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 Me), 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 Me 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.
