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Dwarf galaxies are missing nearly all of their baryons and metals from thestellar disk, presumed to be in a bound halo or expelled beyond the virialradius. The virial temperature for galaxies with $M_{\rm h} \sim 10^9 -10^{10}$ $M_{\odot}$ is similar to the collisional ionization equilibriumtemperature for the C IV ion. We searched for UV absorption from C IV in sixsightlines toward three dwarf galaxies in the anti-M31 direction and at theperiphery of the Local Group ($D \approx$ 1.3 Mpc; Sextans A, Sextans B, andNGC 3109). The C IV doublet is detected in only one of six sightlines, towardSextans A, with $\log N({\rm C IV})$ = $13.06 \pm 0.08$. This is consistentwith our gaseous halo models, where the halo gas mass is determined by thecooling rate, feedback, and the star formation rate; the inclusion ofphotoionization is an essential ingredient. This model can also reproduce thehigher detection rate of O VI absorption in other dwarf samples (beyond theLocal Group), and with C IV only detectable within $\sim 0.5R_{\rm vir}$.

Absorption Line Search Through Three Local Group Dwarf Galaxy Halos