Feasibility Study of Detection and Characterization of young Planets with High-resolution Spectra

Protoplanetary disks are the first stage of planet formation and evolution, which can embed young planets and embryos. Studying both the protoplanetary disks and the forming planets inside can therefore provide strong constraints into initial conditions for planet formation such as gas density and dust distribution, as well as probing the origin of planetary atmospheres. As a crucial aspect to understand the formation scenarios and early evolution processes, it is important to observe the atmospheric emission from young planets with state of art high-resolution spectrometers in order to measure several physical quantities such as temperature profiles, spin rate, chemical abundance, which help to constrain the initial conditions of planet formation and early evolution. It is always challenging to acquire spectrum from exoplanets. In particular, they are strongly contaminated by the emission from host star and strong turbulence of the Earth’s atmosphere, which makes it difficult to precisely observe the spectral features from exoplanets’ atmosphere. High-dispersion Spectroscopy (HDS) with Adaptive Optics is a potential technique to overcome this difficulty but rarely applied. It is essential to make pre-research with simulation to understand the capability of HDS instruments on the emission of very young planets. Therefore, the objective of this project is to assess the feasibility of using the next-generation high-dispersion spectrometer CRIRES+ on VLT to study atmosphere of young planets undergoing formation processes, and help to optimize the strategies for future observations. Overall, our results support that the spectrum of the planet HD 169142b should be detectable with the observing techniques studied in this thesis work.