SEEDisCS II. Molecular gas in galaxy clusters and their large scale
  structure: low gas fraction galaxies, the case of CL1301.7$-$1139
  This paper is the second of a series that tackles the properties of molecular
gas in galaxies residing in clusters and their related large-scale structures.
Out of 21 targeted fields, 19 galaxies were detected in CO(3-2) with the
Atacama Large Millimeter Array (ALMA), including two detections within a single
field. These galaxies are either bona fide members of the CL1301.7$-$1139
cluster ($z=0.4828$, $\sigma_{cl}=681$ km s$^{-1}$), or located within $\sim 7
\times R_{200}$, its virial radius. They have been selected to sample the range
of photometric local densities around CL1301.7$-$1139, with stellar masses
above log($M_{\rm star}$) = 10, and to be located in the blue clump of
star-forming galaxies derived from the $u$, $g$, and $i$ photometric bands.
Unlike previous works, our sample selection does not impose a minimum star
formation rate or detection in the far-infrared. As such and as much as
possible, it delivers an unbiased view of the gas content of normal
star-forming galaxies at $z \sim 0.5$. Our study highlights the variety of
paths to star formation quenching, and most likely the variety of physical
properties (i.e. temperature, density) of the corresponding galaxy's cold
molecular gas. Just as in the case of CL1411.1$-$1148, although to a smaller
extent, we identify a number of galaxies with lower gas fraction than
classically found in other surveys. These galaxies can still be on the
star-forming main sequence. When these galaxies are not inside the cluster
virialised region, we provide hints that they are linked to their infall
regions within $\sim 4 \times R_{200}$.
