The sizes of BLRs and BH masses of double-peaked broad low-ionization emission line objects

Details The sizes of BLRs and BH masses of double-peaked broad low-ionization emission line objects The sizes of BLRs and BH masses of double-peaked broad low-ionization emission line objects

2007-01-23

arxiv.org/abs/astro-ph/0701657v2

Astronomy and Astrophysics

Astrophysics

7 pages, two figures and one table. Accepted by MNRAS

Scientific paper

10.1111/j.1365-2966.2007.11536.x

In this paper, the sizes of the BLRs and BH masses of DouBle-Peaked broad low-ionization emission line emitters (dbp emitters) are compared using different methods: virial BH masses vs BH masses from stellar velocity dispersions, the size of BLRs from the continuum luminosity vs the size of BLRs from the accretion disk model. First, the virial BH masses of dbp emitters estimated by the continumm luminosity and line width of broad H$\beta$ are about six times (a much larger value, if including another dbp emitters, of which the stellar velocity dispersions are traced by the line widths of narrow emission lines) larger than the BH masses estimated from the relation $M_{BH} - \sigma$ which is a more accurate relation to estimate BH masses. Second, the sizes of the BLRs of dbp emitters estimated by the empirical relation of $R_{BLR} - L_{5100\AA}$ are about three times (a much larger value, if including another dbp emitters, of which the stellar velocity dispersions are traced by the line widths of narrow emission lines) larger than the mean flux-weighted sizes of BLRs of dbp emitters estimated by the accretion disk model. The higher electron density of BLRs of dbp emitters would be the main reason which leads to smaller size of BLRs than the predicted value from the continuum luminosity.

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