The depth of a secondary eclipse contains information of both the thermally emitted light component of a hot Jupiter and the reflected light component . If the dayside atmosphere of the planet is assumed to be isothermal , it is possible to disentangle both . In this work , we analyzed 11 eclipse light curves of the hot Jupiter HAT-P-32 b obtained at 0.89 \mu m in the z ’ band . We obtained a null detection for the eclipse depth with state-of-the-art precision , -0.01 \pm 0.10 ppt . We confirm previous studies showing that a non-inverted atmosphere model is in disagreement to the measured emission spectrum of HAT-P-32 b . We derive an upper limit on the reflected light component , and thus , on the planetary geometric albedo A _ { g } . The 97.5 % confidence upper limit is A _ { g } < 0.2 . This is the first albedo constraint for HAT-P-32 b , and the first z ’ band albedo value for any exoplanet . This finding disfavors the influence of large-sized silicate condensates on the planetary day side . We inferred z ’ band geometric albedo limits from published eclipse measurements also for the ultra-hot Jupiters WASP-12 b , WASP-19 b , WASP-103 b , and WASP-121 b , applying the same method . These values consistently point to a low reflectivity in the optical to near-infrared transition regime for hot to ultra-hot Jupiters .