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Measuring the D/H Ratios of Exoplanets and Brown Dwarfs

  • Authors: Caroline V. Morley, Andrew J. Skemer, Brittany E. Miles, Michael R. Line, Eric D. Lopez, Matteo Brogi, Richard S. Freedman, and Mark S. Marley

2019 The Astrophysical Journal Letters 882 L29.

  • Provider: AAS Journals

Caption: Figure 4.

Detectability of deuterated species vs. temperature. The top and middle panels show the signal to noise needed for a 10σ detection of CH3D and HDO, respectively, assuming a spectrum from 3 to 5 μm with R ∼ 2700. The hatched regions show the S/N predicted per spectral element in the region of the spectrum with CH3D or HDO features in a 2.5 hr observation with JWST. CH3D is detectable at high significance for objects cooler than 800 K; HDO is never detectable at high significance in 2.5 hr. The bottom panel shows a simulated brown dwarf population from Saumon & Marley (2008); it uses a power-law initial mass function (IMF) index α = 1, masses between 0.006 and 0.1 MSun, and uniform age distribution between 0 and 10 Gyr.

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