Recent developments have shed new light on the composition of the upper Venus clouds. An analysis of the Mariner 5 occultation data has led to improved temperature and pressure profiles. When these are combined with transit data, it is concluded that there is an optically thin cloud layer with a top at 81‐km altitude where the temperature and pressure are, respectively, 175°K and 3 mb. The inclusion of temperatures derived from the near‐infrared CO2bands leads to the postulate of a second cloud deck with a top at 61‐km altitude, whereT= 260°K andP= 240 mb. Additional important constraints on cloud models are imposed by the measured abundances of HCl and H2O, by the polarization data, and by the reflection and emission spectra. It is concluded that the leading candidate for the uppermost clouds is liquid drops of HCl‐H2O, that there is no recommended candidate for the second cloud deck, and that H2O ice is at most a minor component of these clou