGAROOBefore the HESS survey Gal. Centre
330°
30° 0°
RX J1713.7-3946
359° 330°
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
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)
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)
The VHE Sky - 1995
Mrk421
Mrk501
Crab
R.A.OngAug 2005
Pulsar Nebula
SNR
AGN
Other, UNID
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
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
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
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)
Galactic Center– Unbroken power-law.– Hard spectrum = 2.2
(HESS).– No evidence for
variability
π0→2γ
CANGAROO-III(stereo)under analysis
HESS
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
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)
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)
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
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’
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)
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
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
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
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
SNR RXJ 0852.0-4622 “Vela Junior”
Bremsstrahlung
Synchrotron
IC
0 decay
Katagiri et al.(2005)
0 decay? Brems.? IC?
GLAST 1yr
Cas A SNR(3/4)
Chandra image
HEGRACenter of TeV excess
Aharonian et al.(2001)IC+Bremsstrahlung?
0 decay?
GLAST 1yr
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)
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
Aharonian et al. (2005)
PSR B1259-63/SS2883
electron origin? Hadronic origin?
Kawachi et al.(2004)
GLAST?
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
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
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
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
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
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
Radio galaxy M87(16Mpc)
Beilicke et al.(2005)
Georganopoulos et al.(2005)
HESS(2003+2004)
5.8
HEGRA
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
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
Future plans of TeV ray observations
Cherenkov telescope network
・ Continuous monitoring of time variable objects such as blazars・ Simultaneous observations with GLAST
+
HAGAR,Mace
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.
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