Planck early results. XXII. The submillimetre properties of a sample of Galactic cold clumps

被引:84
作者
Ade, P. A. R. [71 ]
Aghanim, N. [47 ]
Arnaud, M. [59 ]
Ashdown, M. [5 ,57 ]
Aumont, J. [47 ]
Baccigalupi, C. [69 ]
Balbi, A. [28 ]
Banday, A. J. [1 ,8 ,65 ]
Barreiro, R. B. [54 ]
Bartlett, J. G. [4 ,55 ]
Battaner, E. [76 ]
Benabed, K. [48 ]
Benoit, A. [46 ]
Bernard, J. -P. [1 ,8 ]
Bersanelli, M. [25 ,41 ]
Bhatia, R. [6 ]
Bock, J. J. [55 ]
Bonaldi, A. [37 ]
Bond, J. R. [7 ]
Borrill, J. [64 ,72 ]
Bouchet, F. R. [48 ]
Boulanger, F. [47 ]
Bucher, M. [4 ]
Burigana, C. [40 ]
Cabella, P. [28 ]
Cantalupo, C. M. [64 ]
Cardoso, J. -F. [4 ,48 ,60 ,61 ]
Catalano, A. [4 ,58 ]
Cayon, L. [18 ]
Challinor, A. [9 ,50 ,57 ]
Chamballu, A. [44 ]
Chiang, L. -Y [49 ]
Christensen, P. R. [29 ]
Clements, D. L. [44 ]
Colombi, S. [48 ]
Couchot, F. [63 ]
Coulais, A. [58 ]
Crill, B. P. [55 ]
Cuttaia, F. [40 ]
Danese, L. [69 ]
Davies, R. D. [56 ]
de Bernardis, P. [24 ]
de Gasperis, G. [28 ]
de Rosa, A. [40 ]
de Zotti, G. [37 ,69 ]
Delabrouille, J. [4 ]
Delouis, J. -M. [48 ]
Desert, F. -X. [43 ]
Dickinson, C. [56 ]
Doi, Y. [14 ]
机构
[1] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France
[2] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland
[3] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy
[4] Univ Paris 07, CNRS, UMR7164, Paris, France
[5] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England
[6] ALMA Santiago Cent Off, Santiago, Chile
[7] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada
[8] IRAP, CNRS, F-31028 Toulouse 4, France
[9] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England
[10] CEA Saclay, DSM, SPP, F-91191 Gif Sur Yvette, France
[11] Natl Space Inst, DTU Space, Copenhagen, Denmark
[12] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain
[13] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada
[14] Univ Tokyo, Dept Earth Sci & Astron, Meguro Ku, Tokyo 1538902, Japan
[15] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada
[16] Univ Helsinki, Dept Phys, Helsinki, Finland
[17] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[18] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA
[19] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[20] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA
[21] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[22] Univ Illinois, Dept Phys, Urbana, IL USA
[23] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy
[24] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy
[25] Univ Milan, Dipartimento Fis, Milan, Italy
[26] Univ Trieste, Dipartimento Fis, Trieste, Italy
[27] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy
[28] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy
[29] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark
[30] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain
[31] Eotvos Lorand Univ, Dept Astron, H-1117 Budapest, Hungary
[32] ESO Vitacura, European So Observ, Santiago, Chile
[33] Planck Sci Off, European Space Agcy, ESAC, Madrid, Spain
[34] ESTEC, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands
[35] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland
[36] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy
[37] Osserv Astron Padova, INAF, Padua, Italy
[38] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy
[39] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy
[40] IASF Bologna, INAF, Bologna, Italy
[41] IASF Milano, INAF, Milan, Italy
[42] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France
[43] Univ Grenoble 1, CNRS, IPAG, INSU,UMR 5274, F-38041 Grenoble, France
[44] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England
[45] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA
[46] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France
[47] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France
[48] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, Paris, France
[49] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan
[50] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
基金
美国国家航空航天局; 美国国家科学基金会;
关键词
ISM: clouds; dust; extinction; stars: formation; ISM: structure; submillimeter: ISM; stars: protostars; PRE-LAUNCH STATUS; ROSETTE MOLECULAR CLOUD; INFRARED DARK CLOUDS; C2D LEGACY CLOUDS; STAR-FORMATION; DENSE CORES; TEMPERATURE-DEPENDENCE; PHYSICAL-PROPERTIES; INITIAL HIGHLIGHTS; DUST-TEMPERATURE;
D O I
10.1051/0004-6361/201116481
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 (150 pc) and remote (2 kpc) 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 20 pc in the remote sources. The thickness of these filaments ranges between 0.3 and 3 pc, for column densities N-H2 similar to 0.1 to 1.6 x 10(22) cm(-2), and with linear mass density covering a broad range, between 15 and 400 M-circle dot 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 7 K. 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-circle dot 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.
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页数:24
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