The SAMI galaxy survey: Satellite galaxies undergo little structural change during their quenching phase

L. Cortese, J. Van De Sande, C. P. Lagos, B. Catinella, L. J.M. Davies, S. M. Croom, S. Brough, J. J. Bryant, J. S. Lawrence, M. S. Owers, S. N. Richards, S. M. Sweet, J. Bland-Hawthorn

Research output: Contribution to journalReview article

3 Citations (Scopus)
18 Downloads (Pure)

Abstract

At fixed stellar mass, satellite galaxies show higher passive fractions than centrals, suggesting that environment is directly quenching their star formation. Here, we investigate whether satellite quenching is accompanied by changes in stellar spin (quantified by the ratio of the rotational to dispersion velocity V/σ) for a sample of massive (M > 1010 M☉) satellite galaxies extracted from the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey. These systems are carefully matched to a control sample of main sequence, high V/σ central galaxies. As expected, at fixed stellar mass and ellipticity, satellites have lower star formation rate (SFR) and spin than the control centrals. However, most of the difference is in SFR, whereas the spin decreases significantly only for satellites that have already reached the red sequence. We perform a similar analysis for galaxies in the Evolution and Assembly of GaLaxies and their Environments (EAGLE) hydrodynamical simulation and recover differences in both SFR and spin similar to those observed in SAMI. However, when EAGLE satellites are matched to their true central progenitors, the change in spin is further reduced and galaxies mainly show a decrease in SFR during their satellite phase. The difference in spin observed between satellites and centrals at z ∼ 0 is primarily due to the fact that satellites do not grow their angular momentum as fast as centrals after accreting into bigger haloes, not to a reduction of V/σ due to environmental effects. Our findings highlight the effect of progenitor bias in our understanding of galaxy transformation and they suggest that satellites undergo little structural change before and during their quenching phase.

Original languageEnglish
Pages (from-to)2656-2665
Number of pages10
JournalMonthly Notices of the Royal Astronomical Society
Volume485
Issue number2
DOIs
Publication statusPublished - 15 Feb 2019

Fingerprint

structural change
spectrographs
quenching
galaxies
star formation rate
stellar mass
assembly
environment simulation
ellipticity
environmental effect
angular momentum
star formation
halos
rate

Cite this

Cortese, L. ; Van De Sande, J. ; Lagos, C. P. ; Catinella, B. ; Davies, L. J.M. ; Croom, S. M. ; Brough, S. ; Bryant, J. J. ; Lawrence, J. S. ; Owers, M. S. ; Richards, S. N. ; Sweet, S. M. ; Bland-Hawthorn, J. / The SAMI galaxy survey : Satellite galaxies undergo little structural change during their quenching phase. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 485, No. 2. pp. 2656-2665.
@article{02466cd2d93e47d8b608eb8b39509cfe,
title = "The SAMI galaxy survey: Satellite galaxies undergo little structural change during their quenching phase",
abstract = "At fixed stellar mass, satellite galaxies show higher passive fractions than centrals, suggesting that environment is directly quenching their star formation. Here, we investigate whether satellite quenching is accompanied by changes in stellar spin (quantified by the ratio of the rotational to dispersion velocity V/σ) for a sample of massive (M∗ > 1010 M☉) satellite galaxies extracted from the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey. These systems are carefully matched to a control sample of main sequence, high V/σ central galaxies. As expected, at fixed stellar mass and ellipticity, satellites have lower star formation rate (SFR) and spin than the control centrals. However, most of the difference is in SFR, whereas the spin decreases significantly only for satellites that have already reached the red sequence. We perform a similar analysis for galaxies in the Evolution and Assembly of GaLaxies and their Environments (EAGLE) hydrodynamical simulation and recover differences in both SFR and spin similar to those observed in SAMI. However, when EAGLE satellites are matched to their true central progenitors, the change in spin is further reduced and galaxies mainly show a decrease in SFR during their satellite phase. The difference in spin observed between satellites and centrals at z ∼ 0 is primarily due to the fact that satellites do not grow their angular momentum as fast as centrals after accreting into bigger haloes, not to a reduction of V/σ due to environmental effects. Our findings highlight the effect of progenitor bias in our understanding of galaxy transformation and they suggest that satellites undergo little structural change before and during their quenching phase.",
keywords = "Dynamics, Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: kinematics",
author = "L. Cortese and {Van De Sande}, J. and Lagos, {C. P.} and B. Catinella and Davies, {L. J.M.} and Croom, {S. M.} and S. Brough and Bryant, {J. J.} and Lawrence, {J. S.} and Owers, {M. S.} and Richards, {S. N.} and Sweet, {S. M.} and J. Bland-Hawthorn",
year = "2019",
month = "2",
day = "15",
doi = "10.1093/mnras/stz485",
language = "English",
volume = "485",
pages = "2656--2665",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "OXFORD UNIV PRESS UNITED KINGDOM",
number = "2",

}

Cortese, L, Van De Sande, J, Lagos, CP, Catinella, B, Davies, LJM, Croom, SM, Brough, S, Bryant, JJ, Lawrence, JS, Owers, MS, Richards, SN, Sweet, SM & Bland-Hawthorn, J 2019, 'The SAMI galaxy survey: Satellite galaxies undergo little structural change during their quenching phase' Monthly Notices of the Royal Astronomical Society, vol. 485, no. 2, pp. 2656-2665. https://doi.org/10.1093/mnras/stz485

The SAMI galaxy survey : Satellite galaxies undergo little structural change during their quenching phase. / Cortese, L.; Van De Sande, J.; Lagos, C. P.; Catinella, B.; Davies, L. J.M.; Croom, S. M.; Brough, S.; Bryant, J. J.; Lawrence, J. S.; Owers, M. S.; Richards, S. N.; Sweet, S. M.; Bland-Hawthorn, J.

In: Monthly Notices of the Royal Astronomical Society, Vol. 485, No. 2, 15.02.2019, p. 2656-2665.

Research output: Contribution to journalReview article

TY - JOUR

T1 - The SAMI galaxy survey

T2 - Satellite galaxies undergo little structural change during their quenching phase

AU - Cortese, L.

AU - Van De Sande, J.

AU - Lagos, C. P.

AU - Catinella, B.

AU - Davies, L. J.M.

AU - Croom, S. M.

AU - Brough, S.

AU - Bryant, J. J.

AU - Lawrence, J. S.

AU - Owers, M. S.

AU - Richards, S. N.

AU - Sweet, S. M.

AU - Bland-Hawthorn, J.

PY - 2019/2/15

Y1 - 2019/2/15

N2 - At fixed stellar mass, satellite galaxies show higher passive fractions than centrals, suggesting that environment is directly quenching their star formation. Here, we investigate whether satellite quenching is accompanied by changes in stellar spin (quantified by the ratio of the rotational to dispersion velocity V/σ) for a sample of massive (M∗ > 1010 M☉) satellite galaxies extracted from the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey. These systems are carefully matched to a control sample of main sequence, high V/σ central galaxies. As expected, at fixed stellar mass and ellipticity, satellites have lower star formation rate (SFR) and spin than the control centrals. However, most of the difference is in SFR, whereas the spin decreases significantly only for satellites that have already reached the red sequence. We perform a similar analysis for galaxies in the Evolution and Assembly of GaLaxies and their Environments (EAGLE) hydrodynamical simulation and recover differences in both SFR and spin similar to those observed in SAMI. However, when EAGLE satellites are matched to their true central progenitors, the change in spin is further reduced and galaxies mainly show a decrease in SFR during their satellite phase. The difference in spin observed between satellites and centrals at z ∼ 0 is primarily due to the fact that satellites do not grow their angular momentum as fast as centrals after accreting into bigger haloes, not to a reduction of V/σ due to environmental effects. Our findings highlight the effect of progenitor bias in our understanding of galaxy transformation and they suggest that satellites undergo little structural change before and during their quenching phase.

AB - At fixed stellar mass, satellite galaxies show higher passive fractions than centrals, suggesting that environment is directly quenching their star formation. Here, we investigate whether satellite quenching is accompanied by changes in stellar spin (quantified by the ratio of the rotational to dispersion velocity V/σ) for a sample of massive (M∗ > 1010 M☉) satellite galaxies extracted from the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey. These systems are carefully matched to a control sample of main sequence, high V/σ central galaxies. As expected, at fixed stellar mass and ellipticity, satellites have lower star formation rate (SFR) and spin than the control centrals. However, most of the difference is in SFR, whereas the spin decreases significantly only for satellites that have already reached the red sequence. We perform a similar analysis for galaxies in the Evolution and Assembly of GaLaxies and their Environments (EAGLE) hydrodynamical simulation and recover differences in both SFR and spin similar to those observed in SAMI. However, when EAGLE satellites are matched to their true central progenitors, the change in spin is further reduced and galaxies mainly show a decrease in SFR during their satellite phase. The difference in spin observed between satellites and centrals at z ∼ 0 is primarily due to the fact that satellites do not grow their angular momentum as fast as centrals after accreting into bigger haloes, not to a reduction of V/σ due to environmental effects. Our findings highlight the effect of progenitor bias in our understanding of galaxy transformation and they suggest that satellites undergo little structural change before and during their quenching phase.

KW - Dynamics

KW - Galaxies: evolution

KW - Galaxies: fundamental parameters

KW - Galaxies: kinematics

UR - http://www.scopus.com/inward/record.url?scp=85067084226&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz485

DO - 10.1093/mnras/stz485

M3 - Review article

VL - 485

SP - 2656

EP - 2665

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -