TY - GEN
T1 - Carbon and oxygen in the spectrum of HR 8799c
AU - Konopacky, Q. M.
AU - Barman, T. S.
AU - Macintosh, B. A.
AU - Marois, C.
PY - 2013/6
Y1 - 2013/6
N2 - 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.
AB - 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.
KW - Planetary systems: formation
KW - Techniques: spectroscopic
UR - http://www.scopus.com/inward/record.url?scp=84891850732&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84891850732&partnerID=8YFLogxK
U2 - 10.1017/S1743921313008673
DO - 10.1017/S1743921313008673
M3 - Conference contribution
AN - SCOPUS:84891850732
SN - 9781107045200
T3 - Proceedings of the International Astronomical Union
SP - 297
EP - 298
BT - Exploring the Formation and Evolution of Planetary Systems
PB - Cambridge University Press
ER -