The VLA-COSMOS 3 GHz Large Project: Evolution of specific star formation rates out to $zsim5$. (arXiv:2006.13937v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Leslie_S/0/1/0/all/0/1">Sarah Leslie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schinnerer_E/0/1/0/all/0/1">Eva Schinnerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_D/0/1/0/all/0/1">Daizhong Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magnelli_B/0/1/0/all/0/1">Benjamin Magnelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Algera_H/0/1/0/all/0/1">Hiddo Algera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karim_A/0/1/0/all/0/1">Alexander Karim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davidzon_I/0/1/0/all/0/1">Iary Davidzon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gozaliasl_G/0/1/0/all/0/1">Ghassem Gozaliasl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_Andrade_E/0/1/0/all/0/1">Eric F. Jiménez-Andrade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lang_P/0/1/0/all/0/1">Philipp Lang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sargent_M/0/1/0/all/0/1">Mark Sargent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Novak_M/0/1/0/all/0/1">Mladen Novak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Groves_B/0/1/0/all/0/1">Brent Groves</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smolcic_V/0/1/0/all/0/1">Vernesa Smolčić</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamorani_G/0/1/0/all/0/1">Giovanni Zamorani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vaccari_M/0/1/0/all/0/1">Mattia Vaccari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battisti_A/0/1/0/all/0/1">Andrew Battisti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vardoulaki_E/0/1/0/all/0/1">Eleni Vardoulaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peng_Y/0/1/0/all/0/1">Yingjie Peng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kartaltepe_J/0/1/0/all/0/1">Jeyhan Kartaltepe</a>
We provide a coherent, uniform measurement of the evolution of the
logarithmic star formation rate (SFR) – stellar mass ($M_*$) relation, called
the main sequence of star-forming galaxies (MS), for galaxies out to $zsim5$.
We measure the MS using mean stacks of 3 GHz radio continuum images to derive
average SFRs for $sim$200,000 mass-selected galaxies at $z>0.3$ in the COSMOS
field. We describe the MS relation adopting a new model that incorporates a
linear relation at low stellar mass (log($M_*$/M$_odot$)$<$10) and a
flattening at high stellar mass that becomes more prominent at low redshift
($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 ($M_* = 1 – 4 times
10^{10}mathrm{M}_odot$) that contributes the most to the overall SFR density.
This characteristic mass increases with redshift, at least to $zsim2.5$. 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 $zsim0.75$. 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.
We provide a coherent, uniform measurement of the evolution of the
logarithmic star formation rate (SFR) – stellar mass ($M_*$) relation, called
the main sequence of star-forming galaxies (MS), for galaxies out to $zsim5$.
We measure the MS using mean stacks of 3 GHz radio continuum images to derive
average SFRs for $sim$200,000 mass-selected galaxies at $z>0.3$ in the COSMOS
field. We describe the MS relation adopting a new model that incorporates a
linear relation at low stellar mass (log($M_*$/M$_odot$)$<$10) and a
flattening at high stellar mass that becomes more prominent at low redshift
($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 ($M_* = 1 – 4 times
10^{10}mathrm{M}_odot$) that contributes the most to the overall SFR density.
This characteristic mass increases with redshift, at least to $zsim2.5$. 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 $zsim0.75$. 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.
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