Probing the massive star forming environment - a multiwavelength investigation of the filamentary IRDC G333.73+0.37

TL;DR

This multiwavelength study of IRDC G333.73+0.37 reveals its physical properties, star formation activity, and filament dynamics, providing insights into massive star formation in filamentary clouds.

Contribution

It offers a comprehensive analysis of the physical conditions, star formation signatures, and dynamics of the IRDC using multiwavelength data, highlighting the filament's supercritical nature and accretion flows.

Findings

Identification of 10 high-density clumps with temperatures 14.3-22.3 K.

Detection of protostellar activity and massive star formation signatures.

Observation of a velocity gradient indicating accretion flows.

Abstract

We present a multiwavelength study of the filamentary infrared dark cloud (IRDC) G333.73+0.37. The region contains two distinct mid-infrared sources S1 and S2 connected by dark lanes of gas and dust. Cold dust emission from the IRDC is detected at seven wavelength bands and we have identified 10 high density clumps in the region. The physical properties of the clumps such as temperature: 14.3-22.3 K and mass: 87-1530 M_sun are determined by fitting a modified blackbody to the spectral energy distribution of each clump between 160 micron and 1.2 mm. The total mass of the IRDC is estimated to be $~4700 M_sun. The molecular line emission towards S1 reveals signatures of protostellar activity. Low frequency radio emission at 1300 and 610 MHz is detected towards S1 (shell-like) and S2 (compact morphology), confirming the presence of newly formed massive stars in the IRDC. Photometric analysis of near and mid-infrared point sources unveil the young stellar object population associated with the cloud. Fragmentation analysis indicates that the filament is supercritical. We observe a velocity gradient along the filament, that is likely to be associated with accretion flows within the filament rather than rotation. Based on various age estimates obtained for objects in different evolutionary stages, we attempt to set a limit to the current age of this cloud.