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Astronomy and Astrophysics 543 (2012) L3
The spine of the swan: A Herschel study of the DR21 ridge and filaments in Cygnus X
M. Hennemann 1, F. Motte 2, 3, N. Schneider 4, P. Didelon 1, T. Hill 1, D. Arzoumanian, S. Bontemps 5, 6, 7, 8, T. Csengeri 1, Ph. Andre 1, V. Konyves, F. Louvet 9, A. Marston, A. Men'shchikov 1, V. Minier 2, 3, Q. Nguyen Luong, P. Palmeirim, N. Peretto 1, M. Sauvage 1, A. Zavagno, L. D. Anderson, J. -Ph. Bernard 10, J. Di Francesco 11, D. Elia, J. Z. Li 12, P. G. Martin 13, S. Molinari 14, S. Pezzuto 14, D. Russeil, K. L. J. Rygl, E. Schisano, L. Spinoglio 15, T. Sousbie 16, D. Ward-Thompson 17, G. J. White 18
(2012)

In order to characterise the cloud structures responsible for the formation of high-mass stars, we present Herschel observations of the DR21 environment. Maps of the column density and dust temperature unveil the structure of the DR21 ridge and several connected filaments. The ridge has column densities larger than 1e23/cm^2 over a region of 2.3 pc^2. It shows substructured column density profiles and branching into two major filaments in the north. The masses in the studied filaments range between 130 and 1400 Msun whereas the mass in the ridge is 15000 Msun. The accretion of these filaments onto the DR21 ridge, suggested by a previous molecular line study, could provide a continuous mass inflow to the ridge. In contrast to the striations seen in e.g., the Taurus region, these filaments are gravitationally unstable and form cores and protostars. These cores formed in the filaments potentially fall into the ridge. Both inflow and collisions of cores could be important to drive the observed high-mass star formation. The evolutionary gradient of star formation running from DR21 in the south to the northern branching is traced by decreasing dust temperature. This evolution and the ridge structure can be explained by two main filamentary components of the ridge that merged first in the south.
1:  Astrophysique Interactions Multi-échelles (AIM)
CNRS : UMR7158 – INSU – Université Paris VII - Paris Diderot – CEA : DSM/IRFU
2:  Laboratoire AIM (AIM)
CEA – Université Paris VII - Paris Diderot
3:  Institut de Recherches sur les lois Fondamentales de l'Univers (ex DAPNIA) (IRFU)
CEA : DSM/IRFU
4:  Laboratory for Atmospheric and Space Physics
University of Colorado
5:  Observatoire aquitain des sciences de l'univers (OASU)
CNRS : UMS2567 – INSU – Université Sciences et Technologies - Bordeaux I
6:  Université Sciences et Technologies - Bordeaux 1
Université Sciences et Technologies - Bordeaux I
7:  Laboratoire d'Astrophysique de Bordeaux (LAB)
CNRS : UMR5804 – INSU – Université Sciences et Technologies - Bordeaux I
8:  Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB)
CNRS : UMR5804 – INSU – Université Sciences et Technologies - Bordeaux I
9:  Groupe d'Etudes des Matériaux Hétérogènes (GEMH)
Ecole Nationale Supérieure de Céramique Industrielle – Université de Limoges : EA3178 – Institut des Procédés Appliqués aux Matériaux
10:  Centre d'étude spatiale des rayonnements (CESR)
CNRS : UMR5187 – Observatoire Midi-Pyrénées – INSU – Université Paul Sabatier [UPS] - Toulouse III
11:  National Research Council of Canada, Herzberg Institute of Astrophysics
Herzberg Institute of Astrophysics
12:  National Astronomical Observatories
Chinese Academy of Sciences
13:  Laboratoire des Lois de Comportement du Combustible (LLCC)
CEA : DEN/DEC/SESC/LLCC
14:  Interplanetary Space Physics Institute (IFSI) (IFSI-INAF)
Interplanetary Space Physics Institute
15:  Antarctic Research a European Network for Astrophysics (ARENA)
CEA
16:  Centre de Recherche Astrophysique de Lyon (CRAL)
CNRS : UMR5574 – INSU – Université Claude Bernard - Lyon I – École Normale Supérieure - Lyon
17:  School of Physics & Astronomy
Cardiff University
18:  Engineering Department
University of Cambridge
FORMATION STELLAIRE 2012
Sciences of the Universe/Astrophysics/Solar and Stellar Astrophysics

Physics/Astrophysics/Solar and Stellar Astrophysics
Fulltext link: 
http://fr.arXiv.org/abs/1206.1243