Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245

Duronea N. Cichowolski S. Bronfman L. Mendoza E. Finger R. Suad L.A. Corti M. Reynoso E.M.
Astronomy and Astrophysics
Doi 10.1051/0004-6361/202039074
Volumen 646
2021-02-01
Citas: 1
Abstract
© ESO 2021.Aims. With the aim of studying the physical properties of Galactic IR bubbles and to explore their impact in massive star formation, we present a study of the IR bubble S169, associated with the massive star forming region IRAS 12326-6245. Methods. We used CO (2-1),13CO (2-1), C18O (2-1), HCN (3-2), and HCO+ (3-2) line data obtained with the APEX telescope using the on-the-fly full sampling technique to study the properties of the molecular gas in the nebula and the IRAS source. To analyze the properties and distribution of the dust, we made use of images obtained from the IRAC-GLIMPSE, Herschel, and ATLASGAL archives. The properties of the ionized gas in the nebula were studied using radio continuum and H? images obtained from the SUMSS survey and SuperCOSMOS database, respectively. In our search for stellar and protostellar objects in the region, we used point source calalogs obtained from the MSX, WISE, GLIMPSE, 2MASS, AAVSO, ASCC-2.5V3, and GAIA databases. Results. The new APEX observations allowed us to identify three molecular components, each one associated with different regions of the nebula, namely: at -39 km s-1 (component A), -25 km s-1 (component B), and -17 km s-1 (component C). Component A is shown to be the most dense and clumpy. Six molecular condensations (MC1 to MC6) were identified in this component, with MC3 (the densest and more massive one) being the molecular counterpart of IRAS 12326-6245. For this source, we estimated an H2 column density up to 8 × 1023 cm-2. An LTE analysis of the high density tracer lines HCO+ (3-2) and HCN (3-2) on this source, assuming 50 and 150 K, respectively, indicates column densities of N(HCO+) = (5.2 ± 0.1) × 1013 cm-2 and N(HCN) = (1.9 ± 0.5) × 1014 cm-2. To explain the morphology and velocity of components A, B, and C, we propose a simple model consisting of a partially complete semisphere-like structure expanding at ~12 km s-1. The introduction of this model has led to a discussion about the dis...
HII regions, ISM: bubbles, ISM: kinematics and dynamics, ISM: molecules
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