A Comprehensive Study of the Young Cluster IRAS 05100+3723: Properties, Surrounding Interstellar Matter, and Associated Star Formation

TL;DR

This study provides a detailed multiwavelength analysis of the young cluster IRAS 05100+3723, revealing its properties, surrounding interstellar matter, and star formation processes, highlighting the role of feedback and filamentary cloud dynamics.

Contribution

It offers a comprehensive characterization of IRAS 05100+3723 and its environment, emphasizing the influence of HII region expansion on star formation in filamentary clouds.

Findings

IRAS 05100+3723 is a ~3 Myr old, 500 Msun cluster at 3.2 kpc with an O8.5V star.

The HII region has a size of ~2.7 pc, temperature ~5700 K, and electron density ~165 cm$^{-3}$.

Star formation is likely triggered by HII region expansion compressing the surrounding filament.

Abstract

We present a comprehensive multiwavelength investigation of a likely massive young cluster `IRAS 05100+3723' and its environment with the aim to understand its formation history and feedback effects. We find that IRAS 05100+3723 is a distant ($\sim$3.2 kpc), moderate mass ($\sim$500 \msun), young ($\sim$3 Myr) cluster with its most massive star being an O8.5V-type. From spectral modeling, we estimate the effective temperature and log $g$ of the star as $\sim$33,000 K and $\sim$3.8, respectively. Our radio continuum observations reveal that the star has ionized its environment forming an HII region of size $\sim$2.7 pc, temperature $\sim$5,700 K, and electron density $\sim$165 cm$^{-3}$. However, our large-scale dust maps reveal that it has heated the dust up to several parsecs ($\sim$10 pc) in the range 17$-$28 K and the morphology of warm dust emission resembles a bipolar HII region. From dust and $^{13}$CO gas analyses, we find evidences that the formation of the HII region has occurred at the very end of a long filamentary cloud around 3 Myr ago, likely due to edge collapse of the filament. We show that the HII region is currently compressing a clump of mass $\sim$2700 \msun at its western outskirts, at the junction of the HII region and filament. We observe several 70 $\mu$m point sources of intermediate-mass and class 0 nature within the clump. We attribute these sources as the second generation stars of the complex. We propose that the star formation in the clump is either induced or being facilitated by the compression of the expanding HII region onto the inflowing filamentary material.