Physical properties and evolution of (Sub-)millimeter selected galaxies in the galaxy formation simulation Shark. (arXiv:2007.09853v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lagos_C/0/1/0/all/0/1">Claudia del P. Lagos</a> (1,2,3), <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:+Robotham_A/0/1/0/all/0/1">Aaron S.G. Robotham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Obreschkow_D/0/1/0/all/0/1">Danail Obreschkow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_F/0/1/0/all/0/1">Francesco Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fujimoto_S/0/1/0/all/0/1">Seiji Fujimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magdis_G/0/1/0/all/0/1">Georgios E. Magdis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tobar_R/0/1/0/all/0/1">Rodrigo Tobar</a> (1: ICRAR/UWA, 2: ASTRO 3D, 3: Cosmic Dawn Center)
We thoroughly explore the properties of (sub)-millimeter (mm) selected
galaxies (SMGs) in the Shark semi-analytic model of galaxy formation. Compared
to observations, the predicted number counts at wavelengths (lambda) 0.6-2mm
and redshift distributions at 0.1-2mm, agree well. At the bright end (>1mJy),
Shark galaxies are a mix of mergers and disk instabilities. These galaxies
display a stacked FUV-to-FIR spectrum that agrees well with observations. We
predict that current optical/NIR surveys are deep enough to detect bright
(>1mJy) lambda=0.85-2mm-selected galaxies at z<5, but too shallow to detect
counterparts at higher redshift. A JWST 10,000s survey should detect all
counterparts for galaxies with $S_{rm 0.85mm}>0.01$mJy. We predict SMG’s disks
contribute significantly (negligibly) to the rest-frame UV (IR). We investigate
the 0<z<6 evolution of the intrinsic properties of >1mJy
lambda=0.85-2mm-selected galaxies finding their: (i) stellar masses are
$>10^{10.2}M_{odot}$, with the 2mm ones tracing the most massive galaxies in
Shark ($>10^{11}M_{odot}$); (ii) average specific star formation rates (SFR)
are mildly (~3-10x) above the main sequence (MS); (iii) host halo masses are
$>10^{12.3}M_{odot}$, with the 2mm galaxies tracing the most massive halos
(proto-clusters); (iv) SMGs have lower dust masses ($sim 10^{8}M_{odot}$),
higher dust temperatures (~40-45K) and higher rest-frame V-band attenuation
(>1.5) than MS galaxies; (v) sizes decrease with redshift, from 4kpc at z=1 to
1kpc at z=4; (vi) the Carbon Monoxide spectral line energy distributions of
$S_{rm 0.85mm}>1$mJy sources peak at 4->3. Finally, we study the contribution
of SMGs to the molecular gas and cosmic SFR density (CSFRD) at 0<z<10, finding
that >1mJy sources make a negligible contribution at z>3 and z>5, respectively,
suggesting current observations have unveiled the majority of the star
formation at 0<z<10.
We thoroughly explore the properties of (sub)-millimeter (mm) selected
galaxies (SMGs) in the Shark semi-analytic model of galaxy formation. Compared
to observations, the predicted number counts at wavelengths (lambda) 0.6-2mm
and redshift distributions at 0.1-2mm, agree well. At the bright end (>1mJy),
Shark galaxies are a mix of mergers and disk instabilities. These galaxies
display a stacked FUV-to-FIR spectrum that agrees well with observations. We
predict that current optical/NIR surveys are deep enough to detect bright
(>1mJy) lambda=0.85-2mm-selected galaxies at z<5, but too shallow to detect
counterparts at higher redshift. A JWST 10,000s survey should detect all
counterparts for galaxies with $S_{rm 0.85mm}>0.01$mJy. We predict SMG’s disks
contribute significantly (negligibly) to the rest-frame UV (IR). We investigate
the 0<z<6 evolution of the intrinsic properties of >1mJy
lambda=0.85-2mm-selected galaxies finding their: (i) stellar masses are
$>10^{10.2}M_{odot}$, with the 2mm ones tracing the most massive galaxies in
Shark ($>10^{11}M_{odot}$); (ii) average specific star formation rates (SFR)
are mildly (~3-10x) above the main sequence (MS); (iii) host halo masses are
$>10^{12.3}M_{odot}$, with the 2mm galaxies tracing the most massive halos
(proto-clusters); (iv) SMGs have lower dust masses ($sim 10^{8}M_{odot}$),
higher dust temperatures (~40-45K) and higher rest-frame V-band attenuation
(>1.5) than MS galaxies; (v) sizes decrease with redshift, from 4kpc at z=1 to
1kpc at z=4; (vi) the Carbon Monoxide spectral line energy distributions of
$S_{rm 0.85mm}>1$mJy sources peak at 4->3. Finally, we study the contribution
of SMGs to the molecular gas and cosmic SFR density (CSFRD) at 0<z<10, finding
that >1mJy sources make a negligible contribution at z>3 and z>5, respectively,
suggesting current observations have unveiled the majority of the star
formation at 0<z<10.
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