Molecular gas in the star-forming region IRAS 08589-4714

TL;DR

This study characterizes the molecular environment of IRAS 08589-4714, revealing a collapsing molecular clump with embedded young stellar objects and associated molecular outflows, using multi-line molecular observations.

Contribution

First detailed molecular analysis of IRAS 08589-4714 linking gas distribution, dynamics, and star formation activity.

Findings

Identified a 0.45 pc molecular clump with 310 solar masses.

Detected overdensities indicating potential star-forming cores.

Evidence of molecular outflows driven by young stellar objects.

Abstract

We present an analysis of the region IRAS 08589-4714 with the aim of characterizing the molecular environment. We observed the CO(3-2), ^{13}CO(3-2), C^{18}O(3-2), HCO+(3-2), and HCN(3-2) molecular lines in a region of 150" x 150", centered on the IRAS source, to analyze the distribution and characteristics of the molecular gas linked to the IRAS source. The molecular gas distribution reveals a molecular clump that is coincident with IRAS 08589-4714 and with a dust clump detected at 1.2 mm. The molecular clump is 0.45 pc in radius and its mass and H_2 volume density are 310 Mo and 1.2 x 10^4 cm^{-3}, respectively. Two overdensities were identified within the clump in HCN and HCO lines. A comparison of the LTE and virial masses suggests that the clump is collapsing in regions that harbor young stellar objects. An analysis of the molecular lines suggests that they are driving molecular outflows.