2018ApJ...856..147O


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.10CEST22:21:17

2018ApJ...856..147O - Astrophys. J., 856, 147-147 (2018/April-1)

Gravitationally unstable condensations revealed by ALMA in the TUKH122 prestellar core in the Orion A cloud.

OHASHI S., SANHUEZA P., SAKAI N., KANDORI R., CHOI M., HIROTA T., NGUYEN-LU'O'NG Q. and TATEMATSU K.

Abstract (from CDS):

We have investigated the TUKH122 prestellar core in the Orion A cloud using ALMA 3 mm dust continuum, N2H+ (J = 1-0), and CH3OH (JK=2K-1K) molecular-line observations. Previous studies showed that TUKH122 is likely on the verge of star formation because the turbulence is almost dissipated and chemically evolved among other starless cores in the Orion A cloud. By combining ALMA 12 m and ACA data, we recover extended emission with a resolution of ∼5'' corresponding to 0.01 pc and identify six condensations with a mass range of 0.1-0.4 M and a radius of <=0.01 pc. These condensations are gravitationally bound following a virial analysis and are embedded in the filament, including the elongated core with a mass of ∼29 M and a radial density profile of r–1.6 derived by Herschel. The separation of these condensations is ∼0.035 pc, consistent with the thermal Jeans length at a density of 4.4 x 105 cm–3. This density is similar to the central part of the core. We also find a tendency for the N2H+ molecule to deplete at the dust peak condensation. This condensation may be beginning to collapse because the line width becomes broader. Therefore, the fragmentation still occurs in the prestellar core by thermal Jeans instability, and multiple stars are formed within the TUKH122 prestellar core. The CH3OH emission shows a large shell-like distribution and surrounds these condensations, suggesting that the CH3OH molecule formed on dust grains is released into the gas phase by nonthermal desorption such as photoevaporation caused by cosmic-ray-induced UV radiation.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): ISM: clouds - ISM: individual objects: Orion Nebula, Orion Molecular Cloud - ISM: molecules - ISM: structure - stars: formation

Nomenclature: Table 2: [OSS2018] MMN (Nos MM1-MM6).

Simbad objects: 28

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Number of rows : 28

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 LDN 1471 DNe 03 48.0 +32 54           ~ 289 0
2 LDN 1498 DNe 04 11.0 +24 58           ~ 255 0
3 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1090 3
4 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1410 0
5 NAME [BM89] L1517B cor 04 55 18.8 +30 38 04           ~ 133 0
6 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 725 0
7 QSO B0507+179 QSO 05 10 02.36912982 +18 00 41.5816534   20.0 19.0 19.09   ~ 345 1
8 QSO B0521-365 BLL 05 22 57.9839686440 -36 27 30.847737786   15.26 14.62 14.48   ~ 741 2
9 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1051 2
10 M 42 HII 05 35 17.3 -05 23 28           ~ 3786 0
11 OMC 3 MoC 05 35 20.0 -05 01 00           ~ 234 1
12 OMC 2 MoC 05 35 27 -05 10.1           ~ 404 1
13 NAME OMC-2/3 reg 05 35 33.0 -05 00 32           ~ 60 0
14 NAME Ori A MoC 05 38 -07.1           ~ 2756 0
15 LDN 1641 MoC 05 39.0 -07 00           ~ 438 0
16 [OSS2018] MM2 cor 05 39 42.30 -07 29 56.0           ~ 1 0
17 [OSS2018] MM1 cor 05 39 42.34 -07 29 43.0           ~ 1 0
18 [TUK93] 122 cor 05 39 42.5 -07 30 09           ~ 9 0
19 [OSS2018] MM3 cor 05 39 42.78 -07 30 01.0           ~ 1 0
20 [OSS2018] MM4 cor 05 39 43.37 -07 30 15.0           ~ 1 0
21 [OSS2018] MM5 cor 05 39 43.76 -07 30 31.0           ~ 1 0
22 [OSS2018] MM6 cor 05 39 44.48 -07 30 10.0           ~ 1 0
23 NAME LDN 1641 South DNe 05 40 27.6 -07 27 28           ~ 50 1
24 ICRF J054255.8-091331 Bz? 05 42 55.8774826 -09 13 31.005835       23.77   ~ 20 0
25 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 897 1
26 QSO J0854+2006 BLL 08 54 48.8749311881 +20 06 30.642936668   15.91 15.43 15.56   ~ 2071 1
27 LDN 57 DNe 17 22 38.2 -23 49 34           ~ 286 1
28 MSXDC G028.23-0.19 DNe 18 43 31.3 -04 13 18           ~ 23 0

    Equat.    Gal    SGal    Ecl

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