A Lyman limit system associated with galactic winds
  Projected quasar galaxy pairs provide powerful means to study the
circumgalactic medium (CGM) that maintains the relics of galactic feedback and
the accreted gas from the intergalactic medium. Here, we study the nature of a
Lyman Limit system (LLS) with N(HI)=10$^{19.1\pm0.3}$ cm$^{-2}$ and a
dust-uncorrected metallicity of [Fe/H]$=-1.1\pm0.3$ at $z=0.78$ towards
Q0152$-020$. The MgII absorption profiles are composed of a main saturated and
a few weaker optically thin components. Using MUSE observations we detect one
galaxy close to the absorption redshift at an impact parameter of 54 kpc. This
galaxy exhibits nebular emission lines from which we measure a dust-corrected
star formation rate of $10^{+8}_{-5}$ M$_\odot$ yr$^{-1}$ and an emission
metallicity of [O/H]$=-0.1\pm0.2$. By combining the absorption line kinematics
with the host galaxy morphokinematics we find that while the main absorption
component can originate from a galactic wind at $V_{\rm w}=110\pm4$ km s$^{-1}$
the weaker components cannot. We estimate a mass ejection rate of $\dot
M\gtrsim0.8$ M$_\odot$ yr$^{-1}$ that translates to a loading factor of
$\eta\gtrsim0.1$. Since the local escape velocity of the halo, $V_{\rm
esc}\simeq430$ km s$^{-1}$, is a few times larger than $V_{\rm w}$, we expect
this gas will remain bound to the host galaxy. These observations provide
additional constraints on the physical properties of winds predicted by galaxy
formation models. We also present the VLT/X-Shooter data analysis of 4 other
absorbing systems at $1.1<z<1.5$ in this sightline with their host galaxies
identified in the MUSE data.
