The ESO UVES Advanced Data Products Quasar Sample-V. Identifying the
  Galaxy Counterpart to the sub-Damped Ly-alpha System towards Q2239-2949
  Gas flows in and out of galaxies are one of the key unknowns in todays'
galaxy evolution studies. Because gas flows carry mass, energy and metals, they
are believed to be closely connected to the star formation history of galaxies.
Most of these processes take place in the circum-galactic medium (CGM) which
remains challenging to observe in emission. A powerful tool to study the CGM
gas is offered by combining observations of the gas traced by absorption lines
in quasar spectra with detection of the stellar component of the same
absorbing-galaxy. To this end, we have targeted the zabs=1.825 sub-Damped
Ly-alpha absorber (sub-DLA) towards the zem=2.102 quasar 2dF J 223941.8-294955
(hereafter Q2239-2949) with the ESO VLT/X-Shooter spectrograph. Our aim is to
investigate the relation between its properties in emission and in absorption.
The derived metallicity of the sub-DLA with log N(HI) = 19.84+/-0.14 cm-2 is
[M/H] >-0.75. Using the Voigt profile optical depth method, we measure
Delta_v90(FeII)=64 kms-1. The sub-DLA galaxy counterpart is located at an
impact parameter of 2."4+/-0."2 (20.8+/-1.7 kpc at z = 1.825). We have detected
Ly-alpha and marginal [OII] emissions. The mean measured flux of the Ly-alpha
line is F(Ly-alpha) ~ 5.7x10^-18 erg s-1 cm-2 A-1, corresponding to a dust
uncorrected SFR of ~ 0.13 M(solar) yr-1.
