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Star Formation Under the Outflow: The Discovery of a Non-thermal Jet from OMC-2 FIR 3 and Its Relationship to the Deeply Embedded FIR 4 Protostar

Osorio, Mayra and Díaz-Rodríguez, Ana K. and Anglada, Guillem and Megeath, S. Thomas and Rodríguez, Luis F. and Tobin, John J. and Stutz, Amelia M. and Furlan, Elise and Fischer, William J. and Manoj, P. and Gómez, José F. and González-García, Beatriz and Stanke, Thomas and Watson, Dan M. and Loinard, Laurent and Vavrek, Roland and Carrasco-González, Carlos (2017) Star Formation Under the Outflow: The Discovery of a Non-thermal Jet from OMC-2 FIR 3 and Its Relationship to the Deeply Embedded FIR 4 Protostar. Astrophysical Journal, 840 (1). Art. No. 36. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20170503-110229099

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Abstract

We carried out multiwavelength (0.7–5 cm), multi-epoch (1994–2015) Very Large Array (VLA) observations toward the region enclosing the bright far-IR sources FIR 3 (HOPS 370) and FIR 4 (HOPS 108) in OMC-2. We report the detection of 10 radio sources, 7 of them identified as young stellar objects. We image a well-collimated radio jet with a thermal free–free core (VLA 11) associated with the Class I intermediate-mass protostar HOPS 370. The jet features several knots (VLA 12N, 12C, 12S) of non-thermal radio emission (likely synchrotron from shock-accelerated relativistic electrons) at distances of ~7500–12,500 au from the protostar, in a region where other shock tracers have been previously identified. These knots are moving away from the HOPS 370 protostar at ~100 km s^(−1). The Class 0 protostar HOPS 108, which itself is detected as an independent, kinematically decoupled radio source, falls in the path of these non-thermal radio knots. These results favor the previously proposed scenario in which the formation of HOPS 108 is triggered by the impact of the HOPS 370 outflow with a dense clump. However, HOPS 108 has a large proper motion velocity of ~30 km s^(−1), similar to that of other runaway stars in Orion, whose origin would be puzzling within this scenario. Alternatively, an apparent proper motion could result because of changes in the position of the centroid of the source due to blending with nearby extended emission, variations in the source shape, and/or opacity effects.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa6975DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa6975/metaPublisherArticle
https://arxiv.org/abs/1703.07877arXivDiscussion Paper
ORCID:
AuthorORCID
Megeath, S. Thomas0000-0001-7629-3573
Rodríguez, Luis F.0000-0003-2737-5681
Tobin, John J.0000-0002-6195-0152
Stutz, Amelia M.0000-0003-2300-8200
Furlan, Elise0000-0001-9800-6248
Fischer, William J.0000-0002-3747-2496
Manoj, P.0000-0002-3530-304X
Loinard, Laurent0000-0002-5635-3345
Additional Information:© 2017 The American Astronomical Society. Received 2017 February 12; revised 2017 March 22; accepted 2017 March 22; published 2017 May 3. A.K.D.R. acknowledges a Spanish MECD FPU fellowship. G.A., A.K.D.R., J.F.G., and M.O. acknowledge support from MINECO (Spain) AYA2014-57369-C3-3-P grant (co-funded by FEDER). A.S. is thankful for funding from the "Concurso Proyectos Internacionales de Investigacion, Convocatoria 2015" (project code PII20150171) and the BASAL Centro de Astrofisica y Tecnologias Afines (CATA) PFB-06/2007. The authors thank Alvaro Sanchez-Monge for helpful suggestions and Jouni Kainulainen for providing the 3 mm ALMA image of this region. Facility: VLA. Software: CASA (v 4.2.2), AIPS.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Ministerio de Educación, Cultura y Deporte (MECD)UNSPECIFIED
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2014-57369-C3-3-P
Fondo Europeo de Desarrollo Regional (FEDER)UNSPECIFIED
Concurso Proyectos Internacionales de Investigacion, Convocatoria 2015PII20150171
Basal-CATAPFB-06/2007
Subject Keywords:ISM: jets and outflows – proper motions – radio continuum: stars – stars: formation – stars: individual (OMC-2 FIR 3, HOPS 370, OMC-2 FIR 4, HOPS 108) – stars: protostars
Issue or Number:1
Record Number:CaltechAUTHORS:20170503-110229099
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170503-110229099
Official Citation:Mayra Osorio et al 2017 ApJ 840 36
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:77156
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:03 May 2017 18:14
Last Modified:07 Nov 2019 00:18

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