The TOP-SCOPE survey of PGCCs: PMO and SCUBA-2 observations of 64 PGCCs in the 2nd Galactic Quadrant

TL;DR

This study investigates 64 Planck Galactic Cold Clumps in the Milky Way's second quadrant using molecular line and continuum observations, revealing their properties and potential for low-mass star formation.

Contribution

It provides a comprehensive analysis of PGCCs' physical properties and star formation potential, highlighting their low core formation efficiency and differences between clumps and cores.

Findings

Most PGCCs are low-mass star-forming candidates.

850 μm cores are more turbulent and dense than 13CO clumps.

The mass-size relation follows m∼r^{1.67}.

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 \textit{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\,$\mu$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\,$\mu$m continuum maps, respectively. We make 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 $m\sim r^{1.67}$. 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 ($\sim$3.0\%), and most PGCCs are likely low-mass star-forming candidates. Statistical study indicates that the 850\,$\mu$m cores are more turbulent, more optically thick, and denser than the $^{13}$CO clumps for star formation candidates, suggesting that the 850\,$\mu$m cores are likely more appropriate future star-formation candidates than the $^{13}$CO clumps.