Constraining the scatter in the galaxy-halo connection at Milky Way masses

We develop and implement two new methods for constraining the scatter in the relationship between galaxies and dark matter haloes. These new techniques are sensitive to the scatter at low halo masses, making them complementary to previous constraints that are dependent on clustering amplitudes or rich galaxy groups, both of which are only sensitive to more massive haloes. In both of our methods, we use a galaxy group finder to locate central galaxies in the Sloan Digital Sky Survey main galaxy sample. Our first technique uses the small-scale cross-correlation of central galaxies with all lower mass galaxies. This quantity is sensitive to the satellite fraction of low-mass galaxies, which is in turn driven by the scatter between haloes and galaxies. The second technique uses the kurtosis of the distribution of line-of-sight velocities between central galaxies and neighbouring galaxies. This quantity is sensitive to the distribution of halo masses that contain the central galaxies at fixed stellar mass. Theoretical models are constructed using peak halo circular velocity, V-peak, as our property to connect galaxies to haloes, and all comparisons between theory and observation are made after first passing the model through the group-finding algorithm. We parametrize scatter as a lognormal distribution in M-* at fixed V-peak, sigma[M-*vertical bar V-peak]. The cross-correlation technique yields a constraint of sigma[M-*vertical bar V-peak] = 0.27 +/- 0.05 dex at a mean V-peak of 168 km s(-1), corresponding to a scatter in logM(*) at fixed M-h of sigma[M-*vertical bar M-h] = 0.38 +/- 0.06 dex at M-h = 10(11.8)M(circle dot). The kurtosis technique yields sigma[M-*vertical bar V-peak] = 0.30 +/- 0.03 at V-peak = 209 km s(-1), corresponding to sigma[M-*vertical bar M-h] = 0.34 +/- 0.04 at M-h = 10(12.2)M(circle dot). The values of sigma[M-*vertical bar M-h] are significantly larger than the constraints at higher masses, in agreement with the results of hydrodynamic simulations. This increase is only partly due to the scatter between V-peak and M-h, and it represents an increase of nearly a factor of 2 relative to the values inferred from clustering and group studies at high masses.