On the base of the Galaxy survey in OH lines at 1665 and 1667 MHz (Turner (1979,Astron. Astrophys. Suppl. Ser. 37, 1)) the method of distance determination to molecular clouds was proposed. It was shown (Kolesnik and Yurevich (1985,Astrofizika 22,461)) that the Δv - a linewidth (in km·s−1) and TA - a linedepth (in K) of the OH absorption features could be combined into a parameter D(r) = (Δv2/TA)1/3 that is sensitive to the distance r (in kpc) of molecular cloud where this OH absorption is formed. The calibration of (D-r)-relation gives