Elemental abundances in late type stars are of interest in several ways: they determine the location of HR diagram and therefore age determination of stars, atmospheric structure in middle and upper photosphere. Especially in the case of chromospherically active late type stars the question arises to what degree is mainly upper photosphere influenced by nearby chromosphere. Analysing S/N 200 and \Delta \lambda / \lambda ~20000 data we found mean metallicity index [M/H} = 0.2 for programme K and M field stars based on analysis of spectra in the region 5500-9000 \AA. We also found the CaI 6162 \AA transition as potentionally surface gravity indicator for K type stars. Given the Chromospheric activity interval 4.4 < logF _{MgII} < 6.6 we did not find any chromospheric activity impact onto photospheric and upper photospheric transitions. With derived metallicity we confirmed Li abundance from our previous paper and thus its dependence on MgII chromospheric activity index. The nature of spectrum of active M type star Gl896 \AA is explained by pure rotation with 14 km/s. As far as lithium-rotation relation concerns the spectrum of Gl517 is rotationally broadened as well, by 12 km/s and the Li abundance is the second highest one in sample of stars. However, there is no link between very high Li abundance ,2.2 dex, in K dwarf star Gl5 and stellar rotation.