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• W4384283325 abstract "Abstract We present the first JWST spectral energy distribution of a Y dwarf. This spectral energy distribution of the Y0 dwarf WISE J035934.06−540154.6 consists of low-resolution ( λ /Δ λ ∼100) spectroscopy from 1–12 μ m and three photometric points at 15, 18, and 21 μ m. The spectrum exhibits numerous fundamental, overtone, and combination rotational–vibrational bands of H 2 O, CH 4 , CO, CO 2 , and NH 3 , including the previously unidentified ν 3 band of NH 3 at 3 μ m. Using a Rayleigh–Jeans tail to account for the flux emerging at wavelengths greater than 21 μ m, we measure a bolometric luminosity of 1.523 ± 0.090 × 10 20 W. We determine a semiempirical effective temperature estimate of <?CDATA ${467}_{-18}^{+16}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:msubsup> <mml:mrow> <mml:mn>467</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>18</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>16</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> K using the bolometric luminosity and evolutionary models to estimate a radius. Finally, we compare the spectrum and photometry to a grid of atmospheric models and find reasonably good agreement with a model having T eff = 450 K, log g = 3.25 [cm s −2 ], and [M/H] = −0.3. However, the low surface gravity implies an extremely low mass of 1 M Jup and a very young age of 20 Myr, the latter of which is inconsistent with simulations of volume-limited samples of cool brown dwarfs." @default.
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• W4384283325 date "2023-07-01" @default.
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• W4384283325 title "The First JWST Spectral Energy Distribution of a Y Dwarf" @default.
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• W4384283325 doi "https://doi.org/10.3847/2041-8213/ace32c" @default.
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