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tokens: spectroscopic analysis. Results for 11 SB1 are shown as open circles. The atmospheric parameters we determined for 402 GK stars are presented in Table 1 (Cols. 69), where the numerical values of , , , and [Fe/H] are presented together with their intrinsic uncertainties. The values of resulting atmospheric parameters generally remain within the range of the TGVIT model grids. Figure 5 shows the relations between the atmospheric parameters presented in Table 1. We note that the results obtained for single-line spectroscopic binaries (SB1) agree very well with those for apparently single stars. The effective temperature lies between 4398 K and 6394 K with a median value of 5167 K. The distribution of , presented in Fig. 6 a, shows two maxima, one for giants (cooler) and one for subgiants (warmer), which are the two most numerous groups of stars in our sample. The intrinsic uncertainty distribution in is presented in Fig. 6 e. The gravitational accelerations for our sample range between 1.49 and 4.72 with a median of 3.65. The distribution of is presented in Fig. 6 b. We found that 5 stars have , 60 have , 277 have and 60 stars have . Most of our stars (194) have of which means that generally they are subgiants. The uncertainty distribution in is presented in Fig. 6 f. The microturbulence velocity, , reaches values from to and has a median at . Most of our stars have between and (Fig. 6 c). The uncertainty distribution in is presented in Fig. 6 g. The metallicity of the stars in our sample, [Fe/H], remains within the limit of to with a median value at . Most of our objects have [Fe/H] in the range of to . Figure 6 d presents the distribution, which clearly shows that our stars are mostly less metal abundant than the Sun. The uncertainty distribution in [Fe/H] is presented in Fig. 6 h. Fig. 6 Histograms of of , , , and [Fe/H] obtained for 402 stars with complete spectroscopic analysis. Results for 11 SB1 are shown in black. 3.6. Uncertainy estimates of the atmospheric parameters The mean intrinsic uncertainties of our determinations, that is, those delivered by TGVIT, are K, , , and [Fe/H] . Figure 7 shows the intrinsic uncertainties of these three parameters as a function of . No correlation exists between the uncertainties and the obtained parameter values for any of the atmospheric parameters in the wide range of between 4500 K6000 K. The scatter of the uncertainties is uniformly distributed over the whole range of resulting parameters. We note, however, that for stars with below 4500 K or above 6000 K the uncertainties are slightly higher, especially in and [Fe/H]. To test the effect of the shift in EWs between DAOSPEC and ARES measurements presented in Sect. 3.4 , we calculated stellar atmospheric parameters for the same five stars using DAOSPEC and ARES EWs separately. We obtained agreement within 1 intrinsic in all parameters except for the microturbulence velocity, in which the results differ by 23 intrinsic . We therefore assume that