2006A&A...447..577G


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.23CET19:10:03

2006A&A...447..577G - Astronomy and Astrophysics, volume 447, 577-587 (2006/2-4)

Tracing the base of protostellar wind(s) towards the high-mass star forming region AFGL 5142: VLA continuum and VLBA H2O maser observations.

GODDI C. and MOSCADELLI L.

Abstract (from CDS):

We have conducted phase-reference multi-epoch observations of the 22.2GHz water masers using the Very Long Baseline Array (VLBA) and a multi-frequency study of the continuum emission using the Very Large Array (VLA) towards the high-mass star forming region (SFR) AFGL 5142. 29 maser features were identified and most of them were persistent over the four observing epochs, allowing absolute proper motions to be determined. The water maser emission comes from two elongated structures (indicated as Group I and Group II), with the measured proper motions aligned along the structures' elongation axes. Each group consists of two (blue- and red-shifted) clusters of features separated by a few hundreds and thousands of AU respectively for Group I and Group II. The maser features of Group II have both positions and velocities aligned along a direction close to the axis of the outflow traced by HCO+ and SiO emission on angular scales of tens of arcsec. We predict that the maser emission arises from dense, shocked molecular clumps displaced along the axis of the molecular outflow. The two maser clusters of Group I are oriented on the sky along a direction forming a large angle (>60°) with the axis of the jet/outflow traced by Group II maser features. We have detected a compact (8.4 and 22GHz) continuum source (previously reported at 4.9 and 8.4GHz) that falls close to the centroid of Group I masers, indicating that the source ionizing the gas is also responsible for the excitation of the water masers. The kinematic analysis indicates that the Group I masers trace outflowing rather than rotating gas, discarding the Keplerian disk scenario proposed in a previous paper for Group I. Since the axis joining the two maser clusters of Group II does not cross the position of the continuum source, Group II masers might be excited by an (undetected) massive YSO, distinct from the one (pinpointed by the VLA continuum emission) responsible for the excitation of the Group I masers. Our results give support to models of accretion and jet ejection related to the formation of high-mass stars.

Abstract Copyright:

Journal keyword(s): masers - stars: formation - ISM: kinematics and dynamics - ISM: jets and outflows - accretion, accretion disks - radio continuum: ISM

CDS comments: Table 3: H2O Maser features in AFGL 5142 not in SIMBAD.

Simbad objects: 20

goto Full paper

goto View the reference in ADS

Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 324 0
2 4C 32.14 QSO 03 36 30.10760600 +32 18 29.3422210     17.50 16.6   ~ 572 1
3 NVSS J051805+330612 Rad 05 18 05.14244722 +33 06 13.3646794           ~ 11 1
4 GAL 174.20-00.08 Cld 05 30 45.9 +33 47 56           ~ 182 2
5 NAME AFGL 5142 IRS 2 * 05 30 46.0699160885 +33 47 54.255210315           ~ 5 0
6 2MASS J05304798+3347549 Y*O 05 30 47.982 +33 47 54.94           ~ 7 0
7 QSO J0530+13 QSO 05 30 56.41672 +13 31 55.1495     20.0 19.35   ~ 876 1
8 OMC 2 MoC 05 35 27 -05 10.1           ~ 376 1
9 ICRF J054236.1+495107 Sy1 05 42 36.13789843 +49 51 07.2337251   18.45 17.80 17.210   ~ 1244 1
10 [PGS81] IRS 3 IR 05 47 04.63 +00 21 47.9           ~ 50 0
11 [PGS81] IRS 1 Y*O 05 47 04.78 +00 21 42.8           ~ 73 0
12 [PGS81] IRS 2 Y*O 05 47 05.388 +00 21 50.05           ~ 30 0
13 7C 055201.39+394824.00 QSO 05 55 30.80561150 +39 48 49.1649664     18.0 17.5   ~ 459 2
14 NAME SH 2-255 IRS 1 Y*O 06 12 54.0060 +17 59 22.958           ~ 312 0
15 IC 2162 HII 06 13 04.1 +17 58 44           ~ 336 2
16 7C 064253.00+445430.00 QSO 06 46 32.02599463 +44 51 16.5901237   19.57 18.49 18.64   ~ 316 1
17 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 392 0
18 [HRB81] W75N(Ba) HII 20 38 36.445 +42 37 34.82           ~ 43 0
19 IRAS 23004+5642 FIR 23 02 34.712 +56 59 17.02           ~ 24 0
20 IRAS 23139+5939 MoC 23 16 10.03 +59 55 31.3           ~ 69 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2006A&A...447..577G and select 'bookmark this link' or equivalent in the popup menu


2020.02.23-19:10:03

© Université de Strasbourg/CNRS

    • Contact