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The Spectro Point Spread Function for GAIA

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Abstract

We discuss the point spread function for the Spectro instrument based on realistic effects of the time delayed integration, transverse image motion and pixelization, but assuming rather small wave front errors. Stars brighter than 10 mag, which will saturate the CCD, may be observed photometrically using the image wings, but the central wavelengths will be slightly shifted towards the red.

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References

  • ESA: 2000, 'GAIA: Composition, Formation and Evolution of the Galaxy', Technical Report, ESA-SCI(2000)4.

  • Fabricius, C. and Lindegren, L.: 2000, Point spread function for spectro, Technical Report from Copenhagen University Observatory, GAIA-CUO-85.

  • Høg, E.: 2001, Photometric and imaging performance, in: O. Bienaymé and C. Turon (eds.), J. Phys. IV France, Gaia, a European Space Project, in press.

  • Lattanzi, M., Carollo, D. and Gai, M.: 1998, Aberrated point spread function's for the MMS configuration and astrometric error, Technical Report, SAG-ML-014.

  • Lindegren, L.: 1998, Point spread functions for GAIA including aberrations, Technical Report from Lund Observatory, SAG-LL-025.

  • Matra Marconi Space (MMS): 1999, GAIA CTS Study.

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Authors and Affiliations

  1. Copenhagen University Observatory, Juliane Maries Vej 30, DK-2100, Copenhagen Ø, Denmark

    Claus Fabricius

  2. Lund Observatory, Box 43, SE-22100, Lund, Sweden

    Lennart Lindegren

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  1. Claus Fabricius
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  2. Lennart Lindegren
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Fabricius, C., Lindegren, L. The Spectro Point Spread Function for GAIA. Astrophysics and Space Science 280, 51–56 (2002). https://doi.org/10.1023/A:1015587924410

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  • DOI: https://doi.org/10.1023/A:1015587924410

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