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Properties of interstellar filaments as derived from Herschel, Planck, and molecular line observations

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

Doris Arzoumanian ,
Philippe André  and
François Boulanger
Doris Arzoumanian
Affiliation:
Institut d'Astrophysique Spatiale (IAS), CNRS (UMR 8617), Université Paris-Sud 11, Bâtiment 121, 91400 Orsay, France
Philippe André
Affiliation:
Laboratoire AIM, CEA/DSM–CNRS–Université Paris Diderot, IRFU/Service d'Astrophysique, C.E.A. Saclay, Orme des Merisiers, 91191 Gif-sur-Yvette, France
François Boulanger
Affiliation:
Institut d'Astrophysique Spatiale (IAS), CNRS (UMR 8617), Université Paris-Sud 11, Bâtiment 121, 91400 Orsay, France
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Abstract

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Recent Herschel and Planck observations of submillimeter dust emission revealed the omnipresence of filamentary structures in the interstellar medium (ISM). The ubiquity of filaments in quiescent clouds as well as in star-forming regions indicates that the formation of filamentary structures is a natural product of the physics at play in the magnetized turbulent cold ISM. An analysis of more than 270 filaments observed with Herschel in 8 regions of the Gould Belt, shows that interstellar filaments are characterized by a narrow distribution of central width sharply peaked at ~0.1 pc, while they span a wide column density range. Molecular line observations of a sample of these filaments show evidence of an increase in the velocity dispersion of dense filaments with column density, suggesting an evolution in mass per unit length due to accretion of surrounding material onto these star-forming filaments. The analyses of Planck dust polarization observations show that both the mean magnetic field and its fluctuations along the filaments are different from those of their surrounding clouds. This points to a coupling between the matter and the $\vec{B}$-field in the filament formation process. These observational results, derived from dust and gas tracers in total and polarized intensity, set strong constraints on our understanding of the formation and evolution of filaments in the ISM. They provide important clues on the initial conditions of the star formation process along interstellar filaments.

Keywords

ISMstar formationinterstellar filament formation and evolutionmagnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , pp. 53 - 60
Copyright
Copyright © International Astronomical Union 2016 

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