2021A&A...655A..12T


Query : 2021A&A...655A..12T

2021A&A...655A..12T - Astronomy and Astrophysics, volume 655A, 12-12 (2021/11-1)

Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde. IV. The ALMA view of N113 and N159W in the LMC.

TANG X.D., HENKEL C., MENTEN K.M., GONG Y., CHEN C.-H.R., LI D.L., LEE M.-Y., MANGUM J.G., AO Y.P., MUHLE S., AALTO S., GARCIA-BURILLO S., MARTIN S., VITI S., MULLER S., COSTAGLIOLA F., ASIRI H., LEVSHAKOV S.A., SPAANS M., OTT J., IMPELLIZZERI C.M.V., FUKUI Y., HE Y.X., ESIMBEK J., ZHOU J.J., ZHENG X.W., ZHAO X. and LI J.S.

Abstract (from CDS):

We mapped the kinetic temperature structure of two massive star-forming regions, N113 and N159W, in the Large Magellanic Cloud (LMC). We have used ∼1.6" (∼0.4pc) resolution measurements of the para-H2CO JKaKc=303-202, 322-221, and 321-220 transitions near 218.5 GHz to constrain RADEX non local thermodynamic equilibrium models of the physical conditions. The gas kinetic temperatures derived from the para-H2CO line ratios 322-221/303-202 and 321-220/303-202 range from 28 to 105 K in N113 and 29 to 68 K in N159W. Distributions of the dense gas traced by para-H2CO agree with those of the 1.3 mm dust and Spitzer 8.0 µm emission, but they do not significantly correlate with the Hα emission. The high kinetic temperatures (Tkin≥50K) of the dense gas traced by para-H2CO appear to be correlated with the embedded infrared sources inside the clouds and/or young stellar objects in the N113 and N159W regions. The lower temperatures (Tkin < 50 K) were measured at the outskirts of the H2CO-bearing distributions of both N113 and N159W. It seems that the kinetic temperatures of the dense gas traced by para-H2CO are weakly affected by the external sources of the Hα emission. The non thermal velocity dispersions of para-H2CO are well correlated with the gas kinetic temperatures in the N113 region, implying that the higher kinetic temperature traced by para-H2CO is related to turbulence on a ∼0.4 pc scale. The dense gas heating appears to be dominated by internal star formation activity, radiation, and/or turbulence. It seems that the mechanism heating the dense gas of the star-forming regions in the LMC is consistent with that in Galactic massive star-forming regions located in the Galactic plane.

Abstract Copyright: © ESO 2021

Journal keyword(s): stars: formation - ISM: clouds - ISM: molecules - radio lines: ISM

VizieR on-line data: <Available at CDS (J/A+A/655/A12): list.dat fits/*>

Simbad objects: 13

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Number of rows : 13
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 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6558 1
2 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1567 0
3 LHA 120-N 113 HII 05 13 21.7 -69 21 33           ~ 108 1
4 NAME Pic A Sy1 05 19 49.7229323856 -45 46 43.852662732   15.73 15.77 14.85   ~ 629 1
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16512 1
6 NAME Orion S reg 05 35 12.9 -05 24 10           ~ 139 0
7 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1127 2
8 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2207 1
9 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1908 1
10 LHA 120-N 159W MoC 05 39 32.510 -69 46 02.74           ~ 88 0
11 QSO J0635-7516 QSO 06 35 46.5079301472 -75 16 16.816418256   15.96 15.75 15.82   ~ 558 1
12 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5678 6
13 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13437 0

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2023.02.01-06:53:55

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