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CARMA-NRO Orion Survey. Filamentary structure as seen in C^(18)O emission

Suri, Sümeyye and Sánchez-Monge, Álvaro and Schilke, Peter and Clarke, Seamus D. and Smith, Rowan J. and Ossenkopf-Okada, Volker and Klessen, Ralf and Padoan, Paolo and Goldsmith, Paul and Arce, Héctor G. and Bally, John and Carpenter, John M. and Ginsburg, Adam and Johnstone, Doug and Kauffmann, Jens and Kong, Shuo and Lis, Dariusz C. and Mairs, Steve and Pillai, Thushara and Pineda, Jaime E. and Duarte-Cabral, Ana (2019) CARMA-NRO Orion Survey. Filamentary structure as seen in C^(18)O emission. Astronomy and Astrophysics, 623 . Art. No. A142. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20190404-090350372

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Abstract

Context. We present an initial overview of the filamentary structure in the Orion A molecular cloud utilizing a high angular and velocity resolution C^(18)O(1–0) emission map that was recently produced as part of the CARMA-NRO Orion Survey. Aims. The main goal of this study is to build a credible method to study varying widths of filaments which has previously been linked to star formation in molecular clouds. Due to the diverse star forming activities taking place throughout its ~20 pc length, together with its proximity of 388 pc, the Orion A molecular cloud provides an excellent laboratory for such an experiment to be carried out with high resolution and high sensitivity. Methods. Using the widely-known structure identification algorithm, DisPerSE, on a three-dimensional (PPV) C18O cube, we identify 625 relatively short (the longest being 1.74 pc) filaments over the entire cloud. We studied the distribution of filament widths using FilChaP, a python package that we have developed and made publicly available. Results. We find that the filaments identified in a two square-degree PPV cube do not overlap spatially, except for the complex OMC-4 region that shows distinct velocity components along the line of sight. The filament widths vary between 0.02 and 0.3 pc depending on the amount of substructure that a filament possesses. The more substructure a filament has, the larger is its width. We also find that despite this variation, the filament width shows no anticorrelation with the central column density which is in agreement with previous Herschel observations.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/201834049DOIArticle
ORCID:
AuthorORCID
Suri, Sümeyye0000-0003-0412-8522
Schilke, Peter0000-0003-2141-5689
Clarke, Seamus D.0000-0001-9751-4603
Smith, Rowan J.0000-0002-0820-1814
Klessen, Ralf0000-0002-0560-3172
Padoan, Paolo0000-0002-5055-5800
Goldsmith, Paul0000-0002-6622-8396
Arce, Héctor G.0000-0001-5653-7817
Bally, John0000-0001-8135-6612
Carpenter, John M.0000-0003-2251-0602
Ginsburg, Adam0000-0001-6431-9633
Johnstone, Doug0000-0002-6773-459X
Kong, Shuo0000-0002-8469-2029
Lis, Dariusz C.0000-0002-0500-4700
Mairs, Steve0000-0002-6956-0730
Pineda, Jaime E.0000-0002-3972-1978
Alternate Title:CARMA-NRO Orion Survey. Filamentary structure as seen in C18O emission
Additional Information:© 2019 ESO. Article published by EDP Sciences. Received 8 August 2018; Accepted 2 January 2019; Published online 21 March 2019. We thank the referee for their insightful comments that helped improve this manuscript and FilChaP. S.S., A.S.M., P.S. and V.O.O. acknowledge funding by the Deutsche Forschungsgemeinschaft (DFG) via the Sonderforschungsbereich SFB 956 Conditions and Impact of Star Formation (subprojects A4, A6, C1, and C3) and the Bonn-Cologne Graduate School. S.D.C. acknowledges support from the ERC starting grant No. 679852 RADFEEDBACK. R.J.S. gratefully acknowledges support from an STFC Ernest Rutherford fellowship. This research was carried out in part at the Jet Propulsion Laboratory which is operated for NASA by the California Institute of Technology. P.P. acknowledges support by the Spanish MINECO under project AYA2017-88754-P (AEI/FEDER,UE). H.G.A. and S.K. acknowledge support from the National Science Foundation through grant AST-1140063. H.G.A. and S.K. acknowledge support from the National Science Foundation through grant AST-1140063. Software: astropy (Price-Whelan et al. 2018), matplotlib (Hunter 2007), scipy (Jones et al. 2001), pandas (McKinney 2010), APLpy (Robitaille & Bressert 2012).
Funders:
Funding AgencyGrant Number
Deutsche Forschungsgemeinschaft (DFG)SFB 956
Bonn-Cologne Graduate SchoolUNSPECIFIED
European Research Council (ERC)679852
Science and Technology Facilities Council (STFC)UNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2017-88754-P
NSFAST-1140063
Subject Keywords:ISM: clouds – stars: formation – ISM: structure – ISM: individual objects: Orion A – methods: statistical
Record Number:CaltechAUTHORS:20190404-090350372
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190404-090350372
Official Citation:The CARMA-NRO Orion Survey - Filamentary structure as seen in C18O emission. Sümeyye Suri, Álvaro Sánchez-Monge, Peter Schilke, Seamus D. Clarke, Rowan J. Smith, Volker Ossenkopf-Okada, Ralf Klessen, Paolo Padoan, Paul Goldsmith, Héctor G. Arce, John Bally, John M. Carpenter, Adam Ginsburg, Doug Johnstone, Jens Kauffmann, Shuo Kong, Dariusz C. Lis, Steve Mairs, Thushara Pillai, Jaime E. Pineda and Ana Duarte-Cabral. A&A, 623 (2019) A142. DOI: https://doi.org/10.1051/0004-6361/201834049
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:94448
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:04 Apr 2019 17:11
Last Modified:09 Mar 2020 13:19

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