8-12 juin, 2014


AGNs: Line Width Distribution of MHD Disc Winds

Laura S. Chajet (York University)

Patrick B. Hall, York University

We present results on modelling AGN disc wind broad emission line pro les for a set of black hole masses and luminosities. It is now increasingly accepted that AGN broad emission form in winds emerging from the accretion disc, the same wind that has been invoked to explain broad absorption lines. Those outflows have been recognized as a likely feedback mechanism by the SMBHs to their host galaxy, thus regulating their co-evolution. Due to their ubiquity, some authors regard emission lines as a more powerful tool to studying AGN than absorption lines. We study AGN emission line pro les with a model that combines an improved version of the accretion disc wind model of Murray & Chiang (1997) with the magnetohydrodynamic driving of Emmering et al. (1992). We have compared the dispersions in our model CIV linewidth distributions to observational upper limit on that dispersion. We found that the allowed region in the inclination-launch angle plane has an upper limit that depends on the torus half-opening angle. For our ducial case, with a mass M = 10^8 M_Sun and L = 10^46 erg/s, the maximum torus half-opening torus angle compatible with the observations is about 47 degrees. We extended the analysis to consider different masses and luminosities and found that the dispersion of the linewidth (and, thus, the torus half-opening angle) depends fairly strongly on both AGN parameters.

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