| Abstract : | Since the discovery of the first exoplanet in 1995, the field of exoplanet studies has been rapidly accelerating, with current efforts mainly focused on understanding spectral signatures of exoplanet atmospheres, star-planet interactions, the interaction of the planet with their satellites, and habitability. Our current understanding of exoplanets is severely limited due to limitations of our instrumentation technology, atmospheric dispersion and the interstellar medium. Currently, models play an essential role in bridging this knowledge gap. Models require a lot of theoretical inputs like atomic data, molecular data, temperature, pressure, etc., of the exoplanetary systems. In this context, the past decade has seen an extensive amount of work on Sun-as-a-star studies (refer to Dumusque et al., 2021). Essential data from other Solar System objects can be extrapolated to further our understanding of exoplanetary systems. In this work, we are modifying the feed to the High-Resolution Echelle Spectrograph of the 2.3m Vainu Bappu Telescope (VBT) such that we can feed the disc-integrated flux from the various Solar System objects directly to the spectrograph. One of our major objectives is to create a high-resolution template of the Solar System objects, including faint objects like Uranus and Neptune. The center-to-limb variation of Jupiter can be modelled with much higher accuracy and can also be extrapolated for gas giant exoplanets. Signatures obtained from the Galilean moons of Jupiter, when they are observed together with Jupiter as an integrated source, can put a limit on the detectability of exo-moons. We also expect to take continuous in-transit and out-transit spectra to obtain the velocity signal in high-resolution. |
