The star-forming main sequence and the contribution of dust-obscured star formation since $zsim4$ from the FUV+IR luminosity functions. (arXiv:2008.06514v2 [astro-ph.GA] UPDATED)

The star-forming main sequence and the contribution of dust-obscured star formation since $zsim4$ from the FUV+IR luminosity functions. (arXiv:2008.06514v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_Puebla_A/0/1/0/all/0/1">Aldo Rodriguez-Puebla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_Reese_V/0/1/0/all/0/1">Vladimir Avila-Reese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cano_Diaz_M/0/1/0/all/0/1">Mariana Cano-Diaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faber_S/0/1/0/all/0/1">S. M. Faber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Primack_J/0/1/0/all/0/1">Joel R. Primack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franco_J/0/1/0/all/0/1">Jose Franco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aretxaga_I/0/1/0/all/0/1">I. Aretxaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santiago_Mayoral_E/0/1/0/all/0/1">Eder Santiago-Mayoral</a>

An analytical approach is proposed to study the evolution of the star-forming
galaxy (SFG) main sequence (MS) and the fraction of dust-obscured SF up to
$zsim4$. Far-ultraviolet (FUV) and infrared (IR) star formation rates, SFRs,
are described as conditional probability functions of $M_{ast}$. We convolve
them with the galaxy stellar mass function (GSMF) of SFGs to derive the FUV and
IR LFs. The 2 SF modes formalism is used to describe starburst galaxies. By
fitting observed FUV and IR LFs, the parametrization of SFR$_{rm
FUV}-M_{ast}$ and SFR$_{rm IR}-M_{ast}$ are constrained. Our derived
SFR$_{rm FUV+IR}-M_{ast}$ reproduces the evolution of the MS as compared to
other observational inferences. At any redshift, we find that the sSFR$_{rm
FUV+IR}-M_{ast}$ relation for MS SFGs approaches to a power law at the
high-mass end. At lower masses, it bends and eventually the slope sign changes
from negative to positive at very low masses. At $zsim0$, this change of sign
is at $M_{ast}sim5times10^{8}{rm M}_{odot}$ close to dust-obscured SF
regime, $M_{ast}sim6times10^{8}{rm M}_{odot}$. The slope sign change is
related to the knee of the FUV LF. Our derived dust-obscured fractions agree
with previous determinations at $0leq zleq2.5$. Dust-obscured fractions
depend strongly on mass with almost no dependence with redshift at
$zgtrsim1.2$. At $zlesssim0.75$ high-mass galaxies become more “transparent”
compared to their high redshift counterparts. On the opposite, low- and
intermediate-mass galaxies have become more obscured by dust. The joint
evolution of the GSMF and the FUV and IR LFs is a promising approach to study
mass growth and dust formation/destruction mechanisms.

An analytical approach is proposed to study the evolution of the star-forming
galaxy (SFG) main sequence (MS) and the fraction of dust-obscured SF up to
$zsim4$. Far-ultraviolet (FUV) and infrared (IR) star formation rates, SFRs,
are described as conditional probability functions of $M_{ast}$. We convolve
them with the galaxy stellar mass function (GSMF) of SFGs to derive the FUV and
IR LFs. The 2 SF modes formalism is used to describe starburst galaxies. By
fitting observed FUV and IR LFs, the parametrization of SFR$_{rm
FUV}-M_{ast}$ and SFR$_{rm IR}-M_{ast}$ are constrained. Our derived
SFR$_{rm FUV+IR}-M_{ast}$ reproduces the evolution of the MS as compared to
other observational inferences. At any redshift, we find that the sSFR$_{rm
FUV+IR}-M_{ast}$ relation for MS SFGs approaches to a power law at the
high-mass end. At lower masses, it bends and eventually the slope sign changes
from negative to positive at very low masses. At $zsim0$, this change of sign
is at $M_{ast}sim5times10^{8}{rm M}_{odot}$ close to dust-obscured SF
regime, $M_{ast}sim6times10^{8}{rm M}_{odot}$. The slope sign change is
related to the knee of the FUV LF. Our derived dust-obscured fractions agree
with previous determinations at $0leq zleq2.5$. Dust-obscured fractions
depend strongly on mass with almost no dependence with redshift at
$zgtrsim1.2$. At $zlesssim0.75$ high-mass galaxies become more “transparent”
compared to their high redshift counterparts. On the opposite, low- and
intermediate-mass galaxies have become more obscured by dust. The joint
evolution of the GSMF and the FUV and IR LFs is a promising approach to study
mass growth and dust formation/destruction mechanisms.

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