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

¹ Instituto de Astrofísica de La Plata (UNLP - CONICET), La Plata, Argentina
e-mail: nduronea@fcaglp.unlp.edu.ar
² Instituto de Astronomía y Física del Espacio (UBA, CONICET), CC 67, Suc. 28, 1428 Buenos Aires, Argentina
³ Departamento de Astronomía, Universidad de Chile, Casilla 36, Santiago de Chile, Chile
⁴ Observatório do Valongo, Universidade Federal do Rio de Janeiro, Ladeira Pedro Antônio, 43, Rio de Janeiro 20080-090, Brazil
⁵ Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina
⁶ Instituto Argentino de Radioastronomía (CCT-La Plata, CONICET; CICPBA), C.C. No. 5, 1894 Villa Elisa, Argentina

Received: 31 July 2020
Accepted: 3 December 2020

Abstract

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 Hα 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 distance to both S169 and IRAS 12326-6245, which was estimated to be ~2 kpc. Several candidate YSOs were identified, projected mostly onto the molecular condensations MC3, MC4, and MC5, which indicates that the star-formation process is very active at the borders of the nebula. A comparison between observable and modeled parameters was not enough to discern whether the collect-and-collapse mechanism is acting at the edge of S169. However, other processes such as radiative-driven implosion or even a combination of both mechanisms, namely, collect-and-collapse and radiative-driven implosion, could be acting simultaneously in the region.