  Understanding the atmospheric parameters of stars on the top of the RGB is
essential to reveal the chemical composition of the Milky Way, as they can be
used to probe the farthest parts of our Galaxy. Our goal is to determine the
chemical composition of 21 RGB stars with $T_{\mathrm{eff}}<4200$K selected
from the APOGEE-2 DR17 database using new observations carried out with the
spectrograph mounted on the 1-m telescope of the Hungarian Piszk\'estet\H{o}
Observatory and the SONG spectrograph (R=77000) on the Hertzsprung SONG
telescope in the 4500$-$5800\r{A} wavelength range. This is the first time the
spectrograph (R=18000) on the 1-m telescope at Piszk\'estet\H{o} Observatory
was used to measure the abundances of stars. We created a new LTE spectral
library using MARCS model atmospheres and SYNSPEC by including the line list of
23 molecules to determine atmospheric parameters ($T_{\mathrm{eff}}$, $\log g$,
[Fe/H], [$\alpha$/Fe]) and abundances of Si, Ca, Ti, V, Cr, Mn, and Ni with
FERRE. The resulting parameters were compared to that of APOGEE. We found a
good agreement in general, the average difference is $-$11.2K in
$T_{\mathrm{eff}}$, 0.11dex in $\log g$, 0.10dex in [Fe/H], and $-$0.01dex in
[$\alpha$/Fe]. Our analysis successfully demonstrates the ability of the
spectrograph at Piszk\'estet\H{o} Observatory to reliably measure the abundance
of bright stars.
