The SAMI Galaxy Survey: Spatially Resolving the Main Sequence of Star
  Formation
  We present the ~800 star formation rate maps for the SAMI Galaxy Survey based
on H{\alpha} emission maps, corrected for dust attenuation via the Balmer
decrement, that are included in the SAMI Public Data Release 1. We mask out
spaxels contaminated by non-stellar emission using the [O III]/H{\beta}, [N
II]/H{\alpha}, [S II]/H{\alpha}, and [O I]/H{\alpha} line ratios. Using these
maps, we examine the global and resolved star-forming main sequences of SAMI
galaxies as a function of morphology, environmental density, and stellar mass.
Galaxies further below the star-forming main sequence are more likely to have
flatter star formation profiles. Early-type galaxies split into two populations
with similar stellar masses and central stellar mass surface densities. The
main sequence population has centrally-concentrated star formation similar to
late-type galaxies, while galaxies >3{\sigma} below the main sequence show
significantly reduced star formation most strikingly in the nuclear regions.
The split populations support a two-step quenching mechanism, wherein halo mass
first cuts off the gas supply and remaining gas continues to form stars until
the local stellar mass surface density can stabilize the reduced remaining fuel
against further star formation. Across all morphologies, galaxies in denser
environments show a decreased specific star formation rate from the outside in,
supporting an environmental cause for quenching, such as ram-pressure stripping
or galaxy interactions.
