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In the last decade ground based high resolution Doppler spectroscopy (HRS)has detected numerous species in transiting and non-transiting hot Jupiters,and is ideally placed for atmospheric characterisation of warm Neptunes andsuper Earths. Many of these cooler and smaller exoplanets have shown cloudyatmospheres from low resolution near infrared observations, making constraintson chemical species difficult. We investigate how HRS can improve on thesegiven its sensitivity to spectral line cores which probe higher altitudes abovethe clouds. We model transmission spectra for the warm Neptune GJ~3470~b anddetermine the detectability of H$_2$O with the CARMENES, GIANO and SPIRouspectrographs. We also model a grid of spectra for another warm Neptune,GJ~436~b, over a range of cloud-top pressure and H$_2$O abundance. We showH$_2$O is detectable for both planets with modest observational time and thatthe high H$_2$O abundance-high cloud deck degeneracy is broken with HRS.However, meaningful constraints on abundance and cloud-top pressure are onlypossible in the high metallicity scenario. We also show that detections ofCH$_4$ and NH$_3$ are possible from cloudy models of GJ~436~b. Lastly, we showhow the presence of the Earth's transmission spectrum hinders the detection ofH$_2$O for the most cloudy scenarios given that telluric absorption overlapswith the strongest H$_2$O features. The constraints possible with HRS on themolecular species can be used for compositional analysis and to study thechemical diversity of such planets in the future.

Seeing above the Clouds with High Resolution Spectroscopy