Giant Molecular Clouds in the Spiral Arm of IC 342

TL;DR

This study uses high-resolution CO observations to analyze the properties of giant molecular clouds in a spiral arm of IC 342, revealing differences related to star formation activity and insights into cloud evolution.

Contribution

It provides detailed measurements of GMC properties across a spiral arm in IC 342 and compares star-forming and quiescent clouds, highlighting factors influencing star formation.

Findings

Active GMCs are more massive and closer to virial equilibrium.

GMC properties vary with star formation activity.

Cloud dissipation processes are linked to star formation onset.

Abstract

We present results of 12CO (1--0) and 13CO (1--0) observations of the northeastern spiral arm segment of IC 342 with a ~50pc resolution carried out with the Nobeyama Millimeter Array. Zero-spacing components were recovered by combining with the existing data taken with the Nobeyama 45m telescope. The objective of this study is to investigate the variation of cloud properties across the spiral arm with a resolution comparable to the size of giant molecular clouds (GMCs). The observations cover a 1 kpc times 1.5 kpc region located ~2 kpc away from the galactic center, where a giant molecular association is located at trailing side and associated star forming regions at leading side. The spiral arm segment was resolved into a number of clouds whose size, temperature and surface mass density are comparable to typical GMCs in the Galaxy. Twenty-six clouds were identified from the combined data cube and the identified clouds followed the line width-size relation of the Galactic GMCs. The identified GMCs were divided into two categories according to whether they are associated with star formation activity or not. Comparison between both categories indicated that the active GMCs are more massive, have smaller line width, and are closer to virial equilibrium compared to the quiescent GMCs. These variations of the GMC properties suggest that dissipation of excess kinetic energy of GMC is a required condition for the onset of massive star formation.