Supporting material for

A downscaling approach for geological characterization of the Raditladi basin of Mercury

Paolo Mancinelli1*, Francesco Minelli1, Alessandro Mondini2, Cristina Pauselli1, Costanzo Federico1.

1 Sezione di Geologia Strutturale e Geofisica, Dipartimento di Scienze della Terra, Università degli Studi di Perugia, Perugia, Italy.
2 CNR IRPI Perugia, 06128, Perugia, Italy.

* Corresponding author: P. Mancinelli, Sezione di Geologia Strutturale e Geofisica, Dipartimento di Scienze della Terra, Università degli Studi di Perugia, Piazza Università 1, 06100, Perugia, Italy.
(pamancinelli@gmail.com).

The supporting material provided here is composed by two figures and their relative captions (namely Figures S1 and S2).
Figure S1 is a clean and larger version of the global-scale geological map presented in Fig. 1a.
Figure S2 is to contribute to the ‘Discussion for global geology’ section by comparing our geological map with the monochrome basemap and the mosaic of MASCS observations for a sample region (centred at 7°S, 52°E) south of Rachmaninoff basin.

Caption for Figure S1
This map is a clean and larger version of the map shown in Figure 1a. Smooth plains (SP) and Odin terrains are presented as were mapped by Denevi et al. (2013), intercrater plains (IP), bright intercrater plains (BIP), Caloris rough ejecta (CRE), dark material (DM) and ejecta material (EM) are mapped by us and described in the text. Projection is equidistant cylindrical centred at 0°N, 180°E.

Caption for Figure S2
This figure is to compare the monochrome mosaic (top), our geological map (centre) and the MASCS mosaic (NASA/JHUAPL/CIW, PIA 16668, 2012 ) (bottom) on a region south of Rachmaninoff centred at 7°S, 52°E. Terrains of the geological map are defined in text and Figures 1 and S1. Good fit is found for smooth plains in Firdousi region (NE quadrant), dark material terrains and in bright intercrater plains.