An ALMA survey of the SCUBA-2 CLS UDS field: Physical properties of 707 Sub-millimetre Galaxies. (arXiv:1910.07524v1 [astro-ph.GA])

An ALMA survey of the SCUBA-2 CLS UDS field: Physical properties of 707 Sub-millimetre Galaxies. (arXiv:1910.07524v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dudzeviciute_U/0/1/0/all/0/1">U. Dudzevi&#x10d;i&#x16b;t&#x117;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smail_I/0/1/0/all/0/1">Ian Smail</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Swinbank_A/0/1/0/all/0/1">A. M. Swinbank</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stach_S/0/1/0/all/0/1">S. M. Stach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almaini_O/0/1/0/all/0/1">O. Almaini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cunha_E/0/1/0/all/0/1">E. da Cunha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+An_F/0/1/0/all/0/1">Fang Xia An</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arumugam_V/0/1/0/all/0/1">V. Arumugam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Birkin_J/0/1/0/all/0/1">J. Birkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blain_A/0/1/0/all/0/1">A. W. Blain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chapman_S/0/1/0/all/0/1">S. C. Chapman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C.-C. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conselice_C/0/1/0/all/0/1">C. J. Conselice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coppin_K/0/1/0/all/0/1">K. E. K. Coppin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunlop_J/0/1/0/all/0/1">J. S. Dunlop</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Farrah_D/0/1/0/all/0/1">D. Farrah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Geach_J/0/1/0/all/0/1">J. E. Geach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gullberg_B/0/1/0/all/0/1">B. Gullberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartley_W/0/1/0/all/0/1">W. G. Hartley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hodge_J/0/1/0/all/0/1">J. A. Hodge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ivison_R/0/1/0/all/0/1">R. J. Ivison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maltby_D/0/1/0/all/0/1">D. T. Maltby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scott_D/0/1/0/all/0/1">D. Scott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simpson_C/0/1/0/all/0/1">C. J. Simpson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simpson_J/0/1/0/all/0/1">J. M. Simpson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomson_A/0/1/0/all/0/1">A. P. Thomson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walter_F/0/1/0/all/0/1">F. Walter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wardlow_J/0/1/0/all/0/1">J. L. Wardlow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weiss_A/0/1/0/all/0/1">A. Weiss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Werf_P/0/1/0/all/0/1">P. van der Werf</a>

We analyse the physical properties of a large, homogeneously selected sample
of ALMA-located sub-mm galaxies (SMGs) detected in the SCUBA-2 CLS 850-$mu$m
map of the UKIDSS/UDS field. This survey, AS2UDS, identified 707 SMGs across
the ~1 sq.deg. field, including ~17 per cent which are undetected in the
optical/near-infrared to $K$>~25.7 mag. We interpret the UV-to-radio data using
a physically motivated model, MAGPHYS and determine a median photometric
redshift of z=2.61+-0.08, with a 68th percentile range of z=1.8-3.4 and just ~6
per cent at z>4. The redshift distribution is well fit by a model combining
evolution of the gas fraction in halos with the growth of halo mass past a
threshold of ~4×10$^{12}$M$_odot$, thus SMGs may represent the highly
efficient collapse of gas-rich massive halos. Our survey provides a sample of
the most massive, dusty galaxies at z>~1, with median dust and stellar masses
of $M_d$=(6.8+-0.3)x10$^{8}$M$_odot$ (thus, gas masses of ~10$^{11}$M$_odot$)
and $M_ast=$(1.26+-0.05)x10$^{11}$M$_odot$. These galaxies have gas fractions
of $f_{gas}=$0.41+-0.02 with depletion timescales of ~150Myr. The gas mass
function evolution at high masses is consistent with constraints at lower
masses from blind CO-surveys, with an increase to z~2-3 and then a decline at
higher redshifts. The space density and masses of SMGs suggests that almost all
galaxies with $M_ast$>~2×10$^{11}$M$_odot$ have passed through an SMG-like
phase. We find no evolution in dust temperature at a constant far-infrared
luminosity across z~1.5-4. We show that SMGs appear to behave as simple
homologous systems in the far-infrared, having properties consistent with a
centrally illuminated starburst. Our study provides strong support for an
evolutionary link between the active, gas-rich SMG population at z>1 and the
formation of massive, bulge-dominated galaxies across the history of the
Universe.

We analyse the physical properties of a large, homogeneously selected sample
of ALMA-located sub-mm galaxies (SMGs) detected in the SCUBA-2 CLS 850-$mu$m
map of the UKIDSS/UDS field. This survey, AS2UDS, identified 707 SMGs across
the ~1 sq.deg. field, including ~17 per cent which are undetected in the
optical/near-infrared to $K$>~25.7 mag. We interpret the UV-to-radio data using
a physically motivated model, MAGPHYS and determine a median photometric
redshift of z=2.61+-0.08, with a 68th percentile range of z=1.8-3.4 and just ~6
per cent at z>4. The redshift distribution is well fit by a model combining
evolution of the gas fraction in halos with the growth of halo mass past a
threshold of ~4×10$^{12}$M$_odot$, thus SMGs may represent the highly
efficient collapse of gas-rich massive halos. Our survey provides a sample of
the most massive, dusty galaxies at z>~1, with median dust and stellar masses
of $M_d$=(6.8+-0.3)x10$^{8}$M$_odot$ (thus, gas masses of ~10$^{11}$M$_odot$)
and $M_ast=$(1.26+-0.05)x10$^{11}$M$_odot$. These galaxies have gas fractions
of $f_{gas}=$0.41+-0.02 with depletion timescales of ~150Myr. The gas mass
function evolution at high masses is consistent with constraints at lower
masses from blind CO-surveys, with an increase to z~2-3 and then a decline at
higher redshifts. The space density and masses of SMGs suggests that almost all
galaxies with $M_ast$>~2×10$^{11}$M$_odot$ have passed through an SMG-like
phase. We find no evolution in dust temperature at a constant far-infrared
luminosity across z~1.5-4. We show that SMGs appear to behave as simple
homologous systems in the far-infrared, having properties consistent with a
centrally illuminated starburst. Our study provides strong support for an
evolutionary link between the active, gas-rich SMG population at z>1 and the
formation of massive, bulge-dominated galaxies across the history of the
Universe.

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