The Water Abundance of the Directly Imaged Substellar Companion k And b Retrieved from a Near Infrared Spectrum
Kamen O. Todorov, Michael R. Line, Jaime E. Pineda, Michael R. Meyer, Sascha P. Quanz, Sasha Hinkley, Jonathan J. Fortney
(Submitted on 1 Apr 2015)
Recently, spectral retrieval has proven to be a powerful tool for constraining the physical properties and atmospheric compositions of extrasolar planet atmospheres from observed spectra, primarily for transiting objects but also increasingly for directly imaged planets and brown dwarfs. Despite its strengths, this approach has been applied to only about a dozen targets. Determining the abundances of the main carbon and oxygen-bearing compounds in a planetary atmosphere can lead to the C/O ratio of the object, which is crucial in understanding its formation and migration history.
We present a retrieval analysis on the published near-infrared spectrum of {\kappa} And b, a directly imaged substellar companion to a young B9 star. We fit the emission spectrum model utilizing a Markov Chain Monte Carlo algorithm. We estimate the abundance of water vapor, and its uncertainty, in the atmosphere of the object. We also place upper limits on the abundances of carbon dioxide and methane and constrain the pressure-temperature profile of the atmosphere. We compare our results to studies that have applied model retrieval on multiband photometry and emission spectroscopy of hot Jupiters (extrasolar giant planets with orbital periods of several days) and the directly imaged giant planet HR 8799b. We find that the water abundances of the hot Jupiters and the two directly imaged planets inhabit overlapping regions of parameter space and that their P-T profiles are qualitatively similar, despite the wide range of effective temperatures and incident stellar fluxes for these objects.
Comments:9 pages, 7 figures, 3 tables. ApJ, submitted
Subjects:Earth and Planetary Astrophysics (astro-ph.EP)
Cite as:arXiv:1504.00217 [astro-ph.EP] (or arXiv:1504.00217v1 [astro-ph.EP] for this version)
Submission history
From: Kamen Todorov
[v1] Wed, 1 Apr 2015 13:14:43 GMT (52kb)
