tokens: power. In AGN and LI(N)ER galaxies, the molecular component is more dominant than in star-forming galaxies. There is, however, significant variation from galaxy to galaxy. Studying the relative contribution of different phases to the outflow rate and the kinetic power as a function of SFR or α bol revealed no clear trends (see e.g. Section B1 ). Figure 6. Relative contribution of the molecular (blue), ionized (green), and neutral atomic (red) phases to the total kinetic power of the outflow. The galaxies whose names are in red are star-forming galaxies. Next we investigate the mass outflow rate of the three different phases, ionized, neutral atomic, and molecular for galaxies which have measurements (or upper limits) for at least two phases. This comparison can be seen in Fig. 7 , where we plot the different mass outflow rates against each other. The samples in the three plots are slightly different. To increase the statistics, in each plot we show the galaxies with measurements in both of the phases plotted. We distinguish between high-redshift sources ( z > 1, green) and low-redshift sources ( z 0.2, black). The data points with a red edge have no reliable extinction correction for the ionized phase and thus should be treated as lower limits. These figures clearly show that the ionized mass outflow rate is much smaller (up to 2–3 orders of magnitude smaller) than the neutral atomic or molecular mass outflow rate. A major caveat is that some ionized outflow rates might be underestimated because of an uncertain extinction correction. But even if these points are ignored, the ionized outflow rates are significantly lower (cf. Fig. 5 , which only includes galaxies with proper extinction correction). This confirms previous findings which estimate the ionized phase to contribute only minimally (Rupke Veilleux 2013 ; Carniani et al. 2015 ; Ramos Almeida et al. 2019 ). The figure on the top right highlights that outflow rates in the molecular and neutral atomic phase are similar (usually within 1 dex). This picture might be slightly skewed, however, as we include upper limits in the molecular and ionized, but not in the atomic neutral outflow phase. However, the relative contribution of the ionized outflow rate to the total outflow rate varies from galaxy to galaxy (from ≤ 1 to 10’s of ) and a simple prescription as in Fluetsch et al. ( 2019 ) might not be fully appropriate to determine the total outflow budget. If electron densities from auroral or trans-auroral lines are a better estimate than the densities based on the [S ii ] doublet (as suggested by Davies et al. 2020 , see Section 3.2.1 ), then the contribution of the ionized phase would drop even further by additional 1–2 orders of magnitude and hence it would become negligible also in star-forming galaxies. Figure 7. Comparison between the outflow rates in the ionized, molecular, and neutral gas phases. The black symbols represent the low-redshift ( z 0.2) sources while the green symbols
ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O O O O O B-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula O O O O O