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Astronomy and Astrophysics 518 (2010) L100
Clouds, filaments and protostars: the Herschel Hi-GAL Milky Way
S. Molinari1, B. Swinyard, J. Bally, M. Barlow, J. P. Bernard2, 3, P. Martin4, T. Moore, A. Noriega-Crespo, R. Plume, L. Testi5, A. Zavagno6, 7, A. Abergel3, B. Ali, L. Anderson8, P. André9, J. P. Baluteau, C. Battersby, M. T. Beltrán, M. Benedettini10, N. Billot, J. Blommaert, S. Bontemps11, 12, 13, 14, F. Boulanger3, J. Brand, C. Brunt, M. Burton, L. Calzoletti, S. Carey, P. Caselli15, 16, 17, R. Cesaroni18, J. Cernicharo19, S. Chakrabarti20, A. Chrysostomou, M. Cohen, M. Compiegne, P. De Bernardis, G. De Gasperis, A. M. di Giorgio, D. Elia, F. Faustini, N. Flagey, Y. Fukui, G. A. Fuller, K. Ganga21, P. Garcia-Lario22, 23, J. Glenn, P. F. Goldsmith, M. J. Griffin, M. Hoare, M. Huang24, D. Ikhenaode, C. Joblin2, G. Joncas, M. Juvela, J. M. Kirk, G. Lagache3, J. Z. Li24, T. L. Lim25, S. D. Lord, M. Marengo, D. J. Marshall26, S. Masi27, F. Massi, M. Matsuura28, V. Minier20, 29, M. A. Miville-Deschenes3, L. A. Montier, L. Morgan30, F. Motte20, 29, J. C. Mottram, T. G. Mueller, P. Natoli27, J. Neves, L. Olmi31, R. Paladini2, D. Paradis, H. Parsons, N. Peretto29, M. Pestalozzi, S. Pezzuto1, F. Piacentini27, L. Piazzo, D. Polychroni, M. Pomarès7, C. C. Popescu, W. T. Reach, I. Ristorcelli2, J. F. Robitaille, T. Robitaille, J. A. Rodón, A. Roy32, P. Royer33, 34, D. Russeil6, P. Saraceno1, M. Sauvage29, P. Schilke35, E. Schisano, N. Schneider29, F. Schuller35, B. Schulz36, B. Sibthorpe37, H. A. Smith, M. D. Smith38, L. Spinoglio31, D. Stamatellos, F. Strafella, G. S. Stringfellow, E. Sturm, R. Taylor, M. A. Thompson, A. Traficante, R. J. Tuffs, G. Umana, L. Valenziano31, R. Vavrek, M. Veneziani21, 27, S. Viti10, C. Waelkens, D. Ward-Thompson39, G. White25, L. A. Wilcock, F. Wyrowski35, H. W. Yorke, Q. Zhang40
(2010)

We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key-project that will map the inner Galactic Plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2{\deg} x 2{\deg} tiles approximately centered at l=30{\deg} and l=59{\deg}. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call 'cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around A_V of about 1 is exceeded for the regions in the l=59{\deg} field; a A_V value between 5 and 10 is found for the l=30{\deg} field, likely due to the relatively larger distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm-2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows.
1 :  IFSI-INAF - Interplanetary Space Physics Institute (IFSI)
2 :  CESR - Centre d'étude spatiale des rayonnements
3 :  IAS - Institut d'astrophysique spatiale
4 :  CITA
5 :  ESO - European Southern Observatory
6 :  LAM - Laboratoire d'Astrophysique de Marseille
7 :  OAMP - Observatoire Astronomique de Marseille Provence
8 :  LABORATORY OF COMPARATIVE CARCINOGENESIS - Laboratory of Comparative Carcinogenesis
9 :  LINA - Laboratoire d'Informatique de Nantes Atlantique
10 :  LAOG - Laboratoire d'Astrophysique de Grenoble
11 :  LAB - Laboratoire d'Astrophysique de Bordeaux
12 :  OASU - Observatoire aquitain des sciences de l'univers
13 :  Université Sciences et Technologies - Bordeaux 1
14 :  L3AB - Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux
15 :  INAF - Osservatorio Astrofisico di Arcetri
16 :  INAF - Osservatorio di arcetri
17 :  INAF - Osservatorio Astrofisico di Arcetri
18 :  INAF - Osservatorio Astrofisico di Arcetri, Istituto Nazionale di Astrofisica
19 :  CSIC - Centro de Investigaciones Biológicas
20 :  IRFU - Institut de Recherches sur les lois Fondamentales de l'Univers (ex DAPNIA)
21 :  APC - UMR 7164 - AstroParticule et Cosmologie
22 :  ESA - Espagne - ISO Data Centre
23 :  ESA Espagne - Herschel Science Centre
24 :  National Astronomical Observatories
25 :  RAL - Rutherford Appleton Laboratory - Didcot
26 :  Universiti Brunei Darussalam, Biology Department
27 :  Dipartimento di Fisica, Universita` di Roma Tor Vergata
28 :  The University of Manchester [Manchester]
29 :  AIM - UMR 7158 - Astrophysique Interactions Multi-échelles
30 :  Tenovus Centre for Cancer Research
31 :  ARENA - Antarctic Research a European Network for Astrophysics
32 :  Inter University Accelerator Centre
33 :  LSCE - UMR 8212 - Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette]
34 :  LEOSPHERE France
35 :  MPIFR - Max-Planck-Institut für Radioastronomie
36 :  LRA - Laboratoire de Radio Astronomie de l'ENS
37 :  Royal Observatory Edinburgh
38 :  Atmospheric Sciences
39 :  School of Physics & Astronomy
40 :  Shanghai Inst Opt & Fine Mech
FORMATION STELLAIRE 2010
APC - Cosmologie et Gravitation
Planète et Univers/Astrophysique/Astrophysique stellaire et solaire

Physique/Astrophysique/Astrophysique stellaire et solaire
Lien vers le texte intégral : 
http://fr.arXiv.org/abs/1005.3317