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

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 (similar to 3.2 kpc), moderate-mass (similar to 500 M (circle dot)), young (similar to 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 to be similar to 33,000 K and similar to 3.8, respectively. Our radio continuum observations reveal that the star has ionized its environment, forming a H ii region of size similar to 2.7 pc, temperature similar to 5700 K, and electron density similar to 165 cm(-3). However, our large-scale dust maps reveal that it has heated the dust up to several parsecs (similar to 10 pc) in the range 17-28 K and the morphology of warm dust emission resembles a bipolar H ii region. From dust and (CO)-C-13 gas analyses, we find evidence that the formation of the H ii 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 H ii region is currently compressing a clump of mass similar to 2700 M (circle dot) at its western outskirts, at the junction of the H ii 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 H ii region onto the inflowing filamentary material.