Abstract
Abstract We present the distance-calibrated spectral energy distribution (SED) of the d/sdL7 SDSS J14162408+1348263A (J1416A) and an updated SED for SDSS J14162408+1348263B (J1416B). We also present the first retrieval analysis of J1416A using the Brewster retrieval code base and the second retrieval of J1416B. We find that the primary is best fit by a nongray cloud opacity with a power-law wavelength dependence but is indistinguishable between the type of cloud parameterization. J1416B is best fit by a cloud-free model, consistent with the results from Line et al. Most fundamental parameters derived via SEDs and retrievals are consistent within 1σ for both J1416A and J1416B. The exceptions include the radius of J1416A, where the retrieved radius is smaller than the evolutionary model-based radius from the SED for the deck cloud model, and the bolometric luminosity, which is consistent within 2.5σ for both cloud models. The pair’s metallicity and carbon-to-oxygen ratio point toward formation and evolution as a system. By comparing the retrieved alkali abundances while using two opacity models, we are able to evaluate how the opacities behave for the L and T dwarf. Lastly, we find that relatively small changes in composition can drive major observable differences for lower-temperature objects.
Highlights
Brown dwarfs are a class of astronomical objects that straddle the mass boundary between stars and planets with masses 75 MJup (Saumon et al 1996; Chabrier & Baraffe 1997) and effective temperatures of 250–3000 K, corresponding to late-type M, L, T, or Y spectral types (Burgasser et al 2002; Kirkpatrick 2005; Cushing et al 2011)
We present the first retrieval of J1416A and the second retrieval of J1416B
J1416A is best parameterized by a power-law deck cloud model; it is indistinguishable from a power-law slab cloud model, while J1416B is best fit by a cloud-free model, agreeing with previous results from Line et al (2017)
Summary
Brown dwarfs are a class of astronomical objects that straddle the mass boundary between stars and planets with masses 75 MJup (Saumon et al 1996; Chabrier & Baraffe 1997) and effective temperatures of 250–3000 K, corresponding to late-type M, L, T, or Y spectral types (Burgasser et al 2002; Kirkpatrick 2005; Cushing et al 2011). Field-age brown dwarfs anchor the spectral type scheme; low-gravity, low-metallicity, and color outliers expand the standard scheme. Low-metallicity sources, known as subdwarfs, have unusually blue near-infrared (NIR) J − K colors (Burgasser et al 2003, 2009) compared with equivalent field sources.
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