Measuring Carbon and Oxygen Abundances in Hot Jupiter Atmospheres with High-Resolution Spectroscopy
Jayne Birkby NASA Sagan Fellow, Harvard-Smithsonian Center for Astrophysics Remco de Kok, Matteo Brogi, Ignas Snellen, Henriette Schwarz (Leiden Observatory) Planet formation mechanisms operate on different timescales at different locations in disk
HR 8799 (Marois et al. (2010)
Core accretion or gravitational instability alone cannot reproduce system and significant migration is unlikely C/O ratio could reveal where and how a planet formed in its protoplanetary disk
Öberg et al. (2011)
Measure the relative abundances: CO, H2O, CO2, CH4 Detect molecules in exoplanet atmospheres using ground-based High Dispersion Spectroscopy (HDS)
A CRIRES/VLT survey of hot Jupiter atmospheres
• CRIRES: CRyogenic high-resolution InfraRed Echelle Spectrograph • R=100,000 • 155hrs • 5 brightest host stars visible from Paranal, Chile:
HD 209458 b, HD 189733 b, 51 Peg b, � Boo b, HD 179499 b Detecting molecules with high dispersion spectroscopy HDS detects the radial velocity shift of the planetary spectrum
0.8 Blue-shifted Toy model of CO lines Dayside Secondary eclipse
0.6
Nightside Transit Secondary eclipse
Red-shifted 0.4 Phase KP Model H2O lines
5 0.2
0.0 Transit
Model CO lines Relativeline depth10 x Model CO lines
-0.2 2.309 2.310 2.311 2.312 2.313 Wavelength / μm H2O absorption in the dayside atmosphere of the transiting hot Jupiter HD 189733 b
Birkby et al. 2013 HDS also reveals complex molecules in non-transiting planets
Mayor & Queloz (1995)
KS
(km/s)
p K
H2O in 51 Peg b 51 Peg
79.6° < i < 82.2°
MP = 0.46MJ ± 0.02MJ Birkby et al. (in prep)
See also LockwoodNon-transiting et al. (2014) detection planet of H2O in =non-transiting spectroscopic � Boo b with Keck/NIRSPEC binary (R~25,000) Simple CO molecule routinely detected in hot Jupiter atmospheres with HDS