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Planck intermediate results. XXXIX. The Planck list of high-redshift source candidates

Ade, P. A. R. and Crill, B. P. and Doré, O. and Helou, G. and Hildebrandt, S. R. and Pearson, T. J. and Rocha, G. and Rusholme, B. (2016) Planck intermediate results. XXXIX. The Planck list of high-redshift source candidates. Astronomy and Astrophysics, 596 . Art. No. A100. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20190701-074006145

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Abstract

The Planck mission, thanks to its large frequency range and all-sky coverage, has a unique potential for systematically detecting the brightest, and rarest, submillimetre sources on the sky, including distant objects in the high-redshift Universe traced by their dust emission. A novel method, based on a component-separation procedure using a combination of Planck and IRAS data, has been validated and characterized on numerous simulations, and applied to select the most luminous cold submillimetre sources with spectral energy distributions peaking between 353 and 857 GHz at 5′ resolution. A total of 2151 Planck high-z source candidates (the PHZ) have been detected in the cleanest 26% of the sky, with flux density at 545 GHz above 500 mJy. Embedded in the cosmic infrared background close to the confusion limit, these high-z candidates exhibit colder colours than their surroundings, consistent with redshifts z > 2, assuming a dust temperature of T_(xgal) = 35 K and a spectral index of β_(xgal) = 1.5. Exhibiting extremely high luminosities, larger than 10^(14)L⊙, the PHZ objects may be made of multiple galaxies or clumps at high redshift, as suggested by a first statistical analysis based on a comparison with number count models. Furthermore, first follow-up observations obtained from optical to submillimetre wavelengths, which can be found in companion papers, have confirmed that this list consists of two distinct populations. A small fraction (around 3%) of the sources have been identified as strongly gravitationally lensed star-forming galaxies at redshift 2 to 4, while the vast majority of the PHZ sources appear as overdensities of dusty star-forming galaxies, having colours consistent with being at z > 2, and may be considered as proto-cluster candidates. The PHZ provides an original sample, which is complementary to the Planck Sunyaev-Zeldovich Catalogue (PSZ2); by extending the population of virialized massive galaxy clusters detected below z < 1.5 through their SZ signal to a population of sources at z > 1.5, the PHZ may contain the progenitors of today’s clusters. Hence the Planck list of high-redshift source candidates opens a new window on the study of the early stages of structure formation, particularly understanding the intensively star-forming phase at high-z.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/201527206DOIArticle
https://arxiv.org/abs/1508.04171arXivDiscussion Paper
ORCID:
AuthorORCID
Ade, P. A. R.0000-0002-5127-0401
Crill, B. P.0000-0002-4650-8518
Doré, O.0000-0002-5009-7563
Helou, G.0000-0003-3367-3415
Pearson, T. J.0000-0001-5213-6231
Rocha, G.0000-0002-4150-8076
Rusholme, B.0000-0001-7648-4142
Additional Information:© 2016 ESO. Article published by EDP Sciences. Received 17 August 2015; Accepted 7 October 2016; Published online 12 December 2016. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
European Space Agency (ESA)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Institut National des Sciences de l'Univers (INSU)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Consiglio Nazionale delle Ricerche (CNR)UNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
NASAUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
Consejo Superior de Investigaciones Científicas (CSIC)UNSPECIFIED
Ministerio de Economía, Industria y Competitividad (MINECO) UNSPECIFIED
Junta de AndalucíaUNSPECIFIED
Spanish Supercomputing Network (RES)UNSPECIFIED
Finnish Ministry of Employment and the EconomyUNSPECIFIED
Academy of FinlandUNSPECIFIED
Finnish IT Center for Science (CSC)UNSPECIFIED
Deutsches Zentrum für Luft- und Raumfahrt (DLR)UNSPECIFIED
Max Planck SocietyUNSPECIFIED
Canadian Space Agency (CSA)UNSPECIFIED
DTU Space (Denmark)UNSPECIFIED
State Secretariat for Education and Research (Switzerland)UNSPECIFIED
Swiss Space Office (SSO)UNSPECIFIED
Research Council of NorwayUNSPECIFIED
Science Foundation, IrelandUNSPECIFIED
Fundação para a Ciência e a Tecnologia (FCT)UNSPECIFIED
Ministério da Ciência, Tecnologia e Ensino Superior (MCTES) UNSPECIFIED
European Research Council (ERC)UNSPECIFIED
Partnership for Advanced Computing in Europe (PRACE)UNSPECIFIED
Subject Keywords:catalogs – submillimeter: galaxies – galaxies: high-redshift – galaxies: clusters: general – large-scale structure of Universe
Record Number:CaltechAUTHORS:20190701-074006145
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190701-074006145
Official Citation:Planck intermediate results - XXXIX. The Planck list of high-redshift source candidates. Planck Collaboration, P. A. R. Ade, et. al., A&A, 596 (2016) A100. DOI: https://doi.org/10.1051/0004-6361/201527206
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96850
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:02 Jul 2019 18:25
Last Modified:09 Mar 2020 13:19

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