Spectral Analysis Code: PARAS SPEC

TL;DR

PARAS SPEC is an IDL-based automated tool for analyzing high-resolution stellar spectra to determine atmospheric parameters using synthetic spectral fitting and equivalent width methods, adaptable to various spectrographs.

Contribution

The paper introduces a versatile IDL code, PARAS SPEC, for automated stellar parameter estimation from high-resolution spectra, compatible with multiple spectrographs.

Findings

Successfully estimates stellar parameters from spectra.

Provides consistent results with literature values.

Applicable to data from different high-resolution spectrographs.

Abstract

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.