2018/05/10 by Chuan-Peng Zhang, Tie Liu, Jinghua Yuan +24 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Galactic plane #Milky Way #Molecular cloud #Protostar #Star cluster #Star formation #Stars #Stellar, planetary, and galactic studies #Virial theorem #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.3847/1538-4365/aac513
51 pages, 13 figures, 5 tables; Accepted for publication in ApJS; Supplementary figures can be downloaded in https://zcp521.github.io/pub/Figs.zip
arxiv created 2018/05/10 · openalex created_date 2018/05/17 · openalex publication_date 2018/06/01 · arxiv updated 2018/06/21 · openalex updated_date 2026/08/05
Abstract In order to understand the initial conditions and early evolution of star formation in a wide range of Galactic environments, we carried out an investigation of 64 Planck Galactic cold clumps (PGCCs) in the second quadrant of the Milky Way. Using the 13 CO and C 18 O J = 1–0 lines and 850 μ m continuum observations, we investigated cloud fragmentation and evolution associated with star formation. We extracted 468 clumps and 117 cores from the 13 CO line and 850 μ m continuum maps, respectively. We made use of the Bayesian distance calculator and derived the distances of all 64 PGCCs. We found that in general, the mass–size plane follows a relation of m ∼ r 1.67 . At a given scale, the masses of our objects are around 1/10 of that of typical Galactic massive star-forming regions. Analysis of the clump and core masses, virial parameters, densities, and mass–size relation suggests that the PGCCs in our sample have a low core formation efficiency (∼3.0%), and most PGCCs are likely low-mass star-forming candidates. Statistical study indicates that the 850 μ m cores are more turbulent, more optically thick, and denser than the 13 CO clumps for star formation candidates, suggesting that the 850 μ m cores are likely more appropriate future star formation candidates than the 13 CO clumps.