PDS_VERSION_ID = PDS3 LABEL_REVISION_NOTE = "2022-02-02, KDM, Initial version" RECORD_TYPE = STREAM RELEASE_ID = 0001 REVISION_ID = 0000 OBJECT = INSTRUMENT INSTRUMENT_HOST_ID = MEX INSTRUMENT_ID = HRSC OBJECT = INSTRUMENT_INFORMATION INSTRUMENT_NAME = "HIGH RESOLUTION STEREO CAMERA" INSTRUMENT_TYPE = "CCD CAMERA" INSTRUMENT_DESC = " Instrument Overview =================== The High Resolution Stereo Camera (HRSC), originally developed for the Russian-led Mars-96 mission, was selected as part of the Orbiter payload for ESA s Mars Express mission. The HRSC is a pushbroom scanning instrument with nine CCD line detectors mounted in parallel in the focal plane. Its unique feature is the ability to obtain near-simultaneous imaging data of a specific site at high resolution, with along-track triple stereo, four colours and five different phase angles, thus avoiding any time- dependent variations of the observational conditions. An additional Super-Resolution Channel (SRC) a framing device will yield nested images in the metre-resolution range for detailed photogeologic studies. The spatial resolution from the nominal periapsis altitude of 250 km will be 10 m px 1, with an image swath of 53 km, for the HRSC and 2.3 m px 1 for the SRC. During the mission s nominal operational lifetime of 1 Martian year (2 Earth years) and assuming an average HRSC data transfer share of 40%, it will be possible to cover at least 50% of the Martian surface at a spatial resolution of d 15 m px 1. More than 70% of the surface can be observed at a spatial resolution of d 30 m px 1, while more than 1% will be imaged at better than 2.5 m px 1. The HRSC will thus close the gap between the medium- to low resolution coverage and the very high-resolution images of the Mars Observer Camera on the Mars Global Surveyor mission and the in situ observations and measurements by landers. The HRSC will make a major contribution to the study of Martian geosciences, with special emphasis on the evolution of the surface in general, the evolution of volcanism, and the role of water throughout Martian history. The instrument will obtain images containing morphologic and topographic information at high spatial and vertical resolution, allowing the improvement of the cartographic base down to scales of 1:50 000. The experiment will also address atmospheric phenomena and atmosphere-surface interactions, and will provide urgently needed support for current and future lander missions as well as for exobiological studies. The goals of HRSC on Mars Express will not be met by any other planned mission or instrument. Science Objectives ================== The HRSC directly addresses two of the main scientific goals of the Mars Express mission (high-resolution photogeology and surface-atmosphere interactions) and significantly supports another two (atmospheric studies and mineralogical mapping). In addition, the imagery will make a major contribution to characterising the landing site geology and its surroundings for the Mars Express and other Mars missions (e.g. NASA's Mars Exploration Rovers). The scientific objectives and measurement goals have been formulated by an international team of 45 Co-Investigators (Co- Is) from 10 countries under the leadership of the Principal Investigator (PI). The image data will focus on: - characterisation of the surface structure and morphology at high spatial resolution of e10 m px 1; - characterisation of the surface topography at high spatial and vertical resolution; - characterisation of morphological details at super-resolution of up to 2 m px 1; - terrain classification at high spatial resolution by means of colour imaging; refinement of the geodetic control network and the Martian cartographic base; - characterisation of atmospheric phenomena; - characterisation of physical properties of the surface through multi-phase angle measurement; - observation of Phobos and Deimos. Investigators and Other Key Personnel ===================================== Principal Investigator: G. Neukum, FU Berlin, Germany Experiment Manager: R. Jaumann, DLR Berlin, Germany Data Processing Manager: T. Roatsch, DLR Berlin, Germany HRSC Co-Investigators: J. Albertz, TU Berlin, Germany G. Bellucci, Istituto di Fisica Spazio Interplanetario (INAF), Italy J.-P. Bibring, Institut d Astrophysique Spatiale, CNRS, France M. Buchroithner, TU Dresden, Germany E. Dorrer, Universitaet der Bundeswehr, Muenchen, Germany H. Ebner, TU Muenchen, Germany E. Hauber, Institut fuer Planetenforschung, DLR, Berlin, Germany C. Heipke, TU Hannover, Germany H. Hoffmann, Institut fuer Planetenforschung, DLR, Berlin, Germany W.-H. Ip, Max-Planck-Institut fuer Aeronomie, Katlenburg-Lindau, Germany R. Jaumann, Institut fuer Planetenforschung, DLR, Berlin, Germany H.-U. Keller, Max-Planck-Institut fuer Aeronomie, Katlenburg- Lindau, Germany P. Kronberg, TU Clausthal, Germany W. Markiewicz, Max-Planck-Inst. fuer Aeronomie, Katlenburg- Lindau, Germany H. Mayer, Universitaet der Bundeswehr, Muenchen, Germany F.M. Neubauer, Universitaet Koeln, Germany J. Oberst, Institut fuer Planetenforschung, DLR, Berlin, Germany M. Paetzold, Universitaet Koeln, Germany R. Pischel, Institut fuer Planetenforschung, DLR, Berlin, Germany G. Schwarz, DLR Oberpfaffenhofen,, Germany T. Spohn, Institut fuer Planetenforschung, DLR, Berlin, Germany B.H. Foing, ESA - ESTEC, Noordwijk, Netherlands K. Kraus, TU Wien, Austria K. Lumme, University of Helsinki, Finland P. Masson, Univ. Paris-Sud, France J.-P. Muller, University College London, United Kingdom J.B. Murray, The Open University, Buckinghamshire, United Kingdom G. Gabriele Ori, Universita d Annunzio, Italy P. Pinet, GRGS, Observatoire de Midi-Pyrenees, France J. Raitala, University of Oulu, Finland A.T. Basilevsky, Russian Academy of Science, Moscow, Russia B.A. Ivanov, Russian Academy of Science, Moscow, Russia R. Kuzmin, Russian Academy of Science, Moscow, Russia M.H. Carr, US Geological Survey, Menlo Park, USA T.C. Duxbury, NASA-JPL, USA R. Greeley, Arizona State University, Phoenix, USA. J.W. Head, Brown University, Providence, USA R. Kirk, US Geological Survey, Flagstaff, USA T.B. McCord, University of Hawaii, USA S.W. Squyres, Cornell University, Ithaca, USA A. Inada, Kobe University, Japan HRSC Experiment Team. DLR: T. Behnke, U. Carsenty, K. Eichentopf, J. Flohrer, B. Giese, K. Gwinner, E. Hauber, H. Hirsch, H. Hoffmann, A. Hoffmeister, R. Jaumann, D. Jobs, U. Koehler, K.-D. Matz, V. Mertens, J. Oberst, S. Pieth, R. Pischel, C. Reck, E. Ress, D. Reifl, T. Roatsch, F. Scholten, G. Schwarz, I. Sebastian, S. Sujew, W. Tost, M. Tschentscher, M. Waehlisch, I. Walter, M. Weiss, S. Weifle, M. Weiland, K. Wesemann; FU Berlin: T. Denk, O. Fabel, S. van Gasselt, C. Georgi, S. Huber, G. Mygiakis, G. Neukum, S. Preuschmann, B. Schreiner, S. Werner, W. Zuschneid; Subcontractors: A. Zaglauer, U. Schoenfeldt, K. Eckhardt, J. Krieger, D, Tennef, S. Govaers, A. Kasemann, M. Langfeld (DLR/Anagramm), E. Rickus (Levicki microelectronic), J. Schoeneich (Jena-Optronik) Instrument Specification ======================== The HRSC instrument consists of the camera unit containing the HRSC stereo colour scanner and the Super-Resolution Channel (SRC), and of the digital unit. The unique capability of the HRSC stereo colour scanner is to obtain quasi-simultaneously high- resolution images in three-line stereo, in four colours and at five phase angles. The combination with the SRC makes it a five- in-one camera: - the along-track acquisition of stereo imagery avoids changes in atmospheric and illumination conditions which so far have caused severe problems in the photogrammetric evaluation of stereo images acquired at well-separated times; - the triple stereo images permit robust stereo reconstruction, yielding Digital Terrain Models (DTMs) at a vertical resolution similar to the high pixel resolution of the nadir sensor, with 10 m px 1 at 250 km altitude (periapsis); - the colour images enable terrain classification and provide information on compositional variations and surface weathering as a complement to the more specific (but with lower spatial resolution) mineralogical information obtained by the imaging spectrometer of Mars Express; - the multiphase imagery will address the physical properties of the Martian soil (roughness, grain size, porosity) via photogrammetric data evaluation by providing a second stereo angle triplet (in essence quintuple stereo); - the super-resolution imagery, nested in the broader swath of the scanner with a spatial resolution of 2.3 m px 1 at periapsis, will serve as the magnifying lens to analyse surface morphology at even greater detail. The HRSC stereo colour scanner is a multi-sensor pushbroom instrument, with nine CCD line sensors mounted in parallel delivering nine superimposed image swaths. Originally, it was developed as the HRSC instrument for the Russian Mars-96 mission. Two fully tested and calibrated Flight Models were prepared, and only minor modifications to the remaining version were required to satisfy the Mars Express interface requirements. The stereo colour scanner comprises a baffle, optics, optical bench, spectral filters, CCD sensors lines, sensor electronics and thermal control system. The technical design is defined by: - single-optics design; - CCD line arrays with 5272 pixels each; - nine detectors for simultaneous stereo and colour imaging, and for multi-phase angle measurements; - CCDs and sensor electronics implemented in high-reliability hybrid, low-noise and low-power technology; - implementation of the CCD-control unit in ASICs. The SRC is a framing device and uses an interline CCD detector to cope with the very short exposure and read-out times. It is based on an instrument development for the Rosetta Lander and the design is characterised by: - CCD area array interline detector with 1024 x 1032 pixels; - highly miniaturised and low-power detector and control electronics; - compact 3D multi-chip module technology using thin-film multilayer metallisation, dycostrate, plasma-etching and chip- on-wire technology; - selectable dynamic range of 8- and 14-bit per pixel; - internal data buffer to store eight 8-bit (or four 14-bit) images; - lightweight Maksutov-Cassegrain telescope with a focal length of 975 mm INSTRUMENT OPERATION ==================== In general, the HRSC (Camera Head) and the SRC will be operated simultaneously. However, the Camera Head and the SRC also can be operated separately. The SRC can be operated - in the direct mode (direct input into the DU) In the case of joint operations with the Camera Head (CH) this mode requires that the 9 CCD line signals are processed by three of the four signal chains (which reduces the possible number of configurations or macro modes). The fourth signal chain is exclusively used for SRC. The SRC data is fully integrated in the basic HRSC data stream. - in the buffer mode This mode is applicable for all HRSC macro modes. Eight 8-bit or four 14-bit SRC images can be stored in an internal buffer. At the end of an imaging session these images are processed by the signal chain #4. For each of the SRC operational modes the following exposure modes can be selected by command: - spot mode: single images - raster mode: images taken at a predefined time distance - contiguous imaging: raster imaging with such a distance between subsequent exposures that a contiguous image strip is generated The HRSC instrument output rate is mainly defined by the scan frequency of the Camera Head, i.e. it changes with the S/C altitude. The SRC images are fully embedded in the HRSC instrument data stream. They reach not more than 10% in the entire data stream even in the contiguous mode. The HRSC data output rate is reduced by two measures: - pixel binning Each of the four signal chains can be commanded to sum pixels in flight and across flight direction: 1x1, 2x2, 4x4 and 8x8 (macropixel formats). One signal chain can handle only - one sensor 1x1 or - up to two sensors 2x2 or - up to four sensors 4x4 or - up to eight sensors 8x8 or - SRC images - Data compression Each of the four signal chains performs in parallel an on-line (hardware) data compression with a modified JPEG algorithm. The compression rate is defined not directly but only through a quality factor given by command. In general we assume compression factors from 6..10 for nominal operations. The actual output at a certain time instance rate depends on the compression behaviour (scene contents, buffer handling of the hardware etc) and cannot be exactly predicted. " END_OBJECT = INSTRUMENT_INFORMATION OBJECT = INSTRUMENT_REFERENCE_INFO REFERENCE_KEY_ID = "NEUKUM&JAUMANN2004" END_OBJECT = INSTRUMENT_REFERENCE_INFO END_OBJECT = INSTRUMENT END