The SAMI Galaxy Survey: Spatially resolving the main sequence of star formation

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Creator
  • Medling, A.M.
    • Other Affiliation: California Institute of Technology
  • Cortese, L.
    • Other Affiliation: University of Western Australia
  • Croom, S.M.
    • Other Affiliation: University of Sydney
  • Green, A.W.
    • Other Affiliation: Australian Astronomical Observatory
  • Groves, B.
    • Other Affiliation: Australian National University
  • Hampton, E.
    • Other Affiliation: Australian National University
  • Ho, I.-T.
    • Other Affiliation: Max-Planck-Institut für Astronomie
  • Davies, L.J.M.
    • Other Affiliation: University of Western Australia
  • Kewley, L.J.
    • Other Affiliation: Australian National University
  • Moffett, A.J.
    • Other Affiliation: Vanderbilt University
  • Schaefer, A.L.
    • Other Affiliation: University of Sydney
  • Taylor, E.
    • Other Affiliation: Swinburne University of Technology
  • Zafar, T.
    • Other Affiliation: Australian Astronomical Observatory
  • Bekki, K.
    • Other Affiliation: University of Western Australia
  • Bland-Hawthorn, J.
    • Other Affiliation: University of Sydney
  • Bloom, J.V.
    • Other Affiliation: University of Sydney
  • Brough, S.
    • Other Affiliation: University of New South Wales
  • Bryant, J.J.
    • Other Affiliation: Australian Astronomical Observatory
  • Catinella, B.
    • Other Affiliation: University of Western Australia
  • Cecil, G.
    • Affiliation: College of Arts and Sciences, Department of Physics and Astronomy
  • Colless, M.
    • Other Affiliation: Australian National University
  • Couch, W.J.
    • Other Affiliation: Australian Astronomical Observatory
  • Drinkwater, M.J.
    • Other Affiliation: University of Queensland
  • Driver, S.P.
    • Other Affiliation: University of Western Australia
  • Federrath, C.
    • Other Affiliation: Australian National University
  • Foster, C.
    • Other Affiliation: Australian Astronomical Observatory
  • Goldstein, G.
    • Other Affiliation: Macquarie University
  • Goodwin, M.
    • Other Affiliation: Australian Astronomical Observatory
  • Hopkins, A.
    • Other Affiliation: Australian Astronomical Observatory
  • Lawrence, J.S.
    • Other Affiliation: Australian Astronomical Observatory
  • Leslie, S.K.
    • Other Affiliation: Max-Planck-Institut für Astronomie
  • Lewis, G.F.
    • Other Affiliation: University of Sydney
  • Lorente, N.P.F.
    • Other Affiliation: Australian Astronomical Observatory
  • Owers, M.S.,
    • Other Affiliation: Australian Astronomical Observatory
  • McDermid, R.
    • Other Affiliation: Australian Astronomical Observatory
  • Richards, S.N.
    • Other Affiliation: NASA Armstrong Flight Research Center
  • Sharp, R.
    • Other Affiliation: Australian National University
  • Scott, N.
    • Other Affiliation: University of Sydney
  • Sweet, S.M.
    • Other Affiliation: Swinburne University of Technology
  • Taranu, D.S.
    • Other Affiliation: University of Western Australia
  • Tescari, E.
    • Other Affiliation: University of Melbourne
  • Tonini, C.
    • Other Affiliation: University of Melbourne
  • van de Sande, J.
    • Other Affiliation: University of Sydney
  • Walcher, C.J.
    • Other Affiliation: Leibniz-Institut für Astrophysik Potsdam
  • Wright, A.
    • Other Affiliation: Universität Bonn
Abstract
  • 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 central stellar mass surface densities. The main-sequence population has centrally concentrated star formation similar to late-type galaxies, while galaxies > 3σ 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.
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DOI
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Resource type
  • Article
Rights statement
  • In Copyright
Journal title
  • Monthly Notices of the Royal Astronomical Society
Journal volume
  • 475
Journal issue
  • 4
Page start
  • 5194
Page end
  • 5214
Language
  • English
Version
  • Publisher
ISSN
  • 0035-8711
Publisher
  • Oxford University Press

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