JANUS on JUICE: a Camera to Investigate Ganymede, Europa, Callisto and the Jovian System

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JANUS on JUICE: a Camera to Investigate Ganymede, Europa, Callisto and the Jovian System JANUS on JUICE: A Camera to Investigate Ganymede, Europa, Callisto and the Jovian System. N. Schmitz1, P. Palumbo9, R. Jaumann1, V. Della Corte2, M. Zusi3, J. M. Castro4, M. Leese5, S. Debei6, D. Magrin7, H. Michalik8, G. Cremonese7, H. Hoffmann1, A. Holland5, L. M. Lara4, B. Fiethe8, E. Friso6, D. Greggio7, M. Her- ranz4, A. Koncz1, A. Lichopoj1, I. Martinez-Navajas4, E. Mazzotta Epifani3, H. Michaelis1, T. Behnke1, R. Rag- azzoni7, T. Roatsch1, J. Rodrigo4, E. Rodriguez4, P. Schipani3, M. Soman5, M. Zaccariotto6, & the JANUS team. 1 DLR-Institute for Planetary Research, Berlin, Germany; 2 INAF-IAPS, Rome, Italy; 3 INAF-OAC, Naples, Italy; 4 IAA-CSIC, Granada, Spain; 5 CEI-Open University, Milton Keynes, UK; 6 CISAS, University of Padova, Pado- va, Italy, 7 INAF-OAPd, Padova Italy; 8 IDA, Technical University of Braunschweig, Germany; 9 DIST, Partheno- pe University, Napoli, Italy. Introduction: The detailed investigation of three of response of ices and ice/salt/clathrate mixtures w.r.t. Jupiter‘s Galilean satellites (Ganymede, Europa, and tectonic stress? To what extent are surfaces altered by Callisto), which are believed to harbour subsurface cosmic weathering and what are the major exogenic water oceans, is central to elucidating the conditions surface alteration processes (micrometeorites, radia- for habitability of icy worlds in planetary systems. The tion, charged particles)? What are the fine-scale char- study of the Jupiter system and the possible existence acteristics of non-ice materials on Callisto? By which of habitable environments offer the best opportunity intriguing mechanisms is CO2-replenishment taking for understanding the origins and formation of the gas place on Callisto? giants and their satellite systems. The JUpiter Icy moons Explorer (JUICE) camera system JANUS (Jo- Further science objectives of JANUS are to vis, Amorum ac Natorum Undique Scrutator) will de- • Characterize the exospheres of the Galilean satel- termine the formation and characteristics of magmatic, lites and search for potential water plumes; tectonic, and impact features, relate them to surface • Characterize and study the physical properties of forming processes, constrain global and regional sur- other satellites of the Jupiter system, including Io, face ages, and investigate the processes of erosion and the irregular and inner satellites; deposition. Global medium resolution imaging of Gan- • Perform a physical characterization of the ring ymede and important parts of the surface of Callisto system; better than 400 m/pixel will provide context infor- • Study the Jupiter troposphere, imaging the active mation. While the resolution capability of the instru- dynamical processes, cloud systems, waves, vor- ment would allow to provide global coverage at a reso- tices, and other instabilities, determining cloud lution of 75m/pixel, the achievable resolution during structure in discrete features, and detecting light- the mission will be limited by mission data volume. ning; Selected targets will be investigated with high- • Observe Jupiter stratospheric variations due to resolution imaging with spatial resolution from 30 vigorous water meteorology and disturbances m/pixel down to <10m/pixel. The camera system has from large vortices, such as the Great Red Spot; 14 panchromatic, broad- and narrow-band filters in the • Investigate the Jupiter upper atmosphere by imag- 0.36 µm to 1.1 µm range, and provides stereo imaging ing auroral activity and particle precipitation in capabilities. JANUS will also allow relating spectral, the form of polar hazes; laser and radar measurements to geomorphology and • Contribute to the study of the interaction between thus will provide the overall geological context. the Jupiter magnetosphere and the bodies embed- ded in it. The JANUS experiment’s science objectives: Outstanding questions that will be addressed Required Performance of the Instrument to Satisfy by JUICE Imaging [1]: What are the relative roles of the Objectives: tectonism and cryovolcanism in shaping the dark and JANUS is the next logical step after the impressive bright terrains on Ganymede? What does the distribu- successes of the imaging studies by Voyager, Galileo tion of craters on the Galilean satellites tell us about and Cassini of the Jovian system. JANUS will allow the evolution of the impactor population in the Jovian orders-of-magnitude steps ahead in terms of coverage system through time? How is the geological evolution and/or resolution and/or time evolution on many tar- of Ganymede and Europa related to the impact, tecton- gets in the Jupiter system. The JANUS camera’s spa- ic and cryovolcanic history and how is the geological tial resolution ranges from 400 m/pixel to < 10m/pixel evolution correlated with differentiation processes and for the three main Galilean satellites, and from a few stages? What are the ages of specific geological units km/pixel to few tens of km/pixel for Jupiter and the on Ganymede and Europa, and how will these findings other targets in the Jovian system. Based on current contribute to our understanding of the origin and evo- best assumptions on the available data volume, JANUS lution of the Jupiter system? What is the rheological observations will cover about 100% of Ganymede in 4 high- and low-resolution imaging requirements of colours at 400 m/pixel. About 3% of the surface of the mission; Ganymede will be covered with resolutions better than • instrument operations are flexible enough to op- 30 m/pixel down to 7.5m/pixel during the 500 km cir- timize the acquisition parameters with respect to cular orbit. Stereo imaging at Ganymede is doable at the many different observation requirements and resolutions between 5 to 10 m/pixel and around 25 conditions that JANUS will face. The instrument m/pixel. Stereo images will be acquired both in nadir design will allow to adjust the resolution through pointing and by tilting the spacecraft in a subsequent binning, the field of view through windowing, the orbit. Medium-resolution stereo coverage of Gany- signal levels and SNR through integration time mede will be acquired during the flybys. For Callisto, and the instrument calibration parameters through assuming only nadir pointing, JANUS will cover 100 in-flight calibration and data pre-processing. % of the surface at ≤2 km/pixel, 41 % at ≤1 km/pixel, 14 % at ≤ 400 m/pixel, 6.5% at ≤ 200 m/pixel, and The JANUS design concept has been optimized to some targets at resolutions ~ 10 m/pixel, with 4 colour have the highest probability to guarantee a scientific imaging at medium resolutions. 55% of Europa’s sur- success of the mission by the best usage of the re- face can be covered at ≤ 3 km/pixel, 35 % at ≤1 sources allocated to imaging through the implementa- km/pixel, 30% at ≤ 500 m/pixel, 1% at≤ 100 m/pixel tion of a single NAC channel, with WAC capabilities, and about 0.2% at ~ 10 m/pixel. Low- to medium- with high reliability due to the redundancy philosophy. resolution imaging (i.e. km to ~100 m-range) is ob- The JANUS concept has also the advantage to obtain tained in four colours. Spatial resolutions at Io will the low to medium resolution Ganymede global cover- reach 6 to 20 km/pixel with long monitoring times also age early during the mission, allowing an informed at NIR wavelengths. The rings and minor satellites can choice of observation targets for the high-resolution be observed at maximum resolutions of ~7km/pixel. phase. The resolution at Jupiter’s atmosphere will reach The JANUS camera consists of three units with physi- 9km/pixel. The SNR > 100 can be maintained in al- cal I/F with the JUICE spacecraft: a) the optical head most all observational scenarios. including the telescope and mounting structure, the aperture cover, the filter wheel, and the focal plane; b) the proximity electronics; c) the main electronics in- cluding camera control, data handling, compression and power supply. Figure 1: Expected ground resolution and surface cov- erage for Ganymede by JANUS compared to Galileo JANUS instrument design: Figure 2: JANUS overall configuration General design concept A trade-off between different design solutions, performed by the JANUS team in Optical Head: The Optical Head Unit will be integrat- order to satisfy all JUICE mission’s scientific require- ed on a stable platform together with star- tracker and ments, has led to the following architectural choices: other remote sensing instruments in order to allow co- alignment stability. It includes the optics, the external • a catadioptric telescope is coupled with a framing baffle, the mechanisms (filter wheel and cover) and the detector, avoiding a scanning mechanism and any thermo-mechanical module supporting and condition- operational requirement on the S/C; ing the Focal Plane Assembly (FPA). Iso-static mount- • a fine tuning of instrument parameters coupled ings are foreseen to cope with S/C thermal and me- with the mission design allows to have an instru- chanical constraints. ment designed to be fully compliant with both the For multispectral observations, a set of 14 optical fil- ters is implemented in a filterwheel. Figure 5 lists the different bandwidths and central wavelengths for 13 of them. λ / width Filter id. Note [nm] (tbc) Panchromatic – monochromatic FPAN 650/500 imaging FBLUE 450/60 Blue – satellite colours Green, background for Na – FGREEN 530/60 satellite colours Red, background for Ha– Figure 3: JANUS Optical Head Unit with main optical FRED 656/60 satellite colours and functional elements (design details are under re- Continuum for strong Methane view) CMT medium 750/20 band on Jupiter, geology The optical solution adopted as JANUS camera base- Na 590/10 Sodium D-lines in exospheres line is a Three Mirror Anastigmat (TMA). The camera MT strong 889/20 Strong Methane band on Jupiter Continuum for medium is composed by three mirrors sharing the same optical 2+ axis. The first mirror is a concave off-axis hyperboloid, CMT strong 940/20 Methane band on Jupiter, Fe the secondary mirror is convex with a spherical shape, on satellites Medium Methane band on while the tertiary mirror is a concave off-axis oblate MT medium 727/10 ellipsoid [2].
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