Thermal emission from the nightside of Venus has been observed at 1.0 μm during fall 1991 on the 1.05 m reflector at Pic-du-Midi. The instrumental spectral response was centred in the 1.0 μm window of the Venus atmosphere, located between strong absorptions of CO2. Synthetic calculations by a radiative transfer model of the atmosphere of Venus show that the atmosphere is transparent enough at these wavelengths to allow a contribution from the surface to be transmitted through the clouds. The flux is sensitive to the surface temperature, which is controlled by the altitude. Low flux features are observed on the disc, which are well correlated with the topographic maps of Magellan; these features do follow the solid rotation of the planet. An upper limit of about 10% can be put on the variations of the emissivity of the surface at 1.0 μm, in the Aphrodite Terra region where large radar emissivity variations have been observed by Magellan. © 1993.