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

Western Sydney University

Research output: Contribution to journal › Article › peer-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 Â± 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.

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

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10.1093/mnras/sty3258

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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{05c7ec6cebf041f5820b20e00046a85e,

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 {\^A}± 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.}",

year = "2019",

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: 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.

PY - 2019

Y1 - 2019

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 Â± 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 Â± 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.

UR - https://hdl.handle.net/1959.7/uws:66836

U2 - 10.1093/mnras/sty3258

DO - 10.1093/mnras/sty3258

M3 - Article

SN - 0035-8711

VL - 483

SP - 2851

EP - 2870

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

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

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