  The physical processes by which gas is accreted onto galaxies, transformed
into stars and then expelled from galaxies are of paramount importance to
galaxy evolution studies. Observationally constraining each of these baryonic
components in the same systems however, is challenging. Furthermore,
simulations indicate that the stellar mass of galaxies is a key factor
influencing CGM properties. Indeed, absorption lines detected against
background quasars offer the most compelling way to study the cold gas in the
circumgalactic medium (CGM). The MUSE-ALMA Haloes survey is composed of quasar
fields covered with VLT/MUSE observations, comprising 32 \ion{H}{i} absorbers
at 0.2 $<$ $z$ $<$ 1.4 and 79 associated galaxies, with available or upcoming
molecular gas measurements from ALMA. We use a dedicated 40-orbit HST UVIS and
IR WFC3 broad-band imaging campaign to characterise the stellar content of
these galaxies. By fitting their spectral energy distribution, we establish
they probe a wide range of stellar masses: 8.1 $<$ log($M_*$/M$_{\odot}$) $<$
12.4. Given their star-formation rates, most of these objects lie on the main
sequence of galaxies. We also confirm a previously reported anti-correlation
between the stellar masses and CGM hydrogen column density N(\ion{H}{i}),
indicating an evolutionary trend where higher mass galaxies are less likely to
host large amounts of \ion{H}{i} gas in their immediate vicinity up to 120 kpc.
Together with other studies from the MUSE-ALMA Haloes survey, these data
provide stellar masses of absorber hosts, a key component of galaxy formation
and evolution, and observational constraints on the relation between galaxies
and their surrounding medium.
