The brightness of the sky of the Caucasian Mountain Observatory of MSU in the near infrared
- Authors: Tatarnikova A.M.1, Zheltoukhov S.G.1, Nikishev G.E.1, Tarasenkova A.N.1,2, Sharonova A.V.1
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Affiliations:
- Lomonosov Moscow State University
- Institute of Astronomy of the Russian Academy of Sciences
- Issue: Vol 101, No 1 (2024)
- Pages: 42-55
- Section: Articles
- URL: https://journals.rcsi.science/0004-6299/article/view/261217
- DOI: https://doi.org/10.31857/S0004629924010053
- EDN: https://elibrary.ru/LFSZBU
- ID: 261217
Cite item
Abstract
The results of measurements of background brightness in the near-infrared range (bands J, H, K), carried out in 2016–2023 at the Caucasus Mountain Observatory of Moscow State University was analyzed. It is shown that the instrumental background associated with the thermal radiation of the telescope is noticeable only in the K band, and at operating temperatures its contribution mainly determines the level of the overall background in this band. The coefficients of a polynomial taking into account the contribution of instrumental and extra-atmospheric backgrounds are presented. It is shown that the brightness of the sky background does not depend on air temperature, but a weak dependence on the water vapor content is observed, close to that expected from model calculations: in the J and H bands, the background brightness decreases at a rate of ≈1%/1 mm, and in the K band it grows at a rate of ≈2.5%/1 mm. The maximum amplitude of background brightness variability on short time scales (~30 minutes) has been estimated: ≈10% in the J and K bands and ≈30% in the H band. The maximum contribution of Moon’s radiation scattered in the atmosphere to the overall background level has been determined. It is shown that this contribution can be ignored at an angular distance of the observation point from the Moon greater than ~10° even during a full moon. The average background surface brightness mag/arcsec² in the J, H and K bands was calculated: mJ = 15.7, mH = 13.9 and mK = 13.1.
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About the authors
A. M. Tatarnikova
Lomonosov Moscow State University
Author for correspondence.
Email: andrew@sai.msu.ru
Russian Federation, Moscow
S. G. Zheltoukhov
Lomonosov Moscow State University
Email: andrew@sai.msu.ru
Russian Federation, Moscow
G. E. Nikishev
Lomonosov Moscow State University
Email: andrew@sai.msu.ru
Russian Federation, Moscow
A. N. Tarasenkova
Lomonosov Moscow State University; Institute of Astronomy of the Russian Academy of Sciences
Email: andrew@sai.msu.ru
Russian Federation, Moscow; Moscow
A. V. Sharonova
Lomonosov Moscow State University
Email: andrew@sai.msu.ru
Russian Federation, Moscow
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