  The scientific community's interest on the stellar parameters of M dwarfs has
been increasing over the last few years, with potential applications ranging
from galactic characterization to exoplanet detection. The main motivation for
this work is to develop an alternative and objective method to derive stellar
parameters for M dwarfs using the H-band spectra provided by the Apache Point
Observatory Galactic Evolution Experiment (APOGEE). Synthetic spectra generated
with \textit{iSpec}, \textit{Turbospectrum}, \textit{MARCS} models atmospheres
and a custom made line list including over 1 000 000 water lines, are compared
to APOGEE observations, and parameters are determined through $\chi^2$
minimization. Spectroscopic parameters ($T_\mathrm{eff}$, $[M/H]$, $\log g$,
$v_{mic}$) are presented for a sample of 313 M dwarfs, obtained from their
APOGEE H-band spectra. The generated synthetic spectra reproduce observed
spectra to a high accuracy level. The impact of the spectra normalization on
the results are analyzed as well. Our output parameters are compared with the
ones obtained with APOGEE Stellar Parameter and Chemical Abundances Pipeline
(ASPCAP) for the same stellar spectrum, and we find that the values agree
within the expected uncertainties. Comparisons with other previous
near-infrared and optical literature are also available, with median
differences within our estimated uncertainties found in most cases. Possible
reasons for these differences are explored. The full H-band line list, the line
selection for the synthesis, and the synthesized spectra are available for
download, as are the calculated stellar parameters.
