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; 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

doi:10.1093/mnras/sty3258

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. McElroyA. 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 journal › Review article › peer-review

36 Citations (Scopus)

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 (M_G ≥ 10^12.5M_⊙). 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 M_G = 10^12.5M_⊙, 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.

Original language	English
Pages (from-to)	2851-2870
Number of pages	20
Journal	Monthly Notices of the Royal Astronomical Society
Volume	483
Issue number	3
DOIs	https://doi.org/10.1093/mnras/sty3258
Publication status	Published - 2019 Mar 1

Bibliographical note

Funding Information:
The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney-AAO Multi-object Integral field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the Galaxy And Mass Assembly (GAMA) Survey, and the VST ATLAS Survey. The SAMI Galaxy Survey is supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013, the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and other participating institutions. The SAMI Galaxy Survey website is http://sami-survey.org/.

Funding Information:
M.S.O. acknowledges the funding support from the Australian Research Council (ARC) through a Future Fellowship (FT140100255). J.T.A. acknowledges the award of a Science and Industry Endowment Fund (SIEF) John Stocker Fellowship. J.v.d.S. is funded under Bland-Hawthorn’s ARC Laureate Fellowship (FL140100278). S.B. acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). S.K.Y. acknowledges support from the Korean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22-0064). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. C.F. gratefully acknowledges funding provided by the Australian Research Council’s Discovery Projects (grants DP150104329 and DP170100603). Support for A.M.M. is provided by National Aeronautics and Space Ad-minsitration (NASA) through Hubble Fellowship grant #HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555.

Funding Information:
M.S.O. acknowledges the funding support from the Australian Research Council (ARC) through a Future Fellowship (FT140100255). J.T.A. acknowledges the award of a Science and Industry Endowment Fund (SIEF) John Stocker Fellowship. J.v.d.S. is funded under Bland-Hawthorn's ARC Laureate Fellowship (FL140100278). S.B. acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). S.K.Y. acknowledges support from theKorean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22- 0064). This studywas performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. C.F. gratefully acknowledges funding provided by the Australian Research Council's Discovery Projects (grants DP150104329 and DP170100603). Support for A.M.M. is provided by National Aeronautics and Space Adminsitration (NASA) through Hubble Fellowship grant #HST-HF2- 51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555.

Publisher Copyright:
© 2018 The Author(s).

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/sty3258

Cite this

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., ... 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

@article{d6a5405622434edf8872f782af128243,

title = "The SAMI Galaxy Survey: Observing the environmental quenching of star formation in GAMA groups",

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.",

author = "Schaefer, {A. L.} and Croom, {S. M.} and N. Scott and S. Brough and Allen, {J. T.} and K. Bekki and J. Bland-Hawthorn and Bloom, {J. V.} and Bryant, {J. J.} and L. Cortese and Davies, {L. J.M.} and C. Federrath and Fogarty, {L. M.R.} and Green, {A. W.} and B. Groves and Hopkins, {A. M.} and Konstantopoulos, {I. S.} and L{\'o}pez-S{\'a}nchez, {A. R.} and Lawrence, {J. S.} and McElroy, {R. E.} and Medling, {A. M.} and Owers, {M. S.} and Pracy, {M. B.} and Richards, {S. N.} and Robotham, {A. S.G.} and {Van De Sande}, J. and C. Tonini and Yi, {S. K.}",

note = "Funding Information: The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney-AAO Multi-object Integral field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the Galaxy And Mass Assembly (GAMA) Survey, and the VST ATLAS Survey. The SAMI Galaxy Survey is supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013, the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and other participating institutions. The SAMI Galaxy Survey website is http://sami-survey.org/. Funding Information: M.S.O. acknowledges the funding support from the Australian Research Council (ARC) through a Future Fellowship (FT140100255). J.T.A. acknowledges the award of a Science and Industry Endowment Fund (SIEF) John Stocker Fellowship. J.v.d.S. is funded under Bland-Hawthorn{\textquoteright}s ARC Laureate Fellowship (FL140100278). S.B. acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). S.K.Y. acknowledges support from the Korean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22-0064). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. C.F. gratefully acknowledges funding provided by the Australian Research Council{\textquoteright}s Discovery Projects (grants DP150104329 and DP170100603). Support for A.M.M. is provided by National Aeronautics and Space Ad-minsitration (NASA) through Hubble Fellowship grant #HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Funding Information: M.S.O. acknowledges the funding support from the Australian Research Council (ARC) through a Future Fellowship (FT140100255). J.T.A. acknowledges the award of a Science and Industry Endowment Fund (SIEF) John Stocker Fellowship. J.v.d.S. is funded under Bland-Hawthorn's ARC Laureate Fellowship (FL140100278). S.B. acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). S.K.Y. acknowledges support from theKorean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22- 0064). This studywas performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. C.F. gratefully acknowledges funding provided by the Australian Research Council's Discovery Projects (grants DP150104329 and DP170100603). Support for A.M.M. is provided by National Aeronautics and Space Adminsitration (NASA) through Hubble Fellowship grant #HST-HF2- 51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Publisher Copyright: {\textcopyright} 2018 The Author(s).",

year = "2019",

month = mar,

day = "1",

doi = "10.1093/mnras/sty3258",

language = "English",

volume = "483",

pages = "2851--2870",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

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

TY - JOUR

T1 - The SAMI Galaxy Survey

T2 - Observing the environmental quenching of star formation in GAMA groups

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.

N1 - Funding Information: The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney-AAO Multi-object Integral field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the Galaxy And Mass Assembly (GAMA) Survey, and the VST ATLAS Survey. The SAMI Galaxy Survey is supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013, the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and other participating institutions. The SAMI Galaxy Survey website is http://sami-survey.org/. Funding Information: M.S.O. acknowledges the funding support from the Australian Research Council (ARC) through a Future Fellowship (FT140100255). J.T.A. acknowledges the award of a Science and Industry Endowment Fund (SIEF) John Stocker Fellowship. J.v.d.S. is funded under Bland-Hawthorn’s ARC Laureate Fellowship (FL140100278). S.B. acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). S.K.Y. acknowledges support from the Korean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22-0064). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. C.F. gratefully acknowledges funding provided by the Australian Research Council’s Discovery Projects (grants DP150104329 and DP170100603). Support for A.M.M. is provided by National Aeronautics and Space Ad-minsitration (NASA) through Hubble Fellowship grant #HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Funding Information: M.S.O. acknowledges the funding support from the Australian Research Council (ARC) through a Future Fellowship (FT140100255). J.T.A. acknowledges the award of a Science and Industry Endowment Fund (SIEF) John Stocker Fellowship. J.v.d.S. is funded under Bland-Hawthorn's ARC Laureate Fellowship (FL140100278). S.B. acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). S.K.Y. acknowledges support from theKorean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22- 0064). This studywas performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. C.F. gratefully acknowledges funding provided by the Australian Research Council's Discovery Projects (grants DP150104329 and DP170100603). Support for A.M.M. is provided by National Aeronautics and Space Adminsitration (NASA) through Hubble Fellowship grant #HST-HF2- 51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Publisher Copyright: © 2018 The Author(s).

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.

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U2 - 10.1093/mnras/sty3258

DO - 10.1093/mnras/sty3258

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JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

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

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