Corona, Jet, and Relativistic Line Models for Suzaku/RXTE/Chandra-HETG Observations of the Cygnus X-1 Hard State

Details Corona, Jet, and Relativistic Line Models for Suzaku/RXTE/Chandra-HETG Observations of the Cygnus X-1 Hard State Corona, Jet, and Relativistic Line Models for Suzaku/RXTE/Chandra-HETG Observations of the Cygnus X-1 Hard State

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.4313n&link_type=abstract

American Astronomical Society, HEAD meeting #11, #43.13; Bulletin of the American Astronomical Society, Vol. 41, p.733

Astronomy and Astrophysics

Astronomy

Scientific paper

We conducted a series of four simultaneous Suzaku-RXTE observations of the galactic black hole Cyg X-1 in what were historically low flux, hard spectral states. The last of these observations (April 2008) was also simultaneous with every X-ray and gamma-ray satellite flying at that time, including Chandra-HETG. The HETG spectra are crucial for modeling the ionized absorbtion from the "focused-wind" of the secondary, which is present and must be accounted for in all of our spectra. Our data give an unprecedented view of the 0.8-300 keV spectra of Cyg X-1, and hence bear upon both corona and X-ray emitting jet models of black hole hard states. Three models fit the spectra well: coronae with thermal or mixed thermal/non-thermal electron populations, and jets. All three agree that the known spectral break at 10 keV is not solely due to the presence of reflection, but give different underlying explanations for the augmentation of this break. Thus whereas all three models agree that there must be a relativistically broadened Fe line, the strength and inner radius of such a line is dependent upon the specific model. We look at the relativistic line in detail, accounting for the narrow Fe emission and ionized absorption detected by HETG. Although the specific relativistic parameters of the line are continuum-dependent, none of these models allow for an inner disk radius that extends to radii greater than 40 GM/c2.

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