# TOA reflectance computation

CHRIS products are provided in top of the atmosphere (TOA) radiance (radiometrically calibrated data).

The TOA apparent reflectance is estimated according to:

where * L(x, y, λ_{i})* is the provided at-sensor upward radiance at the image location

*is the extraterrestrial instantaneous solar irradiance, and*

**(x, y), I(λ**_{i})*is the angle between the illumination direction and the vector perpendicular to the surface.*

**θ(x, y)**In the proposed algorithm, * θ(x, y)* is approximated by the Solar Zenith Angle provided in the CHRIS attributes since one can assume flat landscape and constant illumination angle for the area observed in a CHRIS image. Finally, the Sun irradiance,

*is taken from Thuillier et al. (2003), corrected for the acquisition day, and convolved with the CHRIS spectral channels.*

**I(λ,)**Sun irradiance corrected for the day of the year and the CHRIS channels (left) and TOA apparent reflectance estimated from the sensor radiance (right).

The extraterrestrial solar irradiance * I(λ)* given in Thuillier et al. (2003) is provided from 200 to 2400 nm in mW/m

^{2}/nm. It shall be corrected for the Julian day of year (DOY), J, according to the following approximate formulae:

where the day of year can be easily obtained from the Image Date metadata of the CHRIS file.

Since the reference extraterrestrial solar irradiance presents a different spectral sampling, it is resampled to the CHRIS spectral channels. A specific CHRIS band, * i*, consists of the addition of one or more CCD detector pixel elements depending on the band width. Therefore, the spectral response of a CHRIS band,

*is the sum of the the spectral response*

**S**_{i}(λ,)*of the corresponding detectors of the CCD array. Then, the mean solar irradiance for a given band,*

**S(λ)***, is obtained by integrating the extraterrestrial solar irradiance by its spectral response:*

**I(λ**_{i})The theoretical half-width of the instrument line-spread functions correspond to spectral resolutions of 1.25 nm at 415 nm, increasing to 11.25 nm at 1050 nm. One could assume a Gaussian response function, * S(λ)*, for each element using its full-width half-maximum (FWHM) and sum up all the elements of the band. However, in the header of the CHRIS files, although the CCD row number for lower and upper wavelengths of each band is provided, the FWHM of each CCD element is not. Therefore, for the shake of simplicity, the spectral response of a CHRIS band,

*, is defined as a bell-shaped function depending on the mid-wavelength,*

**S**_{i}(λ)*, and the band width,*

**λ**_{i}*, of the band, directly:*

**Δλ**_{i}where both the mid-wavelength and the band width values for each channel are included in the CHRIS file.