tokens: for both efficient and inefficient conduction appear to follow the general shape of the data. High velocities also correspond to high q values, reflecting the effects of shocks on both the cloudlets within a cooling run and the filaments in the conduction runs to compress the gas. 5. Application: Down-the-barrel Outflow Observations As an illustration of the types of studies enabled by our results, we consider an application of our tabulated fits. We consider the observations in Chisholm et al. ( 2018 ) in particular as many of our assumptions, including radiation background and ionization parameter, are derived from these observations. Chisholm et al. ( 2018 ) report absorption profiles from down-the-barrel observations, of a lensed galaxy with z ≈ 2.9. Observations are made of both low and high ionization profiles that indicate that the two phases are cospatial, much like the wind-cloud interaction considered here. We aim to determine an appropriate scaling of our column density profiles by accounting for two factors that can influence the optical depth of the absorbing clouds. To approximate an absorption profile for these ions, we estimate the observed optical depth for a particular ion aswhere is the average number density of the ion, where x is the number of points within the column density profile and N i is the column density for the i th point. Here τ is approximated with the center of the absorption profile at the average velocity of the cloud, v 0 , with a velocity dispersion determined by the b parameter estimated for each ion, and v is the velocity bin within the absorption profile. We consider velocities between −600 and 200 km s −1 offset from line center. This average optical depth approximates a single cloud. There are then two ways to parameterize the absorption profile, we consider the two parameters independently. The first method is altering covering fraction, which describes the fraction of the area within the sightline that is obscured by the cloud. With this covering fraction parameter, the observed flux from the derived column density profiles can be expressed aswhere τ ( v ) is the average optical depth above and f is the free parameter describing the covering fraction. The second way to parameterize the absorption profile considers scaling the optical depth either to represent multiple clouds along the sightline or one cloud with scaled density. For this, we assume that the intervening cloud has the average optical depth of a single cloud from Equation ( 16 ), which is then scaled by the parameter α , which describes the number of clouds within the sightline or the scaling factor of the density for a single cloud. In this case, the observed flux can be described aswhere τ ( v ) is again the average optical depth above and α is the second free parameter we consider, describing the number of clouds. Best-fit covering fraction and α are found by performing χ 2 minimizations for each of the parameters independently
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