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Title: 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

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{sup −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{sup −1}, similar to that of other runaway stars in Orion,more » 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.« less

Authors:
; ; ;  [1];  [2]; ; ;  [3];  [4];  [5];  [6];  [7];  [8]; ;  [9];  [10];  [11]
  1. Instituto de Astrofísica de Andalucía (CSIC) Glorieta de la Astronomía s/n E-18008 Granada (Spain)
  2. Ritter Astrophysical Research Center, Department of Physics and Astronomy University of Toledo 2801 West Bancroft Street Toledo, OH 43606 (United States)
  3. Instituto de Radioastronomía y Astrofísica, UNAM Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacán (Mexico)
  4. Homer L. Dodge Department of Physics and Astronomy University of Oklahoma, Norman, OK 73019 (United States)
  5. Department of Astronomy, University of Concepción Concepción (Chile)
  6. IPAC, Mail Code 314-6, Caltech 1200 E. California Boulevard, Pasadena, CA 91125 (United States)
  7. Space Telescope Science Institute 3700 San Martin Drive, Baltimore, MD 21218 (United States)
  8. Tata Institute of Fundamental Research Homi Bhabha Road, Mumbai 400 005 (India)
  9. European Space Astronomy Center, ESA P.O. Box 78, E-28691 Villanueva de la Cañada, Madrid (Spain)
  10. European Southern Observatory Garching bei München (Germany)
  11. Department of Physics and Astronomy, University of Rochester Rochester, NY 14627 (United States)
Publication Date:
OSTI Identifier:
22663651
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 840; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; DETECTION; DISTANCE; ELECTRONS; EMISSION; MASS; MIXING; OPACITY; PROPER MOTION; PROTOSTARS; RELATIVISTIC RANGE; STARS; SYNCHROTRON RADIATION; VELOCITY

Citation Formats

Osorio, Mayra, Díaz-Rodríguez, Ana K., Anglada, Guillem, Gómez, José F., Megeath, S. Thomas, Rodríguez, Luis F., Loinard, Laurent, Carrasco-González, Carlos, Tobin, John J., Stutz, Amelia M., Furlan, Elise, Fischer, William J., Manoj, P., González-García, Beatriz, Vavrek, Roland, Stanke, Thomas, and Watson, Dan M., E-mail: osorio@iaa.es. 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. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA6975.
Osorio, Mayra, Díaz-Rodríguez, Ana K., Anglada, Guillem, Gómez, José F., Megeath, S. Thomas, Rodríguez, Luis F., Loinard, Laurent, Carrasco-González, Carlos, Tobin, John J., Stutz, Amelia M., Furlan, Elise, Fischer, William J., Manoj, P., González-García, Beatriz, Vavrek, Roland, Stanke, Thomas, & Watson, Dan M., E-mail: osorio@iaa.es. 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. United States. doi:10.3847/1538-4357/AA6975.
Osorio, Mayra, Díaz-Rodríguez, Ana K., Anglada, Guillem, Gómez, José F., Megeath, S. Thomas, Rodríguez, Luis F., Loinard, Laurent, Carrasco-González, Carlos, Tobin, John J., Stutz, Amelia M., Furlan, Elise, Fischer, William J., Manoj, P., González-García, Beatriz, Vavrek, Roland, Stanke, Thomas, and Watson, Dan M., E-mail: osorio@iaa.es. Mon . "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". United States. doi:10.3847/1538-4357/AA6975.
@article{osti_22663651,
title = {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},
author = {Osorio, Mayra and Díaz-Rodríguez, Ana K. and Anglada, Guillem and Gómez, José F. and Megeath, S. Thomas and Rodríguez, Luis F. and Loinard, Laurent and Carrasco-González, Carlos and Tobin, John J. and Stutz, Amelia M. and Furlan, Elise and Fischer, William J. and Manoj, P. and González-García, Beatriz and Vavrek, Roland and Stanke, Thomas and Watson, Dan M., E-mail: osorio@iaa.es},
abstractNote = {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{sup −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{sup −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.},
doi = {10.3847/1538-4357/AA6975},
journal = {Astrophysical Journal},
number = 1,
volume = 840,
place = {United States},
year = {Mon May 01 00:00:00 EDT 2017},
month = {Mon May 01 00:00:00 EDT 2017}
}