2017/10/30 by Yusuke Aso, Nagayoshi Ohashi, Yuri Aikawa +8 · 1 citation
Chemistry · Physics and Astronomy · #Astrophysics #Astrophysics and Star Formation Studies #Cluster (spacecraft) #Computer science #Molecular Spectroscopy and Structure #Physics #Protostar #Serpens #Star formation #Stars #Stellar, planetary, and galactic studies #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.3847/2041-8213/aa9701
8 pages, 4 figures, accepted by ApJL
arxiv created 2017/10/30 · openalex created_date 2017/11/10 · openalex publication_date 2017/11/10 · arxiv updated 2017/11/15 · openalex updated_date 2026/08/05
Abstract We report the discovery of an extremely young protostar, SMM11, located in the associated submillimeter condensation in the Serpens Main cluster using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 3 at 1.3 mm and an angular resolution of . SMM11 is a Class 0 protostar without any counterpart at 70 μ m or shorter wavelengths. The ALMA observations show 1.3 mm continuum emission associated with a collimated 12 CO bipolar outflow. Spitzer and Herschel data show that SMM11 is extremely cold ( 26 K) and faint ( 0.9 ). We estimate the inclination angle of the outflow to be , almost parallel to the plane of the sky, from simple fitting using a wind-driven-shell model. The continuum visibilities consist of Gaussian and power-law components, suggesting a spherical envelope with a radius of ∼600 au around the protostar. The estimated low C 18 O abundance, X (C 18 O) = 1.5–3 , is also consistent with its youth. The high outflow velocity, a few 10 at a few 1000 au, is much higher than theoretical simulations of first hydrostatic cores, and we suggest that SMM11 is a transitional object right after the second collapse of the first core.