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CARMA Large Area Star Formation Survey: Structure and Kinematics of Dense Gas in Serpens Main

Lee, Katherine I. and Fernández-López, Manuel and Storm, Shaye and Looney, Leslie W. and Mundy, Lee G. and Segura-Cox, Dominique and Teuben, Peter and Rosolowsky, Erik and Arce, Héctor G. and Ostriker, Eve C. and Shirley, Yancy L. and Kwon, Woojin and Kauffmann, Jens and Tobin, John J. and Plunkett, Adele L. and Pound, Marc W. and Salter, Demerese M. and Volgenau, N. H. and Chen, Che-Yu and Tassis, Konstantinos and Isella, Andrea and Crutcher, Richard M. and Gammie, Charles F. and Testi, Leonardo (2014) CARMA Large Area Star Formation Survey: Structure and Kinematics of Dense Gas in Serpens Main. Astrophysical Journal, 797 (2). Art. No. 76. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20150115-103442804

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Abstract

We present observations of NL_2H^+ (J = 1 -> 0), HCO^+ (J = 1 -> 0), and HCN (J = 1 -> 0) toward the Serpens Main molecular cloud from the CARMA Large Area Star Formation Survey (CLASSy). We mapped 150 arcmin(2) of Serpens Main with an angular resolution of ~7". The gas emission is concentrated in two subclusters (the NW and SE subclusters). The SE subcluster has more prominent filamentary structures and more complicated kinematics compared to the NW subcluster. The majority of gas in the two subclusters has subsonic to sonic velocity dispersions. We applied a dendrogram technique with N_2H^+(1-0) to study the gas structures; the SE subcluster has a higher degree of hierarchy than the NW subcluster. Combining the dendrogram and line fitting analyses reveals two distinct relations: a flat relation between nonthermal velocity dispersion and size, and a positive correlation between variation in velocity centroids and size. The two relations imply a characteristic depth of 0.15 pc for the cloud. Furthermore, we have identified six filaments in the SE subcluster. These filaments have lengths of ~0.2 pc and widths of ~0.03 pc, which is smaller than a characteristic width of 0.1 pc suggested by Herschel observations. The filaments can be classified into two types based on their properties. The first type, located in the northeast of the SE subcluster, has larger velocity gradients, smaller masses, and nearly critical mass-per-unit-length ratios. The other type, located in the southwest of the SE subcluster, has the opposite properties. Several YSOs are formed along two filaments which have supercritical mass per unit length ratios, while filaments with nearly critical massper- unit-length ratios are not associated with YSOs, suggesting that stars are formed on gravitationally unstable filaments.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/797/2/76DOIArticle
http://iopscience.iop.org/0004-637X/797/2/76/PublisherArticle
http://arxiv.org/abs/1410.3514arXivDiscussion Paper
ORCID:
AuthorORCID
Tobin, John J.0000-0002-6195-0152
Additional Information:© 2014 American Astronomical Society. Received 2014 July 20; accepted 2014 October 7; published 2014 November 26. We thank the anonymous referee for valuable comments to improve the paper. CLASSy was supported by AST-1139950 (University of Illinois) and AST-1139998 (University of Maryland). Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of Illinois, California, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA consortium universities.
Funders:
Funding AgencyGrant Number
NSFAST-1139950
NSFAST-1139998
Gordon and Betty Moore FoundationUNSPECIFIED
Kenneth T. and Eileen L. Norris FoundationUNSPECIFIED
James S. McDonnell FoundationUNSPECIFIED
Caltech AssociatesUNSPECIFIED
University of ChicagoUNSPECIFIED
states of California, Illinois, and MarylandUNSPECIFIED
CARMA consorutim universitiesUNSPECIFIED
Subject Keywords:ISM: clouds; ISM: kinematics and dynamics; ISM: molecules; ISM: structure; stars: formation
Record Number:CaltechAUTHORS:20150115-103442804
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20150115-103442804
Official Citation:CARMA Large Area Star Formation Survey: Structure and Kinematics of Dense Gas in Serpens Main Katherine I. Lee et al. 2014 ApJ 797 76
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:53774
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:15 Jan 2015 20:11
Last Modified:26 May 2017 18:15

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