Spitzer catalog of Herschel-selected ultrared dusty, star-forming galaxies. (arXiv:1908.08043v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ma_J/0/1/0/all/0/1">Jingzhe Ma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cooray_A/0/1/0/all/0/1">Asantha Cooray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nayyeri_H/0/1/0/all/0/1">Hooshang Nayyeri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_A/0/1/0/all/0/1">Arianna Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghotbi_N/0/1/0/all/0/1">Noah Ghotbi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ivison_R/0/1/0/all/0/1">Rob Ivison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oteo_I/0/1/0/all/0/1">Ivan Oteo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duivenvoorden_S/0/1/0/all/0/1">Steven Duivenvoorden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Greenslade_J/0/1/0/all/0/1">Joshua Greenslade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clements_D/0/1/0/all/0/1">David Clements</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wardlow_J/0/1/0/all/0/1">Julie Wardlow</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:+Cunha_E/0/1/0/all/0/1">Elisabete da Cunha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ashby_M/0/1/0/all/0/1">Matthew L. N. Ashby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_Fournon_I/0/1/0/all/0/1">Ismael Perez-Fournon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riechers_D/0/1/0/all/0/1">Dominik Riechers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oliver_S/0/1/0/all/0/1">Seb Oliver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eales_S/0/1/0/all/0/1">Stephen Eales</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Negrello_M/0/1/0/all/0/1">Mattia Negrello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dye_S/0/1/0/all/0/1">Simon Dye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunne_L/0/1/0/all/0/1">Loretta Dunne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Omont_A/0/1/0/all/0/1">Alain Omont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scott_D/0/1/0/all/0/1">Douglas Scott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cox_P/0/1/0/all/0/1">Pierre Cox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serjeant_S/0/1/0/all/0/1">Stephen Serjeant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maddox_S/0/1/0/all/0/1">Steve Maddox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valiante_E/0/1/0/all/0/1">Elisabetta Valiante</a>
The largest Herschel extragalactic surveys, H-ATLAS and HerMES, have selected
a sample of “ultrared” dusty, star-forming galaxies (DSFGs) with rising SPIRE
flux densities ($S_{500} > S_{350} > S_{250}$; so-called “500 $mu$m-risers”)
as an efficient way for identifying DSFGs at higher redshift ($z > 4$). In this
paper, we present a large Spitzer follow-up program of 300 Herschel ultrared
DSFGs. We have obtained high-resolution ALMA, NOEMA, and SMA data for 63 of
them, which allow us to securely identify the Spitzer/IRAC counterparts and
classify them as gravitationally lensed or unlensed. Within the 63 ultrared
sources with high-resolution data, $sim$65% appear to be unlensed, and
$sim$27% are resolved into multiple components. We focus on analyzing the
unlensed sample by directly performing multi-wavelength spectral energy
distribution (SED) modeling to derive their physical properties and compare
with the more numerous $z sim 2$ DSFG population. The ultrared sample has a
median redshift of 3.3, stellar mass of 3.7 $times$ 10$^{11}$ $M_{odot}$,
star formation rate (SFR) of 730 $M_{odot}$yr$^{-1}$, total dust luminosity of
9.0 $times$ 10$^{12}$ $L_{odot}$, dust mass of 2.8 $times$ 10$^9$
$M_{odot}$, and V-band extinction of 4.0, which are all higher than those of
the ALESS DSFGs. Based on the space density, SFR density, and stellar mass
density estimates, we conclude that our ultrared sample cannot account for the
majority of the star-forming progenitors of the massive, quiescent galaxies
found in infrared surveys. Our sample contains the rarer, intrinsically most
dusty, luminous and massive galaxies in the early universe that will help us
understand the physical drivers of extreme star formation.
The largest Herschel extragalactic surveys, H-ATLAS and HerMES, have selected
a sample of “ultrared” dusty, star-forming galaxies (DSFGs) with rising SPIRE
flux densities ($S_{500} > S_{350} > S_{250}$; so-called “500 $mu$m-risers”)
as an efficient way for identifying DSFGs at higher redshift ($z > 4$). In this
paper, we present a large Spitzer follow-up program of 300 Herschel ultrared
DSFGs. We have obtained high-resolution ALMA, NOEMA, and SMA data for 63 of
them, which allow us to securely identify the Spitzer/IRAC counterparts and
classify them as gravitationally lensed or unlensed. Within the 63 ultrared
sources with high-resolution data, $sim$65% appear to be unlensed, and
$sim$27% are resolved into multiple components. We focus on analyzing the
unlensed sample by directly performing multi-wavelength spectral energy
distribution (SED) modeling to derive their physical properties and compare
with the more numerous $z sim 2$ DSFG population. The ultrared sample has a
median redshift of 3.3, stellar mass of 3.7 $times$ 10$^{11}$ $M_{odot}$,
star formation rate (SFR) of 730 $M_{odot}$yr$^{-1}$, total dust luminosity of
9.0 $times$ 10$^{12}$ $L_{odot}$, dust mass of 2.8 $times$ 10$^9$
$M_{odot}$, and V-band extinction of 4.0, which are all higher than those of
the ALESS DSFGs. Based on the space density, SFR density, and stellar mass
density estimates, we conclude that our ultrared sample cannot account for the
majority of the star-forming progenitors of the massive, quiescent galaxies
found in infrared surveys. Our sample contains the rarer, intrinsically most
dusty, luminous and massive galaxies in the early universe that will help us
understand the physical drivers of extreme star formation.
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