of theoretic variants explaining the bursts, at least for a chosen class of galactic models discussed in the literature (Boer et al., 1993; Greiner et al., 1995; Hartmann, 1994).

Formulating below the statement of an observational problem at the 6 m telescope, we mean single compact objects of neutron star type cooled down to a temperature $\approx10^{5}\,\rm K$ and lower. Analogous considerations have already been used in the literature in interpretation of the results of deep photometric study of several [$\gamma$]{}–ray boxes (Hartmann et al., 1989; Motch et al., 1990). Ultimately, in any galactic model of the sources of [$\gamma$]{}–ray bursts, in which attempts of allowing for new data have been made, a problem can be stated of search for [*closest*]{} objects in other wavelength ranges. In this case we are concerned with the sources of short [$\gamma$]{}–ray bursts, that show a $\rm -3/2\,\, logN-logP$ power law at high intensities (Kouveliotou et al., 1993). In particular, these can be optical objects of low luminosity related to these bursts and having a density distribution in the [*B, V, R*]{} bands close to that of a black body. With the help of deep CCD photometry of the localization region of the [$\gamma$]{}–ray 