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We have developed a new retrieval approach to modelling near-infrared spectraof Uranus that represents a significant improvement over previous modellingmethods. We reanalysed IRTF/SpeX observations of Uranus observed in 2009covering the wavelength range 0.8 to 1.8 microns and reported by Tice et al.(2013). By retrieving the imaginary refractive index spectra of cloud particleswe are able to consistently define the real part of the refractive indexspectra, through a Kramers-Kronig analysis, and thus determine self-consistentextinction cross-section, single-scattering and phase-function spectra for theclouds and hazes in Uranus' atmosphere. We tested two different cloud-modellingschemes used in conjunction with the temperature/methane profile of Baines etal. (1995), a reanalysis of the Voyager-2 radio-occultation observationsperformed by Sromovsky, Fry and Tomasko (2011), and a recent determination fromSpitzer (Orton et al., 2014). We find that both cloud-modelling schemesrepresent the observed centre-of-disc spectrum of Uranus well, and both requiresimilar cloud scattering properties of the main cloud residing at approximately2 bars. However, a modified version of the Sromovsky, Fry and Tomasko (2011)model, with revised spectral properties of the lowest cloud layer, fitsslightly better at shorter wavelengths and is more consistent with the expectedvertical position of Uranus' methane cloud. We find that the bulk of thereflected radiance from Uranus arises from a thick cloud at approximately the 2bar level, composed of particles that are significantly more absorbing atwavelengths > 1.0 micron than they are at wavelengths < 1.0 micron. Thisspectral information provides a possible constraint on the identity of the mainparticle type.

Reanalysis of Uranus' cloud scattering properties from IRTF/SpeX observations using a self-consistent scattering cloud retrieval scheme