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In comparison with spectroscopy of extended extragalactic objects, the task
of observing stars with a high spectral resolution is traditionally given
lower priority. The reason is fundamental: in spectroscopy of extended
objects the limiting magnitude is proportional to the squared telescope
mirror diameter, whereas in high spectral resolution spectroscopy of stars
(i.e. when the angular diameter of the turbulent disk of a star is larger
than the spectrograph slit width) the limiting magnitude is proportional to
the telescope mirror diameter. A ``natural'' response of some researchers of
stars and starlike objects is preferential use of low and moderate spectral
resolution techniques, where one succeeds in minimizing losses at the
spectrograph input. However, over the last decade new problems of
spectroscopy of cool stars, interstellar and intergalactic medium, mapping of
stars' surfaces, search for low-mass companion stars have been posed and
being solved. All these problems are limiting for large
telescopes, that is why the development of high-resolution spectroscopy
facilities at large telescopes is of great concern. Suffice it
document
to mention that the first device put into operation at the 10 m Keck
telescope is the high-resolution echelle spectrograph HIRES (Fogt et al.,
1994). In order to show how the achievements in technology of manufacturing
solid-state light detectors and the development of cross-dispersion
spectral systems alter psychology of a spectroscopist, we now present some
considerations on the relationship of principal characteristics determined in
the process of observations.
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