Physics
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21720605r&link_type=abstract
American Astronomical Society, AAS Meeting #217, #206.05; Bulletin of the American Astronomical Society, Vol. 43, 2011
Physics
Scientific paper
A large body of recent work points towards feedback processes related to the active accretion of matter onto supermassive black holes in the centers of most massive galaxies as being one of the primary regulatory processes for pc to Mpc scales in the Universe. We seek to close the gap in our knowledge of the physics behind active galactic nuclei (AGN) feedback processes by improving in our knowledge of 1) the spectral energy distribution (SED) of AGNs from the mid-IR through UV and 2) the relationship between the SED and the accretion disk wind. Using a sample of up to 30,000 SDSS quasars, we explore the range of properties exhibited by high-ionization, broad emission lines, such as CIV (specifically the Baldwin effect and the
``blueshifting'' of the high-ionization emission lines). We consider these phenomena within the context of an accretion disk wind model that is modulated by the shape of the SED. Composite spectra are constructed as a function of CIV emission line properties in attempt to reveal empirical relationships between different line species and the SED. Within a two component disk+wind model of the BELR where the wind filters the continuum seen by the disk component, we find that radio-loud quasars are dominated by the disk component, while broad absorption line quasars are dominated by the wind component. Our results suggest that there could be significant systematic errors in the determination of LBol and black hole mass that make it difficult
to place these findings in a more physical context. However, it is possible to classify quasars in a paradigm where the diversity of broad emission line region parameters are due to changes in an accretion disk wind between quasars (and over time) that are underlied by the SED, which ultimately must be tied to mass and accretion rate.
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