  Multiwavelength photometry of the secondary eclipses of extrasolar planets is
able to disentangle the reflected and thermally emitted light radiated from the
planetary dayside. This leads to the measurement of the planetary geometric
albedo $A_g$, which is an indicator of the presence of clouds in the
atmosphere, and the recirculation efficiency $\epsilon$, which quantifies the
energy transport within the atmosphere. In this work we aim to measure $A_g$
and $\epsilon$ for the planet WASP-178 b, a highly irradiated giant planet with
an estimated equilibrium temperature of 2450 K.} We analyzed archival spectra
and the light curves collected by Cheops and Tess to characterize the host
WASP-178, refine the ephemeris of the system and measure the eclipse depth in
the passbands of the two respective telescopes. We measured a marginally
significant eclipse depth of 70$\pm$40 ppm in the Tess passband and
statistically significant depth of 70$\pm$20 ppm in the Cheops passband.
Combining the eclipse depth measurement in the Cheops (lambda_eff=6300 AA) and
Tess (lambda_eff=8000 AA) passbands we constrained the dayside brightness
temperature of WASP-178 b in the 2250-2800 K interval. The geometric albedo
0.1<$\rm A_g$<0.35 is in general agreement with the picture of poorly
reflective giant planets, while the recirculation efficiency $\epsilon>$0.7
makes WASP-178 b an interesting laboratory to test the current heat
recirculation models.
