http://arxiv.org/abs/1905.08201
Quasar outflows are fundamental components of quasar environments that might play an important role in feedback to galaxy evolution. We report on the emergence of a remarkable new outflow absorption-line system in the quasar PG1411+442 (redshift ~0.089) detected in the UV and visible with the Hubble Space Telescope Cosmic Origins Spectrograph and the Gemini Multi-Object Spectrograph, respectively. This new “transient” system contains thousands of lines, including FeII and FeII* from excited states up to 3.89 eV, HI* Balmer lines, NaI D 5890,5896, and the first detection of HeI* 5876 in a quasar. The transient absorber is spatially inhomogeneous and compact, with sizes ~<0.003 pc, based on covering fractions on the quasar continuum source ranging from ~0.45 in strong UV lines to ~0.04 in NaI D. Cloudy photoionization simulations show that large total column densities log N_H(cm^-2) >~ 23.4 and an intense radiation field ~<0.4~pc from the quasar are needed to produce the observed lines in thick zones of both fully-ionised and partially-ionised gas. The densities are conservatively log n_H(cm-3) >~ 7 based on FeII*, HI*, and HeI* but they might reach log n_H(cm^-3) >~ 10 based on NaI D. The transient lines appear at roughly the same velocity shift, v ~ -1900 km/s, as a “mini-BAL” outflow detected previously, but with narrower Doppler widths, b ~ 100 km/s, and larger column densities in more compact outflow structures. We propose that the transient lines identify a clumpy outflow from the broad emission-line region that, at its current speed and location, is still gravitationally bound to the central black hole.
F. Hamann, T. Tripp, D. Rupke, et. al.
Tue, 21 May 19
22/71
Comments: 21 pages, submitted to MNRAS
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