  Past occultation and phase-curve observations of the ultra-short period
super-Earth 55 Cnc e obtained at visible and infrared wavelengths have been
challenging to reconcile with a planetary reflection and emission model. In
this study, we analyse a set of 41 occultations obtained over a two-year
timespan with the CHEOPS satellite. We report the detection of 55 Cnc e's
occultation with an average depth of $12\pm3$ ppm. We derive a corresponding
2-$\sigma$ upper limit on the geometric albedo of $A_g < 0.55$ once
decontaminated from the thermal emission measured by Spitzer at 4.5$\mu$m.
CHEOPS's photometric performance enables, for the first time, the detection of
individual occultations of this super-Earth in the visible and identifies
short-timescale photometric corrugations likely induced by stellar granulation.
We also find a clear 47.3-day sinusoidal pattern in the time-dependent
occultation depths that we are unable to relate to stellar noise, nor
instrumental systematics, but whose planetary origin could be tested with
upcoming JWST occultation observations of this iconic super-Earth.
