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

• Other Authors: Brent Groves (Creator), Intl Centre for Radio Astronomy Research (ICRAR) (isManagedBy), Kenji Bekki (Creator), Luca Cortese (Creator), Luke Davies (Creator)
• Format: Dataset
• Language: unknown
• Published: The University of Western Australia
• Subjects: galaxies: evolution; galaxies: interactions; galaxies: star formation; galaxies: structure; galaxies: groups: general; Astrophysics - Astrophysics of Galaxies; Bryant; Schaefer; McElroy; sami
• Online Access: https://researchdata.edu.au/data-the-sami-gama-groups/1712388; https://doi.org/10.1093/mnras/sty3258

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) 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.