high energy sky with advancing technology the galactic center view from tenma--suzaku hakucho...
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High Energy Sky with Advancing Technology
The Galactic Center View From Tenma--Suzaku
Hakucho (1979)96 kg
Tenma (1983) 216kg Ginga( 1987) 420 kg
ASCA( 1993) 417 kg
Suzaku (2005) 1600 kg
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Si S Fe
Tenma: Gas Scintilation Proportional Counter(2 times better resolution)
We found Kα lines from highly ionized Fe, S and Si in the Galactic RidgePresence of High temperature plasma
6.7 keV line
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Ginga (large proportional counter) surveyed the Glactic Plane with the 6.7 keV and continuum found excess emision at the Galactic Center
GC
2-10 keV band flux (log scale)
Fe K-line (6.7 keV) flux (linear scale)
Galactic longitude at b=0 deg
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The Closed-up View Near the Galactic Center
○ The 6.7 keV line region is extended
Center Energy =6.7 keV He-like iron (West) Center Energy < 6.7 keV (East)
2-10 keV
6.7 keV line
Beam size
Center Energy
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ASCA (X-ray CCD + Telescope) separated the K-shell lines into the 6.7 (He-like), 7.0 (H-like) and 6.4 keV (neutral) lines
We found 6.4 keV clumps at the molecular clouds, Sgr B and Sgr A.---> puzzle is solved.The spectrum has strong iron line and large absorption near the iron K-edge at 7.1 keV. Fluorescence by external X-raysNo bright X-ray source is found
The illuminating source was bright in the past, but faint at present
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The Center of the Galaxy in the Recent Past: A view from GRANAT
Sunyaev et al. 1993,
ASCA View of Our Galactic Center: Remains of Past Activities in X-Rays? Koyama et al., 1996, PASJ, 48.
Rasid Sunyaev and I met with each other with the same idea.
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Suzaku found K α lines of highly ionized Ar, Ca, Cr, Mn , Fe and Ni (red) and those of neutral (blue )
:Z= 1.6 solar 4 solar
The EWs ( absolute values and distribution pattern) are consistent with the X-ray fluorescent origin from clouds of 1.6 solar abundances. Electron origin requires more than 4 solar for all elements !
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l-distribution of the 6.4 keV lines
Sgr A
Discoveries of New 6.4 keV Clouds
Sgr B2Sgr B1M0.74-0.09
M359.43-0.07M359.47-0.15M359.43-0.12M359.38-0.00 M359.23-0.04
M0.1-0.1Arches G0.174-0.223G0.162-0.127
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1994 年 2004 年
2005 年2000 年
Rapid Time-Varaibility of Sgr B2
6.4 keV line :Koyama et al. 2008, Inui et al. 2009, Hard X-rays :Terrier et al. 2010
ASCA XMM-Newton
Chandra Suzaku
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Suzaku found simultaneous variablity of the 6.4 keV line & Hard X-rays in Sgr B2
2005 2009
The rapid/simultaneous variability strongly supports the X-ray fluorescence origin irradiated by an external big but short X-ray flare.
What is the external flare ?
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Parabolax2+y2=(300-y)2
(Unit is light-year)Sgr A* Flare ~300 years agoFermi bubble ?Quasar-like activity 1Myears ago ( Su, M. et al. 2010)
Face-on View of the 6.4 keV cloud(e.g. Ryu et al. 2009)
Near side GCDX is not absorbed by the cloud, while far side is heavily absorbed by the cloud.=> Face on position of the cloud
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The END