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Atomic ionised regions with strong continuum emission are often associatedwith regions of high-mass star formation and low-frequency (<2GHz) observationsof these regions are needed to help build star formation models. The regiontoward the Vela Supernova Remnant is particularly interesting as it is acomplex structure of recent supernova explosions and molecular cloudscontaining a number of HII regions that are not well characterised. We searchedpublicly available catalogues for HII regions, both candidate and identified,which also have low-frequency emission. In the area of ~400 square degreestoward the Vela Supernova remnant, we found 10 such HII regions, some of whichhave multiple components in catalogues. In this work we use data from theAustralian Square Kilometre Array Pathfinder and previously unpublished datafrom the Murchison Widefield Array and the Australian Telescope Compact Arrayto analyse these sources. The high-mass star forming region RCW 38, withobservations specifically targeted on the source, is used as a pilot study todemonstrate how low-frequency, wide-field continuum observations can identifyand study HII regions in our Galaxy. For the 9 other HII regions, we discusstheir properties; including information about which clouds are interacting,their ages, whether they are dominated by infrared or optical H$\alpha$ lines,distances, ionising photon flux, and upper limits on the infrared luminosity.In future work, these 9 regions will be analysed in more detail, similar to theresult for RCW 38 presented here.

A Low Frequency Pilot Survey of Southern HII Regions in the Vela Constellation