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Filaments in the Lupus molecular clouds

Benedettini, M.; Schisano, E.; Pezzuto, S.; Elia, D.; André, P.; Könyves, V.; Schneider, N.; Tremblin, P.; Arzoumanian, D.; di Giorgio, A. M.; Di Francesco, J.; Hill, T.; Molinari, S.; Motte, F.; Nguyen-Luong, Q.; Palmeirim, P.; Rivera-Ingraham, A.; Roy, A.; Rygl, K. L. J.; Spinoglio, L.; Ward-Thompson, D. and White, G. J. (2015). Filaments in the Lupus molecular clouds. Monthly Notices of the Royal Astronomical Society, 453(2) pp. 2036–2049.

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URL: http://dx.doi.org/10.1093/mnras/stv1750
DOI (Digital Object Identifier) Link: https://doi.org/10.1093/mnras/stv1750
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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.

Item Type: Journal Item
Copyright Holders: 2015 The Authors
ISSN: 1365-2966
Keywords: stars: formation; ISM: clouds
Academic Unit/School: Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
Item ID: 45581
Depositing User: G. J. White
Date Deposited: 15 Mar 2016 10:51
Last Modified: 09 Dec 2018 19:49
URI: http://oro.open.ac.uk/id/eprint/45581
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