Measurements of the near-infrared stellar scintillation above the Observatorio del Teide (Tenerife)

Fuentes, F. J.; Fuensalida, J. J.; Sanchez-Magro, C.

doi:10.1093/mnras/226.4.769

Cited by 8 publications

(6 citation statements)

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“…These results agree reasonably with the experiments [65]. The later investigations [65][66][67][68] have shown that dependence (27) is valid for small and moderate zenith angles or for highly elevated optical ground stations. For large zenith angles measured stellar scintillations exhibit a saturation or decrease in its value.…”

Section: B Aperture-averaged Scintillationssupporting

confidence: 89%

“…5 with observer's elevation of 602 m above sea level. The saturation region may even vanish at particularly high altitudes, the phenomenon which is known in optical astronomy [62,67,68]. This observation makes observatories in mountains especially attractive as a OGS node for quantum free-space communication with satellites.…”

Section: Application: Decoy State Protocolmentioning

confidence: 99%

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Satellite-mediated quantum atmospheric links

2019

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The establishment of quantum communication links over a global scale is enabled by satellite nodes. We examine the influence of Earth's atmosphere on the performance of quantum optical communication channels with emphasis on the downlink scenario. We derive the geometrical path length between a moving low Earth orbit satellite and an optical ground station as a function of the ground observer's zenith angle, his geographical latitude, and the meridian inclination angle of the satellite. We show that the signal distortions due to regular atmospheric refraction, atmospheric absorption, and turbulence have a strong dependence on the zenith angle. The observed saturation of transmittance fluctuations for large zenith angles is explained. The probability distribution of the transmittance for slant propagation paths is derived, which enables us to perform the security analysis of decoy state protocols implemented via satellite-mediated links.

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Section: B Aperture-averaged Scintillationssupporting

confidence: 89%

Section: Application: Decoy State Protocolmentioning

confidence: 99%

Satellite-mediated quantum atmospheric links

2019

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“…The later investigations [65][66][67][68] have shown that dependence ( 27) is valid for small and moderate zenith angles or for highly elevated optical ground stations. For large zenith angles measured stellar scintillations exhibit a saturation or decrease in its value.…”

Section: B Aperture-averaged Scintillationsmentioning

confidence: 99%

Satellite-mediated quantum atmospheric links

Vasylyev,

Vogel,

Moll

2019

Preprint

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“…Although, at shorter wavelengths, the characteristic variability is expected to occur on shorter time scales, there exist but few previous measurements of this dependence. At Observatorio del Teide on Tenerife (the neighbor island of La Palma), Fuentes et al (1987) measured scintillation in the 7, H, K, and L near-infrared atmospheric windows, finding the autocorrelation time to be some 30% longer in L(\3.5 ¡jum) than in /(X1.2 ¡jlvsx). Also, the relative variances between pairs of passbands showed consistently less scintillation at longer wavelengths.…”

Section: Differences In Time Scalementioning

confidence: 99%

Atmospheric Intensity Scintillation of Stars. II. Dependence on Optical Wavelength

Dravins¹,

Lindegren²,

Mezey³

et al. 1997

PASP

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ABSTRACT. Atmospheric intensity scintillation of stars on milli-and microsecond time scales was extensively measured at the astronomical observatory on La Palma (Canary Islands). Scintillation statistics and temporal changes were discussed in Paper I, while this paper shows how scintillation depends on optical wavelength. Such effects originate from the changing refractive index of air, and from wavelength-dependent diffraction in atmospheric inhomogeneities. The intensity variance aj increases for shorter wavelengths, at small zenith distances approximately consistent with a theoretical X -7/6 slope, but with a tendency for a somewhat weaker dependence. Scintillation in the blue is more rapid than in the red. The increase with wavelength of autocorrelation time scales (roughly proportional to >/\) is most pronounced in very small apertures, but was measured up to 0 20 cm. Scintillation at different wavelengths is not simultaneous: atmospheric chromatic dispersion stretches the atmospherically induced "flying shadows" into "flying spectra" on the ground. As the "shadows" fly past the telescope aperture, a time delay appears between fluctuations at different wavelengths whenever the turbulence-carrying winds have components parallel to the direction of dispersion. These effects increase with zenith distance (reaching -100 ms cross-correlation delay between blue and red at Z = 60° ), and also with increased wavelength difference. This time delay between scintillation in different colors is a property of the atmospheric flying shadows, and thus a property that remains unchanged even in very large telescopes. However, the wavelength dependence of scintillation amplitude and time scale is "fully" developed only in small telescope apertures ( ^ 5 cm), the scales where the "flying shadows" on the Earth's surface become resolved. Although these dependences rapidly vanish after averaging in larger apertures, an understanding of chromatic effects may still be needed for the most accurate photometric measurements. These will probably require a sampling of the (stellar) signal with full spatial, temporal, and chromatic resolution to segregate the scintillation signatures from those of astrophysical variability.

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Measurements of the near-infrared stellar scintillation above the Observatorio del Teide (Tenerife)

Cited by 8 publications

References 0 publications

Satellite-mediated quantum atmospheric links

Satellite-mediated quantum atmospheric links

Satellite-mediated quantum atmospheric links

Atmospheric Intensity Scintillation of Stars. II. Dependence on Optical Wavelength

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