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

Anne M. Medling, Luca Cortese, Scott M. Croom, Andrew W. Green, Brent Groves, Elise Hampton, I. Ting Ho, Luke J.M. Davies, Lisa J. Kewley, Amanda J. Moffett, Adam L. Schaefer, Edward Taylor, Tayyaba Zafar, Kenji Bekki, Joss Bland-Hawthorn, Jessica V. Bloom, Sarah Brough, Julia J. Bryant, Barbara Catinella, Gerald Cecil & 25 others Matthew Colless, Warrick J. Couch, Michael J. Drinkwater, Simon P. Driver, Christoph Federrath, Caroline Foster, Gregory Goldstein, Michael Goodwin, Andrew Hopkins, J. S. Lawrence, Sarah K. Leslie, Geraint F. Lewis, Nuria P.F. Lorente, Matt S. Owers, Richard McDermid, Samuel N. Richards, Robert Sharp, Nicholas Scott, Sarah M. Sweet, Dan S. Taranu, Edoardo Tescari, Chiara Tonini, Jesse van de Sande, C. Jakob Walcher, Angus Wright

Research output: Contribution to journalArticle

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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.

Original languageEnglish
Pages (from-to)5194-5214
Number of pages21
JournalMonthly Notices of the Royal Astronomical Society
Volume475
Issue number4
DOIs
Publication statusPublished - 1 Apr 2018

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spectrographs
star formation
galaxies
stellar mass
star formation rate
gas supply
quenching
H lines
stars
interacting galaxies
ram
stripping
gases
dust
halos
masks
cut-off
attenuation
gas
causes

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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. / The SAMI Galaxy Survey : Spatially resolving the main sequence of star formation. In: Monthly Notices of the Royal Astronomical Society. 2018 ; Vol. 475, No. 4. pp. 5194-5214.
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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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author = "Medling, {Anne M.} and Luca Cortese and Croom, {Scott M.} and Green, {Andrew W.} and Brent Groves and Elise Hampton and Ho, {I. Ting} and Davies, {Luke J.M.} and Kewley, {Lisa J.} and Moffett, {Amanda J.} and Schaefer, {Adam L.} and Edward Taylor and Tayyaba Zafar and Kenji Bekki and Joss Bland-Hawthorn and Bloom, {Jessica V.} and Sarah Brough and Bryant, {Julia J.} and Barbara Catinella and Gerald Cecil and Matthew Colless and Couch, {Warrick J.} and Drinkwater, {Michael J.} and Driver, {Simon P.} and Christoph Federrath and Caroline Foster and Gregory Goldstein and Michael Goodwin and Andrew Hopkins and Lawrence, {J. S.} and Leslie, {Sarah K.} and Lewis, {Geraint F.} and Lorente, {Nuria P.F.} and Owers, {Matt S.} and Richard McDermid and Richards, {Samuel N.} and Robert Sharp and Nicholas Scott and Sweet, {Sarah M.} and Taranu, {Dan S.} and Edoardo Tescari and Chiara Tonini and {van de Sande}, Jesse and Walcher, {C. Jakob} and Angus Wright",
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Medling, AM, Cortese, L, Croom, SM, Green, AW, Groves, B, Hampton, E, Ho, IT, Davies, LJM, Kewley, LJ, Moffett, AJ, Schaefer, AL, Taylor, E, Zafar, T, Bekki, K, Bland-Hawthorn, J, Bloom, JV, Brough, S, Bryant, JJ, Catinella, B, Cecil, G, Colless, M, Couch, WJ, Drinkwater, MJ, Driver, SP, Federrath, C, Foster, C, Goldstein, G, Goodwin, M, Hopkins, A, Lawrence, JS, Leslie, SK, Lewis, GF, Lorente, NPF, Owers, MS, McDermid, R, Richards, SN, Sharp, R, Scott, N, Sweet, SM, Taranu, DS, Tescari, E, Tonini, C, van de Sande, J, Walcher, CJ & Wright, A 2018, 'The SAMI Galaxy Survey: Spatially resolving the main sequence of star formation' Monthly Notices of the Royal Astronomical Society, vol. 475, no. 4, pp. 5194-5214. https://doi.org/10.1093/mnras/sty127

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

In: Monthly Notices of the Royal Astronomical Society, Vol. 475, No. 4, 01.04.2018, p. 5194-5214.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The SAMI Galaxy Survey

T2 - Spatially resolving the main sequence of star formation

AU - Medling, Anne M.

AU - Cortese, Luca

AU - Croom, Scott M.

AU - Green, Andrew W.

AU - Groves, Brent

AU - Hampton, Elise

AU - Ho, I. Ting

AU - Davies, Luke J.M.

AU - Kewley, Lisa J.

AU - Moffett, Amanda J.

AU - Schaefer, Adam L.

AU - Taylor, Edward

AU - Zafar, Tayyaba

AU - Bekki, Kenji

AU - Bland-Hawthorn, Joss

AU - Bloom, Jessica V.

AU - Brough, Sarah

AU - Bryant, Julia J.

AU - Catinella, Barbara

AU - Cecil, Gerald

AU - Colless, Matthew

AU - Couch, Warrick J.

AU - Drinkwater, Michael J.

AU - Driver, Simon P.

AU - Federrath, Christoph

AU - Foster, Caroline

AU - Goldstein, Gregory

AU - Goodwin, Michael

AU - Hopkins, Andrew

AU - Lawrence, J. S.

AU - Leslie, Sarah K.

AU - Lewis, Geraint F.

AU - Lorente, Nuria P.F.

AU - Owers, Matt S.

AU - McDermid, Richard

AU - Richards, Samuel N.

AU - Sharp, Robert

AU - Scott, Nicholas

AU - Sweet, Sarah M.

AU - Taranu, Dan S.

AU - Tescari, Edoardo

AU - Tonini, Chiara

AU - van de Sande, Jesse

AU - Walcher, C. Jakob

AU - Wright, Angus

PY - 2018/4/1

Y1 - 2018/4/1

N2 - 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.

AB - 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.

KW - Galaxies: evolution

KW - Galaxies: star formation

KW - Surveys

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U2 - 10.1093/mnras/sty127

DO - 10.1093/mnras/sty127

M3 - Article

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SP - 5194

EP - 5214

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

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ER -