X-ray Iron Line Emission From Sagittarius A*

Details X-ray Iron Line Emission From Sagittarius A* X-ray Iron Line Emission From Sagittarius A*

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aspc..439..434j&link_type=abstract

The Galactic Center: a Window to the Nuclear Environment of Disk Galaxies. Proceedings of a workshop held at Shanghai, China on

Astronomy and Astrophysics

Astronomy

Scientific paper

The line features between [6, 7] keV contain the critical information about the physical origin of the steady X-ray emission from Sagittarius A* and its vicinity. The observations by Baganoff et al. (2003) show that the line center detected outside of Bondi radius is about 6.5+0.1-0.2 keV, which indicates that the iron ions are not in a collisional ionization equilibrium (CIE). Indeed current models assume CIE and hence predict that iron ions are dominated by H and He-like ions with the line center being close to 6.7 keV. New spectral data from about 1 Ms of Chandra ACIS observations allow us to better constrain iron line features, which offers a good indicator to discriminate different models. We aim to examine non-equilibrium ionization (NEI) effects for Sgr A* and its vicinity using the various dynamic models based on the NEI code by Ji et al. (2006). Our preliminary results for the vicinity of Sgr A* show that the center of Fe ion features is 6.48+0.01-0.02 keV and σ = 87.2+1.5-1.7 eV.

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