Infrared study of the southern galactic star-forming region associated with IRAS 14416-5937

Abstract

Aims: Our goal was to carry out an infrared study of the southern Galactic massive star-forming region associated with IRAS 14416-5937. Methods: This star-forming region has been mapped simultaneously in two far infrared bands at ~150 and 210 µm, using the TIFR 1-m balloon borne telescope with ~1' angular resolution. We have used 2MASS JHK_s, as well as Spitzer-GLIMPSE data of this region to study the stellar populations of the embedded young cluster. This region comprises two sources, designated as A and B and separated by ~2 pc. The spectrum of a region located close to the source A obtained using the Long Wavelength Spectrometer (LWS) on board the Infrared Space Observatory (ISO) is presented. Emission from warm dust and from Unidentified Infrared Bands (UIBs) is estimated using the mid-infrared data of the MSX survey. Results: The spatial distributions of (1) the temperature of cool dust and (2) optical depth at 200 μm have been obtained taking advantage of the similar beams in both the TIFR bands. A number of atomic fine structure lines have been detected in the ISO-LWS spectrum, which have been used to estimate the electron density and the effective temperature of the ionising radiation in this region. From the near- and mid-infrared images, we identify a dust lane due north-west of source A. The dust lane is populated by Class I type sources. Class II type sources are found further along the dust lane as well as below it. Self consistent radiative transfer models of the two sources (A and B) are in good agreement with the observed spectral energy distributions. Conclusions: The spatial distribution of young stellar objects in and around the dust lane suggests that active star formation is taking place along the dust lane and is possibly triggered by the expanding HII regions of A and B.