An extreme protocluster of luminous dusty starbursts in the early universe

Oteo, I., Ivison, R. J., Dunne, L. ORCID: https://orcid.org/0000-0001-9880-2543, Manilla-Robles, A., Maddox, S. ORCID: https://orcid.org/0000-0001-5549-195X, Lewis, A. J. R., de Zotti, G., Bremer, M., Clements, D. L., Cooray, A., Dannerbauer, H., Eales, S. ORCID: https://orcid.org/0000-0002-7394-426X, Greenslade, J., Omont, A., Perez-Fournón, I., Riechers, D., Scott, D., van der Werf, P., Weiss, A. and Zhang, Z-Y. 2018. An extreme protocluster of luminous dusty starbursts in the early universe. Astrophysical Journal 856 (1) , 72. 10.3847/1538-4357/aaa1f1

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Abstract

We report the identification of an extreme protocluster of galaxies in the early universe whose core (nicknamed Distant Red Core, DRC, because of its very red color in Herschel SPIRE bands) is formed by at least 10 dusty star-forming galaxies (DSFGs), spectroscopically confirmed to lie at ${z}_{mathrm{spec}}=4.002$ via detection of [C i](1–0), 12CO(6–5), 12CO(4–3), 12CO(2–1), and ${{ m{H}}}_{2}{ m{O}}({2}_{11}mbox{--}{2}_{02})$ emission lines with ALMA and ATCA. These DSFGs are distributed over a $260,mathrm{kpc} imes 310,mathrm{kpc}$ region and have a collective obscured star formation rate (SFR) of $sim 6500,{M}_{odot },{mathrm{yr}}^{-1}$, considerably higher than those seen before in any protocluster at $zgtrsim 4$. Most of the star formation is taking place in luminous DSFGs since no Lyα emitters are detected in the protocluster core, apart from a Lyα blob located next to one of the DRC components, extending over $60,mathrm{kpc}$. The total obscured SFR of the protocluster could rise to $mathrm{SFR}sim { m{14,400}},{M}_{odot },{mathrm{yr}}^{-1}$ if all the members of an overdensity of bright DSFGs discovered around DRC in a wide-field Large APEX BOlometer CAmera 870 μm image are part of the same structure. [C i](1–0) emission reveals that DRC has a total molecular gas mass of at least ${M}_{{{ m{H}}}_{2}}sim 6.6 imes {10}^{11},{M}_{odot }$, and its total halo mass could be as high as $sim 4.4 imes {10}^{13},{M}_{odot }$, indicating that it is the likely progenitor of a cluster at least as massive as Coma at z = 0.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Publisher:	American Astronomical Society
ISSN:	0004-637X
Date of First Compliant Deposit:	26 April 2018
Date of Acceptance:	22 November 2017
Last Modified:	05 May 2023 10:50
URI:	https://orca.cardiff.ac.uk/id/eprint/111023

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