2022A&A...657A.110F


Query : 2022A&A...657A.110F

2022A&A...657A.110F - Astronomy and Astrophysics, volume 657A, 110-110 (2022/1-1)

High-resolution images of two wiggling stellar jets, MHO 1502 and MHO 2147, obtained with GSAOI+GeMS.

FERRERO L.V., GUNTHARDT G., GARCIA L., GOMEZ M., KALARI V.M. and SALDANO H.P.

Abstract (from CDS):


Aims. We investigated the possible cause-effect relation between the wiggling shape of two stellar jets, MHO 1502 and MHO 2147, and the potential binarity of the respective driving stars.
Methods. We present high-angular-resolution H2 (2.122 µm) and K-band images obtained with the Gemini South Adaptive Optics Imager (GSAOI) and the Gemini Multi-conjugate Adaptive Optics System (GeMS). The profiles of the jets are depicted in detail by the H2 images. We used K-band data to search for potential close companions to the previously suggested exciting sources, and used archive data to investigate these sources and the environments in which the jets are located. We also applied a model to reproduce the wiggling profiles of the jets.
Results. MHO 1502 is composed of a chain of knots delineating the wiggling jet, suggesting that the driving source emitted them in an intermittent manner. Our K-band image of the previously proposed exciting star, IRAC 18064, shows two sources separated by ∼240 AU, hinting at its binarity. However, as IRAC 18064 is located off the jet axis at ∼2064 AU, it is questionable as to whether this source is the true exciting star. Moreover, the orbital model centred on IRAC 18064 suggests a binary companion at a much greater distance (∼2200 AU) than the nearby star (at ∼240 AU). On the other hand, the orbital model centred on the axis provides the best fits. Nevertheless, the precession model centred on the axis cannot be discarded, despite having larger residuals and χ2. MHO 2147 displays an S-shaped gentle continuous emission in H2. We identify two other jets in the field of MHO 2147: a previously reported quasi-perpendicular jet, MHO 2148, and a third jet adjacent to MHO 2147. The model that best fits the morphology of the MHO 2147 jet and that of its adjacent jet is precession. The exciting source of MHO 2147 may be a triple system.

Abstract Copyright: © ESO 2022

Journal keyword(s): stars: jets - stars: protostars - infrared: ISM - ISM: jets and outflows - ISM: individual objects: MHO 1502 - ISM: individual objects: MHO 2147

CDS comments: Tables and figures : jets not in SIMBAD.

Simbad objects: 37

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Number of rows : 37
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HW 2 Cl* 00 27 57.0 -74 00 05           ~ 19 0
2 HH 211 Y*O 03 43 56.52 +32 00 52.8           ~ 343 0
3 [SS94] V410 X-ray 7 TT* 04 18 42.5008529280 +28 18 49.922715996       18.02 15.42 M0.5e 41 0
4 V* V1213 Tau Or* 04 31 37.5055489536 +18 12 24.383952396           K7 548 0
5 HH 34 HH 05 35 31.30 -06 28 43.0     16     ~ 479 2
6 NAME V380 Ori-NE * 05 36 40.6 -06 38 03           ~ 38 0
7 V* FU Ori Or* 05 45 22.3647842544 +09 04 12.291320064   10.72 9.60     F0Iab 774 1
8 HH 111 HH 05 51 44.2 +02 48 34           ~ 399 0
9 HH 121 HH 05 51 46.2 +02 48 32           ~ 39 0
10 HH 47 HH 08 25 44.30 -51 00 26.2           ~ 244 0
11 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1190 2
12 NAME Vela-D Molecular Cloud MoC 08 39 -41.0           ~ 46 0
13 MHO 1502 out 08 45 33.94 -43 51 21.8           ~ 1 0
14 [SEC2010] IRAC 18064 IR 08 45 34.51 -43 51 57.3           ~ 2 0
15 [MDE2007] MMS2 mm 08 45 34.80 -43 52 04.1           ~ 8 0
16 GAL 263.62-00.53 HII 08 45 34.9 -43 51 07           ~ 10 1
17 IRAS 08438-4340 * 08 45 35.8 -43 51 02           G3III 26 1
18 IRAS 12272-6240 HII 12 30 03.7 -62 56 49           ~ 10 0
19 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3446 1
20 MHO 2147 EmO 17 55 46.0 -24 40 40           ~ 3 0
21 AGAL G004.827+00.231 cor 17 55 49 -24 40.3           ~ 9 0
22 MHO 2148 EmO 17 55 49.0 -24 40 20           ~ 2 0
23 EGO G004.83+0.23 out 17 55 49.0 -24 40 19           ~ 4 0
24 IRAS 17527-2439 HII 17 55 49.1 -24 40 20           ~ 17 0
25 DOBASHI 0238 DNe 17 56 00.5 -24 41 25           ~ 2 1
26 IRAS 18555+0056 Y*O 18 58 08.4622214520 +01 00 41.630408028           ~ 4 0
27 [DLW84] G35.2N HII 18 58 13.036 +01 40 36.00           ~ 108 0
28 GAL 079.3+00.3 DNe 20 32.3 +40 15           ~ 13 1
29 IRAS 20305+4010 Y*O 20 32 22.08624 +40 20 17.1600           ~ 13 0
30 2MASS J20322301+4019226 Y*O 20 32 23.0150178672 +40 19 22.577908152     17.32   14.32 ~ 4 0
31 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 549 0
32 NAME Cepheus A SFR 22 56 17.9 +62 01 49           ~ 724 2
33 HH 168 HH 22 56 18.0 +62 01 47           ~ 90 0
34 HH 169 HH 22 56 34.8 +62 02 36           ~ 6 0
35 HH 174 HH 22 56 58.5 +62 01 42           ~ 5 0
36 HH 377 HH 23 03 +61.7           ~ 21 2
37 NAME Cep E HII 23 03 12.779 +61 42 25.75           ~ 165 0

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2023.01.27-18:12:16

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