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| Paper: |
Infrared Transit Spectroscopy of HD 209458b |
| Volume: |
294, Scientific Frontiers in Research on Extrasolar Planets |
| Page: |
471 |
| Authors: |
Harrington, J.; Deming, D.; Goukenleuque, C.; Matthews, K.; Richardson, L. J.; Steyert, D.; Wiedemann, G.; Zeehandelaar, D. |
| Abstract: |
We measure spectra during transits of planet HD 209458b in front of its star to determine its composition and temperature. Transits should modulate the stellar spectrum because tangent rays of different wavelengths become extinct at different levels in the extrasolar planet atmosphere, changing the occulting area. S/N calculations show that ground-based spectroscopy can measure or place useful limits on the atmospheric abundances of water, methane, and carbon monoxide. Carbon forms predominantly methane below 1400 K and carbon monoxide if hotter. Since the equilibrium temperature is about 1400 K, detecting methane and/or carbon monoxide would constrain atmospheric temperatures. We have observed on 12 transit and 4 non-transit nights from Palomar, Keck, VLT, and IRTF. The expected modulation of the stellar spectrum is model-dependent. Since the effect is subtle compared to the noise in the data, we correlate model vs. observed spectra and average the correlations to test whether the data support a given model. We are developing a tangent-geometry radiative-transfer model to predict the spectrum of a given planetary model, and we are measuring water, methane, and carbon monoxide in the laboratory at 1300 K, with pressure-broadening by molecular hydrogen, to make our model spectra realistic at these elevated temperatures. We solicit participation by those who wish to test their planetary models. |
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