Gravitational microlensing is a powerful tool for probing the physical properties of quasar accretion disks and properties of the lens galaxy such as its dark matter fraction and mean stellar mass .
Unfortunately the number of lensed quasars ( \sim 90 ) exceeds our monitoring capabilities .
Thus , estimating their microlensing properties is important for identifying good microlensing candidates as well as for the expectations of future surveys .
In this work we estimate the microlensing properties of a sample of 87 lensed quasars .
While the median Einstein radius crossing time scale is 20.6 years , the median source crossing time scale is 7.3 months .
Broadly speaking , this means that on \sim 10 year timescales roughly half the lenses will be quiescent , with the source in a broad demagnified valley , and roughly half will be active with the source lying in the caustic ridges .
We also found that the location of the lens system relative to the CMB dipole has a modest effect on microlensing timescales , and in theory microlensing could be used to confirm the kinematic origin of the dipole .
As a corollary of our study we analyzed the accretion rate parameters in a sub-sample of 32 lensed quasars .
At fixed black hole mass , it is possible to sample a broad range of luminosities ( i.e. , Eddington factors ) if it becomes feasible to monitor fainter lenses .