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We use a sample of ~6000 galaxies detected by the Arecibo Legacy Fast ALFA(ALFALFA) 21cm survey, to measure the clustering properties of HI-selectedgalaxies. We find no convincing evidence for a dependence of clustering on thegalactic atomic hydrogen (HI) mass, over the range M_HI ~ 10^{8.5} - 10^{10.5}M_sun. We show that previously reported results of weaker clustering for low-HImass galaxies are probably due to finite-volume effects. In addition, wecompare the clustering of ALFALFA galaxies with optically selected samplesdrawn from the Sloan Digital Sky Survey (SDSS). We find that HI-selectedgalaxies cluster more weakly than even relatively optically faint galaxies,when no color selection is applied. Conversely, when SDSS galaxies are splitbased on their color, we find that the correlation function of blue opticalgalaxies is practically indistinguishable from that of HI-selected galaxies. Atthe same time, SDSS galaxies with red colors are found to cluster significantlymore than HI-selected galaxies, a fact that is evident in both the projected aswell as the full two-dimensional correlation function. A cross-correlationanalysis further reveals that gas-rich galaxies "avoid" being located within ~3Mpc of optical galaxies with red colors. Next, we consider the clusteringproperties of halo samples selected from the Bolshoi LambdaCDM simulation. Acomparison with the clustering of ALFALFA galaxies suggests that galactic HImass is not tightly related to host halo mass, and that a sizable fraction ofsubhalos do not host HI galaxies. Lastly, we find that we can recover fairlywell the correlation function of HI galaxies by just excluding halos with lowspin parameter. This finding lends support to the hypothesis that halo spinplays a key role in determining the gas content of galaxies.

The clustering of ALFALFA galaxies: dependence on HI mass, relationship to optical samples & clues on host halo properties