2011A&A...529A..24Z


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.17CET09:40:34

2011A&A...529A..24Z - Astronomy and Astrophysics, volume 529A, 24-24 (2011/5-1)

Orion KL: the hot core that is not a ``hot core''.

ZAPATA L.A., SCHMID-BURGK J. and MENTEN K.M.

Abstract (from CDS):

We present sensitive high angular resolution submillimeter and millimeter observations of torsionally/vibrationally highly excited lines of the CH3OH, HC3N, SO2, and CH3CN molecules and of the continuum emission at 870 and 1300µm from the Orion KL region, made with the Submillimeter Array (SMA). These observations and SMA CO J=3-2 and J=2-1 imaging of the explosive flow originating in this region suggest that the molecular Orion ``hot core'' is a pre-existing density enhancement heated from the outside by the explosive event. Unlike in other hot cores, we do not find any self-luminous submillimeter, radio, or infrared source embedded in the hot molecular gas, nor observe filamentary CO flow structures or ``fingers'' in the shadow of the hot core pointing away from the explosion center. The low-excitation CH3CN emission shows the typical molecular heart-shaped structure, traditionally named the hot core, and is centered close to the dynamical origin of the explosion. The highest excitation CH3CN lines all originate from the northeast lobe of the heart-shaped structure, i.e. from the densest and most highly obscured parts of the extended ridge. The torsionally excited CH3OH and vibrationally excited HC3N lines appear to form a shell around the strongest submillimeter continuum source. All of these observations suggest that the southeast and southwest sectors of the explosive flow have impinged on a pre-existing very dense part of the extended ridge, thus creating the bright Orion KL hot core. However, additional theoretical and observational studies are required to test this new heating scenario.

Abstract Copyright:

Journal keyword(s): molecular data - methods: observational - techniques: interferometric - ISM: jets and outflows - ISM: molecules - ISM: kinematics and dynamics

CDS comments: Sources SMMN not used in Simbad.

Simbad objects: 20

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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 W 3 OH HII 02 27 04.1 +61 52 22           ~ 929 2
2 NAME Turner-Welch Object Y*O 02 27 04.717 +61 52 24.73           ~ 31 0
3 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1020 2
4 Mrk 1506 Sy1 04 33 11.0958197353 +05 21 15.617543663   15.72 15.05 10.08   ~ 1808 2
5 QSO J0530+13 QSO 05 30 56.41672 +13 31 55.1495     20.0 19.35   ~ 871 1
6 NAME Orion S reg 05 35 12.9 -05 24 10           ~ 117 0
7 V* V2254 Ori Or* 05 35 14.113 -05 22 22.73           B 277 2
8 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 1945 1
9 NAME Ori N Y*O 05 35 14.35371 -05 22 32.8820           ~ 100 0
10 [RLK73] IRc 2c X 05 35 14.39867 -05 22 30.3648           ~ 22 0
11 [RLK73] IRc 2d IR 05 35 14.45 -05 22 29.9           ~ 19 0
12 [RLK73] IRc 2b IR 05 35 14.473 -05 22 29.61           ~ 20 0
13 JCMTSE J053514.4-052232 Y*? 05 35 14.488 -05 22 32.10           ~ 46 0
14 NAME Orion Core ? 05 35 14.5 -05 22 30           ~ 171 0
15 [RLK73] IRc 2a Y*O 05 35 14.511 -05 22 30.40           ~ 112 0
16 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 560 1
17 COUP 662 * 05 35 14.8982780 -05 22 25.410079           ~ 32 0
18 QSO B0539-057 QSO 05 41 38.08338 -05 41 49.4284     20.4 20.70   ~ 195 2
19 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 812 1
20 QSO B0605-0834 QSO 06 07 59.69923743 -08 34 49.9781718     18.5 17.70   ~ 381 1

    Equat.    Gal    SGal    Ecl

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2019.11.17-09:40:34

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