Molecular gas in the star-forming region IRAS 08589-4714 ⋆
1 Observatorio Astronómico, Universidad Nacional de Córdoba, 5000 Córdoba, Argentina
2 CONICET, Consejo Nacional de Investigaciones Científicas y Técnicas, Argentina
3 Instituto Argentino de Radioastronomía, CONICET, CCT La PLata, C.C.5, 1894 Villa Elisa, Argentina
4 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de la Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina
5 Departamento de Astronomía, Universidad de Chile, Casilla 36, Santiago de Chile, Chile
Received: 7 December 2015
Accepted: 13 July 2016
Aims. We present an analysis of the region IRAS 08589−4714 with the aim of characterizing the molecular environment.
Methods. We observed the 12CO(3 −2), 13CO(3 −2), C18O(3 −2), HCO+(3 −2), and HCN(3 −2) molecular lines in a region of 150′′× 150′′, centered on the IRAS source, to analyze the distribution and characteristics of the molecular gas linked to the IRAS source.
Results. 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 H2 volume density are 310 M⊙ and 1.2 × 104 cm-3, respectively. Two overdensities were identified within the clump in HCN(3−2) and HCO+(3−2) 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.
Key words: ISM: individual objects: IRAS 08589-4714 / stars: formation / stars: massive / ISM: jets and outflows / circumstellar matter / ISM: molecules
Final reduced APEX data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/594/A115
© ESO, 2016