X-rays from the Galactic Center

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Presentation transcript:

X-rays from the Galactic Center 2-10 keV Iron K-shell Line Flux

The Galactic Center X-Rays: Connection withTeV Emissions Si13+Kα S14+Kα Ar16+Kα Fe Kα Fe24+Kα Ca18+Kα Si12+Kα S15+Kα Fe25+Kα Ni26+Kα S14+Kβ Ar16+Kβ Si12+Kβ Ni27+Kα Ar17+Kα Ca19+Kα Fe　Kβ Fe24+Kβ Fe25+Kβ Ni Kα Energy 6 7 K-shell ｌines from neutral atoms K-shell ｌine from highly ionized atoms 8 6.7 keV (He-like Fe) 6.4 keV (Neutral Fe) 2.5 keV (He-like S) (1) ~7 keV Plasma (2) Outburst of Sgr A* (3) Multiple SNR (4) Non-Thermal Filaments and/or PWNe

6.7 keV line Plasma if diffuse kT ~ 7 keV (F6.95/F6.7) L2-10 ~ 2x1036erg/s Size ~ 50pc x 30pc nave ~ 0.1cm-3 npeak ~ 0.4cm-3 Egas ~ 3x1052ergs if diffuse Escape Time scale: tesc = Size/Cs = 2x104yr Heating Rate = Egas/tesc~5x1040ergs/s~10-3 SN yr -1 Very High ! (1) High SN rate ! Many SNRs in the GC (2) Past Activities (Flares) of the Super massive black hole Sgr A* (eg. Koyama et al. 1996)

l-distribution b-distribution Point source Flux (4.8-8 keV) (1) ~7 keV Diffuse Plasma The 6.7 keV line flux vs Integrated point source flux (Chandra deep exposure) Near　GC ( |I| < 0.3 deg) l-distribution b-distribution Sgr A* 10 x 6.7 keV line (EW=0.5 keV) Point source Flux (4.8-8 keV) ( ｂ)

The 6.7 and 6.96 keV lines in the GC and GP 6.7 keV line : Exponential FWHM ~ 0.2 deg 6.7keV lines Point-sources: power-law index = 0.9 (Infrared star numbers, Chandra point sources) 6.96/6.7 keV Temperature F6.96/F6.7 ~0.3 --0.4 (GC) ~ 0.2--0.3 (GR)

6.4keV Clump =XRN (2) Outburst of Sgr A* Sgr B2 Sgr B1 New Sgr C Radio continuum Sgr B2 Sgr B1 New Sgr C

The Sgr B2 Cloud This flux change can not be explained by electrons. Variability time scale of the 6.4 keV flux ~5 - 10 ys (Inui et al. 2008) M 0.66 G 0.570 ~10pc This flux change can not be explained by electrons. We need X-ray irradiation. Where is the X-ray source ?

1994年 X-ray front 10 ly 2000年 2004年 2005年

2ay=x2 - a2: a = 300 light-yr: by Sgr B2 obs. ＊ Sawada et al. 2004 2ay=x2 - a2: a = 300 light-yr: by Sgr B2 obs.

Sgr B Cloud is in font of the GC Plasma sensitive for NH~1023

We found Many SNR Candidates (6 + 1+Sgr A East) Some are Likely Multi-SNe (3) Multiple SNR ~1keV ~3 keV

4) Non-thermal shells and/or PWNe Near the GC Contour: Non-thermal X-rays Colar Image: Radio continuum Large Filaments G359.54+0.18 (Lu et al. 2003) G359.89-0.08 G359.88-0.07 (Sakano et al. 2002)

Non-Thermal Emission of Cas A Extapolation of the power-law to 9—11 keV helser & Vink 2008

Jet 1 Jet 2 Jet 3 13

Conclusion Major fraction of the GCX is diffuse of ~7 keV plasma (2) 6.4 keV line clumps are time variable, hence the most probable origin is the reflection/fluorescence of the Sgr A* X-ray in an outburst of ~ AD 1700. (3) Many SNR Candidates are found in the GC. The plasma temperatures are 1—3 keV. (4) Most of the Non-thermal clumps are due to Sgr A East & Sgr A*. Some are associated to the radio filamnets.

Future observations to search for Possible Connection with the HESS TeV Emission: (1) Spectral study of the non-thermal emissions (2) Observations on the HESS soureces