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tokens: 2 ), are shown in Appendix A . Table 2. Adopted stellar parameters for HD 199178. Notes. (a) In case of no reference, a new parameter value was derived/adopted for this study. In general, a minimum number of ∼10 evenly distributed rotational phases is considered optimal for a fully reliable Doppler image. However, Hackman et al. (2011) demonstrated, that some useful information can be retrieved with a much more limited phase coverage. Therefore, we calculated Doppler images for all sets with n φ ≥ 4. 3. Spectral and stellar parameters The spectral parameters were obtained from the Vienna Atomic Line Database ( Piskunov et al. 1995 ; Ryabchikova et al. 2015 ). Some adjustments were made in the g f -values in order to get a satisfactory fit for all spectral regions. This is a standard procedure in Doppler imaging since the spectra of real stars always show some deviations from calculations based on LTE-models. As we did not intend to derive exact element abundances, it is safe to correct for all discrepancies between the model and the real star by adjusting the g f -values. Furthermore, to the first order all photospheric absorption lines will follow the same behaviour (i.e. a cool spot will cause a “bump” in the spectral line). The adopted parameters for the strongest lines are listed in Table 3 . The largest adjustment was for the line Ca I 6439.075 Å, were VALD listed lg( g f )=0.370 and we adopted the value 0.450. A total number of 917 lines were included in the line synthesis of the seven wavelength regions. Most of these were molecular lines. For the unspotted surface a smaller number, i.e. only the atomic lines, would have been sufficient. For the cool spots molecular lines, in particular TiO-bands, are important. The local line profiles were calculated using the code LOCPRF7 developed at the University of Uppsala. Recent changes in the code include a molecular equilibrium solver ( Piskunov Valenti 2017 ). Table 3. Wavelengths, lower excitation potentials, and adopted lg( g f )-values for the strongest lines. HD 199178 is a rapidly rotating late-type star, which was classified as G 5 III – IV by Herbig (1958) . Strassmeier et al. (1999) calculated its luminosity and mass to be 11 L ⊙ and 1.65 M ⊙ . Hackman et al. (2001) estimated its radius to be ∼5 R ⊙ and adopted the rotation velocity v sin i = 72 km s −1 , inclination angle i = 60°, and gravity lg( g )=3.5. With such a high rotation velocity, the macroturbulence is hard to determine, but in any case should not strongly influence Doppler imaging. In this study we used a radial-tangential macroturbulence of ζ RT = 5.0 km s −1 . We adopted an effective temperature T eff = 5300 K for the unspotted surface as a starting point. The microturbulence was determined by comparing the synthetic spectrum of an unspotted surface to the observations. This yielded ξ = 1.7 km s −1 . Jetsu et al. (1999) and Panov Dimitrov (2007) concluded, that the photometric light curve cannot be modelled using a