Astrobiology13- Page

Top: Maximum A Posteriori (MAP) model and 2σ credible regions from ExoTR retrievals on the fiducial reduction, overlaid with data binned at ∆λ = 0.05 µm. Also shown are the

Experimental set-up for Trial A within the southwestern section of the FLIES lab greenhouse. Pea plants were randomly arranged in eight 2 × 3 arrays atop a rolling mesh-top bench.

Top: Same as Figure 3, but for TIC 80127634, which is a G star that exhibits high amplitude variations that is used for the water loss simulations. Left: Orbit architecture

The three-layer diagram of the outcome of our model. The inner layer is the H2 layer cooled by H+3 , where the highest-energy photons are deposited. The neutral atomic hydrogen

Examples of interior scenarios consistent with the bulk properties of TOI-270 d, spanning different atmospheric temperature structures and water mass fractions. The thickness of the layers are not to scale.

The illustration shows a cutaway revealing the interior of early Earth with a hot, melted layer above the boundary between the core and mantle. Scientists think some material from the

Concentrations are shown in µg/kg. Black circles represent seawater sampling locations; red stars denote the shoreline position of microbialite sampling transects (coordinates listed in Supplementary Table 3). Black lines represent

Hydrothermal deposits on Mars. (A) This image was acquired by the Mars Reconnaissance Orbiter’s High Resolution Imaging Science Experiment camera on November 22, 2006. It shows a bright plateau of

Flux with central regions masked (10 µm; upper row), and corresponding asymmetric flux relative to the planet flux Fp (lower row), following the format of Fig. 6. This masking emphasizes

Hertzsprung–Russell diagram comparing the BGM-simulated stellar population (background) with the subset of Gaia sources (superimposed in red) for which reliable effective temperatures and absolute magnitudes are available. The Gaia sample