Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.4403y&link_type=abstract
American Astronomical Society Meeting 210, #44.03; Bulletin of the American Astronomical Society, Vol. 39, p.158
Other
Scientific paper
The soft X-ray background shows a general enhancement toward the inner region of the Galaxy. But whether this enhancement is a local feature (e.g., a superbubble within a distance of 200 pc or a phenomenon related to energetic outflows from the Galactic center/bulge remains unclear. Here we report a comparative X-ray emission and absorption study of diffuse hot gas along the sight lines toward 3C 273 and Mrk 421, on and off the enhancement, but at similar Galactic latitudes. The diffuse 3/4-keV emission intensity, as estimated from the ROSAT All Sky Survey, is about three times higher toward 3C 273 than toward Mrk 421. Based on archival Chandra grating observations of these two AGNs, we detect z 0 X-ray absorption lines (e.g., OVII Kalpha, Kbeta, and OVIII Kalpha transitions) and find that the mean hot gas thermal and kinematic properties along the two sight lines are significantly different. By subtracting the background contribution, as determined along the Mrk 421 sight line, we isolate the net X-ray absorption and emission produced by the hot gas associated with the enhancement in the direction of 3C 273. From a joint analysis of these differential data sets, we obtain the temperature, dispersion velocity, and hydrogen column density as 2.0E6 K, 200 km/s, and 2E19 cm^{-2}, respectively, assuming that the gas is approximately isothermal, solar in metal abundances, and in collisional ionization equilibrium. We also constrain the effective extent of the gas to be 3.4 kpc, strongly suggesting that the enhancement most likely represents a Galactic central phenomenon.
Wang Qiangguo
Yao Yangsen
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