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We report results from a survey of MgII absorbers in the spectra ofbackground QSOs that are within close angular distances to a foreground galaxyat z<0.5, using the Magellan Echellette Spectrograph. We have established aspectroscopic sample of 94 galaxies at a median redshift of <z> = 0.24 infields around 70 distant background QSOs (z_QSO>0.6), 71 of which are in an'isolated' environment with no known companions and located at rho <~ 120 h^-1kpc from the line of sight of a background QSO. The rest-frame absolute B-bandmagnitudes span a range from M_B-5log h=-16.4 to M_B-5log h=-21.4 andrest-frame B_AB-R_AB colors range from B_AB-R_AB~0 to B_AB-R_AB~1.5. Of these'isolated' galaxies, we find that 47 have corresponding MgII absorbers in thespectra of background QSOs and rest-frame absorption equivalent widthW_r(2796)=0.1-2.34 A, and 24 do not give rise to MgII absorption to sensitiveupper limits. Our analysis shows that (1) Wr(2796) declines with increasingdistance from 'isolated' galaxies but shows no clear trend in 'group'environments; (2) more luminous galaxies possess more extended MgII absorbinghalos with the gaseous radius scaled by B-band luminosity according toR_gas=75x(L_B/L_B*)^(0.35+/-0.03) h^{-1} kpc; (3) there is little dependencebetween the observed absorber strength and galaxy intrinsic colors; and (4)within R_gas, we find a mean covering fraction of <kappa_0.3>~70% for absorbersof Wr(2796)>=0.3 A and <kappa_0.1>~80% for absorbers of Wr(2796)>=0.1 A. Thelack of correlation between Wr(2796) and galaxy colors suggests a lack ofphysical connection between the origin of extended MgII halos and recent starformation history of the galaxies. Finally, we discuss the total gas mass ingalactic halos as traced by MgII absorbers. We also compare our results withprevious studies.

An Empirical Characterization of Extended Cool Gas Around Galaxies Using MgII Absorption Features