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Version devBuilt at: 2026-10-16 08:00:47 EDT

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Chromaticity distribution (top) for all white dwarfs within 20 pc of the Sun (points). Our cuts to exclude objects with non-blackbody colours is shown by the grey dashed lines. The correlated colour temperature distribution for the 20 pc sample (excluding three outliers) is shown in the bottom panel, where the colour gradient under the histogram represents the sRGB colour at each given colour temperature, and the panel background is filled with the colour corresponding to the median (#F9F5FF).
Simplified workflow of pyEDITH. Inputs can be provided via command-line configuration files or Python API. Variables are organized into three independent classes (astrophysical scene, observation parameters, observatory configuration) that communicate through a mediator (shaded region). The observatory class is subdivided into telescope, coronagraph, and detector components, typically loaded from standardized HWO files. After validation, the exposure time calculator computes observation times, signal-to-noise ratios, and noise count rates.
Forward models for the coolest five planets in our sample, ordered by increasing equilibrium temperature, showing the chemical abundances (left) in chemical equilibrium (dashed) and full chemical kinetics (full), and the synthetic transmission spectra (right) for the equilibrium (orange) and kinetics (blue) case. For the computation of the Ariel uncertainties we assumed a Tier 2-scenario.
Elfen’s unique orbit enables comprehensive studies of the role that heavy ions play in the solar wind magnetosphere interaction. Left: Not-to-scale cartoon of heavy ions reaching the Earth’s magnetosphere with representative magnetic field lines, and illustrative orbit crossing upstream, magnetosheath, and plasma sheet regions, and the mission logo. An approximate orbit is drawn in green. Middle top and right top: Science themes 1 and 2 are illustrated in the middle and right columns. Middle top shows the large scatter and therefore non one-to-one relationship between detected SWCX exospheric X-ray emissions at approximately 0.25  keV and the solar wind flux, modified from K. D. Kuntz et al. (2015), showing how understanding dayside heavy ion interactions are important. Top right illustrates select natural and man-made competing input and output ion processes on the dayside magnetosphere, adapted from M. Yamauchi et al. (2024). Middle bottom: Schematic of dual-lobe reconnection (DLR) under northward IMF (NBZ) conditions that can allow ions into the nightside plasma sheet, reproduced from S. E. Milan et al. (2025). Bottom right: Competing processes feeding the plasma sheet on the nightside of Earth, which include outflow, diffusion, and KH instabilities on the dusk-side magnetosheath.
Left: Spectrum of comet C/2016 R2 (PanSTARRS), 2018 January 13, 1.22 m Galileo telescope, 300 lines mm^(−1) grating. Detail of the 3800–5200 Å region. Bands of N^+_2 and CO^+ are dominant, while classical CN and carbon-chain molecules are not detected. Right: Trichrome image of comet C/2022 E3 (ZTF) with B, V, and r photometric filters, 2023 February 11, Schmidt telescope, Cima Ekar Observatory (INAF-OAPd). Following calibration with bias, dark, and flat-field corrections, the individual frames were all aligned using the optocentre of the comet as a reference. Colour calibration was made using field stars.
CH4petitRADTRANS line-by-line transit spectrum and corresponding direct and indirect templates. The top panel shows the transit spectrum computed with the radiative-transfer model. The middle panel displays the corresponding direct template, obtained by normalizing the transit radius with a Gaussian filter. The bottom panel shows the indirect template constructed from the strongest absorption features (75 per cent of lines included here). Only lines that fall within the CRIRES+ spectral orders are included in this step, ensuring that the intensity-based ranking reflects the subset of lines actually used in the cross-correlation analysis. The line intensities in the indirect template are expressed in arbitrary units proportional to the transit-radius contrast; only their relative pattern is used in the cross-correlation. The shaded regions indicate the wavelength coverage of each CRIRES+ spectral order.
Prior and posterior distributions of true mass when accounting for dynamical stability. The left half of each violin is the prior distribution; the right half, the posterior. Each distribution is truncated at the 95 per cent upper limit, which are labelled by horizontal lines. In each case the upper limits are significantly reduced when accounting for stability, due to higher masses making a system less likely to be dynamically stable. The planets’ orbital periods are all in alphabetical order, except for Barnard’s Star whose planets are named d, b, c, e (J. I. González Hernández et al. 2024).
Distribution of log(VMR) for the molecule C_4H_2 across three representative atmospheric layers. The top row corresponds to the equilibrium state, while the bottom row shows the disequilibrium steady state. Each panel displays ≈5000 samples from the test data set, with colour indicating the C/O ratio of each sample. The leftmost panel represents the layer closest to the planet’s surface (highest pressure), and the rightmost panel corresponds to the upper atmosphere (lowest pressure).
The 4.3-m Leuschner Radio Telescope located at the UC Berkeley Leuschner Student Observatory, equipped with the LIMBO FRB detection pipeline.
A sample of the best and worst reconstructed typical sources with their reconstructions as performed by a VQ-VAE trained on the unlabelled data. (Top) Five of the best reconstructed typical sources, having the highest scores and therefore ranked as ‘most typical.’ They are shown with their reconstructions as well as the reconstruction score. (Below) Five of the worst reconstructed typical sources, having the lowest scores and therefore ranked as ‘least typical’. These sources come up as false positives. They are shown with their reconstructions and reconstruction scores.