2003MNRAS.343.1195R

We have measured the column density distribution function, f (N_H i_), at z = 0 using 21-cm Hi emission from galaxies selected from a blind Hi survey. f (N_H i_) is found to be smaller and flatter at z = 0 than indicated by high-redshift measurements of damped Lyman α (DLA) systems, consistent with the predictions of hierarchical galaxy formation. The derived DLA number density per unit redshift, dN_DLA/dz = 0.058, is in moderate agreement with values calculated from low-redshift QSO absorption line studies. We use two different methods to determine the types of galaxies which contribute most to the DLA cross-section: comparing the power-law slope of f (N_H i_) to theoretical predictions and analysing contributions to dN_DLA/dz. We find that comparison of the power-law slope cannot rule out spiral discs as the dominant galaxy type responsible for DLA systems. Analysis of dN_DLA/dz however, is much more discriminating. We find that galaxies with log M_H i_< 9.0 make up 34 per cent of dN_DLA/dz; Irregular and Magellanic types contribute 25 per cent; galaxies with surface brightness {formmu11} account for 22 per cent and sub-L_*galaxies contribute 45 per cent to dN_DLA/dz. We conclude that a large range of galaxy types give rise to DLA systems, not just large spiral galaxies as previously speculated.