Global atmospheric C/O values for directly-imaged (blue) and transiting (purple) planets as a function of semi-major axis (left) and planet mass (right). This plot is reproduced using the data compiled

Maximum predicted emission frequency and radio flux density for known exoplanets (triangle symbols; data from ). The uncertainties on the predictions are estimated to one order of magnitude for the

Cross-correlation signal-to-noise maps of H2O, CO, Fe, and Mg in the atmosphere of WASP-121 b. The dashed vertical and horizontal white lines represent the stellar Vsys (38.12 km s−1, from

Comparison of elemental abundances from the literature and this work (filled circles) for the same stars. The y-axis shows the difference in abundance, literature – this work, plotted against the

Modeled transit spectra of GJ 1214b including haze and graphite scenarios. Planet mass 8.17 M⊕/, radius 2.742 R⊕/, and equilibrium temperature ∼596 K are adopted from R. Cloutier et al.

Artistic illustration of the internal structure of a lava planet in a cold state, showing a day‑side magma ocean overlain by a mineral atmosphere. © Romain Jean-Jacques An international research

The ≈1000 au environment of RW Aur at different wavelengths, as observed by ALMA and JWST. Panel (a): compact dust continuum emission at 1.3 mm wavelength (see Kurtovic et al.