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We studied 102 star forming regions in seven spiral galaxies (NGC 628, NGC783, NGC 2336, NGC 6217, NGC 6946, NGC 7331, and NGC 7678) on the basis ofcomplex spectroscopic, photometric (UBVRI) and spectrophotometric (H alphaline) observations. Using data on the chemical composition and absorption inHII regions, obtained from spectroscopic observations, and using evolutionarymodels, we estimated physical parameters (ages and masses) of young stellargroupings embedded in HII regions. We found that the gas extinction, A(gas),which determined from the Balmer decrement, does not correspond in some casesto the absorption A(stars) in the young stellar associations (complexes). Thisis due to the spatial offset relative HII cloud the stellar group related tohim. It has been found that the condition A(gas) = A(stars) does not satisfiedfor the star forming regions, in which: 1) the contribution to the totalemission of gas in the B and/or V bands is higher than 40%, and 2) EW(H alpha)> 1500A. Extinction A(V) in studied star forming regions corrected for theGalactic absorption A(V)Gal ranges from 0 to 3 mag with a mean valueA(V)-A(V)Gal = 1.18+-0.84 mag. We estimated masses and ages for 63 star formingregions. The regions have ages from 1 to 10 Myr, the most part of them areyounger than 6 Myr. The derived masses of young stellar groupings range from10^4Msun in the nearby galaxies NGC 628 and NGC 6946 to 10^7Msun in the mostdistant NGC 7678. More than 80% of groupings have masses between 10^5Msun and10^6Msun. The lowest mass estimate of 1x10^4Msun for the objects in NGC 628 andNGC 6946 belongs to the mass interval of the youngest Galactic open clusters.

Study of young stellar groupings in HII regions based on the spectral and photometric data