2017ApJ...840...36O


Query : 2017ApJ...840...36O

2017ApJ...840...36O - Astrophys. J., 840, 36-36 (2017/May-1)

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 M., DIAZ-RODRIGUEZ A.K., ANGLADA G., MEGEATH S.T., RODRIGUEZ L.F., TOBIN J.J., STUTZ A.M., FURLAN E., FISCHER W.J., MANOJ P., GOMEZ J.F., GONZALEZ-GARCIA B., STANKE T., WATSON D.M., LOINARD L., VAVREK R. and CARRASCO-GONZALEZ C.

Abstract (from CDS):

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.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): 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 - stars: protostars

CDS comments: Knots VLA 12C, VLA 12N and VLA 12S are not in SIMBAD.

Simbad objects: 25

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Number of rows : 25
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 3C 48 QSO 01 37 41.2996631208 +33 09 35.080388820   16.62 16.20     ~ 2697 2
2 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2174 1
3 V* V1326 Ori BY* 05 35 09.7681644000 -05 23 26.898475704 16.267 14.776 13.806   11.678 K8 62 0
4 V* V2254 Ori Or* 05 35 14.11296 -05 22 22.7316           B 305 2
5 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2176 1
6 [MWZ90] OMC-2 FIR 6 IR 05 35 22.6 -05 12 37           ~ 21 0
7 HOPS 68 Y*O 05 35 24.2999 -05 08 30.686           ~ 57 0
8 [TSO2008] 24 Y*? 05 35 24.6 -05 07 53           ~ 25 0
9 GBS-VLA J053525.96-050543.3 Rad 05 35 25.96 -05 05 43.3           ~ 6 0
10 NAME OMC-2 IRS 3 HII 05 35 26.00 -05 10 16.6           ~ 64 0
11 V* V2457 Ori Or* 05 35 26.97000 -05 09 54.4644         18.858 ~ 140 0
12 OMC 2 MoC 05 35 27 -05 10.1           ~ 433 1
13 HOPS 108 Y*O 05 35 27.07 -05 10 00.4           ~ 22 0
14 JW 808 Y*O 05 35 27.4713701592 -05 09 44.128270008         14.407 M2e 27 0
15 2MASS J05352762-0509337 Y*O 05 35 27.622 -05 09 33.78           ~ 88 0
16 V* V2467 Ori Or* 05 35 27.6431954136 -05 09 37.148090580         19.580 ~ 41 0
17 TKK 870 Y*O 05 35 28.19 -05 03 41.2           ~ 44 0
18 M 43 HII 05 35 31 -05 16.2           ~ 180 0
19 NAME Ori A MoC 05 38 -07.1           ~ 2870 0
20 QSO B0539-057 QSO 05 41 38.0825893728 -05 41 49.441027200     20.4 20.70   ~ 230 2
21 ICRF J054236.1+495107 Sy1 05 42 36.1380355416 +49 51 07.232213736   18.45 17.80 17.210   ~ 1401 1
22 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4118 2
23 HH 80 HH 18 19 06.1 -20 51 49           ~ 97 0
24 HH 81 HH 18 19 06.7 -20 51 06           ~ 86 0
25 HH 80N HH 18 19 19.74 -20 41 34.9           ~ 38 0

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2022.10.03-00:49:08

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