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tokens: K and log g = 3.55 model atmosphere calculated with different treatments of the hydrogen-line opacity, using the codes DETAIL (solid curve), SynthV_NLTE (dotted curve), and SYNTHMAG (dash-dotted curve). The position of the Ca ii IR triplet lines is marked with triangles. The vertical lines indicate the wavelength range covered by the Gaia spectra. Table 5 summarises the results of calcium abundance determination from different groups of reliable lines, i. e. lines of Ca i , lines of Ca ii in the visible spectrum range, and lines of Ca ii in the IR spectrum range 8912−27, 9890 Å. We also show in Fig. 9 the NLTE and LTE abundance differences between these groups of lines. For each star, NLTE leads to average abundances from lines of Ca ii in the visible and the IR spectrum range consistent within 0.1 dex, while the abundance discrepancy between these groups of lines varies from 0.6 dex down to −0.5 dex in LTE (Fig. 9 , top panel). The exception is 21 Peg, where NLTE leads to better agreement between these two groups of lines compared to LTE, however, a discrepancy of 0.2 dex remains. For HD 160762, the LTE abundance difference is not shown in Fig. 9 , because Ca ii 8912−27, 9890 Å lines are observed in emission and cannot be fitted in LTE. Figure 9. NLTE (filled circles) and LTE (open circles) abundance differences between Ca ii lines in the visible and IR spectral range (top panel) and between Ca i lines and Ca ii lines in the visible spectral range (bottom panel) in the investigated stars. Fig. 9 , bottom panel, shows the NLTE and LTE abundance differences between lines of Ca i and Ca ii in the visible spectrum range. For the majority of the investigated stars, an abundance difference = log A(Ca i )–log A(Ca ii , vis) does not exceed 0.1 dex in absolute value, independent of NLTE or LTE. However, for A-type stars, the absolute abundances from Ca i and Ca ii lines are higher in NLTE compared with LTE. 4.3 Calcium NLTE abundance determination with SME code As it was written in Section 3.1 , we calculated departure coefficients of Ca i and Ca ii levels for a grid of LLmodels atmospheres (Shulyak et al. 2004 ). Earlier, the same calculations were performed for grids of MARCS plane-parallel models (Gustafsson et al. 2008 ). These NLTE data are implemented in the current version of the SME (Spectroscopy Made Easy) package of automatic parameters and abundance determination based on high-resolution stellar spectra (Piskunov Valenti 2017 ). Atmospheric parameters and element abundances in SME are derived by the interpolation inside the grid models. For cool stars (MARCS model grids), the accuracy of authomatic NLTE Ca abundance determinations was tested in the paper by Piskunov et al. ( 2017 , see Figs 1 and 3 of this paper). Here, we tested the automatic method for hotter stars with HD 32115 and HD 72660. For HD 32115, the SME abundances are −5.68±0.07 (Ca i ) and −5.60±0.14 (Ca ii ). For HD 72660, the corresponding values are −5.44±0.13 (Ca i ) and