A model of Titan’s aerosols based on measurements made inside the atmosphere\citep{Tomasko_2008}

“At 934 nm, the effective wavelength of the red SA channel, the measured DLVS intensities vary regularly with azimuth angle (see Fig. 19), and require a modest backward peak in the single-scattering phase function. At 491 nm, the effective wavelength of the blue SA channel, no such backward peak was required.”
The only explanation to this, at blue channel real part of RF index should be small or imaginary part should be large or the combination of both whereas in the red channel it should be opposite. Because normally coherent backscattering effect is more pronounced when size-parameter is larger for the same refractive index. 
Continues as;
 
“Hence, in the red we only permitted backscattering peaks below 80 km and retained the fractal phase functions without backward peaks above. This proved sufficient to match the DLVS observations with azimuth. With these trial phase functions we found the profiles of extinction optical depth and single-scattering albedo with altitude necessary to match the ULVS and DLVS observations at the red and blue SA wavelengths.”
"One problem was that the errors due to tip/ tilt uncertainties vary greatly at different altitudes, and it is important to assign reasonable uncertainties to each data set to prevent the fitting algorithm from trying to reduce large residuals in one observation whose pointing geometry is rather uncertain."
”Nevertheless, it is clear that the slope of the power-law fits are significantly greater above 80 km, intermediate between 80 and 30 km, and smallest in the lowest 30 km of the atmosphere. Note that if the particles were much smaller than the wavelength the slopes would be À4 in these fits as for Rayleigh scattering. The shallower slopes here indicate larger particles, with the trend of increasing particle size (or increasing compactness) with increasing depth into the atmosphere.”

Calculating number density of the particles

Dividing the opacity in each layer by the cross section and the thickness of the layers gives an estimate for the number density of the haze particles. This is done for the red and blue SA wavelengths in Fig. 51. Above 80km the number density estimates from the opacity at the red and blue wavelengths agree, with a number density of about 5/cm3 at 80km decreasing with a scale height of 65 km. The fractal aggregates above 80km consist of some 3000 monomers each with a radius of about 0.05 mm. This gives these particles an equal-volume radius of 0.72 mm and an equal projected area radius of 2.03 mm. We modified the fractal phase function for scattering angles 491 slightly at wavelengths between 491 and 934nm for improved fits to the SA observations, while keeping the cross sections computations as given in Appendix A. If the monomer size turns out to be less than 0.05mm after the polarization data are more completely modeled, the projected area of the aggregate particles must still be near the size given here to match the forward scattering

Single scattering albedo btw 30-80km

"Between 30 and 80 km, the haze particles have accumu- lated additional material that has increased their single- scattering albedo. Thus, the particles in this region of the atmosphere may include condensate material in the spaces"

From summary 

In these studies, it is to be expected that Titan’s haze will change in several respects over the disk. However, it is to be hoped that some of the information such as the phase functions and possibly the single-scattering albedos in different layers of atmosphere will change less than other parameters such as number density. In this way, some of the optical properties of the haze determined at the Huygens landing site may be able to contribute to breaking some of the families of solutions that often result from analyses of observations made outside the atmosphere.
The investigation by Rannou et al. (2003) was especially interesting in pointing out the critical role played by the monomer size in fitting many of the existing optical constraints. In our work we adopted a monomer size necessary to produce the large degree of linear polarization we observed in the DISR SA channels looking away from the sun near 901 scattering angle. We have some 50 vertical scans in each of the red and blue SA channels during the descent. The probe attitude is critical in reducing these observations since we have only measured two components of intensity in crossed linear polarizers. However, now that the SA intensity data have been used to constrain the probe attitude when the red and blue integrations were made, it will be possible to reanalyze the DISR polarization measurements. With this further work, we may be able to tighten the constraints on the haze monomer sizes in the altitude range sampled by DISR.
In conclusion, we believe that the addition of the DISR measurements inside Titan’s atmosphere have helped to