  We reanalyse the LIGO-Virgo strain data of the 10 binary black hole mergers
reported to date and compute the likelihood function in terms of chirp mass,
mass ratio and effective spin. We discuss the strong degeneracy between mass
ratio and spin for the three lighter events. We use this likelihood and an
estimate of the horizon volume as a function of intrinsic parameters to
constrain the properties of the population of merging binary black holes. The
data disfavour large spins. Typical spins are constrained to $\overline a
\lesssim 0.4$, even if the underlying population has randomly-oriented spins.
For aligned spins the constraints are tighter, with typical spins required to
be around $\overline a\sim 0.1$ and have comparable dispersion. We detect no
statistically significant tendency towards a positive average spin in the
direction of the orbital angular momentum. We put an upper limit on the
fraction of systems where the secondary could have been tidally locked prior to
the formation of the black holes (corresponding to merger times shorter than
$10^8$ years) $f \lesssim 0.3$. Four events are consistent with having a
maximally-spinning secondary, although one only marginally. We confirm previous
findings that there is a hint of a cutoff at high mass. The data favour
distributions of mass ratios with an average $\overline q \gtrsim 0.7$.
