High-resolution spectroscopic search for the thermal emission of the extrasolar planet HD 217107 b

Abstract

We analyzed the combined near-infrared spectrum of a star-planet system with thermal emission atmospheric models, based on the composition and physical parameters of the system. The main objective of this work is to obtain the inclination of the orbit, the mass of the exoplanet, and the planet-to-star flux ratio. We present the results of our routines on the planetary system HD 217107, which was observed with the high-resolution spectrograph Phoenix at 2.14 microns. We revisited and tuned a correlation method to directly search for the high-resolution signature of a known non-transiting extrasolar planet. We could not detect the planet with our current data, but we present sensitivity estimates of our method and the respective constraints on the planetary parameters. With a confidence level of 3--$\sigma$ we constrain the HD 217107 b planet-to-star flux ratio to be less than $5\times 10^{-3}$. We also carried out simulations on other planet candidates to assess the detectability limit of atmospheric water on realistically simulated data sets for this instrument, and we outline an optimized observational and selection strategy to increase future probabilities of success by considering the optimal observing conditions and the most suitable candidates.

7 pages, 6 figures. Accepted for publication in Astronomy & Astrophysics

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Cited by in corpus (4)

• Weighing The Non-Transiting Hot Jupiter Tau BOO b
• Detectability of Exoplanet Periastron Passage in the Infra-Red
• The HD 217107 Planetary System: Twenty Years of Radial Velocity Measurements
• Estimation of Exoplanetary Planet-to-Star Radius Ratio with Homomorphic Processing