CaltechAUTHORS
  A Caltech Library Service

Characterizing the Low-Mass Molecular Component in the Northern Small Magellanic Cloud

Muller, E. and Ott, J. and Hughes, A. and Pineda, J. L. and Wong, T. and Mizuno, N. and Kawamura, A. and Mizuno, Y. and Fukui, Y. and Onishi, T. and Rubio, M. (2010) Characterizing the Low-Mass Molecular Component in the Northern Small Magellanic Cloud. Astrophysical Journal, 712 (2). pp. 1248-1258. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20100408-095835101

[img]
Preview
PDF - Published Version
See Usage Policy.

883Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20100408-095835101

Abstract

We present here the first results from a high-resolution survey of the ^(12)CO(J = 1-0) emission across the northern part of the poorly enriched Small Magellanic Cloud (SMC), made with the ATNF Mopra telescope. Three molecular complexes detected in the lower resolution NANTEN survey are mapped with a beam FWHM of ~42", to sensitivities of approximately 210 mK per 0.9 km s^(–1) channel, resolving each complex into 4-7 small clouds of masses in the range of M_(vir) ~ 10^(3)-10^(4) M_☉ and with radii no larger than 16 pc. The northern SMC CO clouds follow similar empirical relationships to the southern SMC population, yet they appear relatively under-luminous for their size, suggesting that the star-forming environment in the SMC is not homogeneous. Our data also suggests that the CO cloud population has little or no extended CO envelope on scales ≳30 pc, further evidence that the weak CO component in the north SMC is being disassociated by penetrating UV radiation. The new high-resolution data provide evidence for a variable correlation of the CO integrated brightness with integrated H I and 160 μm emission; in particular CO is often, but not always, found coincident with peaks of 160 μm emission, verifying the need for matching-resolution 160 μm and H I data for a complete assessment of the SMC H_2 mass.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/712/2/1248DOIArticle
http://iopscience.iop.org/0004-637X/712/2/1248PublisherArticle
ORCID:
AuthorORCID
Ott, J.0000-0001-8224-1956
Additional Information:© 2010 American Astronomical Society. Issue 2 (2010 April 1): received 2009 June 5; accepted for publication 2010 January 26; published 2010 March 12. All astronomical images used in this publication were made with the use of the karma package (Gooch 1997). J.L.P. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered byOak Ridge Associated Universities through a contract with NASA. M.R. wishes to acknowledge support from FONDECYT (CHILE) grant No. 1080335. M.R. is supported by the Chilean Center for Astrophysics FONDAP No. 15010003.
Funders:
Funding AgencyGrant Number
NASA Postdoctoral ProgramUNSPECIFIED
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1080335
Fondo de Financiamiento de Centros de Investigación en Áreas Prioritarias (FONDAP)15010003
Subject Keywords:galaxies: dwarf; ISM: molecules; Magellanic Clouds; radio lines: galaxies; stars: evolution
Classification Code:PACS: 98.56.Si; 98.58.Db; 98.58.Bz
Record Number:CaltechAUTHORS:20100408-095835101
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20100408-095835101
Official Citation:E. Muller et al 2010 ApJ 712 1248 doi: 10.1088/0004-637X/712/2/1248
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17897
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:08 Apr 2010 18:34
Last Modified:03 Nov 2017 20:26

Repository Staff Only: item control page