DETECTION OF MOLECULAR ABSORPTION IN THE DAYSIDE OF EXOPLANET 51 PEGASI b? by Brogi, M., Snellen, I. A. G., de Kok, R. J., Albrecht, Simon H., Birkby, J. L., de Mooij, E. J. W.

“…In this paper, we present ground-based high-resolution spectroscopy of 51 Pegasi using CRIRES at the Very Large Telescope. …”
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Oscillations in solar-type stars tidally induced by orbiting planets by Terquem, C, Papaloizou, J, Nelson, R, Lin, D

“…We show that, in the case of 51 Pegasi, this velocity is too small to be observed. …”

Non–adiabatic tidal oscillations induced by a planetary companion by Bunting, A, Papaloizou, J, Terquem, C

“…We discuss the implication of this on the possibility of detecting such tidally excited oscillations, including the prospect of utilising the large horizontal motion for observations of systems such as 51 Pegasi.…”

Doppler cross-correlation spectroscopy as a path to the detection of Earth-like planets by Mayor, Michel

“…Gradually the accuracy of the new generation of spectrographs using cross-correlation is improved from 300 m/s to 0.1 m/s. ...An idea that will contribute in an important way to the discovery of 51 Pegasi b and several hundreds of planetary systems.Will visible or infrared cross-correlation spectrographs today be able to detect rocky planets in the habitable zone associated with their host star?…”
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On the tidal interaction of a solar-type star with an orbiting companion: Excitation of g mode oscillation and orbital evolution by Terquem, C, Papaloizou, J, Nelson, R, Lin, D

“…These calculations are applied to 51 Pegasi. We show that the perturbed velocity induced by the tides at the stellar surface is too small to be observed.…”

Applications of a Gaussian process framework for modelling of high-resolution exoplanet spectra by Meech, A, Aigrain, S, Brogi, M, Birkby, JL

“…We use two archival CRyogenic Infra-Red Echelle Spectrograph (CRIRES)/Very Large Telescope (VLT) data sets as test cases, observations of the hot Jupiters HD 189733 b and 51 Pegasi b, recovering injected signals with average line contrast ratios of ∼4.37 × 10-3 and ∼1.39 × 10-3, and planet radial velocities ΔKp = 1.45 ± 1.53 km s-1 and ΔKp = 0.12 ± 0.12 km s-1 from the injection velocities, respectively. …”