Abstract
The tilt is the phase gradient across the entire telescope pupil. At the telescope focus it results in image wandering. For the tilt, the atmosphere can be simulated as a two-dimensional prism whose angle continuously varies. The typical characteristic time of the tilt varies from a few milli-arcsecs (mas) to a few hundred mas depending on the wavelength and on the seeing. This is significantly longer than the round trip time of light to the mesosphere, which is between 0.6 and 1.2 ms, respectively, at the zenith and at 60° from the zenith. Consequently, the laser beam of a laser guide star (LGS) is equally deflected on its path to and from the mesosphere and the laser spot appears fixed with respect to the telescope’s optical axis, independent of the true position of the spot in the mesosphere. This prevents us measuring the tilt[1].
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Foy, R. (2000). The Tilt Problem — Multiwavelength. In: Ageorges, N., Dainty, C. (eds) Laser Guide Star Adaptive Optics for Astronomy. NATO ASI Series, vol 551. Springer, Dordrecht. https://doi.org/10.1007/978-94-015-9624-4_8
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DOI: https://doi.org/10.1007/978-94-015-9624-4_8
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