Candidate high-z proto-clusters among the Planck compact sources, as revealed by Herschel-SPIRE

Greenslade, J., Clements, D. L., Cheng, T., De Zotti, G., Scott, D., Valiante, Elisabetta, Eales, Stephen ORCID: https://orcid.org/0000-0002-7394-426X, Bremer, M. N., Dannerbauer, H., Birkinshaw, M., Farrah, D., Harrison, D. L., Michałowski, M.J., Valtchanov, I., Oteo, I., Baes, M., Cooray, A., Negrello, Mattia ORCID: https://orcid.org/0000-0002-7925-7663, Wang, L., Van der Werf, P., Dunne, Loretta ORCID: https://orcid.org/0000-0001-9880-2543 and Dye, S. 2018. Candidate high-z proto-clusters among the Planck compact sources, as revealed by Herschel-SPIRE. Monthly Notices of the Royal Astronomical Society 476 (3) , pp. 3336-3359. 10.1093/mnras/sty023

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Abstract

By determining the nature of all the Planck compact sources within 808.4 deg^2 of large Herschel surveys, we have identified 27 candidate proto-clusters of dusty star forming galaxies (DSFGs) that are at least 3{\sigma} overdense in either 250, 350 or 500 μmm sources. We find roughly half of all the Planck compact sources are resolved by Herschel into multiple discrete objects, with the other half remaining unresolved by Herschel. We find a significant difference between versions of the Planck catalogues, with earlier releases hosting a larger fraction of candidate proto-clusters and Galactic Cirrus than later releases, which we ascribe to a difference in the filters used in the creation of the three catalogues. We find a surface density of DSFG candidate proto-clusters of (3.3 ± 0.7) x 10^(-2) sources deg^(-2), in good agreement with previous similar studies. We find that a Planck colour selection of S_{857}/S_{545} < 2 works well to select candidate proto-clusters, but can miss proto-clusters at z < 2. The Herschel colours of individual candidate proto-cluster members indicate our candidate proto-clusters all likely all lie at z > 1. Our candidate proto-clusters are a factor of 5 times brighter at 353 GHz than expected from simulations, even in the most conservative estimates. Further observations are needed to confirm whether these candidate proto-clusters are physical clusters, multiple proto-clusters along the line of sight, or chance alignments of unassociated sources.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Publisher:	Oxford University Press
ISSN:	0035-8711
Date of First Compliant Deposit:	10 January 2018
Date of Acceptance:	22 December 2017
Last Modified:	14 Nov 2024 08:30
URI:	https://orca.cardiff.ac.uk/id/eprint/108063

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