AlFoCS + Fornax3D: resolved star formation in the Fornax cluster with
  ALMA and MUSE
  We combine data from ALMA and MUSE to study the resolved (~300 pc scale) star
formation relation (star formation rate vs. molecular gas surface density) in
cluster galaxies. Our sample consists of 9 Fornax cluster galaxies, including
spirals, ellipticals, and dwarfs, covering a stellar mass range of ~10^8.8 -
10^11 M_Sun. CO(1-0) and extinction corrected Halpha were used as tracers for
the molecular gas mass and star formation rate, respectively. We compare our
results with Kennicutt (1998) and Bigiel et al. (2008). Furthermore, we create
depletion time maps to reveal small-scale variations in individual galaxies. We
explore these further in FCC290, using the 'uncertainty principle for star
formation' (Kruijssen & Longmore, 2014a) to estimate molecular cloud lifetimes,
which we find to be short (<10 Myr) in this galaxy. Galaxy-averaged depletion
times are compared with other parameters such as stellar mass and
cluster-centric distance. We find that the star formation relation in the
Fornax cluster is close to those from Kennicutt (1998) and Bigiel et al.
(2008}), but overlaps mostly with the shortest depletion times predicted by
Bigiel et al. (2008). This slight decrease in depletion time is mostly driven
by dwarf galaxies with disturbed molecular gas reservoirs close to the virial
radius. In FCC90, a dwarf galaxy with a molecular gas tail, we find that
depletion times are a factor >~10 higher in its tail than in its stellar body.
