Limits on the 2.2-μm contrast ratio of the close-orbiting planet HD 189733b

J. R. Barnes, Travis S Barman, L. Prato, D. Segransan, H. R A Jones, C. J. Leigh, A. Collier Cameron, D. J. Pinfield

Research output: Contribution to journalArticle

26 Citations (Scopus)

Abstract

We obtained 238 spectra of the close-orbiting extrasolar giant planet HD 189733b with resolution R ∼ 15 000 during one night of observations with the Near-Infrared High-Resolution Spectrograph (NIRSPEC), at the Keck II Telescope. We have searched for planetary absorption signatures in the 2.0-2.4 μm region where H2O and CO are expected to be the dominant atmospheric opacities. We employ a phase-dependent orbital model and tomographic techniques to search for the planetary absorption signatures in the combined stellar and planetary spectra. Because potential absorption signatures are hidden in the noise of each single exposure, we use a model list of lines to apply a spectral deconvolution. The resulting mean profile possesses a signal-to-noise ratio (S/N) that is 20 times greater than that found in individual lines. Our spectral time series thus yields spectral signatures with a mean S/N = 2720. We are unable to detect a planetary signature at a contrast ratio of log 10(Fp/F*) = -3.40, with 63.8 per cent confidence. Our findings are not consistent with model predictions which nevertheless give a good fit to mid-infrared observations of HD 189733b. The 1σ result is a factor of 1.7 times less than the predicted 2.185-μm planet/star flux ratio of log10(Fp/F*) ∼ -3.16.

Original languageEnglish (US)
Pages (from-to)473-480
Number of pages8
JournalMonthly Notices of the Royal Astronomical Society
Volume382
Issue number1
DOIs
StatePublished - Nov 2007
Externally publishedYes

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planets
planet
signatures
deconvolution
stellar spectra
signal-to-noise ratio
spectral signatures
near infrared
opacity
night
lists
time series
spectrographs
confidence
signal to noise ratios
telescopes
prediction
stars
orbitals
high resolution

Keywords

  • Line: profiles
  • Methods: data analysis
  • Planetary systems
  • Stars: individual: HD 189733
  • Stars: late-type
  • Techniques: spectroscopic

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Limits on the 2.2-μm contrast ratio of the close-orbiting planet HD 189733b. / Barnes, J. R.; Barman, Travis S; Prato, L.; Segransan, D.; Jones, H. R A; Leigh, C. J.; Collier Cameron, A.; Pinfield, D. J.

In: Monthly Notices of the Royal Astronomical Society, Vol. 382, No. 1, 11.2007, p. 473-480.

Research output: Contribution to journalArticle

Barnes, JR, Barman, TS, Prato, L, Segransan, D, Jones, HRA, Leigh, CJ, Collier Cameron, A & Pinfield, DJ 2007, 'Limits on the 2.2-μm contrast ratio of the close-orbiting planet HD 189733b', Monthly Notices of the Royal Astronomical Society, vol. 382, no. 1, pp. 473-480. https://doi.org/10.1111/j.1365-2966.2007.12394.x
Barnes, J. R. ; Barman, Travis S ; Prato, L. ; Segransan, D. ; Jones, H. R A ; Leigh, C. J. ; Collier Cameron, A. ; Pinfield, D. J. / Limits on the 2.2-μm contrast ratio of the close-orbiting planet HD 189733b. In: Monthly Notices of the Royal Astronomical Society. 2007 ; Vol. 382, No. 1. pp. 473-480.
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AU - Collier Cameron, A.

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AB - We obtained 238 spectra of the close-orbiting extrasolar giant planet HD 189733b with resolution R ∼ 15 000 during one night of observations with the Near-Infrared High-Resolution Spectrograph (NIRSPEC), at the Keck II Telescope. We have searched for planetary absorption signatures in the 2.0-2.4 μm region where H2O and CO are expected to be the dominant atmospheric opacities. We employ a phase-dependent orbital model and tomographic techniques to search for the planetary absorption signatures in the combined stellar and planetary spectra. Because potential absorption signatures are hidden in the noise of each single exposure, we use a model list of lines to apply a spectral deconvolution. The resulting mean profile possesses a signal-to-noise ratio (S/N) that is 20 times greater than that found in individual lines. Our spectral time series thus yields spectral signatures with a mean S/N = 2720. We are unable to detect a planetary signature at a contrast ratio of log 10(Fp/F*) = -3.40, with 63.8 per cent confidence. Our findings are not consistent with model predictions which nevertheless give a good fit to mid-infrared observations of HD 189733b. The 1σ result is a factor of 1.7 times less than the predicted 2.185-μm planet/star flux ratio of log10(Fp/F*) ∼ -3.16.

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