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

Abstract

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 (∼3.2 kpc), moderate-mass (∼500 M ⊙), young (∼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 ∼33,000 K and ∼3.8, respectively. Our radio continuum observations reveal that the star has ionized its environment, forming a H ii region of size ∼2.7 pc, temperature ∼5700 K, and electron density ∼165 cm−3. However, our large-scale dust maps reveal that it has heated the dust up to several parsecs (∼10 pc) in the range 17−28 K and the morphology of warm dust emission resembles a bipolar H ii region. From dust and 13CO 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 ∼2700 M ⊙ at its western outskirts, at the junction of the H ii region and filament. We observe several 70 μm 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.