The Spectral Energy Distributions of Active Galactic Nuclei. (arXiv:1902.07595v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Brown_M/0/1/0/all/0/1">M. J. I. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duncan_K/0/1/0/all/0/1">K. J. Duncan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landt_H/0/1/0/all/0/1">H. Landt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kirk_M/0/1/0/all/0/1">M. Kirk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_C/0/1/0/all/0/1">C. Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kamraj_N/0/1/0/all/0/1">N. Kamraj</a>

We present ongoing work on the spectral energy distributions (SEDs) of active
galactic nuclei (AGNs), derived from X-ray, ultraviolet, optical, infrared and
radio photometry and spectroscopy. Our work is motivated by new wide-field
imaging surveys that will identify vast numbers of AGNs, and by the need to
benchmark AGN SED fitting codes. We have constructed 41 SEDs of individual AGNs
and 80 additional SEDs that mimic Seyfert spectra. All of our SEDs span 0.09 to
30 microns, while some extend into the X-ray and/or radio. We have tested the
utility of the SEDs by using them to generate AGN photometric redshifts, and
they outperform SEDs from the prior literature, including reduced redshift
errors and flux density residuals.

We present ongoing work on the spectral energy distributions (SEDs) of active
galactic nuclei (AGNs), derived from X-ray, ultraviolet, optical, infrared and
radio photometry and spectroscopy. Our work is motivated by new wide-field
imaging surveys that will identify vast numbers of AGNs, and by the need to
benchmark AGN SED fitting codes. We have constructed 41 SEDs of individual AGNs
and 80 additional SEDs that mimic Seyfert spectra. All of our SEDs span 0.09 to
30 microns, while some extend into the X-ray and/or radio. We have tested the
utility of the SEDs by using them to generate AGN photometric redshifts, and
they outperform SEDs from the prior literature, including reduced redshift
errors and flux density residuals.

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