Quenching time-scales of galaxies in the eagle simulations

Ruby J. Wright, Claudia Del P. Lagos, Luke J.M. Davies, Chris Power, James W. Trayford, O. Ivy Wong

Research output: Contribution to journalArticle

2 Citations (Scopus)

Abstract

We use the eagle simulations to study the connection between the quenching time-scale, τQ, and the physical mechanisms that transform star-forming galaxies into passive galaxies. By quantifying τQ in two complementary ways-as the time over which (i) galaxies traverse the green valley on the colour-mass diagram, or (ii) leave the main sequence of star formation and subsequently arrive on the passive cloud in specific star formation rate (SSFR)-mass space-we find that the τQ distribution of high-mass centrals, low-mass centrals, and satellites are divergent. In the low stellar mass regime where M <109.6 M·, centrals exhibit systematically longer quenching time-scales than satellites (≈4 Gyr compared to ≈2 Gyr). Satellites with low stellar mass relative to their halo mass cause this disparity, with ram pressure stripping quenching these galaxies rapidly. Low-mass centrals are quenched as a result of stellar feedback, associated with long τQ 3 Gyr. At intermediate stellar masses where $109.7<M☆ <1010.3M⊙, τQ are the longest for both centrals and satellites, particularly for galaxies with higher gas fractions. At M☆1010.3M⊙, galaxy merger counts and black hole activity increase steeply for all galaxies. Quenching time-scales for centrals and satellites decrease with stellar mass in this regime to τQ2 Gyr. In anticipation of new intermediate redshift observational galaxy surveys, we analyse the passive and star-forming fractions of galaxies across redshift, and find that the τQ peak at intermediate stellar masses is responsible for a peak (inflection point) in the fraction of green valley central (satellite) galaxies at z ≈ 0.5-0.7.

Original languageEnglish
Pages (from-to)3740-3758
Number of pages19
JournalMonthly Notices of the Royal Astronomical Society
Volume487
Issue number3
DOIs
Publication statusPublished - 1 Jan 2019

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quenching
galaxies
timescale
stellar mass
simulation
valleys
stars
inflection points
ram
valley
star formation rate
stripping
star formation
halos
merger
diagrams
transform
diagram
color
causes

Cite this

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title = "Quenching time-scales of galaxies in the eagle simulations",
abstract = "We use the eagle simulations to study the connection between the quenching time-scale, τQ, and the physical mechanisms that transform star-forming galaxies into passive galaxies. By quantifying τQ in two complementary ways-as the time over which (i) galaxies traverse the green valley on the colour-mass diagram, or (ii) leave the main sequence of star formation and subsequently arrive on the passive cloud in specific star formation rate (SSFR)-mass space-we find that the τQ distribution of high-mass centrals, low-mass centrals, and satellites are divergent. In the low stellar mass regime where M <109.6 M·, centrals exhibit systematically longer quenching time-scales than satellites (≈4 Gyr compared to ≈2 Gyr). Satellites with low stellar mass relative to their halo mass cause this disparity, with ram pressure stripping quenching these galaxies rapidly. Low-mass centrals are quenched as a result of stellar feedback, associated with long τQ 3 Gyr. At intermediate stellar masses where $109.7<M☆ <1010.3M⊙, τQ are the longest for both centrals and satellites, particularly for galaxies with higher gas fractions. At M☆1010.3M⊙, galaxy merger counts and black hole activity increase steeply for all galaxies. Quenching time-scales for centrals and satellites decrease with stellar mass in this regime to τQ2 Gyr. In anticipation of new intermediate redshift observational galaxy surveys, we analyse the passive and star-forming fractions of galaxies across redshift, and find that the τQ peak at intermediate stellar masses is responsible for a peak (inflection point) in the fraction of green valley central (satellite) galaxies at z ≈ 0.5-0.7.",
keywords = "galaxies: evolution, galaxies: formation",
author = "Wright, {Ruby J.} and Lagos, {Claudia Del P.} and Davies, {Luke J.M.} and Chris Power and Trayford, {James W.} and {Ivy Wong}, O.",
year = "2019",
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Quenching time-scales of galaxies in the eagle simulations. / Wright, Ruby J.; Lagos, Claudia Del P.; Davies, Luke J.M.; Power, Chris; Trayford, James W.; Ivy Wong, O.

In: Monthly Notices of the Royal Astronomical Society, Vol. 487, No. 3, 01.01.2019, p. 3740-3758.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Quenching time-scales of galaxies in the eagle simulations

AU - Wright, Ruby J.

AU - Lagos, Claudia Del P.

AU - Davies, Luke J.M.

AU - Power, Chris

AU - Trayford, James W.

AU - Ivy Wong, O.

PY - 2019/1/1

Y1 - 2019/1/1

N2 - We use the eagle simulations to study the connection between the quenching time-scale, τQ, and the physical mechanisms that transform star-forming galaxies into passive galaxies. By quantifying τQ in two complementary ways-as the time over which (i) galaxies traverse the green valley on the colour-mass diagram, or (ii) leave the main sequence of star formation and subsequently arrive on the passive cloud in specific star formation rate (SSFR)-mass space-we find that the τQ distribution of high-mass centrals, low-mass centrals, and satellites are divergent. In the low stellar mass regime where M <109.6 M·, centrals exhibit systematically longer quenching time-scales than satellites (≈4 Gyr compared to ≈2 Gyr). Satellites with low stellar mass relative to their halo mass cause this disparity, with ram pressure stripping quenching these galaxies rapidly. Low-mass centrals are quenched as a result of stellar feedback, associated with long τQ 3 Gyr. At intermediate stellar masses where $109.7<M☆ <1010.3M⊙, τQ are the longest for both centrals and satellites, particularly for galaxies with higher gas fractions. At M☆1010.3M⊙, galaxy merger counts and black hole activity increase steeply for all galaxies. Quenching time-scales for centrals and satellites decrease with stellar mass in this regime to τQ2 Gyr. In anticipation of new intermediate redshift observational galaxy surveys, we analyse the passive and star-forming fractions of galaxies across redshift, and find that the τQ peak at intermediate stellar masses is responsible for a peak (inflection point) in the fraction of green valley central (satellite) galaxies at z ≈ 0.5-0.7.

AB - We use the eagle simulations to study the connection between the quenching time-scale, τQ, and the physical mechanisms that transform star-forming galaxies into passive galaxies. By quantifying τQ in two complementary ways-as the time over which (i) galaxies traverse the green valley on the colour-mass diagram, or (ii) leave the main sequence of star formation and subsequently arrive on the passive cloud in specific star formation rate (SSFR)-mass space-we find that the τQ distribution of high-mass centrals, low-mass centrals, and satellites are divergent. In the low stellar mass regime where M <109.6 M·, centrals exhibit systematically longer quenching time-scales than satellites (≈4 Gyr compared to ≈2 Gyr). Satellites with low stellar mass relative to their halo mass cause this disparity, with ram pressure stripping quenching these galaxies rapidly. Low-mass centrals are quenched as a result of stellar feedback, associated with long τQ 3 Gyr. At intermediate stellar masses where $109.7<M☆ <1010.3M⊙, τQ are the longest for both centrals and satellites, particularly for galaxies with higher gas fractions. At M☆1010.3M⊙, galaxy merger counts and black hole activity increase steeply for all galaxies. Quenching time-scales for centrals and satellites decrease with stellar mass in this regime to τQ2 Gyr. In anticipation of new intermediate redshift observational galaxy surveys, we analyse the passive and star-forming fractions of galaxies across redshift, and find that the τQ peak at intermediate stellar masses is responsible for a peak (inflection point) in the fraction of green valley central (satellite) galaxies at z ≈ 0.5-0.7.

KW - galaxies: evolution

KW - galaxies: formation

UR - http://www.scopus.com/inward/record.url?scp=85070081722&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz1410

DO - 10.1093/mnras/stz1410

M3 - Article

VL - 487

SP - 3740

EP - 3758

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -