Near-ir Spectra Of The Planets HR8799b And HR8799c

Details Near-ir Spectra Of The Planets HR8799b And HR8799c Near-ir Spectra Of The Planets HR8799b And HR8799c

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21741804m&link_type=abstract

American Astronomical Society, AAS Meeting #217, #418.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

Physics

Optics

Scientific paper

The directly-imaged HR8799 system represents a unique window into exoplanet formation and evolution with three massive coeval planets accesible to characterization using adaptive optics on modern telescopes. One such window is spectroscopic characterization. We have used the OSIRIS near-IR integral field spectrograph on the W.M. Keck telescope to study the two outermost planets. Taking advantage of the 3-dimensional OSIRIS data product we can separate artifact speckles noise from the true planetary signal. H and K band spectra of these two planets, among the coldest planetary bodies ever characterized, significantly diverge from observed brown dwarfs and older models of planetary atmospheres, with evidence for thick clouds and an absence of strong methane absorption in spite of their low (<1100K) effective temperatures.
Portions of this work prepared by LLNL under Contract DE-AC52-07NA27344 and under support from the NASA Origins program.

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