2017/12/13 by Eduardo de la Fuente, E. De la Fuente, Miguel A. Trinidad +20
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Astrophysics of Galaxies (astro-ph.GA) #Cosmology and Gravitation Theories #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1712.05054
Accepted for Publication on Revista Mexicana de Astronomia y Astrofisica (Vol. 54, No. 1, April 2018.)
arxiv created 2017/12/14 · openalex publication_date 2017/12/14 · arxiv updated 2017/12/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present a multiwavelength study of the cometary \hii region G12.21--0.10 using the VLA and OVRO. Both radio continuum (0.3, 0.7, 2 and 3.6~cm) and spectral lines of H41α, 13CS(2-1) & (1-0), and NH\rm 3(2,2) & (4,4) observations are included. We find two 3~mm continuum peaks toward G12.21--0.10, one of them is spatially coincident with the UC~H~II region, while the other coincides spatially with a molecular clump. We also find that the 0.7, 2 and 3.6~cm continuum and H41α line are only detected toward the UC~H~II region, while the 13CS, and NH\rm 3 is spatially associated with the molecular clump. Based on the morphology, kinetic temperature (∼86~K), volumetric density (∼1.5×106~cm-3) and linear size (∼0.22~pc) of the molecular clump, we suggest this source is consistent with a hot molecular core.