Filaments in the Lupus molecular clouds
Date Issued
2015
Author(s)
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André, P.
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Könyves, V.
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Schneider, N.
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Tremblin, P.
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Arzoumanian, D.
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Di Francesco, J.
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Hill, T.
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Motte, F.
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Nguyen-Luong, Q.
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Palmeirim, P.
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Rivera-Ingraham, A.
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Ward-Thompson, D.
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White, G. J.
Description
We thank J. P. Bernard for providing us with the maps of the modelled dust emission at the Herschel wavelengths that we used for removing the Moon stray-light and D. Eden who produced the visual extinction maps. We are grateful to the anonymous referee for his/her comments that helped us to improve the paper. DE is supported by an Italian Space Agency (ASI) fellowship under contract no. I/005/11/0. NS and PA acknowledge support by the ANR-11-BS56-010 project STARFICH. This work has received support from the European Research Council under the European Union's Seventh Framework Programme (ERC Advanced Grant Agreement no. 291294 - ORISTARS). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF–IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA–PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL–MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by the following national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).
Abstract
We have studied the filaments extracted from the column density maps of the nearby Lupus 1, 3, and 4 molecular clouds, derived from photometric maps observed with the Herschel satellite. Filaments in the Lupus clouds have quite low column densities, with a median value of ̃1.5 × 1021 cm-2 and most have masses per unit length lower than the maximum critical value for radial gravitational collapse. Indeed, no evidence of filament contraction has been seen in the gas kinematics. We find that some filaments, that on average are thermally subcritical, contain dense cores that may eventually form stars. This is an indication that in the low column density regime, the critical condition for the formation of stars may be reached only locally and this condition is not a global property of the filament. Finally, in Lupus we find multiple observational evidences of the key role that the magnetic field plays in forming filaments, and determining their confinement and dynamical evolution.
Volume
453
Issue
2
Start page
2036
Issn Identifier
0035-8711
Ads BibCode
2015MNRAS.453.2036B
Rights
open.access
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