The uncertainty in the monomer size is +-0.01um
\cite{Tomasko_2009}
For an assumed, fixed, phase function of single-scattered intensity as a function of scattering angle, the monomer size can be con-strained to two significant digits from the blue channel observations. However, due to the relatively high optical depth of the haze in the blue channel (approximately 3) even at the beginning of the measurements, the effect of dilution of the singly scattered light by multiple scattering makes the computed polarization uncertain by some 5% for a 20% change in the relative value of the single scattering near 90°. This makes the derived monomer size uncertain by about 0.01 lm. Thus, we find the radius of the haze monomers to be 0.04 ± 0.01 lm.
Max Linear Polarization at 491 nm and 934 nm
We found that the linear polarization from single scattering had to be 85–90% to reproduce the multiply scattered light in Titan’s atmosphere at the 491 nm wavelength of our Solar Aureole channel, and some 98% at 934 nm
Tholin analogs from laboratory experiments
From \cite{Sciamma_O_Brien_2012}
"The Cassini Visible and Infrared Mapping Spectrometer (VIMS) images and spectra have also been used to study Titan’s aerosols. The VIMS transmission spectra obtained by occultation have allowed the measurement of an aerosol absorption band at 3.4 lm(Bellucci et al., 2009) as well as the determination of the aerosol vertical distribution under 500 km. The VIMS images of Titan’s atmosphere and surface have also been used to determine the haze vertical and latitudinal distribution as well as the imaginary part of the refractive index of Titan’s aerosols between 0.4 lm and 4.0 lm(Rannou et al., 2010). "
"These indices have been determined using different methods: ellipsometry, spectrophotometry, interferometry measurements, etc.\cite{Khare_1984,Imanaka_2004,Tran_2003,Ramirez_2002,Vuitton_2009}, and recently cavity ring down aerosol extinction spectroscopy \cite{Hasenkopf_2010}. However, even though more recent optical constants have been published in the last decade, the constants published by \citet{Khare_1984} are still used because they are close to what is needed to fit the photometric observations at visible wavelengths, where the haze is optically thick. Another advantage of Khare’s tholin optical constants is that they cover a wide spectral range, from 0.0250 lm to 1000 lm. Nevertheless, recent studies have shown that Khare’s optical constants might not be as representative of Titan’s aerosols, at certain wavelengths, as those of other tholins. \citet{Bellucci_2009} showed that the haze absorption band detected at 3.4 lm cannot be modeled with Khare’s optical constants, and \citet{Rannou_2010} showed that the VIMS data were better fitted with an imaginary part of the refractive index that remained constant between 0.8 and 1.5 lm, which is not the case ofKhare’s optical con- stants. \citet{Rannou_2010} also highlighted that different tholins produced and studied by \citet{Imanaka_2004} as well as some of the tholins studied in \citet{Quirico_2008} were presenting an absorption band at 3.4 lm, and could therefore be analogues more representative of Titan’s aerosols. "