The CGM${}^2$ Survey: Circumgalactic O VI from dwarf to massive star-forming galaxies

Abstract

We combine 126 new galaxy-O VI absorber pairs from the CGM${}^2$ survey with 123 pairs drawn from the literature to examine the simultaneous dependence of the column density of O VI absorbers ($N_{\mathrm{OVI}}$) on galaxy stellar mass, star formation rate, and impact parameter. The combined sample consists of 249 galaxy-O VI absorber pairs covering $z=0$-$0.6$, with host galaxy stellar masses $M^{\ast }=10^{7.8}$-$10^{11.2}$ $M_{\odot }$ and galaxy-absorber impact parameters $R_{\perp }=0$-$400$ proper kiloparsecs. In this work, we focus on the variation of $N_{\mathrm{OVI}}$ with galaxy mass and impact parameter among the star-forming galaxies in the sample. We find that the average $N_{\mathrm{OVI}}$ within one virial radius of a star-forming galaxy is greatest for star-forming galaxies with $M^{\ast }=10^{9.2}$-$10^{10}$ $M_{\odot }$. Star-forming galaxies with $M^{\ast }$ between $10^8$ and $10^{11.2}$ $M_{\odot }$ can explain most O VI systems with column densities greater than 10${}^{13.5}$ cm${}^{-2}$. 60% of the O VI mass associated with a star-forming galaxy is found within one virial radius and 35% is found between one and two virial radii. In general, we find that some departure from hydrostatic equilibrium in the CGM is necessary to reproduce the observed O VI amount, galaxy mass dependence, and extent. Our measurements serve as a test set for CGM models over a broad range of host galaxy masses.

25 pages, 9 figures. Accepted to ApJ

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• Introducing the Descriptive Parametric Model: Gaseous Profiles for Galaxies, Groups, and Clusters
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