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The Identification of Filaments on Far-infrared and Submillimiter Images: Morphology, Physical Conditions and Relation with Star Formation of Filamentary Structure

Schisano, E. and Rygl, K. L. J. and Molinari, S. and Busquet, G. and Elia, D. and Pestalozzi, M. and Polychroni, D. and Billot, N. and Carey, S. and Paladini, R. and Noriega-Crespo, A. and Moore, T. J. T. and Plume, R. and Glover, S. C. O. and Vázquez-Semadeni, E. (2014) The Identification of Filaments on Far-infrared and Submillimiter Images: Morphology, Physical Conditions and Relation with Star Formation of Filamentary Structure. Astrophysical Journal, 791 (1). Art. No. 27. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20140828-085124063

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Abstract

Observations of molecular clouds reveal a complex structure, with gas and dust often arranged in filamentary, rather than spherical geometries. The association of pre- and proto-stellar cores with the filaments suggests a direct link with the process of star formation. Any study of the properties of such filaments requires representative samples from different environments for an unbiased detection method. We developed such an approach using the Hessian matrix of a surface-brightness distribution to identify filaments and determine their physical and morphological properties. After testing the method on simulated, but realistic, filaments, we apply the algorithms to column-density maps computed from Herschel observations of the Galactic plane obtained by the Hi-GAL project. We identified ~500 filaments, in the longitude range of l = 216°.5 to l = 225°.5, with lengths from ~1 pc up to ~30 pc and widths between 0.1 pc and 2.5 pc. Average column densities are between 10^(20) cm^2 and 10^(22) cm^2. Filaments include the majority of dense material with N_H_2> 6 × 10^(21) cm^2. We find that the pre- and proto-stellar compact sources already identified in the same region are mostly associated with filaments. However, surface densities in excess of the expected critical values for high-mass star formation are only found on the filaments, indicating that these structures are necessary to channel material into the clumps. Furthermore, we analyze the gravitational stability of filaments and discuss their relationship with star formation.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/791/1/27DOIArticle
http://iopscience.iop.org/0004-637X/791/1/27/PublisherArticle
http://arxiv.org/abs/1406.4443arXivDiscussion Paper
ORCID:
AuthorORCID
Carey, S.0000-0002-0221-6871
Paladini, R.0000-0002-5158-243X
Noriega-Crespo, A.0000-0002-6296-8960
Additional Information:© 2014 The American Astronomical Society. Received 2013 September 26; accepted 2014 June 16; published 2014 July 23. The authors are grateful to the anonymous referee for the useful comments that improved the presentation of the work. E.S. acknowledges support from the NASA Astrophysics Data Analysis Program grant NNX12AE18G. K.L.J.R. is supported by an Italian Space Agency (ASI) fellowship under contract number I/005/11/0. G.B. is supported by the Spanish MICINN grant AYA2011-30228-C03 (co-funded with FEDER funds). D.P. is funded through the Operational Program “Education and Lifelong Learning,” which is co-financed by the European Union (European Social Fund) and Greek national funds. S.C.O.G. acknowledges support from the Deutsche Forschungsgemeinschaft via SFB 881 “The Milk Way System” (sub-projects B1 and B2). The authors are also grateful to M. Pereira-Santaella and N. Marchili for helpful suggestions. E.S. is very grateful to Antonia Pierni and wishes to thank her for all the moments, dark and bright, they spent together while he was working on this research.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANNX12AE18G
Agenzia Spaziale Italiana (ASI)I/005/11/0
Ministerio de Ciencia e Innovación (MCINN)AYA2011-30228-C03
Fondo Europeo de Desarrollo Regional (FEDER)UNSPECIFIED
Operational Program "Education and Lifelong Learning"UNSPECIFIED
European Union European Social FundUNSPECIFIED
Greek national fundsUNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)SFB 881
Subject Keywords:ISM: clouds; ISM: structure; methods: data analysis; stars: formation
Issue or Number:1
Record Number:CaltechAUTHORS:20140828-085124063
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20140828-085124063
Official Citation:The Identification of Filaments on Far-infrared and Submillimiter Images: Morphology, Physical Conditions and Relation with Star Formation of Filamentary Structure E. Schisano et al. 2014 ApJ 791 27
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:49015
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:28 Aug 2014 17:51
Last Modified:09 Mar 2020 13:19

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