An Approach for Retrieving Temperatures and Abundances in Brown Dwarf   Atmospheres
  Brown dwarf spectra contain a wealth of information about their molecular abundances, temperature structure, and gravity. We present a new data driven retrieval approach, previously used in planetary atmosphere studies, to extract the molecular abundances and temperature structure from brown dwarf spectra. The feasibility of the approach is first demonstrated on a synthetic brown dwarf spectrum. Given typical spectral resolutions, wavelength coverage, and noise properties precisions of tens of percent can be obtained for the molecular abundances and 10s-100s K on the temperature profile. The technique is then applied to the well studied brown dwarf, Gl 570D. From this spectral retrieval the spectroscopic radius is constrained to be 0.75 - 0.83 $R_{\mathrm{J}}$, $\log(g)$ to be 5.13 - 5.46 and $T_{\mathrm{eff}}$ to be between 804 and 849 K. Estimates for the range of abundances and allowed temperature profiles are also derived. The results from our retrieval approach are in agreement with the self-consistent grid modeling results of Saumon et al (2006). This new approach will allow us to address issues of compositional differences between brown dwarfs and possibly their formation environments, disequilibrium chemistry, missing physics in current grid modeling approaches as well as a many other issues. 
Michael R. Line, Jonathan J. Fortney, Mark S. Marley, Satoko Sorahana
astro-ph.SR astro-ph.EP