Imperial College London
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Dr Clements

Faculty of Natural Sciences, Department of Physics

Reader in Astrophysics
 
 
 
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Contact

 

+44 (0)20 7594 7693d.clements

 
 
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Location

 

1011Blackett LaboratorySouth Kensington Campus

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Summary

 

Publications

Citation

BibTex format

@article{Greenslade:2018:mnras/sty023,
author = {Greenslade, J and Clements, DL and Cheng, T and De, Zotti G and Scott, D and Valiante, E and Eales, S and Bremer, MN and Dannerbauer, H and Birkinshaw, M and Farrah, D and Harrison, DL and Michalowski, MJ and Valtchanov, I and Oteo, I and Baes, M and Cooray, A and Negrello, M and Wang, L and van, der Werf P and Dunne, L and Dye, S},
doi = {mnras/sty023},
journal = {Monthly Notices of the Royal Astronomical Society},
pages = {3336--3359},
title = {Candidate high-z protoclusters among the Planck compact sources, as revealed by Herschel-SPIRE},
url = {http://dx.doi.org/10.1093/mnras/sty023},
volume = {476},
year = {2018}
}
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RIS format (EndNote, RefMan)

TY  - JOUR
AB  - By determining the nature of all the Planck compact sources within 808.4 deg2 of large Herschel surveys, we have identified 27 candidate protoclusters of dusty star-forming galaxies (DSFGs) that are at least 3σ overdense in either 250, 350, or 500μm 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 protoclusters 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 protoclusters of (3.3 ± 0.7) × 10−2 sources deg−2, in good agreement with previous similar studies. We find that a Planck colour selection of S857/S545 < 2 works well to select candidate protoclusters, but can miss protoclusters at z < 2. The Herschel colours of individual candidate protocluster members indicate our candidate protoclusters all likely all lie at z > 1. Our candidate protoclusters 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 protoclusters are physical clusters, multiple protoclusters along the line of sight, or chance alignments of unassociated sources.
AU  - Greenslade,J
AU  - Clements,DL
AU  - Cheng,T
AU  - De,Zotti G
AU  - Scott,D
AU  - Valiante,E
AU  - Eales,S
AU  - Bremer,MN
AU  - Dannerbauer,H
AU  - Birkinshaw,M
AU  - Farrah,D
AU  - Harrison,DL
AU  - Michalowski,MJ
AU  - Valtchanov,I
AU  - Oteo,I
AU  - Baes,M
AU  - Cooray,A
AU  - Negrello,M
AU  - Wang,L
AU  - van,der Werf P
AU  - Dunne,L
AU  - Dye,S
DO  - mnras/sty023
EP  - 3359
PY  - 2018///
SN  - 0035-8711
SP  - 3336
TI  - Candidate high-z protoclusters among the Planck compact sources, as revealed by Herschel-SPIRE
T2  - Monthly Notices of the Royal Astronomical Society
UR  - http://dx.doi.org/10.1093/mnras/sty023
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000430944100036&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - http://hdl.handle.net/10044/1/60283
VL  - 476
ER  -
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