A detailed view of a Molecular Cloud in the far outer disk of M33

TL;DR

This study presents high-resolution CO observations of the most distant molecular cloud in M33, revealing its structure, mass, and kinematics, and providing insights into molecular gas in low-metallicity, outer galaxy regions.

Contribution

It offers the first detailed high-resolution analysis of a molecular cloud in the far outer disk of M33, highlighting its properties and potential accretion processes.

Findings

The cloud is a single entity, not multiple smaller clouds.

CO brightness temperature reaches 2.4 K at 10 pc resolution.

Estimated cloud mass is 4.3 x 10^4 solar masses.

Abstract

The amount of H$_2$ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1--0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M 33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize. At a spatial resolution of 10 pc, beyond the optical radius of the M 33, the CO brightness temperature reaches 2.4 Kelvins. A virial mass estimate for the cloud yields a mass of $4.3 \times 10^4$ \msun and a ratio $\ratio \simeq 3.5 \times 10^{20} \Xunit$. While no velocity gradient is seen where the emission is strong, the velocity is redshifted to the extreme SW and blue-shifted to the far NE. If the orientation of the cloud is along the plane of the disk (i.e. not perpendicular), then these velocities correspond to slow infall or accretion. The rather modest infall rate would be about $2 \times 10^{-4}$\moyr.