2011MNRAS.415.2844C


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.21CET07:50:52

2011MNRAS.415.2844C - Mon. Not. R. Astron. Soc., 415, 2844-2858 (2011/August-2)

A multifrequency study of the active star-forming complex NGC 6357 – I. Interstellar structures linked to the open cluster Pis 24.

CAPPA C.E., BARBA R., DURONEA N.U., VASQUEZ J., ARNAL E.M., GOSS W.M. and LAJUS E.F.

Abstract (from CDS):

We investigate the distribution of gas (ionized, neutral atomic and molecular) and interstellar dust in the complex star-forming region NGC 6357 with the goal of studying the interplay between the massive stars in the open cluster Pis 24 and the surrounding interstellar matter.

Our study of the distribution of the ionized gas is based on narrow-band Hα, [S II]and [O III] images obtained with the Curtis–Schmidt Camera at CTIO, Chile, and on radio continuum observations at 1465 MHz taken with the VLA with a synthesized beam of 40 arcsec. The distribution of the molecular gas is analysed using 12CO(1-0) data obtained with the NANTEN radiotelescope, Chile (angular resolution = 2.7 arcmin). The interstellar dust distribution was studied using mid-infrared data from the GLIMPSE survey and far-infrared observations from IRAS.

NGC 6357 consists of a large ionized shell and a number of smaller optical nebulosities. The optical, radio continuum, and near- and mid-IR images delineate the distributions of the ionized gas and interstellar dust in the H II regions and in previously unknown wind-blown bubbles linked to the massive stars in Pis 24 revealing surrounding photodissociation regions. The CO line observations allowed us to identify the molecular counterparts of the ionized structures in the complex and to confirm the presence of photodissociation regions. The action of the WR star HD 157504 on the surrounding gas was also investigated. The molecular mass in the complex is estimated to be (4±2) {x} 105 M. The mean electron densities derived from the radio data suggest electron densities >200/cm3, indicating that NGC 6357 is a complex formed in a region of high ambient density. The known massive stars in Pis 24 and a number of newly inferred massive stars are mainly responsible for the excitation and photodissociation of the parental molecular cloud.


Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS

Journal keyword(s): H {sc ii} regions - ISM: bubbles - ISM: individual objects: NGC 6357 - open clusters and associations: individual: Pis 24

Nomenclature: Figs 2+5, Table 1: [CBD2011] GLLL.ll+BB.bb (Nos G353.12+00.86, G353.19+00.84, G353.24+00.64).

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 Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2036 1
2 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3813 2
3 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1070 1
4 Cl Pismis 24 OpC 17 24 43.0 -34 12 23   11.00 9.6     ~ 110 0
5 2MASS J17244578-3409399 Y*O 17 24 45.7779631255 -34 09 39.853881342 14.53 14.21 12.73 12.30   O6V((f))z 27 1
6 GAL 353.19+00.91 HII 17 24 48 -34 10.8           ~ 24 0
7 [RZM2010] 112 cor 17 24 50.5 -34 14 46           ~ 1 0
8 [RZM2010] 115 cor 17 25 00.6 -34 13 09           ~ 1 0
9 HD 157504 WR* 17 25 08.8534998754 -34 11 12.502902170 12.80 12.10 10.68 10.39 11.546 WC7+O7-9 111 0
10 GAL 353.1+00.6 HII 17 25 37 -34 22.5           ~ 15 0
11 GRS G353.20 +00.70 Rad 17 25.7 -34 17           ~ 4 0
12 NGC 6357 HII 17 26.5 -34 12           ~ 254 0
13 HD 157406 * 17 26 33.0802637650 -58 28 26.598245874   10.13 9.14     G8/K0III/IV 3 0
14 PMN J1751-2524 Rad 17 51 51.26306 -25 24 00.0607           ~ 72 0
15 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 950 2

    Equat.    Gal    SGal    Ecl

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