Bibcode
Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Bernard, J.-P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bucher, M.; Burigana, C.; Cabella, P.; Cantalupo, C. M.; Cardoso, J.-F.; Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L.-Y.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies, R. D.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J.-M.; Désert, F.-X.; Dickinson, C.; Doi, Y.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Helou, G.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Ikeda, N.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kitamura, Y.; Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.-M.; Lasenby, A.; Laureijs, R. J. et al.
Bibliographical reference
Astronomy and Astrophysics, Volume 536, id.A22
Advertised on:
12
2011
Journal
Citations
95
Refereed citations
86
Description
We perform a detailed investigation of sources from the Cold Cores
Catalogue of Planck Objects (C3PO). Our goal is to probe the reliability
of the detections, validate the separation between warm and cold dust
emission components, provide the first glimpse at the nature, internal
morphology and physical characterictics of the Planck-detected sources.
We focus on a sub-sample of ten sources from the C3PO list, selected to
sample different environments, from high latitude cirrus to nearby
(150pc) and remote (2kpc) molecular complexes. We present Planck surface
brightness maps and derive the dust temperature, emissivity spectral
index, and column densities of the fields. With the help of higher
resolution Herschel and AKARI continuum observations and molecular line
data, we investigate the morphology of the sources and the properties of
the substructures at scales below the Planck beam size. The cold clumps
detected by Planck are found to be located on large-scale filamentary
(or cometary) structures that extend up to 20pc in the remote sources.
The thickness of these filaments ranges between 0.3 and 3pc, for column
densities NH2 ~ 0.1 to 1.6 × 1022
cm-2, and with linear mass density covering a broad range,
between 15 and 400 M&sun; pc-1. The dust
temperatures are low (between 10 and 15K) and the Planck cold clumps
correspond to local minima of the line-of-sight averaged dust
temperature in these fields. These low temperatures are confirmed when
AKARI and Herschel data are added to the spectral energy distributions.
Herschel data reveal a wealth of substructure within the Planck cold
clumps. In all cases (except two sources harbouring young stellar
objects), the substructures are found to be colder, with temperatures as
low as 7K. Molecular line observations provide gas column densities
which are consistent with those inferred from the dust. The linewidths
are all supra-thermal, providing large virial linear mass densities in
the range 10 to 300 M&sun; pc-1, comparable within
factors of a few, to the gas linear mass densities. The analysis of this
small set of cold clumps already probes a broad variety of structures in
the C3PO sample, probably associated with different evolutionary stages,
from cold and starless clumps, to young protostellar objects still
embedded in their cold surrounding cloud. Because of the all-sky
coverage and its sensitivity, Planck is able to detect and locate the
coldest spots in massive elongated structures that may be the
long-searched for progenitors of stellar clusters.
Appendix A is available in electronic form at http://www.aanda.orgCorresponding
author: I. Ristorcelli, e-mail: isabelle.ristorcelli [at] irap.omp.eu (isabelle[dot]ristorcelli[at]irap[dot]omp[dot]eu)
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Rafael
Rebolo López