English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

In ground-based measurements of exact posi- tions of celestial objects on the sky the astronomical at- mospheric refraction should be taken into account. In our calculations for refraction we use the Stone code (Stone 1996) where the mean refraction is computed by inte- grating numerically across the passband with Simpson's Rule. The code has been modied for the case of the 10 00 LX200 telescope installed at the Lohrmann Observatory in Dresden. Tabulations of stellar spectral energy from Sviderskiene (1988) together with the quantum eciency of the CCD detector being used, are applied. We have estimated the accuracies of stellar classication required to achieve the desirable accuracies in calculated refraction, the influence of ground-based atmospheric parameters has been discussed too. Some examples of the spectral classi- cation systems which may provide the required classica- tion accuracies, are given. The special case of computing dierential refraction has also been considered. We justify the usefulness of photometric V R and V I indices in calculating refraction. Observations are planned to com- pare calculated and true refraction.

Spectral classification systems and photometry needed in calculations for atmospheric refraction