The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5
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The VLA-COSMOS 3 GHz Large Project : Evolution of Specific Star Formation Rates out to z ∼ 5. / Leslie, Sarah K.; Schinnerer, Eva; Liu, Daizhong; Magnelli, Benjamin; Algera, Hiddo; Karim, Alexander; Davidzon, Iary; Gozaliasl, Ghassem; Jiménez-Andrade, Eric F.; Lang, Philipp; Sargent, Mark T.; Novak, Mladen; Groves, Brent; Smolčić, Vernesa; Zamorani, Giovanni; Vaccari, Mattia; Battisti, Andrew; Vardoulaki, Eleni; Peng, Yingjie; Kartaltepe, Jeyhan.
In: Astrophysical Journal, Vol. 899, No. 1, 58, 01.08.2020.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - The VLA-COSMOS 3 GHz Large Project
T2 - Evolution of Specific Star Formation Rates out to z ∼ 5
AU - Leslie, Sarah K.
AU - Schinnerer, Eva
AU - Liu, Daizhong
AU - Magnelli, Benjamin
AU - Algera, Hiddo
AU - Karim, Alexander
AU - Davidzon, Iary
AU - Gozaliasl, Ghassem
AU - Jiménez-Andrade, Eric F.
AU - Lang, Philipp
AU - Sargent, Mark T.
AU - Novak, Mladen
AU - Groves, Brent
AU - Smolčić, Vernesa
AU - Zamorani, Giovanni
AU - Vaccari, Mattia
AU - Battisti, Andrew
AU - Vardoulaki, Eleni
AU - Peng, Yingjie
AU - Kartaltepe, Jeyhan
PY - 2020/8/1
Y1 - 2020/8/1
N2 - We provide a coherent, uniform measurement of the evolution of the logarithmic star formation rate (SFR)-stellar mass (M*) relation, called the main sequence (MS) of star-forming galaxies , for star-forming and all galaxies out to $z\sim 5$ . We measure the MS using mean stacks of 3 GHz radio-continuum images to derive average SFRs for ∼ 200,000 mass-selected galaxies at z > 0.3 in the COSMOS field. We describe the MS relation by adopting a new model that incorporates a linear relation at low stellar mass (log(M*/M⊙) <10) and a flattening at high stellar mass that becomes more prominent at low redshift (z <1.5). We find that the SFR density peaks at 1.5 <z <2, and at each epoch there is a characteristic stellar mass (M* = 1-4 × 1010M⊙) that contributes the most to the overall SFR density. This characteristic mass increases with redshift, at least to z ∼ 2.5. We find no significant evidence for variations in the MS relation for galaxies in different environments traced by the galaxy number density at 0.3 <z <3, nor for galaxies in X-ray groups at z ∼ 0.75. We confirm that massive bulge-dominated galaxies have lower SFRs than disk-dominated galaxies at a fixed stellar mass at z <1.2. As a consequence, the increase in bulge-dominated galaxies in the local star-forming population leads to a flattening of the MS at high stellar masses. This indicates that "mass quenching" is linked with changes in the morphological composition of galaxies at a fixed stellar mass.
AB - We provide a coherent, uniform measurement of the evolution of the logarithmic star formation rate (SFR)-stellar mass (M*) relation, called the main sequence (MS) of star-forming galaxies , for star-forming and all galaxies out to $z\sim 5$ . We measure the MS using mean stacks of 3 GHz radio-continuum images to derive average SFRs for ∼ 200,000 mass-selected galaxies at z > 0.3 in the COSMOS field. We describe the MS relation by adopting a new model that incorporates a linear relation at low stellar mass (log(M*/M⊙) <10) and a flattening at high stellar mass that becomes more prominent at low redshift (z <1.5). We find that the SFR density peaks at 1.5 <z <2, and at each epoch there is a characteristic stellar mass (M* = 1-4 × 1010M⊙) that contributes the most to the overall SFR density. This characteristic mass increases with redshift, at least to z ∼ 2.5. We find no significant evidence for variations in the MS relation for galaxies in different environments traced by the galaxy number density at 0.3 <z <3, nor for galaxies in X-ray groups at z ∼ 0.75. We confirm that massive bulge-dominated galaxies have lower SFRs than disk-dominated galaxies at a fixed stellar mass at z <1.2. As a consequence, the increase in bulge-dominated galaxies in the local star-forming population leads to a flattening of the MS at high stellar masses. This indicates that "mass quenching" is linked with changes in the morphological composition of galaxies at a fixed stellar mass.
KW - Galaxy evolution
KW - Galaxy quenching
KW - Galaxy bulges
KW - Galaxy environments
KW - Radio continuum emission
KW - Extragalactic radio sources
KW - 594
KW - 2040
KW - 578
KW - 2029
KW - 1340
KW - 508
U2 - 10.3847/1538-4357/aba044
DO - 10.3847/1538-4357/aba044
M3 - Journal article
VL - 899
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 58
ER -
ID: 248148640