оПХБНДЪРЯЪ ПЕГСКЭРЮРШ НОПЕДЕКЕМХЪ ОЮПЮЛЕРПНБ БПЮЫЕМХЪ цЮКЮЙРХЙХ, Ю РЮЙФЕ ОЮПЮЛЕРПНБ ЯОХПЮКЭМНИ БНКМШ ОКНРМНЯРХ ОН БШЯНЙНРНВМШЛ ЮЯРПНЛЕРПХВЕЯЙХЛ пяда-МЮАКЧДЕМХЪЛ 28 ЛЮГЕПМШУ ХЯРНВМХЙНБ, ПЮЯОПЕДЕКЕММШУ Б ЬХПНЙНЛ ДХЮОЮГНМЕ ЦЮКЮЙРНЖЕМРПХВЕЯЙХУ ПЮЯЯРНЪМХИ.

The spatial velocities of all 28 currently known masers having trigonometric parallaxes, proper motion and line-of-site velocities are reanalyzed using the Bottlinger equations. These masers are associated with 25 active star-forming regions and are located in the range of galactocentric distances 3 < Ρ < 14 kpc. To determine the Galactic rotation parameters, we have used the first three Taylor expansion terms of angular rotation velocity _ at the galactocentric distance of the Sun, Ρ₀ = 8 kpc. We have obtained the following solutions:
ω = (-31.0 ± 1.2) km·s^-1·kpc^-1; Oort constants, A = (17.8 ± 0.8) km·s^-1·kpc^-1, B = (-13.2 ± 1.5) km·s^-1·kpc^-1; the circular velocity of the solar neighbourhood rotation V₀ = (248 ± 14) km·s^-1. A Fourier analysis of the galactocentric radial velocities of masers VR has allowed us to estimate the wavelength λ = (2.0 ± 0.2) kpc and peak velocity f_R = (6.5 ± 2) km·s^-1 of periodic perturbations from the density wave. The phase of the Sun in the density wave is estimated as χ₀ ≈ (-130 ± 10)°. Taking into account perturbations evoked by the spiral density wave, we have obtained the following non-perturbed components of the peculiar solar velocity with respect to the local standard of rest (LSR): (U0, V0, W0)LSR = [(5.5, 11, 8.5) ± (2, 2, 1)] km·s^-1.