Abstract

We report results from a survey of Mg ii absorbers in the spectra of background quasi-stellar objects (QSOs) that are within close angular distances to a foreground galaxy at z 0.6), 71 of which are in an "isolated" environment with no known companions and located at ρ ≲ 120 h−1 kpc from the line of sight of a background QSO. The rest-frame absolute B-band magnitudes span a range from MB − 5log h = −16.4 to MB − 5log h = −21.4 and rest-frame BAB − RAB colors range from BAB − RAB ≈ 0 to BAB − RAB ≈ 1.5. Of these "isolated" galaxies, we find that 47 have corresponding Mg ii absorbers in the spectra of background QSOs and rest-frame absorption equivalent width Wr(2796) = 0.1–2.34 Å, and 24 do not give rise to Mg ii absorption to sensitive upper limits. Our analysis shows that (1) Wr(2796) declines with increasing distance from "isolated" galaxies but shows no clear trend in "group" environments; (2) more luminous galaxies possess more extended Mg ii absorbing halos with the gaseous radius scaled by B-band luminosity according to Rgas = 75 × (LB/LB*)(0.35 ± 0.03) h−1 kpc; (3) there is little dependence between the observed absorber strength and galaxy intrinsic colors; and (4) within Rgas, we find a mean covering fraction of 〈κ0.3〉 ≈ 70% for absorbers of Wr(2796) ⩾ 0.3 Å and 〈κ0.1〉 ≈ 80% for absorbers of Wr(2796) ⩾ 0.1 Å. The results confirm that extended Mg ii absorbing halos are a common and generic feature around ordinary galaxies and that the gaseous radius is a fixed fraction of the dark matter halo radius. The lack of correlation between Wr(2796) strength and galaxy colors suggests a lack of physical connection between the origin of extended Mg ii halos and recent star formation history of the galaxies. Finally, we discuss the total gas mass in galactic halos as traced by Mg ii absorbers. We also compare our results with previous studies.