Atmospheric temperature at the lower thermosphere of Venus: comparison and time evolution. A) and B) show our temperatures at the subsolar meridian and the equator compared with results from CO NLTE limb spectra (Gilli et al. 2015; Krasnopolsky 2014), solar occultation with SOIR/VEx (Mahieux et al. 2015a), and numerical VTGCM (Brecht & Bougher 2012); C) subsolar (red) and antisolar temperatures (blue) inferred with CO₂ NLTE spectra taken by VEx/VIRTIS-H (this work) and with stellar occultation using SPICAV (Piccialli et al. 2015). The difference between subsolar and antisolar temperatures are shown in green. Antisolar temperatures are averaged for the same altitude region as the pressure layer 10^-2–10^-5 mb at the subsolar meridian (see Fig. 4); D) and E) indicate long- and short-time evolution of the temperature, averaged for consecutive and single days, respectively, as well as for intervals of latitude (30°S–30°N) and local time (10h–14h shown with red dots, and 14h–16h with purple dots). The solar radio flux at 10.7 cm (Tobiska et al. 2000) is also shown in grey. Sudden changes in temperature are shown in cyan in panel E).