Hironori Matsumoto (Kyoto University)

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Hironori Matsumoto (Kyoto University) Discovery of the Extended X-ray Emission from the Dark Accelerator HESSJ1614-518 Hironori Matsumoto (Kyoto University) H. Uchiyama, M. Sawada, T. G. Tsuru, K. Koyama (Kyoto U.) H. Katagiri, R. Yamazaki (Hiroshima U.), K. Mori (Miyazaki U.), A. Bamba, Y. Uchiyama (ISAS/JAXA), K. Kazunori (Lancaster U.) In print, PASJ, vol. 60, Suzaku Special Issue 2 (astro-ph/0712.0874) Dec. 12, 2007

Outline HESS unID object: HESSJ1614-518 Suzaku observation of HESSJ1614-518 Discovery of an extended X-ray counterpart Other two X-ray objects Discovery of extended soft X-ray emission Discussion Summary Dec. 12, 2007 Suzaku 2007

TeVγ-ray object: HESSJ1614-518 Discovered by the Galactic plane survey with the H.E.S.S. telescope. (Aharonian et al. 2005,2006) Brightest object: F(1-10TeV)=1.8e-11 erg/s/cm2 Dec. 12, 2007 Suzaku 2007

Suzaku Observation (b) TeV image and XIS FOV offset 2006/9/15 45ks (l) Normal mode without the speced-row charge injection Dec. 12, 2007 Suzaku 2007

XIS image (FI CCD) srcA srcC srcB 0.4-3keV 3-10keV Discovery of three X-ray objects srcA, srcB: extended, srcC: point like Dec. 12, 2007 Suzaku 2007

Comparison with the HESS image TeV image 3-10keV srcA 0.4-3keV srcB srcC Src A is spatially coincident with the TeV gamma-ray. Dec. 12, 2007 Suzaku 2007

(The offset observation is not used as a background. Explain later.) Spectral Analysis Definition of spectral regions and a background. 0.4-3keV 3-10keV bgd srcA srcB srcC (The offset observation is not used as a background. Explain later.) Dec. 12, 2007 Suzaku 2007

Spectrum of src A 3-10keV Red:BI Black:FI Featureless = non-thermal Γ=1.73+/-0.33 NH=1.21+/-0.5e22 cm-2 F(2-10keV)=5.3e-13 erg/cm2/s Dec. 12, 2007 Suzaku 2007

Src A is a plausible counterpart to HESSJ1614 Discussion: Src A Src A is a plausible counterpart to HESSJ1614 H.E.S.S. Suzaku srcA B=10μG B=1μG B=0.1μG F(1-10TeV)/F(2-10keV)=34 One of the largest ratios. Other Suzaku results HESSJ1616-508: >55 (Matsumoto et al. 2007) HESSJ1804-216:  25 (Bamba et al. 2007) If the origin of the TeV emission is the inverse Compton of the CMB by high-energy electrons, the magnetic field must be too small. Dec. 12, 2007 Suzaku 2007

Discussion: src A No counterpart in other wavelengths. NH  1.2e22 cm-2 D  10 kpc (c.f. NH (HI survey)  2e22 cm-2) Lx(2-10keV)  6e33 erg/s photon index = 1.7 Harder than the canonical SNR values (2.5-3.0) Non-thermal brems. emission from loss-flattened electron distribution? (e.g., γCygni; Uchiyama et al. 2002) Old SNR? (Yamazaki et al. 2006) PWN? Dec. 12, 2007 Suzaku 2007

Spectrum of srcB Featureless = Non-thermal? Extremely soft! 0.4-3keV Red:BI Black:FI Γ=3.60+/-0.23 NH=1.24+/-0.1e22 cm-2 F(2-10keV)=3.6e-13 erg/cm2/s Dec. 12, 2007 Suzaku 2007

Discussion: src B Spatially coincident with 2MASS J16140610-5152264 The origin of the object is not clarified. Previously detected with Swift XRT in March 2006: variable? F(2-10keV): Swift 1.4e-13 erg/s/cm2 (Landi et al. 2007) Suzaku 3.6e-13 erg/s/cm2 (large err.) Extremely large photon index (3.6) NH  1.2e22 cm-2 Same as that of src A. Physically related to HESSJ1614? Src A= offset PWN and src B = pulsar? (e.g. PSRJ1809-1917 associated with HESSJ1809-193 has a large photon index of 3.2+/-0.4; Kargaltsev & Pavlov 2007) Dec. 12, 2007 Suzaku 2007

Spectrum of src C Red:BI 0.4-3keV Black:FI Thermal spectrum kT=0.63+/-0.1keV Abundance=0.18+/-0.5 solar NH=0.28+/-0.2e22 cm-2 F(2-10keV)=7.6e-15 erg/cm2/s Probably the foreground B9V star HD145703 Dec. 12, 2007 Suzaku 2007

Diffuse soft X-ray emission TeV image BI spectrum Blank-Offset Red:BI Black:FI Γ=2.4 or kT=2.7keV NH=0.1e22cm-2 Offset region. No X-ray and gamma-ray objects. Blank region as a background NHforeground emission? Not related to HESSJ1614? Dec. 12, 2007 Suzaku 2007

Summary Discovery of three X-ray objects. Src A Extended and spatially coincident with HESSJ1614. Plausible counterpart to HESSJ1614. F(1-10TeV)/F(2-10keV) = 34 It is difficult to explain the ratio in terms of high-energy electrons. Photon index = 1.7 Different from the SNR values. Src B Column density suggests that src B may also be physically related to HESSJ1614. Pulsar? Src C … foreground star Discovery of the extended soft X-ray emission. Dec. 12, 2007 Suzaku 2007

他波長イメージ SUMSS 843MHz survey CO map Dec. 12, 2007 Suzaku 2007