ИСТИНА

We have proposed a new photometric method to estimate thicknesses of galactic disks which is working for the galaxies seen under arbitrary inclination. We stress two distinct advantages of our method: firstly, it provides an individual estimate for every galaxy, beyond a statistical approach, and secondly, for the galaxies which orientation differs from edge-on it allows to confront its vertical structure with the radial brightness profile properties. We have applied our method to two small samples of disk galaxies which radial brightness profiles have been already analysed in the literature: to the $r$-band SDSS images of the galaxies which radial structures are described by Erwin et al. (2008) and Guti\'errez et al.(2011) and to the 3.6-- and 4.5--$\mu$m images made by the space telescope Spitzer and collected in the Spitzer Survey of Stellar Structure in Galaxies (S4G). The radial structures of the latter sample are partly described by Munoz-Mateos et al. (2013). We have obtained significantly different thickness distributions for the purely exponential-profile galactic disks and for the antitruncated stellar disks.