Halo Masses of MgII absorbers at z ~ 0.5 from SDSS DR7

We present the cross-correlation function of MgII absorbers with respect to a volume-limited sample of luminous red galaxies (LRGs) at z = 0.45 - 0.60 using the largest MgII absorber sample and a new LRG sample from SDSS DR7. We present the clustering signal of absorbers on projected scales r_p = 0.3 - 35 h^(-1) Mpc in four W^(λ2796)_r bins spanning W^(λ2796)_r = 0.4 - 5.6Å. We found that on average Mg II absorbers reside in halos (log M_h) ≈ 12.1, similar to the halo mass of an L_* galaxy. We report that the weakest absorbers in our sample with W^(λ2796)_r = 0.4-1.1Å reside in relatively massive halos with (log M_h) ≈ 12.5^(+0.6)_(-1.3), while stronger absorbers reside in halos of similar or lower masses (log M_h) 11.6^(+0.9). We compared our bias data points, b, and the frequency distribution function of absorbers, f_W_r, with a simple model incorporating an isothermal density profile to mimic the distribution of absorbing gas in halos. We also compared the bias data points with Tinker & Chen (2008) who developed halo occupation distribution models of Mg II absorbers that are constrained by b and f_W_r. The simple isothermal model can be ruled at a ≈ 2.8σ level mostly because of its inability to reproduce f_W_r. However, b values are consistent with both models, including TC08. In addition, we show that the mean b of absorbers does not decrease beyond W^(λ2796)_r ≈ 1.6Å. The flat or potential upturn of b for W^(λ2796)-r ≳ 1.6Å absorbers suggests the presence of additional cool gas in massive halos