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
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© 2002 Springer Science+Business Media Dordrecht
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Fabricius, C., Lindegren, L. (2002). The Spectro Point Spread Function for GAIA. In: Vansevičius, V., Kučinskas, A., Sūdžius, J. (eds) Census of the Galaxy: Challenges for Photometry and Spectrometry with GAIA. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0361-2_7
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DOI: https://doi.org/10.1007/978-94-010-0361-2_7
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-3911-6
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