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Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
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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 -