tokens: uncertainty: the propagation of the individual uncertainty spectra (left panel) and the jackknife uncertainty (right panel). Vertical ticks and labels mark the expected positions of other lines of interest, color-coded as in Figure 3 . The plotted transitions trace large-scale galactic winds and have ionization potentials of 15.0 eV (Mg ii ) and 16.2 eV (Fe ii ). (b) Same as Figure 5 (a), for transitions with ionization potentials from 13.6 eV (top panel) to 24.4 eV (bottom panel). The weighted average stack is shown in the left panel and the median stack in the right panel. (c) Same as Figure 5 (a), for transitions with high ionization potential. Transitions are plotted in order of increasing ionization potential, from top to bottom, from 28.4 to 97.9 eV. The weighted average stack is shown in the left panel and the median stack in the right panel. In Figure 5 (a), we consider the transitions of Mg ii 2796, Fe ii 2344, and Fe ii 2383. 12 12 Fe ii 2600 is unusable due to adjacent Mn ii absorption. These transitions have ionization potentials of 15.0 eV (Mg ii ) and 16.2 eV (Fe ii ) and are associated with spatially resolved, large-scale outflows in galaxies at –2 (Martin and Bouché 2009 ; Weiner et al. 2009 ; Rubin et al. 2010 , 2011 ; Giavalisco et al. 2011 ; Erb et al. 2012 ; Kornei et al. 2013 ; Bordoloi et al. 2014 ; Rigby et al. 2014 ; Rubin et al. 2014 ). In the M eg a S a ura weighted-average shape-normalized stack, these transitions have a maximum velocity of = 900 km s −1 (Table 3 .) Bordoloi et al. ( 2016 ) analyzed the velocity profiles of four regions within one of these galaxies, RCS-GA 032727−132609, and found 95th percentile velocities of 460–610 km s −1 for these transitions. Mg ii is at the extreme red end of the M eg a S a ura stack and so only four galaxy spectra went into the stack; seven galaxies contribute to the stack for Fe ii 2344 and Fe ii 2383. Knot E of RCS-GA 032727−132609 contributed to the stack for both Mg ii and Fe ii . Despite those small numbers, the maximum velocities we measure for Mg ii and Fe ii confirm and extend the conclusion of Bordoloi et al. ( 2016 ): a substantial fraction of the Mg ii and Fe ii gas column has velocities far exceeding the plausible escape velocity of their galactic hosts. 3.5. Galactic Winds as Probed by Other Low-ionization Transitions We next analyze the absorption velocity profiles of other low-ionization transitions, plotted in Figure 5 (b). The main transitions that trace the neutral gas are Ly α and O i 1302, as they have low ionization potentials (13.6 eV). However, a maximum wind velocity cannot be measured for O i 1302 because of nearby photospheric absorption lines, and Ly α is difficult to interpret due to resonant scattering. Instead, we must estimate the wind velocity from Si ii , Al ii , and C ii , which have ionization potentials of 16.3, 18.8, and 24.4 eV, respectively, and therefore trace a mixture of neutral and ionized gas. This absorption has ∼ 630–940 km s −1 in
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