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Massive objects located between Earth and a compact binary merger can act asa magnifying glass improving the sensitivity of gravitational wave detectors todistant events. Depending on the parameters of the system, a point mass lensbetween the detector and the source can either lead to a smoothfrequency-dependent amplification of the gravitational wave signal, ormagnification combined with the appearance of a second image that interfereswith the first creating a regular, predictable pattern. We map the increase inthe signal to noise ratio for upcoming LVK observations as a function of themass of the lens $M_L$ and dimensionless source position $y$ for any point masslens between the detector and the binary source. To quantify detectability, wecompute the optimal match between the lensed waveform and the waveforms in theunlensed template bank. The higher the mismatch with unlensed templates, themore detectable lensing is. Furthermore, we estimate the probability oflensing, and find that the redshift to which binary mergers are visible withthe LVK increases from z = 1 to about 3.2 for a total detected binary mass of120 $M_\odot$. The overall probability of lensing is $<20\%$ of all detectableevents above the threshold SNR for $120 M_\odot$ and $<5\%$ for more commonevents with $60 M_\odot$. We find that there is a selection bias for detectablelensing that favors events that are close to the line of sight $y \lesssim0.5$. Black hole binary searches could thus improve their sensitivity by takingthis bias into account. Moreover, the match, the SNR increase due to lensing,and the probability of lensing are only weakly dependent on the noise curve ofthe detector with very similar results for both the O3 and predicted O4 noisepower spectral densities. These results are upper limits that assume all darkmatter is composed of $300 M_\odot$ point mass lenses.

Compact Binaries through a Lens: Silent vs. Detectable Microlensing for the LIGO-Virgo-KAGRA Gravitational Wave Observatories