The COS-Dwarfs Survey: The Carbon Reservoir Around sub-L* Galaxies

TL;DR

This study investigates the gaseous halos around low-mass galaxies, revealing a significant carbon reservoir in the circumgalactic medium that correlates with star formation and supports energy-driven wind models.

Contribution

It provides new observational evidence of carbon distribution in the CGM of sub-L* galaxies and compares these findings with hydrodynamical simulations to test galaxy wind models.

Findings

C IV absorption detected out to ~0.5 R_vir

A large carbon reservoir in the CGM, > 1.2×10^6 M_⊙

Energy-driven wind models fit the observations better

Abstract

We report new observations of circumgalactic gas from the COS-Dwarfs survey, a systematic investigation of the gaseous halos around 43 low-mass z $\leq$ 0.1 galaxies using background QSOs observed with the Cosmic Origins Spectrograph. From the projected 1D and 2D distribution of C IV absorption, we find that C IV absorption is detected out to ~ 0.5 R$_{vir}$ of the host galaxies. The C IV absorption strength falls off radially as a power law and beyond 0.5 R$_{vir}$, no C IV absorption is detected above our sensitivity limit of ~ 50-100 m$\AA$. We find a tentative correlation between detected C IV absorption strength and star formation, paralleling the strong correlation seen in highly ionized oxygen for L~L* galaxies by the COS-Halos survey. The data imply a large carbon reservoir in the CGM of these galaxies, corresponding to a minimum carbon mass of $\gtrsim$ 1.2$\times 10^6$ $M_\odot$ out to ~ 110 kpc. This mass is comparable to the carbon mass in the ISM and more than the carbon mass currently in stars of these galaxies. The C IV absorption seen around these sub-L* galaxies can account for almost two-thirds of all $W_r$> 100 m$\AA$ C IV absorption detected at low z. Comparing the C IV covering fraction with hydrodynamical simulations, we find that an energy-driven wind model is consistent with the observations whereas a wind model of constant velocity fails to reproduce the CGM or the galaxy properties.