Bird's eye view of molecular clouds in the Milky Way: II. Cloud kinematics from sub-pc to kpc scales

TL;DR

This study investigates how molecular cloud kinematics and Larson's relations vary across scales from parsecs to kiloparsecs in the Milky Way, revealing scale-dependent behaviors and environmental influences.

Contribution

It provides a comprehensive analysis of CO spectra and Larson's relations across multiple spatial scales within the Milky Way, highlighting the scale-dependency and environmental effects on molecular cloud kinematics.

Findings

Linewidth-size relation at cloud scales: σ_v=1.5*R^{0.3±0.1} with large scatter.

Mass-size relation: M_{CO}=794*R^{1.5±0.5}.

Environmental dependence: higher velocity dispersions near Galactic center and spiral arms.

Abstract

The kinematics of molecular gas are crucial for setting the stage for star formation. One key question related to the kinematic properties of gas is how they depend on the spatial scale. We aim to describe the CO spectra, velocity dispersions, and especially the linewidth-size relation, of molecular gas from cloud (parsec-) scales to kiloparsec scales in a complete region within the Milky Way disk. We utilise the census of molecular clouds within 2 kpc from our earlier work, together with CO emission data for them from the literature. We study the kinematics and the Larson's relations for the sample of individual clouds. We also mimic a face-on view of the Milky Way and analyse the kinematics of the clouds within apertures of 0.25-2 kpc in size. In this way, we describe the scale-dependency of the CO gas kinematics and Larson's relations. We describe the spectra of CO gas at cloud scales and in apertures between 0.25-2 kpc in our survey area. The spectra within the apertures are relatively symmetric but show non-Gaussian high-velocity wings. At cloud-scales, our sample shows a linewidth-size relation \sigma_v=1.5*R^{0.3\pm0.1} with a large scatter. The mass-size relation in the sample of clouds is M_{CO}= 794*R^{1.5\pm0.5}. The relations are also present for the apertures at kpc-scales. A suggestive dependency on galactic environment is seen, with apertures closer to the Galactic centre and the Sagittarius spiral arm having slightly higher velocity dispersions. We explore the possible effect of a diffuse component in the survey area, and find that such a component would widen the CO spectra and could flatten the linewidth-size relation. Understanding the nature of the possible diffuse CO component and its effects on observations is crucial for connecting Galactic and extragalactic data.