The z=0.54 LoBAL Quasar SDSS J085053.12+445122.5: II. The Nature of Partial Covering in the Broad-Absorption-Line Outflow. (arXiv:1811.04174v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Leighly_K/0/1/0/all/0/1">Karen M. Leighly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Terndrup_D/0/1/0/all/0/1">Donald M. Terndrup</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lucy_A/0/1/0/all/0/1">Adrian B. Lucy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallagher_S/0/1/0/all/0/1">Sarah C. Gallagher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richards_G/0/1/0/all/0/1">Gordon T. Richards</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_M/0/1/0/all/0/1">Matthias Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raney_C/0/1/0/all/0/1">Catie Raney</a>
It has been known for 20 years that the absorbing gas in broad absorption
line quasars does not completely cover the continuum emission region, and that
partial covering must be accounted for to accurately measure the column density
of the outflowing gas. However, the nature of partial covering itself is not
understood. Extrapolation of the SimBAL spectral synthesis model of the HST COS
UV spectrum from SDSS J0850+4451 reported by Leighly et al. 2018 to the
rest-frame optical and near-infrared spectra reveals evidence that the covering
fraction has wavelength dependence, and is a factor of 2.5 times higher in the
UV than in the optical and near-infrared bands. Analysis of the spectral energy
distribution and an HST near-infrared image shows that the contribution of the
host galaxy to the near-infrared continuum is negligible. Observed absorption
line variability trends show that it is probably not responsible for the effect
either. The difference in covering fraction can be explained if the outflow
consists of clumps that are small and either structured or clustered relative
to the projected size of the UV continuum emission region, and have a more
diffuse distribution on size scales comparable to the near-infrared continuum
emission region size. This experiment demonstrates that we can compare
rest-frame UV and near-infrared absorption lines, specifically HeI*10830, to
place constraints on the geometry of absorption gas in broad absorption line
quasars.
It has been known for 20 years that the absorbing gas in broad absorption
line quasars does not completely cover the continuum emission region, and that
partial covering must be accounted for to accurately measure the column density
of the outflowing gas. However, the nature of partial covering itself is not
understood. Extrapolation of the SimBAL spectral synthesis model of the HST COS
UV spectrum from SDSS J0850+4451 reported by Leighly et al. 2018 to the
rest-frame optical and near-infrared spectra reveals evidence that the covering
fraction has wavelength dependence, and is a factor of 2.5 times higher in the
UV than in the optical and near-infrared bands. Analysis of the spectral energy
distribution and an HST near-infrared image shows that the contribution of the
host galaxy to the near-infrared continuum is negligible. Observed absorption
line variability trends show that it is probably not responsible for the effect
either. The difference in covering fraction can be explained if the outflow
consists of clumps that are small and either structured or clustered relative
to the projected size of the UV continuum emission region, and have a more
diffuse distribution on size scales comparable to the near-infrared continuum
emission region size. This experiment demonstrates that we can compare
rest-frame UV and near-infrared absorption lines, specifically HeI*10830, to
place constraints on the geometry of absorption gas in broad absorption line
quasars.
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