The SAMI Galaxy Survey: observing the environmental quenching of star formation in GAMA groups

A. L. Schaefer, S. M. Croom, N. Scott, S. Brough, J. T. Allen, K. Bekki, J. Bland-Hawthorn, J. V. Bloom, J. J. Bryant, L. Cortese, L. J. M. Davies, C. Federrath, L. M. R. Fogarty, A. W. Green, B. Groves, A. M. Hopkins, I. S. Konstantopoulos, A. R. López-Sánchez, J. S. Lawrence, R. E. McElroy & 8 others A. M. Medling, M. S. Owers, M. B. Pracy, S. N. Richards, A. S. G. Robotham, J. van de Sande, C. Tonini, S. K. Yi

Research output: Contribution to journalArticleResearchpeer-review

Abstract

We explore the radial distribution of star formation in galaxies in the SAMI Galaxy Survey as a function of their Local Group environment. Using a sample of galaxies in groups (with halo masses less than ≃ 1014M) from the Galaxy And Mass Assembly Survey, we find signatures of environmental quenching in high-mass groups (MG > 1012.5M). The mean integrated specific star formation rate (sSFR) of star-forming galaxies in high-mass groups is lower than for galaxies in low-mass groups or those that are ungrouped, with Δlog(sSFR/yr-1) = 0.45 ± 0.07. This difference is seen at all galaxy stellar masses. In high-mass groups, starforming galaxies more massive than M ∼ 1010M have centrally concentrated star formation. These galaxies also lie below the star formation main sequence, which suggests they may be undergoing outside-in quenching. Lower mass galaxies in high-mass groups do not show evidence of concentrated star formation. In groups less massive than MG = 1012.5M, we do not observe these trends. In this regime, we find a modest correlation between centrally concentrated star formation and an enhancement in the total star formation rate, consistent with triggered star formation in these galaxies.

LanguageEnglish
Pages2851-2870
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume483
Issue number3
DOIs
Publication statusPublished - 1 Mar 2019

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star formation
quenching
galaxies
star formation rate
galactic clusters
stellar mass
radial distribution
halos
assembly
signatures
trends
stars
augmentation
rate

Keywords

  • Galaxies: evolution
  • Galaxies: groups: general
  • Galaxies: interactions
  • Galaxies: star formation
  • Galaxies: structure

Cite this

Schaefer, A. L., Croom, S. M., Scott, N., Brough, S., Allen, J. T., Bekki, K., ... Yi, S. K. (2019). The SAMI Galaxy Survey: observing the environmental quenching of star formation in GAMA groups. Monthly Notices of the Royal Astronomical Society, 483(3), 2851-2870. https://doi.org/10.1093/mnras/sty3258
Schaefer, A. L. ; Croom, S. M. ; Scott, N. ; Brough, S. ; Allen, J. T. ; Bekki, K. ; Bland-Hawthorn, J. ; Bloom, J. V. ; Bryant, J. J. ; Cortese, L. ; Davies, L. J. M. ; Federrath, C. ; Fogarty, L. M. R. ; Green, A. W. ; Groves, B. ; Hopkins, A. M. ; Konstantopoulos, I. S. ; López-Sánchez, A. R. ; Lawrence, J. S. ; McElroy, R. E. ; Medling, A. M. ; Owers, M. S. ; Pracy, M. B. ; Richards, S. N. ; Robotham, A. S. G. ; van de Sande, J. ; Tonini, C. ; Yi, S. K. / The SAMI Galaxy Survey : observing the environmental quenching of star formation in GAMA groups. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 483, No. 3. pp. 2851-2870.
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abstract = "We explore the radial distribution of star formation in galaxies in the SAMI Galaxy Survey as a function of their Local Group environment. Using a sample of galaxies in groups (with halo masses less than ≃ 1014M⊙) from the Galaxy And Mass Assembly Survey, we find signatures of environmental quenching in high-mass groups (MG > 1012.5M⊙). The mean integrated specific star formation rate (sSFR) of star-forming galaxies in high-mass groups is lower than for galaxies in low-mass groups or those that are ungrouped, with Δlog(sSFR/yr-1) = 0.45 ± 0.07. This difference is seen at all galaxy stellar masses. In high-mass groups, starforming galaxies more massive than M∗ ∼ 1010M⊙ have centrally concentrated star formation. These galaxies also lie below the star formation main sequence, which suggests they may be undergoing outside-in quenching. Lower mass galaxies in high-mass groups do not show evidence of concentrated star formation. In groups less massive than MG = 1012.5M⊙, we do not observe these trends. In this regime, we find a modest correlation between centrally concentrated star formation and an enhancement in the total star formation rate, consistent with triggered star formation in these galaxies.",
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Schaefer, AL, Croom, SM, Scott, N, Brough, S, Allen, JT, Bekki, K, Bland-Hawthorn, J, Bloom, JV, Bryant, JJ, Cortese, L, Davies, LJM, Federrath, C, Fogarty, LMR, Green, AW, Groves, B, Hopkins, AM, Konstantopoulos, IS, López-Sánchez, AR, Lawrence, JS, McElroy, RE, Medling, AM, Owers, MS, Pracy, MB, Richards, SN, Robotham, ASG, van de Sande, J, Tonini, C & Yi, SK 2019, 'The SAMI Galaxy Survey: observing the environmental quenching of star formation in GAMA groups', Monthly Notices of the Royal Astronomical Society, vol. 483, no. 3, pp. 2851-2870. https://doi.org/10.1093/mnras/sty3258

The SAMI Galaxy Survey : observing the environmental quenching of star formation in GAMA groups. / Schaefer, A. L.; Croom, S. M.; Scott, N.; Brough, S.; Allen, J. T.; Bekki, K.; Bland-Hawthorn, J.; Bloom, J. V.; Bryant, J. J.; Cortese, L.; Davies, L. J. M.; Federrath, C.; Fogarty, L. M. R.; Green, A. W.; Groves, B.; Hopkins, A. M.; Konstantopoulos, I. S.; López-Sánchez, A. R.; Lawrence, J. S.; McElroy, R. E.; Medling, A. M.; Owers, M. S.; Pracy, M. B.; Richards, S. N.; Robotham, A. S. G.; van de Sande, J.; Tonini, C.; Yi, S. K.

In: Monthly Notices of the Royal Astronomical Society, Vol. 483, No. 3, 01.03.2019, p. 2851-2870.

Research output: Contribution to journalArticleResearchpeer-review

TY - JOUR

T1 - The SAMI Galaxy Survey

T2 - Monthly Notices of the Royal Astronomical Society

AU - Schaefer, A. L.

AU - Croom, S. M.

AU - Scott, N.

AU - Brough, S.

AU - Allen, J. T.

AU - Bekki, K.

AU - Bland-Hawthorn, J.

AU - Bloom, J. V.

AU - Bryant, J. J.

AU - Cortese, L.

AU - Davies, L. J. M.

AU - Federrath, C.

AU - Fogarty, L. M. R.

AU - Green, A. W.

AU - Groves, B.

AU - Hopkins, A. M.

AU - Konstantopoulos, I. S.

AU - López-Sánchez, A. R.

AU - Lawrence, J. S.

AU - McElroy, R. E.

AU - Medling, A. M.

AU - Owers, M. S.

AU - Pracy, M. B.

AU - Richards, S. N.

AU - Robotham, A. S. G.

AU - van de Sande, J.

AU - Tonini, C.

AU - Yi, S. K.

PY - 2019/3/1

Y1 - 2019/3/1

N2 - We explore the radial distribution of star formation in galaxies in the SAMI Galaxy Survey as a function of their Local Group environment. Using a sample of galaxies in groups (with halo masses less than ≃ 1014M⊙) from the Galaxy And Mass Assembly Survey, we find signatures of environmental quenching in high-mass groups (MG > 1012.5M⊙). The mean integrated specific star formation rate (sSFR) of star-forming galaxies in high-mass groups is lower than for galaxies in low-mass groups or those that are ungrouped, with Δlog(sSFR/yr-1) = 0.45 ± 0.07. This difference is seen at all galaxy stellar masses. In high-mass groups, starforming galaxies more massive than M∗ ∼ 1010M⊙ have centrally concentrated star formation. These galaxies also lie below the star formation main sequence, which suggests they may be undergoing outside-in quenching. Lower mass galaxies in high-mass groups do not show evidence of concentrated star formation. In groups less massive than MG = 1012.5M⊙, we do not observe these trends. In this regime, we find a modest correlation between centrally concentrated star formation and an enhancement in the total star formation rate, consistent with triggered star formation in these galaxies.

AB - We explore the radial distribution of star formation in galaxies in the SAMI Galaxy Survey as a function of their Local Group environment. Using a sample of galaxies in groups (with halo masses less than ≃ 1014M⊙) from the Galaxy And Mass Assembly Survey, we find signatures of environmental quenching in high-mass groups (MG > 1012.5M⊙). The mean integrated specific star formation rate (sSFR) of star-forming galaxies in high-mass groups is lower than for galaxies in low-mass groups or those that are ungrouped, with Δlog(sSFR/yr-1) = 0.45 ± 0.07. This difference is seen at all galaxy stellar masses. In high-mass groups, starforming galaxies more massive than M∗ ∼ 1010M⊙ have centrally concentrated star formation. These galaxies also lie below the star formation main sequence, which suggests they may be undergoing outside-in quenching. Lower mass galaxies in high-mass groups do not show evidence of concentrated star formation. In groups less massive than MG = 1012.5M⊙, we do not observe these trends. In this regime, we find a modest correlation between centrally concentrated star formation and an enhancement in the total star formation rate, consistent with triggered star formation in these galaxies.

KW - Galaxies: evolution

KW - Galaxies: groups: general

KW - Galaxies: interactions

KW - Galaxies: star formation

KW - Galaxies: structure

UR - http://www.scopus.com/inward/record.url?scp=85063587208&partnerID=8YFLogxK

UR - http://purl.org/au-research/grants/arc/FT140100255

UR - http://purl.org/au-research/grants/arc/CE170100013

U2 - 10.1093/mnras/sty3258

DO - 10.1093/mnras/sty3258

M3 - Article

VL - 483

SP - 2851

EP - 2870

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -