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The Goldilocks Problem for Detecting Water in Terrestrial Planets: Constraining Water Abundances in the Mid-infrared with LIFE

  • Authors: S. Rugheimer, E. Alei, B.S. Konrad, B. Taysum, J. L. Grenfell, T. Lichtenberg, D. Kitzmann, F. van der Tak, S.P. Quanz

S. Rugheimer et al 2026 The Astrophysical Journal 1003 .

  • Provider: AAS Journals

Caption: Figure 3.

Mid-IR input spectra at R=100 calculated by petitRADTRANS as input to LIFESIM for different H2O abundances and H2O profiles. The top panel shows three spectra for a vertically constant profile with surface H2O concentrations corresponding to a water-rich case of 1 bar (dark blue solid line), an Earth-like surface water case of 10−2 bar (purple line), and a water-poor Mars-like case of 10−6 bar (red line). The bottom panel shows a comparison between spectra with different water altitude profiles with the same surface water concentration of 1 bar for the altitude-invariant profile (dark blue), the Earth-like profile (blue), and the diffusion and photochemistry profile (light blue).

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