Description:
<jats:title>Abstract</jats:title>
<jats:p>We analyze new <jats:italic>HST</jats:italic>/COS spectra for two quasar absorption outflows seen in the quasi-stellar object LBQS 1206+1052. These data cover, for the first time, absorption troughs from S <jats:sc>iv</jats:sc>, Si <jats:sc>ii</jats:sc>, and P <jats:sc>v</jats:sc>. From the ratio of the S <jats:sc>iv</jats:sc>* to S <jats:sc>iv</jats:sc> column densities, we measure the electron number density of the higher-velocity (−1400 km s<jats:sup>−1</jats:sup>, v1400) outflow to be <jats:inline-formula>
<jats:tex-math>
<?CDATA $\mathrm{log}({n}_{e})={4.23}_{-0.09}^{+0.09}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaad817ieqn1.gif" xlink:type="simple" />
</jats:inline-formula> cm<jats:sup>−3</jats:sup> and constrain the lower-velocity (−730 km s<jats:sup>−1</jats:sup>, v700) outflow to log(<jats:italic>n</jats:italic>
<jats:sub>
<jats:italic>e</jats:italic>
</jats:sub>) > 5.3 cm<jats:sup>−3</jats:sup>. The <jats:italic>n</jats:italic>
<jats:sub>
<jats:italic>e</jats:italic>
</jats:sub> associated with the higher-velocity outflow is an order of magnitude larger than reported in prior work. We find that the previous measurement was unreliable since it was based on density-sensitive absorption troughs that were likely saturated. Using photoionization models, we determine the best <jats:italic>χ</jats:italic>
<jats:sup>2</jats:sup>-minimization fit for the ionization parameter and hydrogen column density of the higher-velocity outflow: log(<jats:inline-formula>
<jats:tex-math>
<?CDATA ${U}_{{\rm{H}}})=-{1.73}_{-0.12}^{+0.21}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaad817ieqn2.gif" xlink:type="simple" />
</jats:inline-formula> and log(<jats:inline-formula>
<jats:tex-math>
<?CDATA ${N}_{{\rm{H}}})={21.03}_{-0.15}^{+0.25}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaad817ieqn3.gif" xlink:type="simple" />
</jats:inline-formula> cm<jats:sup>−2</jats:sup>, respectively. We calculate from <jats:italic>U</jats:italic>
<jats:sub>H</jats:sub> and <jats:italic>n</jats:italic>
<jats:sub>
<jats:italic>e</jats:italic>
</jats:sub> a distance of <jats:inline-formula>
<jats:tex-math>
<?CDATA ${500}_{-110}^{+100}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaad817ieqn4.gif" xlink:type="simple" />
</jats:inline-formula> pc from the central source to the outflow. Using an SED attenuated by the v700 outflow yields a two-phase photoionization solution for the v1400 outflow, separated by a <jats:inline-formula>
<jats:tex-math>
<?CDATA ${\rm{\Delta }}U\approxeq 0.7$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaad817ieqn5.gif" xlink:type="simple" />
</jats:inline-formula>. Otherwise, the resultant distance, mass flux, and kinetic luminosity are similar to the unattenuated case. However, the attenuated analysis has significant uncertainties due to a lack of constraints on the v700 outflow in 2017.</jats:p>