# 2009A&A...496..731E

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 Query : 2009A&A...496..731E

2009A&A...496..731E - Astronomy and Astrophysics, volume 496, 731-739 (2009/3-4)

The molecular environment of the massive star forming region NGC 2024: multi CO transition analysis.

EMPRECHTINGER M., WIEDNER M.C., SIMON R., WIECHING G., VOLGENAU N.H., BIELAU F., GRAF U.U., GUESTEN R., HONINGH C.E., JACOBS K., RABANUS D., STUTZKI J. and WYROWSKI F.

Abstract (from CDS):

Sites of massive star formation have complex internal structures. Local heating by young stars and kinematic processes, such as outflows and stellar winds, generate large temperature and velocity gradients. Complex cloud structures lead to intricate emission line shapes. CO lines from high mass star forming regions are rarely Gaussian and show often multiple peaks. Furthermore, the line shapes vary significantly with the quantum number Jup, due to the different probed physical conditions and opacities. The goal of this paper is to show that the complex line shapes of 12CO and 13CO in NGC 2024 showing multiple emission and absorption features, which vary with rotational quantum number J can be explained consistently with a model, whose temperature and velocity structure are based on the well-established scenario of a PDR and the Blister model''. We present velocity-resolved spectra of seven 12CO and 13CO lines ranging from Jup=3 to Jup=13. We combined these data with 12CO high-frequency data from the ISO satellite and analyzed the full set of CO lines using an escape probability code and a one-dimensional full radiative transfer code. We find that the bulk of the molecular cloud associated with NGC 2024 consists of warm (75K) and dense (9x105cm–3) gas. An additional hot (∼300K) component, located at the interface of the HII region and the molecular cloud, is needed to explain the emission of the high-J CO lines. Deep absorption notches indicate that very cold material (∼20K) exists in front of the warm material, too. A temperature and column density structure consistent with those predicted by PDR models, combined with the velocity structure of a Blister model'', appropriately describes the observed emission line profiles of this massive star forming region. This case study of NGC 2024 shows that, with physical insights into these complex regions and careful modeling, multi-line observations of 12CO and 13CO can be used to derive detailed physical conditions in massive star forming regions.

Journal keyword(s): ISM: molecules - ISM: HII regions - submillimeter - stars: formation

Full paper

 Number of rows : 14
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 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 1015 3
2 [EC2006] MM12 HII 05 35 13.41015 -05 24 11.1770           ~ 47 1
3 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 623 1
4 NAME Ori A MoC 05 38 -07.1           ~ 2913 0
5 [MCK88] NGC 2024 FIR 1 FIR 05 41 41.40 -01 53 47.0           ~ 36 0
6 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1311 0
7 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1128 1
8 [BCB89] IRS 3 Y*O 05 41 44.4045095712 -01 55 23.095022772           M1.9 22 0
9 [MCK88] NGC 2024 FIR 5 cor 05 41 44.6 -01 55 38           ~ 93 0
10 [MCK88] NGC 2024 FIR 7 cor 05 41 44.90 -01 56 15.0           ~ 33 0
11 [BCB89] IRS 2b Y*O 05 41 45.490 -01 54 28.78           O8V 45 1
12 [BCB89] IRS 2 Y*O 05 41 45.81 -01 54 29.8           B 98 0
13 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 715 2
14 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1580 0

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2023.03.23-22:51:26