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Suzaku Observations of HESS sources. Hironori Matsumoto (Kyoto Univ.). Hideki Uchiyama (Kyoto Univ.), Aya Bamba, Ryoko Nakamura, Takayasu Anada (ISAS/JAXA), and the Suzaku team. Outline. HESS unID objects: “Dark particle accelerators” Suzaku Observations HESSJ1614-518 HESSJ1616-508 - PowerPoint PPT Presentation
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1/25
Suzaku Observations of HESS sources
Hironori Matsumoto (Kyoto Univ.)
Hideki Uchiyama (Kyoto Univ.), Aya Bamba, Ryoko Nakamura, Takayasu Anada (ISAS/JAX
A), and the Suzaku team
2/25
Outline• HESS unID objects: “Dark particle accelerators”• Suzaku Observations
– HESSJ1614-518– HESSJ1616-508– HESSJ1713-381 (CTB37B)– HESSJ1804-216– HESSJ1825-137– HESSJ1837-069
• Summary
3/25
HESS Galactic Plane Survey
First systematic Galactic plane survey with TeV γ-ray (>200GeV)
New TeV objects with no obvious counterpart.
(Aharonian et al. 2005, 2006)
HESSJ1804-216
HESSJ1616-508
HESSJ1614-518
Gal. Cent.
HESSJ1713-381
HESSJ1837-069
Dark particle accelerators
HESSJ1825-137
4/25
HESSJ1614-518
(l, b)=(331.52, -0.58)
HESS TeV γ-ray image (excess map)
XIS FOV50ks
Brightest among the new objects.
HESSJ1614
5/25
XIS FI (S0+S2+S3): 3-10keV band
Extended object
TeVγ-ray
XIS image
Swift XRT also detected(Landi et al. 2006)
Obs. 50ks
Src A
Src B
6/25
XIS spectra
NH=1.2(±0.5)e22cm-2
Γ=1.7(±0.3)F(2-10keV)=5e-13erg/s/cm2
NH=1.2(±0.1)e22cm-2
Γ=3.6(±0.2)F(2-10keV)=3e-13erg/s/cm2
•Featurelessnon-thermal
Featureless,but extremely soft
Src A
Src B
Src A spectrum
Src B spectrum
7/25
H.E.S.S.
src A
B=10μG
B=1μG
B=0.1μG
Src A
Src B
Src AF(1-10TeV)/F(2-10keV)=34
Plausible X-ray counterpart: src A
Matsumoto et al. 2008, PASJ, 60. S163 (Suzaku special issue No.2)
•Difficult to explain both the TeV gamma-ray and X-ray from the electron origin.•The origin of srcA is not clarified.
8/25
HESSJ1616-508HESS TeV image (excess map)
(l, b)=(332.391, -0.138)
XIS FOV45ks
Provided by S. Funk (MPI)
HESSJ1616
9/25
XIS imageXIS FI (S0+S2+S3): 3—12keV
•No X-ray counterpart•F(2-10keV)<3.1e-13 erg/s/cm2
TeV image
45ks F(TeV)/F(X)>55
10/25
If we assume electrons…
Very weak B(B<1μGauss)
HESSJ1616 SED
Suzaku upper limit
Strong cut-offorrealistic?
Matsumoto et al. 2007, PASJ, 59, 199 (Suzaku Special Issue No.1)
11/25
PSRJ1617-5055?INTEGRAL 18-60keV
PSRJ1617
Landi et al. 2007
XMM-Newton 0.5-10keV
PSRJ1617
Why is there no trace in X-ray band?Why is there no clear PWN in the radio (Kaspi et al. 1998) and X-ray bands?
SNR RCW103
12/25
HESSJ1713-381 (CTB37B)
SNR CTB37B
HESSJ1713-381 coincides with the SNR CTB37B
Color: TeVWhite: radio
13/25
Non-thermal hard X-rayNakamura 2008 in preparationSuzaku 0.3-3.0keV
Suzaku 3.0-10.0keV
Green: TeV (HESS)Blue: radioWhite: X-ray (Suzaku)
reg1
reg1
reg2
reg2
Foreground src
Reg1: coincides with the TeV peakReg2: offset hard emission
14/25
Suzaku 3.0-10.0 keVreg1
reg2
•Thermal (kT=0.9keV)+PL(Γ=3.0)•A point source discovered by Chandra (Aharonian et 1l. 2008) contributes much to the PL component.
Hard PL (Γ=1.5) + Leakage from reg1 due to PSF.•Roll-off energy > 15keV•The hard PL suggests efficient acceleration.
F(TeV)/F(X)~0.2 B~8uG assuming IC.Emax > 170 TeV
15/25
HESSJ1804-216HESS TeV γ-ray image (excess map)
Provided by S. Funk (MPI)(l, b)=(8.401, -0.033)
XIS FOV40ks
Softest TeV spectrum among the new objects.
HESSJ1804
16/25
XIS image
XIS FI (S0+S2+S3): 3-10keV
src1
src2
src1: point-likesrc2: extended or multiple
TeV image
40ks
Swift XRT (Landi et al. 2006)Chandra (Kargaltsev et al. 2007)
Chandra (Kargaltsev et al. 2007)
17/25
XIS spectra
src1
src2
src1: point-like
src2: extended
src1 src2
Γ -0.3±0.5
1.7±1.2
NH (1022cm-2)
0.2(<2.2)
11±8
F(2-10keV)10-13erg/s/cm2
2.5 4.3
See Bamba et al. 2007, PASJ, 59, S209 (Suzaku Special Issue No.1)
F(TeV)/F(X) 50 25
18/25
HESS J 1825-137
30arcmin~30pc@4kpc
HESS J1825-137
Aharonian et al. 2006
H.E.S.S TeV γ excess map
PSR J1826-1334
Distance from Pulsar (deg)
Pho
ton
Inde
x Γ
IC by high-energy electrons from the pulsar?
•Spin-down luminosity ~ 2.8×1036 erg s-1
•Characteristic age 21.4 kyr (Clifton 1992)•D~4kpc
softening
19/25
Previous X-ray study (XMM-Newton)PSR J1826-1334 (B1823-13)
Photon index ~ 2.3NH~1.4×1022/cm2 LX~3×1033 erg s-1
1arcmin~1pc@4kpc
Pulsar
PWN
XMM-Newton0.5-10keV
H.E.S.S TeV γ excess map
Gaensler et al. 2003 Why is the X-ray image much smaller?
More extended if observed with high sensitivity? Suzaku observation!
20/25
Suzaku: Very extended PWN
XIS 3F 1-9 keV
source
6arcmin~6pc@4kpc
2006/9 50ksec
bgd
Suzaku can detect X-rays much more extended than the XMM results.
TeV image
21/25
1.2×(CXB+GRXE)
CXB+GRXE
Galactic Ridge X-ray Emission
CXB
BackgroundSource
Radial profile
UnresolvedPoint sources
X-rays are extended at least up to 15 arcmin (~15 pc)
22/25
X-ray spectraRegion A Region B
Region C Region D
Γ=1.78(1.68-1.88) Γ=1.99(1.91-2.08)
Γ=2.03 (1.95-2.14) Γ=2.03 (1.95-2.14)
A
BC
D
Reg B-D: no change in photon index. electrons reach to 15pc before cooled.
=pulsar+PWN
Synchrotron cooling time~1400yrs.Velectron~10000 km/s
23/25
HESSJ1837-069
HESS image
INTEGRAL/ISGRI(Malizia et al. 2005)
1degx1deg
X-rays were detected up to 300 keV by INTEGRAL
24/25
AXJ1838.0-0655
AXJ1837.3-0652
X-ray counterparts are offset from the TeV gamma-ray peak.
TeV peak
Pulsations of 70.5 ms were recently discovered from AXJ1838 with RXTE (Gotthelf et. al. 2008).
Offset pulsar wind nebulaAnada et al. in preparation
25/25
SummaryX-ray Origin
HESSJ1614-518 O ?
HESSJ1616-508 X ?
HESSJ1713-381 O SNR CTB37B
Efficient acceleration
HESSJ1804-216 2 ?
HESSJ1825-137 Very extended PWN
HESSJ1837-069 2 extended Offset PWN
Can you construct a “Grand Unification Theory (GUT)” of the dark particle accelerators?