Erratum: Major contributor to AGN feedback: VLT X-shooter observations of S IV BALQSO outflows (Astrophysical Journal (2013) 762 (49) DOI: 10.1088/0004-637x/762/1/49)

For the quasar outflow analyzed in SDSS J1106+1939, the published article (Borguet et al. 2013) did not notice that the absorption trough from S IV λ1062.66 is blended with a damped Lyα (DLA) system. In this erratum, we model this DLA system and remeasure the column densities (Nion) from the troughs of S IV λ1062.66 and S IV*λ1072.96. Then we update the key physical parameters of the quasar outflow observed in SDSS J1106+1939, including distance (R) of the outflow to the center ionizing source, the outflow's mass-flow rate (M) and kinetic luminosity (log(Ek)). We also present the updated Figures 3, 4, and Table 5. The DLA trough is located at ∼4172 A in the observed frame (see Figure 3), which blends with the observed S IV trough. The corresponding metal lines for the DLA system are also detected, e.g., from Si II λ1260.42, Si III λ1206.50, C IV λλ1548.20, 1550.77, and Mg II λλ2796.35, 2803.53. By matching these lines, we determine the redshift (z) of the DLA system as z = 2.432. We first model the DLA trough by a Voigt profile (e.g., Prochaska et al. 2005). We vary the logarithm of the total hydrogen column density, i.e., log(NH), between 19.5 and 21.0 in steps of 0.1 dex. We find the best-fitting log(NH) = -20.2+0.1 0.1 cm-2. The bestfitting DLA trough is shown as the purple dashed line in Figure 3. This DLA trough fits the left wing well from 4150-4170 A in the observed frame. However, it is unable to fit the spectral region from 4180-4200 A in the observed frame (see Figure 3). This supports the existence of the S IV absorption trough from 4160-4230 A in the observed frame. Similar to Model 1 discussed in Section 3.2 of the published article, we model the troughs from S IV and S IV* of the outflow system by two Gaussian profiles. In Figure 3, we show the best-fitting models for S IV and S IV* troughs in blue and red solid lines, respectively. For each trough, the high-velocity and low-velocity Gaussian profiles are shown as the dashed and dotted lines, respectively, and are centered at-8250 and-7000 km s-1. The overall model by summing up the damped Lyα, SIV, and S IV* troughs is shown as the solid green line. This overall model fits the quasar spectrum well from 4150-4250 A in the observed frame. The best-fitting S IV and S IV* troughs yield column densities of N(S IV*) = 26,400-2500+1000 and N(S IV) = 30,500-2500+4000 (both in units of 1012 cm-2). This leads to the ratio of N(S IV*)/N(S IV) = 0.87-0.14+0.08. Then we show the corrected Figure 4 by adopting this new ratio. We get an updated electron number density log(ne) = 4.6-0.08+0.12 cm-3. This value is ∼0.5 dex higher than the log(ne) value reported in the published article. In Table 5, we show the updated distance (R) of the outflow to the center ionizing source, the outflow;s mass-flow rate (M) and kinetic luminosity [log(Ek)] in bold face. Compared to the published article, these updated values all decrease by a factor of ∼1.8. We thank Dr. Karen Leighly for pointing out the existence of the DLA system in the spectrum of this object.