Table 2
Comparison of Hapke’s parameters for the surface of Ceres at visible wavelengths as derived from VIR (0.55 μm) and FC observations.
| B0SH | hSH | ξ | w |  |
Reference |
|---|---|---|---|---|---|
| (1.6) | (0.06) | − 0.11 ± 0.08 | 0.14 ± 0.02 | 29 ± 6 | S1, Ciarniello et al. (2017) |
 |
 |
− 0.085 ± 0.08 |  |
29 ± 5 | S2, this work |
| 1 |  |
− 0.062 ± 0.09 |  |
 |
S3, this work |
| 1 |  |
− 0.19 ± 0.04 | 0.13 ± 0.01 |  |
S4, this work |
| 1.6 | 0.054 | −0.11 | 0.116 | 23 | Schröder et al. (2018)(a) |
| (1.6) | (0.06) | − 0.03 |  |
19 ± 6 | Li et al. (2019)(b) |
Notes. Values in parentheses are from Helfenstein & Veverka (1989). For the results of Ciarniello et al. (2017) and this work, the error on the parameters was computed starting from the range of confidence obtained on the roughness average slope 
(see Ciarniello et al. 2017). For each value of the roughness in this interval, the fitting procedure converges to a different set of parameters, and their variability is assumed as the associated uncertainty. (a) Hapke’s model adopting a double-parameter Henyey-Greenstein SPPF (Case C solution) with FC Clear Filter data. Errors on the parameters are of the order of unity on the last digit. (b)Hapke’s model adopting a double-parameter Henyey-Greenstein SPPF (2pHG) at 555 nm (FC F2 filter).
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