<p>Since 2012, we have been monitoring SO₂ and H₂O (using HDO as a proxy) at the cloud top of Venus, using the TEXES high-resolution imaging spectrometer at the NASA InfraRed Telescope Facility (IRTF) at Maunakea Observatory. Sixteen runs have been performed between 2012 and 2022. Maps have been recorded around 1345 cm^-1 (7.4 microns, z = 62 km), where SO₂, CO₂and HDO are observed, and around 530 cm^-1(19 microns, z = 57 km) where SO₂ and CO₂ are observed, as well as around 1162 cm^-1 (8.6 microns, z = 66 km) where CO₂ is observed. From the early beginning, SO₂ plumes have been identified with an evolution time scale of a few hours. In 2020, an anti-correlation has been found in the long-term evolution of H₂O and SO₂; in addition,&#160; the SO₂ plume appearance as a function of local time seems to show two maxima around the terminator, indicating the possible presence of a semi-diurnal wave (Encrenaz et al. A&A 639, A69, 2020). After two years of interruption due to the pandemia, new observations have been performed in July 2021, September 2021, November 2021, and February 2022.&#160;&#160; The main results of the new observations are listed below. (1)The SO₂ abundance, which had been globally increasing from 2014 until 2019, has now decreased with respect to its maximum value. (2) The anti-correlation between H₂O and SO₂, which was maximum between 2014 and 2019 (cc = - 0.9) does not appear clearly in the recent observations. (3) The maximum appearance of the SO₂ plumes at the equator and the terminators is confirmed, but appears stronger on the morning side.(4) A strong activity of the SO₂plumes is observed in September and November 2021, at a time when the disk-integrated SO₂ abundance is low. At the same time, thermal maps at 1162 cm^-1 (8.6 microns, z = 66 km) show a polar enhancement. This behavior could possibly be associated with the topography.</p> <p>&#160;</p> <p>&#160;</p> <p>&#160;</p>