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The Gould's Belt Very Large Array Survey. I. The Ophiuchus Complex

Dzib, Sergio A. and Loinard, Laurent and Mioduszewski, Amy J. and Rodríguez, Luis F. and Ortiz-Leόn, Gisela N. and Pech, Gerardo and Rivera, Juana L. and Torres, Rosa M. and Boden, Andrew F. and Hartmann, Lee and Evans, Neal J., II and Briceño, Cesar and Tobin, John (2013) The Gould's Belt Very Large Array Survey. I. The Ophiuchus Complex. Astrophysical Journal, 775 (1). Art. No. 63. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20131025-091711356

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Abstract

We present large-scale (~2000 arcmin^2), deep (~20 μJy), high-resolution (~1") radio observations of the Ophiuchus star-forming complex obtained with the Karl G. Jansky Very Large Array at λ = 4 and 6 cm. In total, 189 sources were detected, 56 of them associated with known young stellar sources, and 4 with known extragalactic objects; the other 129 remain unclassified, but most of them are most probably background quasars. The vast majority of the young stars detected at radio wavelengths have spectral types K or M, although we also detect four objects of A/F/B types and two brown dwarf candidates. At least half of these young stars are non-thermal (gyrosynchrotron) sources, with active coronas characterized by high levels of variability, negative spectral indices, and (in some cases) significant circular polarization. As expected, there is a clear tendency for the fraction of non-thermal sources to increase from the younger (Class 0/I or flat spectrum) to the more evolved (Class III or weak line T Tauri) stars. The young stars detected both in X-rays and at radio wavelengths broadly follow a Güdel-Benz relation, but with a different normalization than the most radioactive types of stars. Finally, we detect a ~70 mJy compact extragalactic source near the center of the Ophiuchus core, which should be used as gain calibrator for any future radio observations of this region.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/775/1/63DOIArticle
http://iopscience.iop.org/0004-637X/775/1/63PublisherArticle
ORCID:
AuthorORCID
Dzib, Sergio A.0000-0001-6010-6200
Loinard, Laurent0000-0002-5635-3345
Rodríguez, Luis F.0000-0003-2737-5681
Rivera, Juana L.0000-0002-7631-2620
Hartmann, Lee0000-0003-1430-8519
Evans, Neal J., II0000-0001-5175-1777
Briceño, Cesar0000-0001-7124-4094
Tobin, John0000-0002-6195-0152
Additional Information:© 2013 American Astronomical Society. Received 2013 June 5; accepted 2013 July 18; published 2013 September 5. L.L. is grateful to the von Humboldt Stiftung for financial support. S.D., L.L., L.F.R., G.N.O., G.P., and J.L.R. acknowledge the financial support of DGAPA, UNAM, and CONACyT, México. The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. CASA is developed by an international consortium of scientists based at the National Radio Astronomical Observatory (NRAO), the European Southern Observatory (ESO), the National Astronomical Observatory of Japan (NAOJ), the CSIRO Australia Telescope National Facility (CSIRO/ATNF), and the Netherlands Institute for Radio Astronomy (ASTRON) under the guidance of NRAO. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
Funders:
Funding AgencyGrant Number
Alexander von Humboldt FoundationUNSPECIFIED
DGAPA (Mexico)UNSPECIFIED
UNAM (Mexico)UNSPECIFIED
CONACyT (Mexico)UNSPECIFIED
Subject Keywords: astrometry; magnetic fields; radiation mechanisms: non-thermal; radio continuum: stars; techniques: interferometric
Issue or Number:1
Record Number:CaltechAUTHORS:20131025-091711356
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20131025-091711356
Official Citation: The Gould's Belt Very Large Array Survey. I. The Ophiuchus Complex Sergio A. Dzib et al. 2013 ApJ 775 63
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42060
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:25 Oct 2013 16:36
Last Modified:07 Nov 2019 00:43

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