Benchmark of convolution and deconvolution models:
implications for planetary opposition surges
E. Déau*,1, A. Brahic2, L. Dones3 and C. C. Porco4
- 1 Jet Propulsion Laboratory, NASA/CalTech, 4800 Oak Grove Drive Pasadena CA 91109, U.S.A.
- 2 Université Denis Diderot, Laboratoire AIM, 10 rue A. Domon et L. Duquet, 75205 Paris, France.
- 3 Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder CO 80302, U.S.A.
- 4 CICLOPS, 3100 Walnut Street, Suite A535, Boulder CO 80303, U.S.A.
We benchmark several convolution and deconvolution models on phase curves at small phase angles (0.005° - 1°). These curves were provided by several NASA missions (Clementine/UVVIS, Galileo/SSI and Cassini/ISS) when the Sun had different angular radii (α☉ = 0.266°, 0.051°, 0.028°). For the smallest phase angles, the brightness of the objects (Moon, Europa and the Saturn's rings) exhibits a strong flattening below the angular size of the Sun. However, the brightness continues to increase below α☉ before finally flattening at 0.4α☉. These behaviors are consistent with the convolution models tested.
- * Corresponding author