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Carbon and Oxygen in the Spectrum of HR 8799c

Published online by Cambridge University Press:  06 January 2014

Q. M. Konopacky ,
T. S. Barman ,
B. A. Macintosh  and
C. Marois
Q. M. Konopacky
Affiliation:
Dunlap Institute for Astronomy and Astrophysics, University of Toronto Dunlap Fellow
T. S. Barman
Affiliation:
Lowell Observatory
B. A. Macintosh
Affiliation:
Larence Livermore National Laboratory
C. Marois
Affiliation:
National Research Council Canada, Dominion Astrophysical Observatory
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Abstract

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The field of exoplanet spectroscopy has grown tremendously in the last decade. With the discovery of gas giant planets at wide separations from their host stars via direct imaging, it is now possible to obtain exoplanet spectra with unprecedented spectral resolution. We present a medium resolution spectrum of the directly imaged exoplanet HR 8799c. This K-band spectrum was obtained using the integral field spectrograph OSIRIS on the Keck II telescope. Our spectrum shows numerous, well-resolved molecular lines from water and carbon monoxide (CO). There is no clear evidence for methane absorption, in spite of a best fit temperature of ~1100 K. We find a best fit surface gravity log(g) ~ 4.0, consistent with the inferred young age for the system (~30 Myr), and a continuum morphology consistent with previously-inferred dust clouds. Using the water and CO lines, we are able to estimate the C/O ratio for this planet. We find a ratio slightly higher than stellar (~0.65), which provides hints about the planet's formation.

Keywords

planetary systems: formationtechniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 297 - 298
Copyright
Copyright © International Astronomical Union 2013 

References

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