Infrared dust bubble CS51 and its interaction with the surrounding interstellar medium

TL;DR

This study presents a comprehensive multiwavelength analysis of the infrared dust bubble CS51, revealing its complex ionized, dust, and molecular components, and suggesting star formation processes influenced by feedback from high-mass stars.

Contribution

It provides the first detailed multiwavelength characterization of CS51, including radio, infrared, and molecular data, and explores star formation mechanisms like collect and collapse.

Findings

Detection of thermal and non-thermal radio emission components.

Identification of five dust clumps with significant mass and size.

Evidence supporting the collect and collapse star formation process.

Abstract

A multiwavelength investigation of the southern infrared dust bubble CS51 is presented in this paper. We probe the associated ionized, cold dust, molecular and stellar components. Radio continuum emission mapped at 610 and 1300 MHz, using the Giant Metrewave Radio Telescope, India, reveal the presence of three compact emission components (A, B, and C) apart from large-scale diffuse emission within the bubble interior. Radio spectral index map show the coexistence of thermal and non-thermal emission components. Modified blackbody fits to the thermal dust emission using Herschel PACS and SPIRE data is performed to generate dust temperature and column density maps. We identify five dust clumps associated with CS51 with masses and radius in the range 810 - 4600 M{\sun} and 1.0 - 1.9 pc, respectively. We further construct the column density probability distribution functions of the surrounding cold dust which display the impact of ionization feedback from high-mass stars. The estimated dynamical and fragmentation timescales indicate the possibility of collect and collapse mechanism in play at the bubble border. Molecular line emission from the MALT90 survey is used to understand the nature of two clumps which show signatures of expansion of CS51.