ALMA 200-parsec Resolution Imaging of Smooth Cold Dusty Disks in Typical $z sim 3$ Star-Forming Galaxies. (arXiv:1904.04507v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rujopakarn_W/0/1/0/all/0/1">W. Rujopakarn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daddi_E/0/1/0/all/0/1">E. Daddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rieke_G/0/1/0/all/0/1">G. H. Rieke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puglisi_A/0/1/0/all/0/1">A. Puglisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schramm_M/0/1/0/all/0/1">M. Schramm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_Gonzalez_P/0/1/0/all/0/1">P. G. P&#xe9;rez-Gonz&#xe1;lez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magdis_G/0/1/0/all/0/1">G. E. Magdis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alberts_S/0/1/0/all/0/1">S. Alberts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bournaud_F/0/1/0/all/0/1">F. Bournaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elbaz_D/0/1/0/all/0/1">D. Elbaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franco_M/0/1/0/all/0/1">M. Franco</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:+Kawinwanichakij_L/0/1/0/all/0/1">L. Kawinwanichakij</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohno_K/0/1/0/all/0/1">K. Kohno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayanan_D/0/1/0/all/0/1">D. Narayanan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silverman_J/0/1/0/all/0/1">J. D. Silverman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_T/0/1/0/all/0/1">T. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Williams_C/0/1/0/all/0/1">C. C. Williams</a>

We present high-fidelity, 30 milliarcsecond (200-pc) resolution ALMA
rest-frame 240 $mu$m observations of cold dust emission in three typical $z
sim 3$ star-forming galaxies in the Hubble Ultra-Deep Field (HUDF). The cold
dust is distributed within the smooth disk-like central regions of star
formation (SF) $1 – 3$ kpc in diameter, despite their complex and disturbed
rest-frame UV and optical morphologies. No dust substructures or clumps are
seen down to $simeq 1- 3$ $M_odot$yr$^{-1}$ (1$sigma$) per 200-pc beam. No
dust emission is observed at the locations of UV-emitting clumps, which lie
$simeq 2-10$ kpc from the bulk of SF. Clumpy substructures can contribute no
more than $1-8$ % (3$sigma$ upper limits) of the total SF in these galaxies.
The lack of SF substructures in our HUDF galaxies is to be contrasted with the
multiple substructures characteristic of submillimeter-selected galaxies (SMGs)
at the same cosmic epoch, each containing $sim 10-30$ % of their total SF. We
find that individual substructures of SMGs are often as bright in the
far-infrared as (or in some cases brighter than) our HUDF galaxies, suggesting
that these SMGs originate from a class of disruptive event involving multiple
objects at the scale of our HUDF galaxies. The scale of the disruptive event
found in our HUDF galaxies, characterized by the lack of star-forming
substructures at our resolution and sensitivity, could be less violent, e.g.,
gas-rich disk instability or minor mergers.

We present high-fidelity, 30 milliarcsecond (200-pc) resolution ALMA
rest-frame 240 $mu$m observations of cold dust emission in three typical $z
sim 3$ star-forming galaxies in the Hubble Ultra-Deep Field (HUDF). The cold
dust is distributed within the smooth disk-like central regions of star
formation (SF) $1 – 3$ kpc in diameter, despite their complex and disturbed
rest-frame UV and optical morphologies. No dust substructures or clumps are
seen down to $simeq 1- 3$ $M_odot$yr$^{-1}$ (1$sigma$) per 200-pc beam. No
dust emission is observed at the locations of UV-emitting clumps, which lie
$simeq 2-10$ kpc from the bulk of SF. Clumpy substructures can contribute no
more than $1-8$ % (3$sigma$ upper limits) of the total SF in these galaxies.
The lack of SF substructures in our HUDF galaxies is to be contrasted with the
multiple substructures characteristic of submillimeter-selected galaxies (SMGs)
at the same cosmic epoch, each containing $sim 10-30$ % of their total SF. We
find that individual substructures of SMGs are often as bright in the
far-infrared as (or in some cases brighter than) our HUDF galaxies, suggesting
that these SMGs originate from a class of disruptive event involving multiple
objects at the scale of our HUDF galaxies. The scale of the disruptive event
found in our HUDF galaxies, characterized by the lack of star-forming
substructures at our resolution and sensitivity, could be less violent, e.g.,
gas-rich disk instability or minor mergers.

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