Average Spectral Energy Distributions of AGN Host Galaxies at z < 1 and the Geometries of Their Obscuring Clouds

Details Average Spectral Energy Distributions of AGN Host Galaxies at z < 1 and the Geometries of Their Obscuring Clouds Average Spectral Energy Distributions of AGN Host Galaxies at z < 1 and the Geometries of Their Obscuring Clouds

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.0802p&link_type=abstract

American Astronomical Society, HEAD meeting #11, #8.02; Bulletin of the American Astronomical Society, Vol. 41, p.663

Astronomy and Astrophysics

Astronomy

Scientific paper

We present spectral energy distributions (SEDs) of "average" AGN host galaxies at redshifts z < 1, for which the galaxy contributions to the SEDs have been isolated from the AGN contributions. AGNs are here defined as systems exhibiting X-ray luminosities log(L_2-10 keV) > 41.5 [erg/s]. The average SEDs are examined for trends with redshift, color, and X-ray characteristics (e.g., luminosity and obscuration/hardness ratio). Furthermore, we analyze the average SEDs to determine their typical stellar populations and star formation histories. In order to isolate the observed host galaxy SEDs, we match a set of modeled AGN SEDs, created using the Cloudy software and a variety of parameters, to samples of observed SEDs, which naturally represent both the AGNs and their host galaxies. The 250 observed systems are drawn from the 2-square degree COSMOS field and have spectral coverage from the X-ray through the far-infrared. After separating the observed SEDs into several sub-samples based on redshift, optical color, and X-ray luminosity, the median SED from each sub-sample is matched to one or more of the modeled SEDs based on the X-ray spectral slope, which is dominated by the AGN. Finally, we subtract the modeled SEDs from the corresponding median observed SEDs, thereby isolating the SEDs of the host galaxies. The parameters used to create the modeled AGN SEDs represent a variety of obscuration geometries, so that determination of the closest matches between the modeled and observed SEDs provides an indication of the most realistic and/or most common geometry of the obscuring material.

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