The SAMI Galaxy Survey: Spatially resolving the main sequence of star formation
- Medling, A.M.
- Cortese, L.
- Croom, S.M.
- Green, A.W.
- Groves, B.
- Hampton, E.
- Ho, I.-T.
- Davies, L.J.M.
- Kewley, L.J.
- Moffett, A.J.
- Schaefer, A.L.
- Taylor, E.
- Zafar, T.
- Bekki, K.
- Bland-Hawthorn, J.
- Bloom, J.V.
- Brough, S.
- Bryant, J.J.
- Catinella, B.
- Cecil, G.
- Colless, M.
- Couch, W.J.
- Drinkwater, M.J.
- Driver, S.P.
- Federrath, C.
- Foster, C.
- Goldstein, G.
- Goodwin, M.
- Hopkins, A.
- Lawrence, J.S.
- Leslie, S.K.
- Lewis, G.F.
- Lorente, N.P.F.
- Owers, M.S.,
- McDermid, R.
- Richards, S.N.
- Sharp, R.
- Scott, N.
- Sweet, S.M.
- Taranu, D.S.
- Tescari, E.
- Tonini, C.
- van de Sande, J.
- Walcher, C.J.
- Wright, A.
DOIAbstract
We present the ~800 star formation rate maps for the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey based on Ha 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 β, [NII]/H α, [S II]/H α, and [O I]/H α line ratios. Using thesemaps, we examine the global and resolved starforming 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 c...
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