The circular velocity and halo mass functions of galaxies in the nearby Universe

The circular velocity function (CVF) of galaxies is a fundamental test of the Λ Cold Dark Matter (CDM) paradigm as it traces the variation of galaxy number densities with circular velocity (vcirc), a proxy for dynamical mass. Previous observational studies of the CVF have either been based on {H}{I}-rich galaxies, or encompassed low-number statistics and probed narrow ranges in vcirc. We present a benchmark computation of the CVF between 100-350\ km\ s⁻¹ using a sample of 3527 nearby-Universe galaxies, representative for stellar masses between 109.2-1011.9 M_. We find significantly larger number densities above 150 km\ s⁻¹ compared to results from {H}{I} surveys, pertaining to the morphological diversity of our sample. Leveraging the fact that circular velocities are tracing the gravitational potential of halos, we compute the halo mass function (HMF), covering ~1 dex of previously unprobed halo masses (1011.7-1012.7 M_). The HMF for our sample, representative of the galaxy population with M₂₀₀1011.35 M_, shows that spiral morphologies contribute 67 per cent of the matter density in the nearby Universe, while early types account for the rest. We combine our HMF data with literature measurements based on {H}{I} kinematics and group/cluster velocity dispersions. We constrain the functional form of the HMF between 1010.5-1015.5 M_, finding a good agreement with ΛCDM predictions. The halo mass range probed encompasses 72+5 \\ -6 per cent (ΩM,10.5-15.5 = 0.227 ± 0.018) of the matter density in the nearby Universe; 31+5 \\ -6 per cent is accounted for by halos below 1012.7M_ occupied by a single galaxy.