the advancement in enhancing the stability and repeatability of the spectrograph, there is significant progress in the wavelength calibration of the instrument. The RV instruments are often equipped with a variety of calibration sources producing well-known reference lines that can be traced to fundamental laboratory standards. HARPS is one such spectrograph that has achieved a wavelength calibration repeatability of 15 $\textrm{cms}^{-1} $ [@HARPS_repeatability]. In recent years, there is also an advancement in the calibration procedure from the empirical method to physical modeling of the instrument [@model_based]. Several instrument teams have developed improved calibration procedures by incorporating the physical model of the instrument in the wavelength calibration [@FOS; @STIS; @CRIRES; @HESP].

To achieve the desired RV precision in a spectrograph, many of the features mentioned above are incorporated at the design stage itself. Precision in RV measurements is required in many science cases like exoplanet detection, characterization of binary and pulsating stars, analyzing the variability of fundamental constants, exoplanet transit follow- up studies, astro-seismology, etc. Some of these observations require a considerable amount of the telescope time and requires adaptable response time from the telescopes for follow-up observations. In this context, there is a growing demand to utilize the existing spectrographs 