  We have analyzed the complete archive of the Visual and Infrared Mapping
Spectrometer (VIMS) data in order to monitor and analyze the evolution of the
clouds and haze coverage at both poles of Titan during the entire Cassini
mission. Our objective is to give a cartographic synopsis from a VIMS
perspective, to provide a global view of the seasonal evolution of Titan's
atmosphere over the poles. We leave the detailed comparison with the Imaging
Science Subsystem (ISS) and the Composite Infrared Spectrometer (CIRS) data
sets to further studies. We have computed global hyperspectral mosaics for each
of the 127 targeted flybys of Titan to produce synthetic color maps emphasizing
the main atmospheric features. The north pole appears fully covered by a huge
cloud as soon as the first observations in 2004 and up to the equinox in 2009
(Le Mou\'elic et al. 2012). The northern skies then became progressively
clearer, after the circulation turnover in 2009, revealing the underlying lakes
and seas to the optical instruments up to 2017. The reverse situation is
observed over the south pole, which was mostly clear of such a high obscuring
cloud during the first years of the mission, but started to develop a polar
cloud in 2012. This feature grew up month after month until the end of the
mission in 2017, with a poleward latitudinal extent of 75$^\circ$S in 2013 up
to 58$^\circ$S in April 2017. Thanks to the spectral capabilities of VIMS, we
have detected HCN spectral signatures over the north pole in almost all flybys
between 2004 and 2008. These HCN signatures started then to show up over the
south pole in almost all flybys between 2012 and 2017, so perfectly matching
the timing and spatial extent of the northern and southern polar atmospheric
features.
