  UV observations with Cassini ISS Narrow Angle Camera of Titan's detached haze
is an excellent tool to probe its aerosols content without being affected by
the gas or the multiple scattering. Unfortunately, its low extent in altitude
requires a high resolution calibration and limits the number of images
available in the Cassini dataset. However, we show that it is possible to
extract on each profile the local maximum of intensity of this layer and
confirm its stability at $500 \pm 8$ km during the 2005-2007 period for all
latitudes lower than 45$^\circ$N. Using the fractal aggregate scattering model
of Tomasko et al. (2008) and a single scattering radiative transfer model, it
is possible to derive the optical properties required to explain the
observations made at different phase angles. Our results indicates that the
aerosols have at least ten monomers of 60 nm radius, while the typical
tangential column number density is about $2\cdot 10^{10}$ agg.m$^{-2}$.
Moreover, we demonstrate that these properties are constant within the error
bars in the southern hemisphere of Titan over the observed time period. In the
northern hemisphere, the size of the aerosols tend to decrease relatively to
the southern hemisphere and are associated with a higher tangential opacity.
However, the lower number of observations available in this region due to the
orbital constraints is a limiting factor in the accuracy of these results.
Assuming a fixed homogeneous content we notice that the tangential opacity can
fluctuate up to a factor 3 among the observations at the equator. These
variations could be linked with short scale temporal and/or longitudinal events
changing the local density of the layer.
