Space Science Reviews

, Volume 128, Issue 1, pp 397–412



    • IAS, Institut d’Astrophysique Spatiale
  • P. Lamy
    • LAM, Laboratoire d’Astrophysique de Marseille
  • Y. Langevin
    • IAS, Institut d’Astrophysique Spatiale
  • A. Soufflot
    • IAS, Institut d’Astrophysique Spatiale
  • M. Berthé
    • IAS, Institut d’Astrophysique Spatiale
  • J. Borg
    • IAS, Institut d’Astrophysique Spatiale
  • F. Poulet
    • IAS, Institut d’Astrophysique Spatiale
  • S. Mottola
    • IWP/DLR

DOI: 10.1007/s11214-006-9135-5

Cite this article as:
Bibring, J., Lamy, P., Langevin, Y. et al. Space Sci Rev (2007) 128: 397. doi:10.1007/s11214-006-9135-5


CIVA (Comet Infrared and Visible Analyser) is an integrated set of imaging instruments, designed to characterize the 360 panorama (CIVA-P) as seen from the Rosetta Lander Philae, and to study surface and subsurface samples (CIVA-M). CIVA-P is a panoramic stereo camera, while CIVA-M is an optical microscope coupled to a near infrared microscopic hyperspectral imager. CIVA shares a common Imaging Main Electronics (IME) with ROLIS. CIVA-P will characterize the landing site, with an angular sampling (IFOV) of 1.1 mrad: each pixel will image a 1 mm size feature at the distance of the landing legs, and a few metres at the local horizon. The panorama will be mapped by 6 identical miniaturized micro-cameras covering contiguous FOV, with their optical axis 60 apart. Stereoscopic capability will be provided by an additional micro-camera, identical to and co-aligned with one of the panoramic micro-camera, with its optical axis displaced by 10 cm. CIVA-M combines two ultra-compact and miniaturised microscopes, one operating in the visible and one constituting an IR hyperspectral imaging spectrometer: they will characterize, by non-destructive analyses, the texture, the albedo, the molecular and the mineralogical composition of each of the samples provided by the Sample Drill and Distribution (SD2) system. For the optical microscope, the spatial sampling is 7 μm; for the IR, the spectral range (1–4 μm) and the spectral sampling (5 nm) have been chosen to allow identification of most minerals, ices and organics, on each pixel, 40 μm in size. After being studied by CIVA, the sample could be analysed by a subsequent experiment (PTOLEMY and/or COSAC). The process would be repeated for each sample obtained at different depths and/or locations.


cometary compositionin situ imagingmicroscopic analyses

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© Springer Science+Business Media, Inc. 2007