IRAC 8 micro K-band 0.5-2 keV. X-ray Emission Line Spectroscopy of Diffuse Hot Plasma. Chandra ACIS-I. XMM-Newton RGS Liu, Wang, Li, & Peterson 2010. T ~ 3 x 10 6 K Lx ~2x10 38 erg/ s. Li & Wan 2007. X-ray spectroscopy: He-like ions. R ( or W) : Resonance line (allowed)
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IRAC 8 micro
Liu, Wang, Li, & Peterson 2010
T ~ 3 x 106 K
Li & Wan 2007
electronic dipole transition
1s2p 3P1 1s2 1S0 (y)
1s2p 3P21s2 1S0 (x)
Triple or quadruplet
1s2s 3S1 1s2 1S0
relativistic magnetic dipole transition (Ajivery low)
Simplified Grotrian diagram
Porquet & Dubau (2000)
Photo-ionized plasma as seen in an AGN can have stronger forbidden lines.
From Dennerl 2010
CX is also expected at the heliosphere
Futamoto et al. 2004, Wang et al. 05, Yao & Wang 05/06, Yao et al. 06/07/08
ROSAT all-sky survey in the ¾-keV band
Fe XVII K
LETG+HETG spectrum of LMXB 1820-303
Yao & Wang 2006, Yao et al. 2006, Futamoto et al 2004
(Credit: NASA/CXC/SAO/R.DiStefano et al.)
Soria& Wu (2002)
Charge exchange may be responsible for much of diffuse soft X-ray emission in both normal and starburst galaxies.
Li, Mao, Wang 2011
Soft X-ray arises primarily from the interplay between a superwind and entrained cool gas clouds.
Composite of optical (HST), infrared (Spitzer), and X-ray (Chandra) images
OVIII contours on HST image
OVIII contours on OVII image
Ha+[NII] image (Kenney et al. 1995).
Chandra 0.3-2 keV image, Machacek et al. 2004
Astro-H, planned for launch in 2013