Intrinsic Absorption in the QSO FIRST J121442.3+280329

Abstract

This paper presents an analysis of a Keck HIRES spectrum of the QSO FIRST J121442.3]280329, covering the rest wavelength range from 2300 to 3500The line of sight toward this quasar (QSO) A . contains an outÑow giving rise to many blueshifted absorption lines. The outÑow consists of material with a continuous range of velocities from [1200 to [2800 km s~1. SigniÐcant substructure is present in the absorption line proÐles. The spectrum is dominated by absorption lines of Mg II and the singly ionized iron group elements Fe II, Cr II, and Mn II, including absorption lines from excited levels with energies above 30,000 cm~1 (D4 eV).We derive constraints on the physical conditions in the outÑow by Ðtting a model to the observed spectrum that simultaneously optimizes the values for the column densities of all species, the excitation temperature, the shape of the unabsorbed continuum, and the covering factor. By comparing these constraints with ionization models, we conclude that the ionization parameter, density, and column density of the outÑow is characterized by [2.0 \ log U \ [0.7, 7.5 \ and These values place the absorbing outÑow at a distance between 1 log n H \ 9.5, 21.4 \ log N H \ 22.2. and 30 pc from the QSO core.

VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7

“…Using this method, r ∼ 310 pc has been measured for the low-velocity system in FIRST J084044.5+363328, whereas r ∼ 1.35 pc is found for the high-velocity system in the same object using different diagnostic (de Kool et al 2002b). However, analysis of the similar NAL in FIRST J121442.3+280329 yielded a small distance range ∼1−30 pc for the entire outflow (de Kool et al 2002a), similar to that found for LBQS 0059-2735 (Wampler et al 1995). The largest distance found by this method has been for the low-ionization BAL in FIRST J104459.6+365605…”

Broad absorption line disappearance and emergence using multiple-epoch spectroscopy from the Sloan Digital Sky Survey

“…Studies using variable Fe ii and Mg ii BALs constrained outflows to exist within tens of parsecs of the central source (Hall et al 2011;McGraw et al 2015). Previous studies using photoionization models have also constrained some BAL outflows to exist from parsecs to tens of parsecs from the SMBH using transitions from Fe ii, Cr ii, Mg ii, and Mn ii (Everett, Königl & Arav 2002;de Kool et al 2002).…”

A Self‐consistent NLTE‐Spectra Synthesis Model of FeLoBAL QSOs

“…The first consisted of a linear combination of five sets of Fe ii BELs from theoretical model calculations (Verner et al 1999), and the second was the observed Fe ii BEL spectrum of the strong emission-line QSO 2226À3905 (Graham et al 1996). For the absorption features, de Kool et al (2002) obtained a template distribution of line optical depth with respect to velocity in the broad absorption line region ( BALR) from the observed absorption profile of Fe ii k3004, an apparently unblended line of moderate strength. Given the assumption that only absorption takes place in the BALR, the optical depth was obtained from (v) ¼ log F k , where F k is the fractional residual flux in the absorption feature.…”

“…In that paper, the FeLoBAL 3 FIRST J121442+280329 was modeled using SYNOW, a parameterized, spherically symmetric, resonant-scattering, synthetic spectrum code more typically used to model supernovae ( Fisher 2000). The difference between this treatment and a more typical one applied to the same data by de Kool et al (2002) is that SYNOW assumes that emission and absorption are produced in the same outflowing gas. In contrast, the approach taken by de Kool et al (2002) assumes that absorption is imprinted on a typical continuum + emission line quasar spectrum; that is, the absorbing gas is separated from the emission-line region.…”