We analyze new HST/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 iv, Si ii, and P v. From the ratio of the S iv* to S iv column densities, we measure the electron number density of the higher-velocity (?1400 km s?1, v1400) outflow to be cm?3 and constrain the lower-velocity (?730 km s?1, v700) outflow to log(n e )?>?5.3?cm?3. The n e 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 χ 2-minimization fit for the ionization parameter and hydrogen column density of the higher-velocity outflow: log( and log( cm?2, respectively. We calculate from U H and n e a distance of 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 . 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.
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机译：我们分析了在准星体物体LBQS 1206 + 1052中看到的两个类星体吸收流出的新HST / COS光谱。这些数据首次覆盖了S iv，Si ii和P v的吸收谷。根据S iv *与S iv柱密度的比值，我们测量了较高速度的电子数密度（？1400 km s？1，v1400）的流出量为cm？3，并将较低速度（？730 km s？1，v700）的流出量限制为log（ne）？>？5.3？cm？3。与高速流出相关的n e比以前的工作报道的数量级大。我们发现先前的测量是不可靠的，因为它是基于对密度敏感的吸收槽（可能已饱和）。使用光电离模型，我们确定了较高流速的电离参数和氢柱密度的最佳χ2最小拟合：log（和log（cm？2）。使用通过v700流出衰减的SED，可以为v1400流出产生两相光电离溶液，并以a分隔。否则，所得的距离，质量通量和动力学亮度与未衰减的情况相似。 ，由于2017年对v700的流出缺乏限制，因此衰减分析具有很大的不确定性。
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