Detection of Exoplanet Thermal Emission with Future High-Resolution Spectrometers

Details Detection of Exoplanet Thermal Emission with Future High-Resolution Spectrometers Detection of Exoplanet Thermal Emission with Future High-Resolution Spectrometers

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21943208g&link_type=abstract

American Astronomical Society, AAS Meeting #219, #432.08

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Detection of planetary atmospheres is an important step in constraining models of their formation as well as current state. All atmospheres spectroscopically detected to date have been those of transiting exoplanets, either by observing the transmission spectrum during transit or the thermal emission out of transit. The latter has so far mostly been done with low to medium resolution spectroscopy from space using Spitzer or HST. With high-resolution spectroscopy of the planet's thermal emission, the radial velocity of a planet can be determined. Combining this with the stellar radial velocity can give the true mass of the planet, even for non-transiting planets. Since most planets are not transiting, this technique could be used to improve statistics on the true mass distribution of exoplanets and be used to improve planetary formation models. Here we present simulated data taken using the future near-IR instruments IGRINS and GMTNIRS, and show their ability to detect planetary atmospheres and determine their inclination and true mass. We develop a technique that can effectively remove the stellar spectrum from SNR > 200 observations of a system, by utilizing the motion of the planetary lines relative to the stellar lines at different phases of the planet's orbit. We find that these two instruments, and any other future instruments like them, should be able to detect a planetary atmosphere and measure the true mass of a planet. We acknowledge the University of Texas at Austin for support in this project.

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