The properties of the cool circumgalactic gas probed with the SDSS, WISE and GALEX surveys

TL;DR

This study investigates the distribution and properties of cool gas around galaxies using multi-wavelength surveys, revealing differences in gas behavior between star-forming and passive galaxies and linking gas properties to galaxy characteristics.

Contribution

It provides new insights into the CGM by cross-correlating large survey data to analyze MgII absorber distributions and their dependence on galaxy type, SFR, and orientation.

Findings

Cool gas exists around both galaxy types at large scales.

Stronger MgII absorbers are associated with star-forming galaxies.

MgII absorption is enhanced along the minor axis of star-forming galaxies.

Abstract

We explore the distribution of cool (~$10^4$K) gas around galaxies and its dependence on galaxy properties. By cross-correlating about 50,000 MgII absorbers with millions of sources from the SDSS (optical), WISE (IR), and GALEX (UV) surveys we effectively extract about 2,000 galaxy-absorber pairs at z~0.5 and probe relations between absorption strength and galaxy type, impact parameter and azimuthal angle. We find that cool gas traced by MgII absorbers exists around both star-forming and passive galaxies with a similar incidence rate on scales greater than 100 kpc but each galaxy type exhibits a different behavior on smaller scales: MgII equivalent width does not correlate with the presence of passive galaxies whereas stronger MgII absorbers tend to be found in the vicinity of star-forming galaxies. This effect is preferentially seen along the minor axis of these galaxies, suggesting that some of the gas is associated with outflowing material. In contrast, the distribution of cool gas around passive galaxies is consistent with being isotropic on the same scales. We quantify the average excess MgII equivalent width $<\delta W_{0}^{\rm MgII}>$ as a function of galaxy properties and find $<\delta W_0^{\rm MgII}>\propto SFR^{1.2}, sSFR^{0.5}$ and $M_\ast^{0.4}$ for star-forming galaxies. This work demonstrates that the dichotomy between star-forming and passive galaxies is reflected in the CGM traced by low-ionized gas. We also measure the covering fraction of MgII absorption and find it to be about 2-10 times higher for star-forming galaxies than passive ones within 50 kpc. We estimate the amount of neutral gas in the halo of $<\log M_\ast/{\rm M_\odot}>$~10.8 galaxies to be a few x$10^9 \rm M_\odot$ for both types of galaxies. Finally, we find that correlations between absorbers and sources detected in the UV and IR lead to physical trends consistent with those measured in the optical.