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Fragmentation and dynamics in Massive Dense Cores in Cygnus-X

Published online by Cambridge University Press:  27 April 2011

T. Csengeri ,
S. Bontemps ,
N. Schneider  and
F. Motte
T. Csengeri
Affiliation:
Laboratoire AIM, CEA - INSU/CNRS - Université Paris Diderot, IRFU/SAp CEA-Saclay, 91191 Gif-sur-Yvette, France email: timea.csengeri@cea.fr
S. Bontemps
Affiliation:
OASU/LAB-UMR5804, CNRS, Université Bordeaux 1, 33270 Floirac, France
N. Schneider
Affiliation:
Laboratoire AIM, CEA - INSU/CNRS - Université Paris Diderot, IRFU/SAp CEA-Saclay, 91191 Gif-sur-Yvette, France email: timea.csengeri@cea.fr
F. Motte
Affiliation:
Laboratoire AIM, CEA - INSU/CNRS - Université Paris Diderot, IRFU/SAp CEA-Saclay, 91191 Gif-sur-Yvette, France email: timea.csengeri@cea.fr
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Abstract

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A systematic, high angular-resolution study of IR-quiet Massive Dense Cores (MDCs) of Cygnus-X in continuum and high-density molecular tracers is presented. The results are compared with the quasi-static and the dynamical evolutionary scenario. We find that the fragmentation properties are not compatible with the quasi-static, monolithic collapse scenario, nor are they entirely compatible with the formation of a cluster of mostly low-mass stars. The kinematics of MDCs shows individual velocity components appearing as coherent flows, which indicate important dynamical processes at the scale of the mass reservoir around high-mass protostars.

Keywords

stars: formationISM: kinematics and dynamics

References

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