We provide a detailed characterization of the planetary system orbiting HD 85426 (TOI-1774). This bright G-type star ( $M_{\ast }$: 0.99 $\text{M}_{\odot }$; $R_{\ast }$: 1.13 $\text{R}_{\odot }$; age: 7.4 Gyr; V mag: 8.25) hosts a transiting sub-Neptune, HD 85426 b, with an orbital period of 16.71 d and a blackbody equilibrium temperature of $824^

We provide a detailed characterization of the planetary system orbiting HD 85426 (TOI-1774). This bright G-type star ( $M_{\ast }$: 0.99 $\text{M}_{\odot }$; $R_{\ast }$: 1.13 $\text{R}_{\odot }$; age: 7.4 Gyr; V mag: 8.25) hosts a transiting sub-Neptune, HD 85426 b, with an orbital period of 16.71 d and a blackbody equilibrium temperature of $824^

Aims. Mass-modeling methods are used to infer the gravitational field of stellar systems, from globular clusters to giant elliptical galaxies. While many methods already exist, most require assumptions on the form of the underlying distribution function or binning the data, leading to some loss of information. Furthermore, when only line-of-sight

Context. Accurate determination of the chemical abundances in stars plays a pivotal role in understanding stellar structure and evolution, nucleosynthesis, and the chemical enrichment history of the Milky Way. Benchmark stars with precise and accurate atmospheric parameters and abundances are indispensable for calibrating spectroscopic surveys and

We introduce a fast method to measure the conversion gain in complementary metal-oxide-semiconductor active pixel sensors, which accounts for nonlinearity and interpixel capacitance (IPC). The standard "mean-variance" method is biased because it assumes that pixel values depend linearly on the signal, and existing methods to correct for

The Euclid mission and other next-generation large-scale structure surveys will enable high-precision measurements of the cosmic matter distribution. Understanding the impact of baryonic processes such as star formation and active galactic nuclei (AGN) feedback on matter clustering is crucial to ensure precise and unbiased cosmological inference