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

DURONEA N. U. ; CICHOWOLSKI, S.; BRONFMAN L; MENDOZA, E.; FINGER, R. ; SUAD, L.A.; CORTI, M. A.; REYNOSO, E. M.

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Lugar: Paris; Año: 2021 vol. 646

0004-6361

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), 13 CO(2-1), C 18 O(2-1), HCN(3-2), and HCO + (3-2) line data obtained with the APEX telescope usingthe on-the-fly full sampling technique to study the properties of the molecular gas in the nebula and the IRAS source . To analyzethe properties and distribution of the dust, we made use of images obtained from the IRAC-GLIMPSE, Herschel, and ATLASGALarchives. The properties of the ionized gas in the nebula were studied using radio continuum and Hα images obtained from the SUMSSsurvey and SuperCOSMOS database, respectively. In our search for stellar and protostellar objects in the region, we used point sourcecalalogs 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 regionsof 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 isshown 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 H 2 columndensity up to 8×10 23 cm −2 . An LTE analysis of the high density tracer lines HCO + (3-2) and HCN(3-2) on this source, assuming 50and 150 K, respectively, indicates column densities of N(HCO + ) = (5.2 ± 0.1) × 10 13 cm −2 and N(HCN) = (1.9 ± 0.5) × 10 14 cm −2 .To explain the morphology and velocity of components A, B, and C , we propose a simple model consisting of a partially completesemisphere-like structure expanding at ∼ 12 km s −1 . The introduction of this model has led to a discussion about the distance to bothS169 and IRAS 12326-6245, which was estimated to be ∼ 2 kpc. Several candidate YSOs were identified, projected mostly ontothe molecular condensations MC3, MC4, and MC5, which indicates that the star-formation process is very active at the borders ofthe nebula. A comparison between observable and modeled parameters was not enough to discern whether the collect-and-collapsemechanism is acting at the edge of S169. However, other processes such as radiative-driven implosion or even a combination of bothmechanisms, namely, collect-and-collapse and radiative-driven implosion, could be acting simultaneously in the region.