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

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.

6 pages, accepted for publication in A&A

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Cited by in corpus (5)

• Giant Molecular Cloud Catalogues for PHANGS-ALMA: Methods and Initial Results
• Rise and fall of molecular clouds across the M33 disk
• First Detection of the Molecular Cloud Population in the Extended Ultraviolet (XUV) Disk of M83
• Molecular Cloud Matching in CO and Dust in M33 I. High-Resolution Hydrogen Column Density Maps from Herschel
• Compact and High Excitation Molecular Clumps in the Extended Ultraviolet Disk of M83