The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Adam Schaefer, Scott Croom, James Allen, Sarah Brough, Anne Medling, I.-T. Ho, Nic Scott, Michael Pracy, Madusha Gunawardhana, P Norberg, M Alpaslan, A Bauer, Kenji Bekki, J Bland-Hawthorn, J Bloom, J Bryant, W Couch, Simon Driver, L Fogarty, C Foster & 14 others G Goldstein, A Green, A Hopkins, I Konstantopoulos, J Lawrence, A Lopez-Sanchez, N Lorente, M Owers, R Sharp, S Sweet, E.N. Taylor, J van de Sande, C Walcher, Ivy Wong

Research output: Contribution to journalArticle

25 Citations (Scopus)

Abstract

We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission, we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M*; 108.1-1010.95 M⊙) and in fifth nearest neighbour local environment density (Σ5; 10-1.3-102.1 Mpc-2). We show that star formation rate gradients in galaxies are steeper in dense (log10(Σ5/Mpc2) > 0.5) environments by 0.58 ± 0.29 dex re^{-1} in galaxies with stellar masses in the range 10^{10} < M_{*}/M_{⊙} < 10^{11} and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density, the star formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scale-radius ratio (r50,Hα/r50,cont), which compares the extent of ongoing star formation to previous star formation. With this metric, we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ˜5 ± 4 per cent in low-density environments (log10(Σ5/Mpc2) < 0.0) to 30 ± 15 per cent in the highest density environments (log10(Σ5/Mpc2) > 1.0). These lines of evidence strongly suggest that with increasing local environment density, the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.
Original languageEnglish
Pages (from-to)121-142
JournalMonthly Notices of the Royal Astronomical Society
Volume464
Issue number1
DOIs
Publication statusPublished - Jan 2017

Fingerprint

star formation
assembly
quenching
galaxies
stellar mass
dust
star formation rate
spectrographs
coverings
signatures
stars
gradients
profiles

Cite this

Schaefer, Adam ; Croom, Scott ; Allen, James ; Brough, Sarah ; Medling, Anne ; Ho, I.-T. ; Scott, Nic ; Pracy, Michael ; Gunawardhana, Madusha ; Norberg, P ; Alpaslan, M ; Bauer, A ; Bekki, Kenji ; Bland-Hawthorn, J ; Bloom, J ; Bryant, J ; Couch, W ; Driver, Simon ; Fogarty, L ; Foster, C ; Goldstein, G ; Green, A ; Hopkins, A ; Konstantopoulos, I ; Lawrence, J ; Lopez-Sanchez, A ; Lorente, N ; Owers, M ; Sharp, R ; Sweet, S ; Taylor, E.N. ; van de Sande, J ; Walcher, C ; Wong, Ivy. / The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 464, No. 1. pp. 121-142.
@article{a7d6496e83b44ee89dcef6939433daa6,
title = "The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies",
abstract = "We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission, we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M*; 108.1-1010.95 M⊙) and in fifth nearest neighbour local environment density (Σ5; 10-1.3-102.1 Mpc-2). We show that star formation rate gradients in galaxies are steeper in dense (log10(Σ5/Mpc2) > 0.5) environments by 0.58 ± 0.29 dex re^{-1} in galaxies with stellar masses in the range 10^{10} < M_{*}/M_{⊙} < 10^{11} and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density, the star formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scale-radius ratio (r50,Hα/r50,cont), which compares the extent of ongoing star formation to previous star formation. With this metric, we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ˜5 ± 4 per cent in low-density environments (log10(Σ5/Mpc2) < 0.0) to 30 ± 15 per cent in the highest density environments (log10(Σ5/Mpc2) > 1.0). These lines of evidence strongly suggest that with increasing local environment density, the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.",
author = "Adam Schaefer and Scott Croom and James Allen and Sarah Brough and Anne Medling and I.-T. Ho and Nic Scott and Michael Pracy and Madusha Gunawardhana and P Norberg and M Alpaslan and A Bauer and Kenji Bekki and J Bland-Hawthorn and J Bloom and J Bryant and W Couch and Simon Driver and L Fogarty and C Foster and G Goldstein and A Green and A Hopkins and I Konstantopoulos and J Lawrence and A Lopez-Sanchez and N Lorente and M Owers and R Sharp and S Sweet and E.N. Taylor and {van de Sande}, J and C Walcher and Ivy Wong",
year = "2017",
month = "1",
doi = "10.1093/mnras/stw2289",
language = "English",
volume = "464",
pages = "121--142",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "OXFORD UNIV PRESS UNITED KINGDOM",
number = "1",

}

Schaefer, A, Croom, S, Allen, J, Brough, S, Medling, A, Ho, I-T, Scott, N, Pracy, M, Gunawardhana, M, Norberg, P, Alpaslan, M, Bauer, A, Bekki, K, Bland-Hawthorn, J, Bloom, J, Bryant, J, Couch, W, Driver, S, Fogarty, L, Foster, C, Goldstein, G, Green, A, Hopkins, A, Konstantopoulos, I, Lawrence, J, Lopez-Sanchez, A, Lorente, N, Owers, M, Sharp, R, Sweet, S, Taylor, EN, van de Sande, J, Walcher, C & Wong, I 2017, 'The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies' Monthly Notices of the Royal Astronomical Society, vol. 464, no. 1, pp. 121-142. https://doi.org/10.1093/mnras/stw2289

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies. / Schaefer, Adam; Croom, Scott; Allen, James; Brough, Sarah; Medling, Anne; Ho, I.-T.; Scott, Nic; Pracy, Michael; Gunawardhana, Madusha; Norberg, P; Alpaslan, M; Bauer, A; Bekki, Kenji; Bland-Hawthorn, J; Bloom, J; Bryant, J; Couch, W; Driver, Simon; Fogarty, L; Foster, C; Goldstein, G; Green, A; Hopkins, A; Konstantopoulos, I; Lawrence, J; Lopez-Sanchez, A; Lorente, N; Owers, M; Sharp, R; Sweet, S; Taylor, E.N.; van de Sande, J; Walcher, C; Wong, Ivy.

In: Monthly Notices of the Royal Astronomical Society, Vol. 464, No. 1, 01.2017, p. 121-142.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

AU - Schaefer, Adam

AU - Croom, Scott

AU - Allen, James

AU - Brough, Sarah

AU - Medling, Anne

AU - Ho, I.-T.

AU - Scott, Nic

AU - Pracy, Michael

AU - Gunawardhana, Madusha

AU - Norberg, P

AU - Alpaslan, M

AU - Bauer, A

AU - Bekki, Kenji

AU - Bland-Hawthorn, J

AU - Bloom, J

AU - Bryant, J

AU - Couch, W

AU - Driver, Simon

AU - Fogarty, L

AU - Foster, C

AU - Goldstein, G

AU - Green, A

AU - Hopkins, A

AU - Konstantopoulos, I

AU - Lawrence, J

AU - Lopez-Sanchez, A

AU - Lorente, N

AU - Owers, M

AU - Sharp, R

AU - Sweet, S

AU - Taylor, E.N.

AU - van de Sande, J

AU - Walcher, C

AU - Wong, Ivy

PY - 2017/1

Y1 - 2017/1

N2 - We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission, we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M*; 108.1-1010.95 M⊙) and in fifth nearest neighbour local environment density (Σ5; 10-1.3-102.1 Mpc-2). We show that star formation rate gradients in galaxies are steeper in dense (log10(Σ5/Mpc2) > 0.5) environments by 0.58 ± 0.29 dex re^{-1} in galaxies with stellar masses in the range 10^{10} < M_{*}/M_{⊙} < 10^{11} and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density, the star formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scale-radius ratio (r50,Hα/r50,cont), which compares the extent of ongoing star formation to previous star formation. With this metric, we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ˜5 ± 4 per cent in low-density environments (log10(Σ5/Mpc2) < 0.0) to 30 ± 15 per cent in the highest density environments (log10(Σ5/Mpc2) > 1.0). These lines of evidence strongly suggest that with increasing local environment density, the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.

AB - We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission, we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M*; 108.1-1010.95 M⊙) and in fifth nearest neighbour local environment density (Σ5; 10-1.3-102.1 Mpc-2). We show that star formation rate gradients in galaxies are steeper in dense (log10(Σ5/Mpc2) > 0.5) environments by 0.58 ± 0.29 dex re^{-1} in galaxies with stellar masses in the range 10^{10} < M_{*}/M_{⊙} < 10^{11} and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density, the star formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scale-radius ratio (r50,Hα/r50,cont), which compares the extent of ongoing star formation to previous star formation. With this metric, we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ˜5 ± 4 per cent in low-density environments (log10(Σ5/Mpc2) < 0.0) to 30 ± 15 per cent in the highest density environments (log10(Σ5/Mpc2) > 1.0). These lines of evidence strongly suggest that with increasing local environment density, the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.

U2 - 10.1093/mnras/stw2289

DO - 10.1093/mnras/stw2289

M3 - Article

VL - 464

SP - 121

EP - 142

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

ER -