  The light emitted from the stellar photosphere serves as a unique signature
for the nature of stars. The behaviour of these stellar lines depend upon the
surface temperature, mass, evolutionary status and chemical composition of the
star. With the advent of high-resolution spectrographs coupled with medium to
large aperture telescopes around the globe, there is plenty of high-resolution
and high signal-to-noise ratio data available to the astronomy community. Apart
from radial velocity (RV) studies, such data offer us the unique opportunity to
study chemical composition and atmospheric properties of the star. The
procedure used to derive these parameters must be automated and well adaptable
to data available from any high-resolution spectrograph. We hereby present an
IDL code, PARAS SPEC, which was primary designed to handle high-resolution
spectroscopy data from PARAS spectrograph coupled with the 1.2~m telescope at
Mt. Abu, India. This code is designed to adapt with data from other
spectrographs as well. The code PARAS SPEC estimates the stellar atmospheric
parameters from the analysis of stellar spectra based on two primary methods,
synthetic spectral fitting and equivalent width method. Synthetic spectral
fitting method involves fitting of the observed spectrum with different
synthetic spectra for a set of stellar parameters. The second method is based
on equivalent widths (EWs) that are used to derive abundances for a set of Fe~I
and Fe~II lines from the observed spectra. The detailed methodology used to
design this code and comparison of the results from literature values are
presented in this paper.
