Data

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

The University of Western Australia
Schaefer, Adam L. ; Croom, S. M. ; Scott, N. ; Brough, Sarah ; Allen, James T. ; Bekki, Kenji ; Bland-Hawthorn, Joss ; Bloom, Jessica V. ; Bryant, J. J. ; Cortese, Luca ; Davies, Luke ; Federrath, Christoph ; Fogarty, Lisa M R ; Green, A. W. ; Groves, Brent ; Hopkins, Andrew M. ; Konstantopoulos, Iraklis S. ; López-Sánchez, Ángel R. ; Lawrence, Jon S. ; McElroy, Rebecca
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ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Adc&rfr_id=info%3Asid%2FANDS&rft_id=info:doi10.1093/mnras/sty3258&rft.title=Data from : The SAMI Galaxy Survey: observing the environmental quenching of star formation in GAMA groups&rft.identifier=10.1093/mnras/sty3258&rft.publisher=SAO/NASA Astrophysics Data System (ADS)&rft.description=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 ∼eq 10^{14} M_☉) from the Galaxy And Mass Assembly Survey, we find signatures of environmental quenching in high-mass groups (M_{ G} > 10^{12.5} M_{☉}). 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 ∆ log ( sSFR/yr^{-1}) = 0.45 ± 0.07. This difference is seen at all galaxy stellar masses. In high-mass groups, star-forming galaxies more massive than M_{*} ∼ 10^{10} M_{☉} 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^{12.5} M_{☉}, 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.&rft.creator=Schaefer, Adam L. &rft.creator=Croom, S. M. &rft.creator=Scott, N. &rft.creator=Brough, Sarah &rft.creator=Allen, James T. &rft.creator=Bekki, Kenji &rft.creator=Bland-Hawthorn, Joss &rft.creator=Bloom, Jessica V. &rft.creator=Bryant, J. J. &rft.creator=Cortese, Luca &rft.creator=Davies, Luke &rft.creator=Federrath, Christoph &rft.creator=Fogarty, Lisa M R &rft.creator=Green, A. W. &rft.creator=Groves, Brent &rft.creator=Hopkins, Andrew M. &rft.creator=Konstantopoulos, Iraklis S. &rft.creator=López-Sánchez, Ángel R. &rft.creator=Lawrence, Jon S. &rft.creator=McElroy, Rebecca &rft.date=2019&rft.relation=http://research-repository.uwa.edu.au/en/publications/141395f2-70d4-4bb8-bf99-beb4256d173f&rft_subject=galaxies: evolution&rft_subject=galaxies: interactions&rft_subject=galaxies: star formation&rft_subject=galaxies: structure&rft_subject=galaxies: groups: general&rft_subject=Astrophysics - Astrophysics of Galaxies&rft.type=dataset&rft.language=English Access the data

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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 ∼eq 10^{14} M_☉) from the Galaxy And Mass Assembly Survey, we find signatures of environmental quenching in high-mass groups (M_{ G} > 10^{12.5} M_{☉}). 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 ∆ log ( sSFR/yr^{-1}) = 0.45 ± 0.07. This difference is seen at all galaxy stellar masses. In high-mass groups, star-forming galaxies more massive than M_{*} ∼ 10^{10} M_{☉} 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^{12.5} M_{☉}, 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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External Organisations
University of Sydney; ARC Centre of Excellence for All-sky Astrophysics; Australian Astronomical Observatory; The University of Western Australia; ARC Centre of Excellence for Astrophysics in Three Dimensions (ASTRO3D); University of Wisconsin Madison; University of New South Wales; Macquarie University; Western Sydney University; University of California Berkeley; ARC Australian Research Council; University of Birmingham; Australian National University; Sydney Institute for Astronomy; Australian Astronomical Optics; Envizi; Atlassian; Max Planck Institute for Astronomy
Associated Persons
Adam L. Schaefer (Creator); S. M. Croom (Creator); N. Scott (Creator); Sarah Brough (Creator); James T. Allen (Creator); Joss Bland-Hawthorn (Creator); Jessica V. Bloom (Creator); J. J. Bryant (Creator); Christoph Federrath (Creator); Lisa M R Fogarty (Creator); A. W. Green (Creator); Andrew M. Hopkins (Creator); Iraklis S. Konstantopoulos (Creator); Ángel R. López-Sánchez (Creator); Jon S. Lawrence (Creator); Rebecca McElroy (Creator)

Issued: 2019-03

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