2015ApJ...811...79D


Query : 2015ApJ...811...79D

2015ApJ...811...79D - Astrophys. J., 811, 79 (2015/October-1)

The physical environment of the massive star-forming region W42.

DEWANGAN L.K., LUNA A., OJHA D.K., ANANDARAO B.G., MALLICK K.K. and MAYYA Y.D.

Abstract (from CDS):

We present an analysis of multi-wavelength observations from various data sets and Galactic plane surveys to study the star-formation process in the W42 complex. A bipolar appearance of the W42 complex is evident due to the ionizing feedback from the O5-O6 type star in a medium that is highly inhomogeneous. The Very Large Telescope/NACO adaptive-optics K and L' images (resolutions ∼0."2-0."1) resolved this ionizing source into multiple point-like sources below ∼5000 AU scale. The position angle ∼15° of the W42 molecular cloud is consistent with the H-band starlight mean polarization angle, which in turn is close to the Galactic magnetic field, suggesting the influence of the Galactic field on the evolution of the W42 molecular cloud. Herschel sub-millimeter data analysis reveals three clumps located along the waist axis of the bipolar nebula, with the peak column densities of ~(3-5)x1022/cm2 corresponding to visual extinctions of AV∼ 32-53.5 mag. The Herschel temperature map traces a temperature gradient in W42, revealing regions of 20 K, 25 K, and 30-36 K. Herschel maps reveal embedded filaments (length ∼1-3 pc) that appear to be radially pointed to the denser clump associated with the O5-O6 star, forming a hub-filament system. A total of 512 candidate young stellar objects (YSOs) are identified in the complex, ∼40% of which are present in clusters distributed mainly within the molecular cloud, including the Herschel filaments. Our data sets suggest that the YSO clusters, including the massive stars, are located at the junction of the filaments, similar to those seen in the Rosette Molecular Cloud.

Abstract Copyright:

Journal keyword(s): dust, extinction - H ii regions - ISM: clouds - ISM: individual: W42 - stars: formation - stars: pre-main sequence

Status at CDS : Examining the need for a new acronym.

CDS comments: Table 1: cN1, cN2 et cS1 are not in SIMBAD.

Simbad objects: 15

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Number of rows : 15
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 Perseus Cloud SFR 03 35.0 +31 13           ~ 1154 0
2 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3768 0
3 NAME Rosette Molecular Cloud MoC 06 34.7 +04 02           ~ 239 0
4 GAL 333.6-00.2 HII 16 22 11 -50 05.6           ~ 143 0
5 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3216 1
6 CD-24 13806 ** 18 03 40.3201452689 -24 22 42.860589572 10.26 11.022 10.372 10.267   O7:V 182 0
7 V* EW Sct cC* 18 37 51.1111080562 -06 47 48.495390706   9.50 7.96     F8Ib/II 103 0
8 [CPA2006] N39 bub 18 38 06.0 -06 48 05           ~ 8 0
9 [LDW85] 25.4NW FIR 18 38 06.6 -06 45 45           ~ 9 0
10 GAL 025.38-00.18 HII 18 38 14 -06 47.6           ~ 37 0
11 GRS G024.80 +00.10 SFR 18 38 14.8 -06 47 39           ~ 104 0
12 CORNISH G025.3809-00.1815 HII 18 38 15.00 -06 48 01.2           ~ 3 0
13 CORNISH G025.3824-00.1812 HII 18 38 15.26 -06 47 52.6           ~ 3 0
14 USNO-B1.0 0832-00443053 * 18 38 15.3 -06 47 58       16.06   O5.5 5 0
15 [BCD2000] W42 3 * ~ ~           ~ 2 0

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2021.09.23-05:15:40

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