Gas rich galaxies and the HI mass function

Davies, Jonathan Ivor, de Blok, W. J. G., Smith, Rodney, Kambas, A., Sabatini, Sabina ORCID: https://orcid.org/0000-0003-2076-5767, Linder, S. M. and Salehi-Reyhan, S. A. 2001. Gas rich galaxies and the HI mass function. Presented at: Seeing through the dust :the detection of HI and the exploration of the ISM in galaxies, Penticton, British Columbia, Canada, 20-25 October 2001. Published in: Taylor, A. R., Landecker, T. L. and Willis, A. G. eds. Seeing through the dust :the detection of HI and the exploration of the ISM in galaxies : proceedings of a conference held at Herzberg Institute of Astrophysics, Dominion Radio Astrophysical Observatory, Penticton, British Columbia, Canada, 20-25 October. Astronomical Society of the Pacific conference series (276) San Francisco: Astronomical Society of the Pacific, pp. 449-452.

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Abstract

We have developed an automated cross-correlation technique to detect 21cm emission in sample spectra obtained from the HI Parkes All Sky Survey. The initial sample selection was the nearest spectra to 2435 low surface brightness galaxies in the catalogue of Morshidi-Esslinger et al. (1999). The galaxies were originally selected to have properties similar to Fornax cluster dE galaxies. As dE galaxies are generally gas poor it is not surprising that there were only 26 secure detections. All of the detected galaxies have very high values of $(M_{H}/L_{B})_{\odot}$. Thus the HI selection of faint optical sources leads to the detection of predominately gas rich galaxies. The gas rich galaxies tend to reside on the outskirts of the large scale structure delineated by optically selected galaxies, but they do appear to be associated with it. These objects appear to have similar relative dark matter content to optically selected galaxies. The HI column densities are lower than the 'critical density' necessary for sustainable star formation and they appear, relatively, rather isolated from companion galaxies. These two factors may explain their high relative gas content. We have considered the HI mass function by looking at the distribution of velocities of HI detections in random spectra on the sky. The inferred HI mass function is steep though confirmation of this results awaits a detailed study of the noise characteristics of the HI survey.

Item Type:	Conference or Workshop Item (Paper)
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Publisher:	Astronomical Society of the Pacific
ISBN:	1583811184
Related URLs:	Publisher
Last Modified:	05 Aug 2023 03:18
URI:	https://orca.cardiff.ac.uk/id/eprint/37851

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