ИСТИНА

The kinematical parameters of the local field RR Lyrae population and the zero-point of the log P-<~ngle M_Krangle relation for these variables are inferred by applying the statistical parallax (maximum-likeli-hood) technique to a sample of 182 RR Lyraes with known periods, radial-velocities, metallicities, K-band photometry, and absolute proper motions on the ICRS system. Hipparcos, Tycho-2, SPM, UCAC, NPM1, and the Four-Million Star Catalog (Volchkov et al. 1992) were used as the sources of proper motions; the proper motions of the last two catalogs are reduced to the Hipparcos (ICRS) system (Dambis & Rastorguev 2001). The K-band magnitudes were adopted from the list of Fernley et al. (1998) and supplemented by the data of the 2MASS Second Incremental Data Release. The parameters of the velocity distribution are found to be: (U_0 = -10 ± 10, V_0 = -51 ± 8, W_0 = -14 ± 5) km s^{-1}; (σ_U = 62 ± 10, σ_V = 45 ± 8, σ_W = 28 ± 6) km s^{-1}: and (U_0 = -23 ± 13, V_0 = -213 ± 12, W_0 = -5 ± 8) km s^{-1}; (σ_U = 157 ± 12, σ_V = 98 ± 8, σ_W = 91 ± 7) km s^{-1} for the thick-disk (41 stars) and halo (141 stars) objects, respectively. The zero-point of the infrared PL relation of Jones et al. (1992) (based on the results obtained using the Baade-Wesselink method) is confirmed: we find <~ngle M_Krangle = -2.33 \cdot log P_F-0.82 ± 0.12 compared to <~ngle M_Krangle = -2.33 \cdot log P_F-0.88 as inferred by Jones et al. (1992). A conversion of the resulting log P-<~ngle M_Krangle relation to V-band luminosities yields the metallicity-luminosity relation <~ngle M_Vrangle = +1.04 + 0.14 \cdot [Fe/H] ± 0.11. Our results imply a solar Galactocentric distance of R_0 = 7.6 ± 0.4 kpc and an LMC distance modulus of DM_LMC = 18.18 ± 0.12 (cluster RR Lyraes) or DM_LMC = 18.11 ± 0.12 (field RR Lyraes), thereby favoring the so-called short distance scale.