Precise Clustering and Density Evolution of redMaPPer Galaxy Clusters
  versus MXXL Simulation
  We construct a large, redshift complete sample of distant galaxy clusters by
correlating Sloan Digital Sky Survey (SDSS) Data Release 12 (DR12) redshifts
with clusters identified with the red-sequence Matched-filter Probabilistic
Percolation (redMaPPer) algorithm. Our spectroscopic completeness is 97% for ~
7,000 clusters within the redMaPPer selection limit, $z \leqslant$ 0.325, so
that our cluster correlation functions are much more precise than earlier work
and not suppressed by photometric redshifts. We derive an accurate power-law
mass-richness relation from the observed abundance with respect to the mass
function from Millennium XXL (MXXL) simulation, adjusted to the Planck weighted
cosmology. The number density of clusters is found to decline by 20% over the
range 0.1 $< z <$ 0.3, in good agreement with the evolution predicted by MXXL.
Our projected three-dimensional correlation function scales with richness,
$\lambda$, rising from $r_0=$ 14 h$^{-1}$ Mpc at $\lambda\simeq$ 25, to $r_0=$
22 h$^{-1}$ Mpc at $\lambda\simeq$ 60, with a gradient that matches MXXL when
applying our mass-richness relation, whereas the observed amplitude of the
correlation function at $\left<z\right>=$ 0.24 exceeds the MXXL prediction by
20% at the $\simeq$ 2.5$\sigma$ level. This tension cannot be blamed on
spurious, randomly located clusters as this would reduce the correlation
amplitude. Full consistency between the correlation function and the abundances
is achievable for the pre-Planck values of $\sigma_8=$ 0.9, $\Omega_m=$ 0.25,
and h = 0.73, matching the improved distance ladder estimate of the Hubble
constant.
