The complete Venus IR data-set I obtained in the last 3 months.
Jupos maps are already computed for all 48 days, sync to surface (sys1), to be able to correlate atmospheric features that may be "linked/stationary" to the thermal albedo maps.
Grischa is currently preparing a new Jupos version where atmospheric wind speeds (sys 2), so far locked to the high altitude cloud layer (UV detected), can be tailored (modulated) to other wind speeds more appropriate to analyse IR data (mid-altitude cloud deck/s). When that is available I will produce whole planet IR map projections (there is enough data to produce 8 of these global planispheres) and share them here and in databases.
So far, there is enough food for thought regarding some questions like: what is the morphology of "forming" and "decaying" CDs? Can more than one co-exist? Besides CDs is there another type of repeating/evolving/disappearance sequence for other features? Are spots and/or bright IR clouds frequent, or particularly linked to any special region (latitude? longitude? surface?) Is it possible to follow different drift speeds at different latitudes? Are IR albedo features specifically linked (exclusion/ coincidence) to UV albedo features, besides occasional encounters (they drift at distinct speeds)? Just to name a few... :-)

≪アントニオ  シダダオ  ポルトガル≫
[Antonio Cidadao  Oeiras - Portugal]