A Simultaneous RXTE and XMM-Newton Observation of the Broad-Line Radio Galaxy 3C 111

Details A Simultaneous RXTE and XMM-Newton Observation of the Broad-Line Radio Galaxy 3C 111 A Simultaneous RXTE and XMM-Newton Observation of the Broad-Line Radio Galaxy 3C 111

2004-12-20

arxiv.org/abs/astro-ph/0412537v1

Astrophys.J. 622 (2005) 816-829

Astronomy and Astrophysics

Astrophysics

22 pages, 3 tables, 11 figures, accepted for publication in The Astrophysical Journal

Scientific paper

10.1086/428380

We present the results of simultaneous XMM-Newton and RXTE observations of the Broad-Line Radio Galaxy 3C 111. We find that the Compton reflection bump is extremely weak, however, broad residuals are clearly present in the spectrum near the Fe Kalpha emission line region. When fitted with a Gaussian emission line,the feature has an equivalent width of 40-100eV and full-width at half maximum of greater than 20,000 km/s, however the exact properties of this weak line are highly dependent upon the chosen continuum model. The width of the line suggests an origin in the inner accretion disk, which is, however, inconsistent with the lack of Compton reflection. We find that much of the broad residual emission can be attributed to continuum curvature. The data are consistent with a model in which the primary powerlaw continuum is reprocessed by an accretion disk which is truncated as small radii. Alternatively, the primary source could be partially covered by a dense absorber. The latter model is less attractive than the former because of the small inclination angle of the jet of 3C 111 to the line of sight. We consider it likely that the curved continuum of the partial covering model is fortuitously similar to the continuum shape of the reprocessing model. In both models, the fit is greatly improved by the addition of an unresolved Fe K alpha emission line, which could arise either in a Compton-thin obscuring torus or dense clouds lying along the line of sight. We also find that there are unacceptable residuals at low energies in the MOS data in particular, which were modeled as a Gaussian with an energy of ~1.5 keV; we attribute these residuals to calibration uncertainties of the MOS detectors.

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