[O II] nebular emission from Mg II absorbers: Star formation associated with the absorbing gas

Abstract

We present nebular emission associated with 198 strong Mg II absorbers at 0.35 $\le z\le$ 1.1 in the fibre spectra of quasars from the Sloan Digital Sky Survey. Measured [O II] luminosities (L${}_{[OII]}$) are typical of sub-L${}^{\star }$ galaxies with derived star formation rate (uncorrected for fibre losses and dust reddening) in the range of 0.5-20 ${\mathrm{M}}_{\odot }\mathrm{y}{\mathrm{r}}^{-1}$. Typically less than $\sim$ 3% of the Mg II systems with rest equivalent width, $W_{2796}$ $\ge$ 2 Ã , show L${}_{[OII]}\ge 0.3$ L${}_{[OII]}^{\star }$. The detection rate is found to increase with increasing $W_{2796}$ and $z$. No significant correlation is found between $W_{2796}$ and L${}_{[OII]}$ even when we restrict the samples to narrow $z$-ranges. A strong correlation is seen between L${}_{[OII]}$ and $z$. While this is expected from the luminosity evolution of galaxies, we show finite fibre size plays a very crucial role in this correlation. The measured nebular line ratios (like [O III]/[O II] and [O III]/H${\hat{I}}^2$) and their $z$ evolution are consistent with those of galaxies detected in deep surveys. Based on the median stacked spectra, we infer the average metallicity (log Z $\sim$8.3), ionization parameter (log $q$ $\sim$7.5) and stellar mass (log (M/M${}_{\odot }$)$\sim$9.3). The Mg II systems with nebular emission typically have $W_{2796}$ $\ge 2$ Ã , Mg II doublet ratio close to 1 and W(Fe II$\hat{I}»$2600)/$W_{2796}$ $\sim 0.5$ as often seen in damped Ly$\hat{I}\pm$ and 21-cm absorbers at these redshifts. This is the biggest reported sample of [O II] emission from Mg II absorbers at low impact parameters ideally suited for probing various feedback processes at play in $z\le 1$ galaxies.

18 Pages, 18 Figures, 4 Tables (Accepted for the Publication in MNRAS main-journal)