2017/06/12 by L. K. Dewangan, Lokesh K. Dewangan, D. K. Ojha +3 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Cluster (spacecraft) #H II region #Ionization #Maser #Protostar #Star formation #Stars #Stellar, planetary, and galactic studies #Young stellar object #astro-ph.GA
paper · pdf · doi:10.3847/1538-4357/aa79a5
14 pages, 8 figures, 1 table, Accepted for publication in The Astrophysical Journal
arxiv created 2017/06/12 · openalex created_date 2017/06/23 · openalex publication_date 2017/07/18 · arxiv updated 2017/07/26 · openalex updated_date 2026/08/05
Abstract To probe the star formation (SF) process, we present a multi-wavelength study of IRAS 05480+2545 (hereafter I05480+2545). Analysis of Herschel data reveals a massive clump ( M clump ∼ 1875 peak N (H 2 ) ∼ 4.8 × 10 22 cm −2 ; A V ∼ 51 mag) containing the 6.7 GHz methanol maser and I05480+2545, which is also depicted in a temperature range of 18–26 K. Several noticeable parsec-scale filaments are detected in the Herschel 250 μ m image and seem to be radially directed to the massive clump. It resembles more of a “hub-filament” system. Deeply embedded young stellar objects (YSOs) have been identified using the 1–5 μ m photometric data, and a significant fraction of YSOs and their clustering are spatially found toward the massive clump, revealing the intense SF activities. An infrared counterpart (IRc) of the maser is investigated in the Spitzer 3.6–4.5 μ m images. The IRc does not appear as a point-like source and is most likely associated with the molecular outflow. Based on the 1.4 GHz and H α continuum images, the ionized emission is absent toward the IRc, indicating that the massive clump harbors an early phase of a massive protostar before the onset of an ultracompact H ii region. Together, the I05480+2545 is embedded in a very similar “hub-filament” system to those seen in the Rosette Molecular Cloud. The outcome of the present work indicates the role of filaments in the formation of the massive star-forming clump and cluster of YSOs, which might help channel material to the central hub configuration and the clump/core.