Near infrared spectroscopic search for the close orbiting planet HD 75289b

Abstract

We present a search for the near infrared spectroscopic signature of the close orbiting extrasolar giant planet HD 75289b. We obtained ~230 spectra in the wavelength range 2.18 - 2.19 microns using the Phoenix spectrograph at Gemini South. By considering the direct spectrum, derived from irradiated model atmospheres, we search for the absorption profile signature present in the combined star and planet light. Since the planetary spectrum is separated from the stellar spectrum at most phases, we apply a phase dependent orbital model and tomographic techniques to search for absorption signatures. Because the absorption signature lies buried in the noise of a single exposure we apply a multiline deconvolution to the spectral lines available in order to boost the effective S/N ratio of the data. The wavelength coverage of 80 angstroms is expected to contain ~100 planetary lines, enabling a mean line with S/N ratio of ~800 to be achieved after deconvolution. We are nevertheless unable to detect the presence of the planet in the data and carry out further simulations to show that broader wavelength coverage should enable a planet like HD 75289b to be detected with 99.9 per cent (4 sigma) confidence. We investigate the sensitivity of our method and estimate detection tolerances for mismatches between observed and model planetary atmospheres.

References in corpus (5)

• Detection of Thermal Emission from an Extrasolar Planet
• The phase-dependent Infrared brightness of the extrasolar planet upsilon Andromedae b
• Strong Infrared Emission from the Extrasolar Planet HD189733b
• A Spectrum of an Extrasolar Planet
• Measurement of the Spin-Orbit Alignment in the Exoplanetary System HD 189733

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• Limits on the 2.2 microns contrast ratio of the close orbiting planet HD 189733b
• HD 75289Ab revisited - Searching for starlight reflected from a hot Jupiter
• HD 179949b: A Close Orbiting Extrasolar Giant Planet with a stratosphere?
• On the Effects of Planetary Oblateness on Exoplanet Studies