The Spectral Energy Distributions of Red 2MASS AGN

Details The Spectral Energy Distributions of Red 2MASS AGN The Spectral Energy Distributions of Red 2MASS AGN

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.4601k&link_type=abstract

American Astronomical Society, AAS Meeting #211, #46.01; Bulletin of the American Astronomical Society, Vol. 39, p.800

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the infrared to X-ray spectral energy distributions (SEDs) for 44 red AGN selected from the 2MASS survey on the basis of red J-K>2mag. color and observed by Chandra. The sample consists of Type 1 objects with BALQSOs/NLS1 spectra, intermediate Type 1.2-1.9 sources, many with high polarization (P=4-13%), and Type 2 objects with low absorption, NH=1022 cm-2. In comparison with the blue optically- and radio-selected AGN and hard-X-ray selected AGN, the 2MASS median SED is redder in the optical and near-IR showing little or no big blue bump. We model the red colors as a mixture of a reddened (AV=0-22 mags. i.e. NH=0-3.5*1022 cm-2) AGN, host galaxy emission (approaching 100% at R band in some, heavily reddened sources), and AGN scattered light emission. The obscuration allows us to see weaker emission components which are generally swamped by the AGN.
We have run PCA analysis on the SED properties of our 2MASS AGN. The first four eigenvectors explain 70% of the variance in the sample. Eigenvector 1 (33% of variance) correlates with the ratios of the intrinsic X-ray flux to the observed optical/IR flux (F(1keV)/FB,R,J,K) and F(2-10keV)/F([OIII]), and is primarily driven by accretion rate and strengthened by intrinsic reddening. Eigenvector 2 (18% of variance) correlates with B-K, B-R, J-K colors, and depends on the host galaxy contribution relative to the observed AGN. Eigenvector 3 (12% of variance) correlates with the reddening indicators: hardness ratio, X-ray spectral index, NH, and narrow Halpha/Hbeta, suggesting a common absorber for the optical and X-rays lying outside the NLR, possibly in the host galaxy moderately inclined to our line of sight. Eigenvector 4 (8% of variance) is dominated by the degree of polarization and broad Halpha/Hbeta ratio implying, that dust that scatters the continuum and broad lines also reddens the broad emission lines.

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