Hubble Space Telescope ultraviolet spectroscopy of blazars: emission lines properties and black hole masses

Details Hubble Space Telescope ultraviolet spectroscopy of blazars: emission lines properties and black hole masses Hubble Space Telescope ultraviolet spectroscopy of blazars: emission lines properties and black hole masses

2005-06-29

arxiv.org/abs/astro-ph/0506725v2

Mon.Not.Roy.Astron.Soc.361:919-926,2005

Astronomy and Astrophysics

Astrophysics

published in MNRAS (small changes with respect to preprint previously submitted)

Scientific paper

10.1111/j.1365-2966.2005.09216.x

The ultraviolet (UV) spectra of 16 blazars ( ~1) from the archives of the Hubble Space Telescope Faint Object Spectrograph have been analyzed in order to study in a systematic way the properties oftheir broad UV emission lines. We find that the luminosities of the most prominent and intense lines, Ly_alpha and C IV lambda1549, are similar to those of normal radio-loud quasars at comparable redshifts. However, the equivalent widths of blazar lines are significantly smaller than those of radio-loud quasars. Therefore, while the intrinsic broad line region luminosity of blazars appears to be indistinguishable from that of radio-loud quasars, their continuum must be comparatively higher, most probably due to relativistic beaming. We have combined the UV luminosities of the de-beamed continuum with the emitting gas velocity to derive estimates of the masses of the central supermassive black holes. The size of the broad line region was computed in two ways: 1) via an empirical relationship between UV continuum luminosity and broad line region size, and 2) through the external photon density required by blazar models to reproduce the inverse Compton components observed at gamma-rays. The second method yields significantly different results from the first method, suggesting that it provides only a very rough estimate or a lower limit on the size of the broad line region. We find that the average mass of the central black holes in blazars is ~2.8e8 Msun, with a large dispersion, comparable to those computed for other radio-loud active galactic nuclei.

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