The dependence of halo bias on age, concentration and spin
  Halo bias is the main link between the matter distribution and dark matter
halos. In its simplest form, halo bias is determined by halo mass, but there
are known additional dependencies on other halo properties which are of
consequence for accurate modeling of galaxy clustering. Here we present the
most precise measurement of these secondary-bias dependencies on halo age,
concentration, and spin, for a wide range of halo masses spanning from
10$^{10.7}$ to 10$^{14.7}$ $h^{-1}$ M$_{\odot}$. At the high-mass end, we find
no strong evidence of assembly bias for masses above M$_{vir}$ $\sim10^{14}$
$h^{-1}$ M$_{\odot}$. Secondary bias exists, however, for halo concentration
and spin, up to cluster-size halos, in agreement with previous findings. For
halo spin, we report, for the first time, two different regimes: above
M$_{vir}\sim$10$^{11.5}$ $h^{-1}$ M$_{\odot}$, halos with larger values of spin
have larger bias, at fixed mass, with the effect reaching almost a factor 2.
This trend reverses below this characteristic mass. In addition to these
results, we test, for the first time, the performance of a multi-tracer method
for the determination of the relative bias between different subsets of halos.
We show that this method increases significantly the signal-to-noise of the
secondary-bias measurement as compared to a traditional approach. This analysis
serves as the basis for follow-up applications of our multi-tracer method to
real data.
