SOIM User Manual v6.0

This document will describe the Simulator for Operation of Imaging Missions (SOIM) software used to simulate any Imaging System on board of Missions which take advantage of the Spice Kernels (technology). The document will provide documentation and a description of the input and output files. The experience accumulated by INAF in International Space Missions has demonstrated the impact and the scientific return of Imaging tools. In all mission phases, these instruments have required the development of tools to simulate acquisitions, to verify and optimize the observation strategy, and to define the essential parameters for Operations. The Simulator for Operation of Imaging Missions (SOIM) will be a generic software tool for simulating such payloads. It was developed thanks to the contribution of INAF-OAPD; INAF-IAPS; CNR-IFN and will represent a transversal activity to different research lines favoring the optimization of performances and, with the collaboration of the scientific group, the validation of scientific requirements. At the current date the simulator was applied to 5 instruments: -the three Monitor Cameras (MCAM) on board of BepiColombo Mission -the CaSSIS camera onboard of ExoMars 2016 -the instrument Spectrometers and Imagers for MPO BepiColombo Integrated Observatory SYStem (SIMBIO-SYS) onboard of BepiColombo mission

BepiColombo MCAM Channels Spice Kernels Optimization

The aim of this document is to define the correction to be implemented on the Spice Kernels (SK) of the BepiColombo Monitoring-CAMera (MCAM) to improve the geometric definition of the pinhole models (intrinsic parameters of the cameras) and their pointing (extrinsic parameters) with respect to the BepiColombo Space Craft reference frame

Fisheye Lens Geometric Calibration

In this report we will show the calibration procedure and the obtained results for the definition of the intrinsic parameters of a wide-angle system through the use of a set of acquisitions of a well-known calibration target. In this case the method is applied to a Fujinon fish-eye camera hereafter called FEL (Fish-Eye Lens)

Hyperhemispheric Lens Geometric Calibration

In this report we will show the calibration procedure and the obtained results for the definition of the intrinsic parameters of a wide-angle lens through the use of a set of acquisitions of a well-known calibration target. In this case the method is applied to INAF payload panoramic hereafter called BPL (Bifocal Panoramic Lens

Absolute calibration of the Colour and Stereo Surface Imaging System (CaSSIS)

The Colour and Stereo Surface Imaging System (CaSSIS) onboard the ExoMars Trace Gas Orbiter (TGO) has observed several standard stars and Jupiter with the aim of deriving the absolute calibration factors that convert observed signal into reflectance (”I over F”). The targets were observed through all four colour filters and hence a relative calibration between the filters was possible. In addition, observations of Phobos acquired during the TGO capture orbits in 2016 were analysed in support of the relative colour calibration. The results show that CaSSIS was around 13% less sensitive than predicted (normalised to the RED filter) - a value that is larger than the formal uncertainty and therefore significant. The relative colour calibration shows CaSSIS to be 4% more sensitive in the BLU than modelled which is close to the relative uncertainty. The text describes the analysis approach and methods for the various targets and newly recommended conversion factors are provided in table form

INAF-Padova-TN-3DPD-SUM

The Team at the Observatory of Padova (INAF) developed a stereo 3d reconstruction pipeline for the planetary images, by taking advantage of its know-how from the design, realization and calibration of the stereo camera STC on board the BepiColombo mission. The stereo cameras STC and CaSSIS are different in terms of optical design and stereo strategy, but they both apply the push-frame acquisition mode. In this context, an ad-hoc DTM generation software, called 3DPD, has been developed.This document describes the nowadays procedures for the internal use of the 3DPD software and the associated MATLAB tools finalized to: - update of the CaSSIS images and spice kernels - Read CaSSIS images data and projection matrices assembly - generate the stereo pair mosaic projects - generate the 3D models (DTMs) - update the OAPD Archive (https://cassis.oapd.inaf.it/archive/) All these procedures can be performed only by OAPD Workstations. Changes in the procedures will be documented in the next issues of this report

New simulation of Phobos Stickney crater

In this work we model the Phobos Stickney impact crater using the iSALE hydrocode and considering different scenarios that could form the well-studied crater

Phobos spectral clustering: first results using the MRO-CRISM 0.4-2.5 micron dataset

Whether Phobos is a captured asteroid or it formed in situ around Mars, is still an outstanding question within the scientific community. The proposed Japanese Mars Moon eXploration (MMX) sample return mission has the chief scientific objective to solve this conundrum, reaching Phobos in early 2020s and returning Phobos samples to Earth few years later. Nonetheless, well before surface samples are returned to Earth, there are important spectral datasets that can be mined in order to constrain Phobos' surface properties and address implications regarding Phobos' origin. One of these is the MRO-CRISM multispectral observations of Phobos. The MRO-CRISM visible and infrared observations (0.4-2.5 micron) are here corrected for incidence and emission angles of the observation. Unlike previous studies of the MRO-CRISM data that selected specific regions for analyses, we apply a statistical technique that identifies different clusters based on a K-means partitioning algorithm. Selecting specific wavelength ranges of Phobos' reflectance spectra permits identification of possible mineralogical compounds and the spatial distribution of these on the surface of Phobos. This work paves the way to a deeper analysis of the available dataset regarding Phobos, potentially identifying regions of interest on the surface of Phobos that may warrant more detailed investigation by the MXX mission as potential sampling areas. Acknowledgments: M. Pajola was supported for this research by an appointment to the NASA Postdoctoral Program at the Ames Research Center administered by USRA

BC-SIM-TR-032 HRIC ICO4 REPORT

The present document has been issued to describe the Instrument Check Out Phase (ICO#4) Tests of HRIC, channel of the Spectrometers and Imagers for MPO BepiColombo Integrated Observatory SYStem (SIMBIO-SYS)