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Title:
The SAMI Galaxy Survey: spatially resolving the main sequence of star formation
Authors:
Medling, Anne M.; Cortese, Luca; Croom, Scott M.; Green, Andrew W.; Groves, Brent; Hampton, Elise; Ho, I.-Ting; Davies, Luke J. M.; Kewley, Lisa J.; Moffett, Amanda J.; Schaefer, Adam L.; Taylor, Edward; Zafar, Tayyaba; Bekki, Kenji; Bland-Hawthorn, Joss; Bloom, Jessica V.; Brough, Sarah; Bryant, Julia J.; Catinella, Barbara; Cecil, Gerald; Colless, Matthew; Couch, Warrick J.; Drinkwater, Michael J.; Driver, Simon P.; Federrath, Christoph; Foster, Caroline; Goldstein, Gregory; Goodwin, Michael; Hopkins, Andrew; Lawrence, J. S.; Leslie, Sarah K.; Lewis, Geraint F.; Lorente, Nuria P. F.; Owers, Matt S.; McDermid, Richard; Richards, Samuel N.; Sharp, Robert; Scott, Nicholas; Sweet, Sarah M.; Taranu, Dan S.; Tescari, Edoardo; Tonini, Chiara; van de Sande, Jesse; Walcher, C. Jakob; Wright, Angus
Affiliation:
AA(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, MS 249-17, Pasadena, CA 91125, USA; Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia; 0000-0001-7421-2944), AB(International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia 0000-0002-7422-9823), AC(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia; ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 0000-0003-2880-9197), AD(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia 0000-0003-3052-0819), AE(Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia), AF(Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia), AG(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany), AH(International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia), AI(Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia), AJ(Department of Physics & Astronomy, Vanderbilt University, 2401 Vanderbilt Place, Nashville, TN 37240, USA), AK(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AL(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia), AM(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia 0000-0003-3935-7018), AN(International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia), AO(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AP(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), AQ(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia; ARC Centre of Excellence for All-sky Astrophysics (CAASTRO); School of Physics, University of New South Wales, NSW 2052, Australia 0000-0002-9796-1363), AR(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia; ARC Centre of Excellence for All-sky Astrophysics (CAASTRO); Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), AS(International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia), AT(Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599, USA), AU(Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia 0000-0001-9552-8075), AV(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), AW(ARC Centre of Excellence for All-sky Astrophysics (CAASTRO); School of Mathematics and Physics, University of Queensland, QLD 4072, Australia 0000-0003-4867-0022), AX(International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia), AY(Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia), AZ(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia 0000-0003-0247-1204), BA(Department of Physics and Astronomy, Macquarie University, NSW 2109, Australia), BB(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), BC(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), BD(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), BE(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany 0000-0002-4826-8642), BF(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), BG(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia), BH(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia; Department of Physics and Astronomy, Macquarie University, NSW 2109, Australia), BI(Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia; Department of Physics and Astronomy, Macquarie University, NSW 2109, Australia), BJ(SOFIA Operations Center, USRA, NASA Armstrong Flight Research Center, 2825 East Avenue P, Palmdale, CA 93550, USA 0000-0002-5368-0068), BK(Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia), BL(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia 0000-0001-8495-8547), BM(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia 0000-0002-1576-2505), BN(International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, Australia; ARC Centre of Excellence for All-sky Astrophysics (CAASTRO)), BO(ARC Centre of Excellence for All-sky Astrophysics (CAASTRO); School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia), BP(School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia), BQ(Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia), BR(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), BS(Argelander-Institut für Astronomie (AIfA), Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 475, Issue 4, p.5194-5214 (MNRAS Homepage)
Publication Date:
04/2018
Origin:
OUP
Astronomy Keywords:
surveys, galaxies: evolution, galaxies: star formation
Abstract Copyright:
2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/sty127
Bibliographic Code:
2018MNRAS.475.5194M

Abstract

We present the ˜800 star formation rate maps for the Sydney-AAO Multi-object Integral field spectrograph (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 >3sigma 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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