First results of a site-testing programme at Mount Shatdzhatmaz during 2007-2009

Kornilov, V.; Shatsky, N. I.; Voziakova, O.; Safonov, Boris; Potanin, S.; Kornilov, M.

doi:10.1111/j.1365-2966.2010.17203.x

Cited by 32 publications

(30 citation statements)

References 34 publications

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“…As an example, the magnitudes of the normal and the colour scintillations are presented in Table 1 for different situations. These are calculated using the exact WFs (Figs 6 and 7) and a real turbulence profile from MASS measurements at Mount Shatdzhatmaz (Kornilov et al 2010). One specific turbulence profile was chosen, for which the atmospheric moment M 2 corresponded to its median.…”

Section: Discussionmentioning

confidence: 99%

“…Then, the ratio of the indices can be written as Estimates of the altitude atmospheric moments M p =∫ C 2 n ( z ) z p d z can be obtained from vertical distributions of the optical turbulence measured with the MASS (Kornilov et al 2003). For example, measurements at Mount Shadzhatmaz in 2007–2009 show the median of M 2 = 1.1 × 10 −5 m 7/3 (Kornilov et al 2010). The quantity 〈 z 1/3 〉 depends only weakly on the actual turbulence profile and can be set equal to 24 m 1/3 .…”

Section: Short Exposuresmentioning

confidence: 99%

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How achromatic is the stellar scintillation on large telescopes?

Kornilov¹

2011

Monthly Notices of the Royal Astronomical Society

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The atmospheric scintillation of stars is the main reason why the ground-based photometry of astronomical objects has limited accuracy. This becomes particularly noticeable for a variability study with amplitudes of the order of thousandths of stellar magnitude or less. We examine the problem of colour scintillation (i.e. fluctuations of the difference between light intensities measured simultaneously in two different photometric bands). We derive the relations between the colour scintillation power (index) and the atmospheric turbulence, telescope diameter and the characteristics of the photometric channels. Asymptotic dependences for large telescopes (1-10 m) are obtained, which allow us to predict the value of the colour scintillation for a particular telescope and detector. It is shown that the colour scintillation index is ∝ D −3 for measurements with both short (milliseconds) and long (seconds) exposures. We estimate the impact of the atmospheric dispersion, which amplifies colour scintillation away from the zenith. We show that colour scintillation in the long-exposure regime depends strongly on the wind direction in the upper atmosphere.

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Section: Discussionmentioning

confidence: 99%

Section: Short Exposuresmentioning

confidence: 99%

How achromatic is the stellar scintillation on large telescopes?

Kornilov¹

2011

Monthly Notices of the Royal Astronomical Society

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“…used. The monitor is located at an altitude of 2100 m, and it is near the new 2.5 m telescope built by Lomonosov Moscow State University (MSU) [13]. About 300 thousands minute values were obtained from November 2007 to June 2013.…”

Section: Automatic Seeing Monitormentioning

confidence: 99%

Forecasting seeing and parameters of long-exposure images by means of ARIMA

Kornilov

2015

Exp Astron

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Atmospheric turbulence is the one of the major limiting factors for groundbased astronomical observations. In this paper, the problem of short-term forecasting seeing is discussed. The real data that were obtained by atmospheric optical turbulence (OT) measurements above Mount Shatdzhatmaz in 2007-2013 have been analysed. Linear auto-regressive integrated moving average (ARIMA) models are used for the forecasting. A new procedure for forecasting the image characteristics of direct astronomical observations (central image intensity, full width at half maximum, radius encircling 80 % of the energy) has been proposed. Probability density functions of the forecast of these quantities are 1.5-2 times thinner than the respective unconditional probability density functions. Overall, this study found that the described technique could adequately describe temporal stochastic variations of the OT power.

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“…We apply the above development to the vertical profiles of the OT monitored with the MASS/DIMM instrument (Kornilov et al , ) at Mt Shatdzhatmaz (2127 m above sea level) in the North Caucasus (Kornilov et al ) to estimate the angular correlation for the whole turbulent atmosphere.…”

Section: Prediction Of the Angular Correlation Of The Scintillationmentioning

confidence: 99%

Angular correlation of the stellar scintillation for large telescopes

Kornilov

2012

Monthly Notices of the Royal Astronomical Society

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Stellar scintillation is one of the fundamental limitations to the precision of ground‐based photometry. This paper examines the problem of the correlation of the scintillation of two close stars at the focus of a large telescope. The derived correlation functions were applied to data from the long‐term study of the optical turbulence (OT) in the Northern Caucasus with the MASS (Multi‐Aperture Scintillation Sensor) instrument in order to predict the angular correlation of the scintillation at the Sternberg institute 2.5‐m telescope currently in construction. A median angular radius of the correlation as large as 20 arcsec was found for the case of Kolmogorov OT. On the basis of the obtained relations we also analyse the impact of correlation in ensemble photometry and conjugate plane photometry. It is shown that a reduction of the scintillation noise by up to 8 times can be achieved when using a crowded ensemble of comparison stars. The calculation of the angular correlation can be applied for any large telescope at a site where the OT vertical profiles are known.

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First results of a site-testing programme at Mount Shatdzhatmaz during 2007-2009

Cited by 32 publications

References 34 publications

How achromatic is the stellar scintillation on large telescopes?

How achromatic is the stellar scintillation on large telescopes?

Forecasting seeing and parameters of long-exposure images by means of ARIMA

Angular correlation of the stellar scintillation for large telescopes

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