%ACheng, T. [Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK]%ACheng, T. [Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK]%AClements, D. [Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK]%AClements, D. [Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK]%AGreenslade, J. [Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK]%AGreenslade, J. [Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK]%ACairns, J. [Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK]%ACairns, J. [Astrophysics Group, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, UK]%AAndreani, P. [European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching, Germany]%AAndreani, P. [European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching, Germany]%ABremer, M. [HH Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK]%ABremer, M. [HH Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK]%AConversi, L. [European Space Agency / ESAC, Camino Bajo del Castillo, Villanueva de la Cañada, E-28692 Madrid, Spain]%AConversi, L. [European Space Agency / ESAC, Camino Bajo del Castillo, Villanueva de la Cañada, E-28692 Madrid, Spain]%ACooray, A. [Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA]%ACooray, A. [Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA]%ADannerbauer, H. [Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain, Departmento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain]%ADannerbauer, H. [Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain, Departmento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain]%ADe Zotti, G. [INAF-Osservatorio astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy]%ADe Zotti, G. [INAF-Osservatorio astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy]%AEales, S. [School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA, UK]%AEales, S. [School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA, UK]%AGonzález-Nuevo, J. [Departamento de Física, Universidad de Oviedo, C. Federico García Lorca 18, E-33007 Oviedo, Spain]%AGonzález-Nuevo, J. [Departamento de Física, Universidad de Oviedo, C. Federico García Lorca 18, E-33007 Oviedo, Spain]%AIbar, E. [Instituto de Física y Astronomía, Universidad de Valparaíso, Avda. Gran Bretaña, 1111 Valparaíso, Chile]%AIbar, E. [Instituto de Física y Astronomía, Universidad de Valparaíso, Avda. Gran Bretaña, 1111 Valparaíso, Chile]%ALeeuw, L. [College of Graduate Studies, University of South Africa, Theo van Wijk 9-52, Unisa Muckleneuk Campus, PO Box 392, UNISA, 0003, South Africa]%ALeeuw, L. [College of Graduate Studies, University of South Africa, Theo van Wijk 9-52, Unisa Muckleneuk Campus, PO Box 392, UNISA, 0003, South Africa]%AMa, J. [Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA]%AMa, J. [Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA]%AMichałowski, M. [Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, ul. Słoneczna 36, PL-60-286 Poznań, Poland]%AMichałowski, M. [Astronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, ul. Słoneczna 36, PL-60-286 Poznań, Poland]%ANayyeri, H. [Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA]%ANayyeri, H. [Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA]%ARiechers, D. [Department of Astronomy, Cornell University, Space Sciences Building, Ithaca, NY 14853, USA, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany]%ARiechers, D. [Department of Astronomy, Cornell University, Space Sciences Building, Ithaca, NY 14853, USA, Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany]%AScott, D. [Department of Physics and Astronomy, University of British Columbia, BC V6T1Z1, Vancouver, Canada]%AScott, D. [Department of Physics and Astronomy, University of British Columbia, BC V6T1Z1, Vancouver, Canada]%ATemi, P. [Astrophysics Branch, NASA Ames Research Center, Moffett Field, CA 94035, USA]%ATemi, P. [Astrophysics Branch, NASA Ames Research Center, Moffett Field, CA 94035, USA]%AVaccari, M. [Department of Physics and Astronomy, University of the Western Cape, Private Bag X17, Bellville, 7535 Cape Town, South Africa, INAF – Istituto di Radioastronomia, via Gobetti 101, I-40129 Bologna, Italy]%AVaccari, M. [Department of Physics and Astronomy, University of the Western Cape, Private Bag X17, Bellville, 7535 Cape Town, South Africa, INAF – Istituto di Radioastronomia, via Gobetti 101, I-40129 Bologna, Italy]%AValtchanov, I. [Telespazio Vega UK for ESA, Operations Department, European Space Astronomy Centre, Villanueva de la Cañada, E-28691 Madrid, Spain]%AValtchanov, I. [Telespazio Vega UK for ESA, Operations Department, European Space Astronomy Centre, Villanueva de la Cañada, E-28691 Madrid, Spain]%Avan Kampen, E. [European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching, Germany]%Avan Kampen, E. [European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching, Germany]%AWang, L. [SRON Netherlands Institute for Space Research, Landleven 12, NL-9747 AD Groningen, The Netherlands, Kapteyn Astronomical Institute, University of Groningen, Postbus 800, NL-9700 AV Groningen, The Netherlands]%AWang, L. [SRON Netherlands Institute for Space Research, Landleven 12, NL-9747 AD Groningen, The Netherlands, Kapteyn Astronomical Institute, University of Groningen, Postbus 800, NL-9700 AV Groningen, The Netherlands]%BJournal Name: Monthly Notices of the Royal Astronomical Society; Journal Volume: 490; Journal Issue: 3; Related Information: CHORUS Timestamp: 2020-09-20 20:04:54 %D2019%IOxford University Press %JJournal Name: Monthly Notices of the Royal Astronomical Society; Journal Volume: 490; Journal Issue: 3; Related Information: CHORUS Timestamp: 2020-09-20 20:04:54 %K %MOSTI ID: 10123128 %PMedium: X %TSCUBA-2 observations of candidate starbursting protoclusters selected by Planck and Herschel-SPIRE %XABSTRACT

We present SCUBA-2 850 $\mathrm{ \mu}$m observations of 13 candidate starbursting protoclusters selected using Planck and Herschel data. The cumulative number counts of the 850 $\mathrm{ \mu}$m sources in 9 of 13 of these candidate protoclusters show significant overdensities compared to the field, with the probability <10−2 assuming the sources are randomly distributed in the sky. Using the 250, 350, 500, and 850 $\mathrm{ \mu}$m flux densities, we estimate the photometric redshifts of individual SCUBA-2 sources by fitting spectral energy distribution templates with an MCMC method. The photometric redshift distribution, peaking at 2 < z < 3, is consistent with that of known z > 2 protoclusters and the peak of the cosmic star formation rate density (SFRD). We find that the 850 $\mathrm{ \mu}$m sources in our candidate protoclusters have infrared luminosities of $L_{\mathrm{IR}}\gtrsim 10^{12}\, \mathrm{L}_{\odot }$ and star formation rates of SFR  = (500–1500) M⊙ yr−1. By comparing with results in the literature considering only Herschel photometry, we conclude that our 13 candidate protoclusters can be categorized into four groups: six of them being high-redshift starbursting protoclusters, one being a lower redshift cluster or protocluster, three being protoclusters that contain lensed dusty star-forming galaxies or are rich in 850 $\mathrm{ \mu}$m sources, and three regions without significant Herschel or SCUBA-2 source overdensities. The total SFRs of the candidate protoclusters are found to be comparable or higher than those of known protoclusters, suggesting our sample contains some of the most extreme protocluster population. We infer that cross-matching Planck and Herschel data is a robust method for selecting candidate protoclusters with overdensities of 850 $\mathrm{ \mu}$m sources.

%0Journal Article