High-Velocity Clouds in the Nearby Spiral Galaxy M 83

TL;DR

This study investigates high-velocity neutral hydrogen clouds in the galaxy M 83, revealing a thick disk and multiple anomalous clouds, supporting models of galactic fountains and tidal interactions as formation mechanisms.

Contribution

First detailed HI and optical observations of HVCs in M 83, identifying diverse cloud populations and their likely formation processes.

Findings

Detected a thick, slowly rotating HI disk containing 5.5% of total HI

Identified eight anomalous-velocity HI clouds with masses up to 1.5x10^7 Msolar

Results support galactic fountain and tidal interaction models for cloud origins

Abstract

We present deep HI 21-cm and optical observations of the face-on spiral galaxy M 83 obtained as part of a project to search for high-velocity clouds (HVCs) in nearby galaxies. Anomalous-velocity neutral gas is detected toward M 83, with 5.6x10^7 Msolar of HI contained in a disk rotating 40-50 km/s more slowly in projection than the bulk of the gas. We interpret this as a vertically extended thick disk of neutral material, containing 5.5% of the total HI within the central 8 kpc. Using an automated source detection algorithm to search for small-scale HI emission features, we find eight distinct, anomalous-velocity HI clouds with masses ranging from 7x10^5 to 1.5x10^7 Msolar and velocities differing by up to 200 km/s compared to the HI disk. Large on-disk structures are coincident with the optical spiral arms, while unresolved off-disk clouds contain no diffuse optical emission down to a limit of 27 r' mag per square arcsec. The diversity of the thick HI disk and larger clouds suggests the influence of multiple formation mechanisms, with a galactic fountain responsible for the slowly-rotating disk and on-disk discrete clouds, and tidal effects responsible for off-disk cloud production. The mass and kinetic energy of the HI clouds are consistent with the mass exchange rate predicted by the galactic fountain model. If the HVC population in M 83 is similar to that in our own Galaxy, then the Galactic HVCs must be distributed within a radius of less than 25 kpc.