2012A&A...548A..69N


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.03CET13:41:12

2012A&A...548A..69N - Astronomy and Astrophysics, volume 548A, 69-69 (2012/12-1)

Outflow structure and velocity field of Orion source. I. ALMA imaging of SiO isotopologue maser and thermal emission.

NIEDERHOFER F., HUMPHREYS E.M.L. and GODDI C.

Abstract (from CDS):

Using Science Verification data from the Atacama Large Millimeter/Submillimeter Array (ALMA), we have identified and imaged five rotational transitions (J=5-4 and J=6-5) of the three silicon monoxide isotopologues 28SiO v=0, 1, 2 and 29SiO v=0 and 28Si18O v=0 in the frequency range from 214 to 246 GHz towards the Orion BN/KL region. The emission of the ground-state 28SiO, 29SiO and 28Si18O shows an extended bipolar shape in the northeast-southwest direction at the position of Radio Source I, indicating that these isotopologues trace an outflow (∼18km/s, PA∼50°, ∼5000AU in diameter) that is driven by this embedded high-mass young stellar object (YSO). Whereas on small scales (10-1000AU) the outflow from Source I has a well-ordered spatial and velocity structure, as probed by Very Long Baseline Interferometry (VLBI) imaging of SiO masers, the large scales (500-5000AU) probed by thermal SiO with ALMA reveal a complex structure and velocity field, most likely related to the effects of the environment of the BN/KL region on the outflow emanating from Source I. The emission of the vibrationally-excited species peaks at the position of Source I. This emission is compact and not resolved at an angular resolution of ∼1.5" (∼600AU at a distance of 420pc). 2D Gaussian fitting to individual velocity channels locates emission peaks within radii of 100AU, i.e. they trace the innermost part of the outflow. A narrow spectral profile and spatial distribution of the v=1 J=5-4 line similar to the masing v=1 J=1-0 transition, provide evidence for the most highly rotationally excited (frequency >200GHz) SiO maser emission associated with Source I known to date. The maser emission will enable studies of the Source I disk-outflow interface with future ALMA longest baselines.

Abstract Copyright:

Journal keyword(s): ISM: individual objects: Orion KL - ISM: jets and outflows - stars: formation - masers

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1025 2
2 V* V2254 Ori Or* 05 35 14.11296 -05 22 22.7316           B 291 2
3 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2032 1
4 [GD77] A IR 05 35 14.19 -05 22 34.0           ~ 59 0
5 MLLA 610 IR 05 35 14.278 -05 22 30.65           ~ 70 0
6 COUP 621 Y*O 05 35 14.35371 -05 22 32.8820           ~ 104 0
7 NAME Orion Core ? 05 35 14.5 -05 22 30           ~ 176 0
8 [RLK73] IRc 2a Y*O 05 35 14.511 -05 22 30.40           ~ 112 0
9 [RLK73] IRc 11 IR 05 35 14.71 -05 22 30.8           ~ 8 0
10 [RLK73] IRc 12 IR 05 35 14.81 -05 22 31.3           ~ 10 0
11 QSO B0605-0834 BLL 06 07 59.69923743 -08 34 49.9781718     18.5 17.70   ~ 400 1

    Equat.    Gal    SGal    Ecl

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2020.12.03-13:41:12

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