model is used for prediction and correction of the positional variations of the components. The effect of the perturbation of optical components on the obtained RV was earlier demonstrated in the works of Gibson & Wishnow (2016).[@synthetic_spectrum]. In the view of increasing the computational flexibility, we analyzed the RV sensitivities of the spectrograph and modeling of observations in Zemax using Python for input and output operations. Invoking the capabilities of Zemax and utilizing it for the spectrograph sensitivity analysis using other software has been demonstrated in previous studies [@zemaxmatlab; @HERMES]. The known limitations due to the design and usage of the spectrograph for precision RV studies are discussed in Section \[sect:limitations\]. The approach we have taken address these limitations are presented in Section \[sect:need\]. The sensitivity analysis, procedure, and estimation of RV uncertainties are presented in Section \[sect:sensitivity\]. Matching of the Zemax model with observations is described in Section \[sect:model\]. Inferences and conclusions of this study are discussed in Section \[sect:conclusion\].

Spectrograph design limitations for precision RV studies {#sect:limitations}
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Spectrograph Description
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The stellar light from the f/3 primary mirror of the telescope is picked up using 100 $\mu$m multi-mode optical fiber. The exit of the fiber is fed 