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Quenching or Bursting: the Role of Stellar Mass, Environment, and Specific Star Formation Rate to z ~ 1

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Quenching or Bursting : the Role of Stellar Mass, Environment, and Specific Star Formation Rate to z ~ 1. / Darvish, Behnam; Martin, Christopher; Mobasher, Bahram; Scoville, Nicholas; Sobral, David.

In: The Astrophysical Journal, Vol. 853, 155, 01.02.2018.

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Darvish, Behnam ; Martin, Christopher ; Mobasher, Bahram ; Scoville, Nicholas ; Sobral, David. / Quenching or Bursting : the Role of Stellar Mass, Environment, and Specific Star Formation Rate to z ~ 1. In: The Astrophysical Journal. 2018 ; Vol. 853.

Bibtex

@article{d174b7ae71044f9dabb2d9966f583a43,
title = "Quenching or Bursting: the Role of Stellar Mass, Environment, and Specific Star Formation Rate to z ~ 1",
abstract = "Using a novel approach, we study the quenching and bursting of galaxies as a function of stellar mass (M∗), local environment (Σ), and specific star-formation rate (sSFR) using a large spectroscopic sample of ∼ 123,000 GALEX/SDSS and ∼ 420 GALEX/COSMOS/LEGA-C galaxies to z ∼ 1. We show that out to z ∼ 1 and at fixed sSFR and local density, on average, less massive galaxies are quenching, whereas more massive systems are bursting, with a quenching/bursting transition at log(M∗/M⊙) ∼ 10.5-11 and likely a short quenching/bursting timescale (ﰁ 300 Myr). We find that much of the bursting of star-formation happens in massive (log(M∗/M⊙) ﰀ 11), high sSFR galaxies (log(sSFR/Gyr−1) ﰀ -2), particularly those in the field (log(Σ/Mpc−2) ﰁ 0; and among group galaxies, satellites more than centrals). Most of the quenching of star-formation happens in low-mass (log(M∗/M⊙) ﰁ 9), low sSFR galaxies (log(sSFR/Gyr−1) ﰁ -2), in particular those located in dense environments (log(Σ/Mpc−2) ﰀ 1), indicating the combined effects of M∗ and Σ in quenching/bursting of galaxies since z ∼ 1. However, we find that stellar mass has stronger effects than environment on recent quenching/bursting of galaxies to z ∼ 1. At any given M∗, sSFR, and environment, centrals are quenchier (quenching faster) than satellites in an average sense. We also find evidence for the strength of mass and environmental quenching being stronger at higher redshift. Our preliminary results have potential implications for the physics of quenching/bursting in galaxies across cosmic time.",
keywords = "galaxies: evolution, galaxies: groups: general, galaxies: high-redshift, galaxies: star formation, large-scale structure of universe , ultraviolet: galaxies",
author = "Behnam Darvish and Christopher Martin and Bahram Mobasher and Nicholas Scoville and David Sobral",
year = "2018",
month = feb,
day = "1",
doi = "10.3847/1538-4357/aaa5a4",
language = "English",
volume = "853",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",

}

RIS

TY - JOUR

T1 - Quenching or Bursting

T2 - the Role of Stellar Mass, Environment, and Specific Star Formation Rate to z ~ 1

AU - Darvish, Behnam

AU - Martin, Christopher

AU - Mobasher, Bahram

AU - Scoville, Nicholas

AU - Sobral, David

PY - 2018/2/1

Y1 - 2018/2/1

N2 - Using a novel approach, we study the quenching and bursting of galaxies as a function of stellar mass (M∗), local environment (Σ), and specific star-formation rate (sSFR) using a large spectroscopic sample of ∼ 123,000 GALEX/SDSS and ∼ 420 GALEX/COSMOS/LEGA-C galaxies to z ∼ 1. We show that out to z ∼ 1 and at fixed sSFR and local density, on average, less massive galaxies are quenching, whereas more massive systems are bursting, with a quenching/bursting transition at log(M∗/M⊙) ∼ 10.5-11 and likely a short quenching/bursting timescale (ﰁ 300 Myr). We find that much of the bursting of star-formation happens in massive (log(M∗/M⊙) ﰀ 11), high sSFR galaxies (log(sSFR/Gyr−1) ﰀ -2), particularly those in the field (log(Σ/Mpc−2) ﰁ 0; and among group galaxies, satellites more than centrals). Most of the quenching of star-formation happens in low-mass (log(M∗/M⊙) ﰁ 9), low sSFR galaxies (log(sSFR/Gyr−1) ﰁ -2), in particular those located in dense environments (log(Σ/Mpc−2) ﰀ 1), indicating the combined effects of M∗ and Σ in quenching/bursting of galaxies since z ∼ 1. However, we find that stellar mass has stronger effects than environment on recent quenching/bursting of galaxies to z ∼ 1. At any given M∗, sSFR, and environment, centrals are quenchier (quenching faster) than satellites in an average sense. We also find evidence for the strength of mass and environmental quenching being stronger at higher redshift. Our preliminary results have potential implications for the physics of quenching/bursting in galaxies across cosmic time.

AB - Using a novel approach, we study the quenching and bursting of galaxies as a function of stellar mass (M∗), local environment (Σ), and specific star-formation rate (sSFR) using a large spectroscopic sample of ∼ 123,000 GALEX/SDSS and ∼ 420 GALEX/COSMOS/LEGA-C galaxies to z ∼ 1. We show that out to z ∼ 1 and at fixed sSFR and local density, on average, less massive galaxies are quenching, whereas more massive systems are bursting, with a quenching/bursting transition at log(M∗/M⊙) ∼ 10.5-11 and likely a short quenching/bursting timescale (ﰁ 300 Myr). We find that much of the bursting of star-formation happens in massive (log(M∗/M⊙) ﰀ 11), high sSFR galaxies (log(sSFR/Gyr−1) ﰀ -2), particularly those in the field (log(Σ/Mpc−2) ﰁ 0; and among group galaxies, satellites more than centrals). Most of the quenching of star-formation happens in low-mass (log(M∗/M⊙) ﰁ 9), low sSFR galaxies (log(sSFR/Gyr−1) ﰁ -2), in particular those located in dense environments (log(Σ/Mpc−2) ﰀ 1), indicating the combined effects of M∗ and Σ in quenching/bursting of galaxies since z ∼ 1. However, we find that stellar mass has stronger effects than environment on recent quenching/bursting of galaxies to z ∼ 1. At any given M∗, sSFR, and environment, centrals are quenchier (quenching faster) than satellites in an average sense. We also find evidence for the strength of mass and environmental quenching being stronger at higher redshift. Our preliminary results have potential implications for the physics of quenching/bursting in galaxies across cosmic time.

KW - galaxies: evolution

KW - galaxies: groups: general

KW - galaxies: high-redshift

KW - galaxies: star formation

KW - large-scale structure of universe

KW - ultraviolet: galaxies

U2 - 10.3847/1538-4357/aaa5a4

DO - 10.3847/1538-4357/aaa5a4

M3 - Journal article

VL - 853

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

M1 - 155

ER -