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tokens: detail. As mentioned before, we identified two mild-Am stars, HD 33204 and HD 46304. We show abundance distributions of these stars in Fig. 10 . A typical Am star exhibits overabundances of iron-peak elements and some heavy elements (Zn, Sr, Zr and Ba), but Ca and Sc abundances of these stars are underabundant (Gray Corbally 2009 ). As can be seen in Fig. 10 , the mild-Am stars in our study have nearly solar abundances of Ca and Sc elements. Only HD 33204 shows overabundances in some heavy elements typical for Am star. In the case of HD 46304, most of lines are blended due to high rotation velocity of the star. These blended lines cause difficulties in abundance calculations. The abundance differences between HD 46304 and a typical Am star can be caused by this effect. In the spectral classification process some stars were defined as metal-poor, mostly taking into account Mg, Mn and Fe lines (see Table 2 ). For these stars, the average abundance of Mg (7.57 dex) was found to be close to the solar abundance. However, the average abundances of Mn (5.13 dex) and Fe (7.27 dex) are slightly lower than the solar abundances. For some of our targets (HD 26298, HD 33204, HD 106103, HD 110379, and HD 126516) chemical abundances were already obtained before the present study. We compared our atmospheric parameters and abundance results with the literature values. Abundances of HD 33204 and HD 10613 were derived by Varenne Monier ( 1999 ) and Fossati et al. ( 2008 ), respectively. In their work, similar methods for abundance analysis were used but different atomic data bases were adopted. For HD 33204 higher abundances of Sc, Mg and Y were obtained in the present study. Our result is consistent with the Am: type peculiarity of this star. For HD 106103 only the Y abundance is different. Abundances of HD 26298, HD 110379 and HD 126516 were derived by Bruntt et al. ( 2008 ) using the equivalent width method and the different atomic data base. In the case of these three stars, the marked differences were detected only for V and Ba abundances. Figure 10. Chemical abundances of Am: stars compared with the solar values (Asplund et al. 2009 ). HD 33204 is represented by stars and HD 46304 by triangles. Additionally, we checked the possible correlations of the element abundances with atmospheric parameters, i.e. T eff , log g and ξ. Similar as in Niemczura et al. ( 2015 ), no correlations were found. Moreover, the element abundances do not depend on v sin i . The same result was found by Fossati et al. ( 2008 ). However, Takeda et al. ( 2008 ) reported negative correlations between v sin i and C, O and Ca elements. Finally, we checked the relations between abundances of iron and other elements. Strong positive correlations were found for Mg, Si, Ca, Sc, Ti Cr, Ni, Y and Ba. Similar correlations between Fe abundances and iron-peak elements were found by Niemczura et al. ( 2015 ). On the other hand, a negative correlation was obtained between Fe and O abundances. 6