ALMA twenty-six arcmin$^2$ survey of GOODS-S at one-millimeter (ASAGAO): Near-infrared-dark faint ALMA sources. (arXiv:1903.02744v1 [astro-ph.GA])

ALMA twenty-six arcmin$^2$ survey of GOODS-S at one-millimeter (ASAGAO): Near-infrared-dark faint ALMA sources. (arXiv:1903.02744v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yamaguchi_Y/0/1/0/all/0/1">Yuki Yamaguchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohno_K/0/1/0/all/0/1">Kotaro Kohno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hatsukade_B/0/1/0/all/0/1">Bunyo Hatsukade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_T/0/1/0/all/0/1">Tao Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshimura_Y/0/1/0/all/0/1">Yuki Yoshimura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ao_Y/0/1/0/all/0/1">Yiping Ao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caputi_K/0/1/0/all/0/1">Karina I. Caputi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunlop_J/0/1/0/all/0/1">James S. Dunlop</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Egami_E/0/1/0/all/0/1">Eiichi Egami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Espada_D/0/1/0/all/0/1">Daniel Espada</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:+Hayatsu_N/0/1/0/all/0/1">Natsuki H. Hayatsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ivison_R/0/1/0/all/0/1">Rob J. Ivison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kodama_T/0/1/0/all/0/1">Tadayuki Kodama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kusakabe_H/0/1/0/all/0/1">Haruka Kusakabe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagao_T/0/1/0/all/0/1">Tohru Nagao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ouchi_M/0/1/0/all/0/1">Masami Ouchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rujopakarn_W/0/1/0/all/0/1">Wiphu Rujopakarn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tadaki_K/0/1/0/all/0/1">Ken-ichi Tadaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tamura_Y/0/1/0/all/0/1">Yoichi Tamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ueda_Y/0/1/0/all/0/1">Yoshihiro Ueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Umehata_H/0/1/0/all/0/1">Hideki Umehata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_W/0/1/0/all/0/1">Wei-Hao Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yun_M/0/1/0/all/0/1">Min S. Yun</a>

We report detections of two 1.2 mm continuum sources ($S_mathrm{1.2mm}$ ~
0.6 mJy) without any counterparts in the deep $H$- and/or $K$-band image (i.e.,
$K$-band magnitude $gtrsim$ 26 mag). These near-infrared-dark faint millimeter
sources are uncovered by ASAGAO, a deep and wide-field ($simeq$ 26 arcmin$^2$)
Atacama Large Millimeter/submillimeter Array (ALMA) 1.2 mm survey. One has a
red IRAC (3.6 and 4.5 $mu$m) counterpart, and the other has been independently
detected at 850 and 870 $mu$m using SCUBA2 and ALMA Band 7, respectively.
Their optical to radio spectral energy distributions indicate that they can lie
at $z gtrsim$ 3-5 and can be in the early phase of massive galaxy formation.
Their contribution to the cosmic star formation rate density is estimated to be
~ 1 $times$ 10$^{-3}$ $M_odot$ yr$^{-1}$ Mpc$^{-3}$ if they lie somewhere in
the redshift range of $z$ ~ 3-5. This value can be consistent with, or greater
than that of bright submillimeter galaxies ($S_mathrm{870mu m}>$ 4.2 mJy) at
$z$ ~ 3-5. We also uncover 3 more candidates near-infrared-dark faint ALMA
sources without any counterparts ($S_mathrm{1.2mm}$ ~ 0.45-0.86 mJy). These
results show that an unbiased ALMA survey can reveal the dust-obscured star
formation activities, which were missed in previous deep optical/near-infrared
surveys.

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