  In binary-black-hole systems where the black-hole spins are misaligned with
the orbital angular momentum, precession effects leave characteristic
modulations in the emitted gravitational waveform. Here, we investigate where
in the parameter space we will be able to accurately identify precession, for
likely observations over coming LIGO-Virgo-KAGRA observing runs. Despite the
large number of parameters that characterise a precessing binary, we perform a
large scale systematic study to identify the impact of each source parameter on
the measurement of precession. We simulate a fiducial binary at moderate
mass-ratio, signal-to-noise ratio (SNR), and spins, such that precession will
be clearly identifiable, then successively vary each parameter while holding
the remaining parameters fixed. As expected, evidence for precession increases
with signal-to noise-ratio (SNR), higher in-plane spins, more unequal component
masses, and higher inclination, but our study provides a quantitative
illustration of each of these effects, and informs our intuition on parameter
dependencies that have not yet been studied in detail, for example, the effect
of varying the relative strength of the two polarisations, the total mass, and
the aligned-spin components. We also measure the "precession SNR" $\rho_p$,
which was introduced in Refs[1,2] to quantify the signal power associated with
precession. By comparing $\rho_p$ with both Bayes factors and the recovered
posterior distributions, we find it is a reliable metric for measurability that
accurately predicts when the detected signal contains evidence for precession.
