Context. Small planets transiting bright nearby stars are essential to our understanding of the formation and evolution of exoplanetary systems. However, few constitute prime targets for atmospheric characterization, and even fewer are part of multiple star systems. Aims: This work aims to validate TOI-4336 A b, a sub-Neptune-sized exoplanet

Context. The TOI-421 planetary system contains two sub-Neptune-type planets (P b ~ 5.2 days, T eq, b ~ 900 K, and P c ~ 16.1 days, T eq,c ~ 650 K) and is a prime target to study the formation and evolution of planets and their atmospheres. The inner planet is especially interesting as the existence of a hydrogen-dominated atmosphere at its orbital

In contrast to our understanding of density field tracers, the modeling of direct statistics pertaining to the cosmic velocity field remains open to significant opportunities for improvement. The lack of accurate modeling for the nonlinear domain of pairwise velocities restricts our capacity to fully exploit the information encoded in this

It was known that an ideal spherically symmetric stellar system with isotropic velocities and an inner core cannot reside in a Navarro, Frenk, and White (NFW) gravitational potential. The incompatibility can be pinned down to the radial gradient of the NFW potential in the very center of the system, which differs from zero. The gradient is

HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, P d = 278.36 d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing