Bibcode
Greenslade, J.; Clements, D. L.; Cheng, T.; De Zotti, G.; Scott, D.; Valiante, E.; Eales, S.; Bremer, M. N.; Dannerbauer, H.; Birkinshaw, M.; Farrah, D.; Harrison, D. L.; Michałowski, M. J.; Valtchanov, I.; Oteo, I.; Baes, M.; Cooray, A.; Negrello, M.; Wang, L.; van der Werf, P.; Dunne, L.; Dye, S.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 476, Issue 3, p.3336-3359
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5
2018
Citations
39
Refereed citations
33
Description
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 500 μm 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.
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Two of the most fundamental questions in astrophysics are the conversion of molecular gas into stars and how this physical process is a function of environments on all scales, ranging from planetary systems, stellar clusters, galaxies to galaxy clusters. The main goal of this internal project is to get insight into the formation and evolution of
Helmut
Dannerbauer