We investigate galaxy populations in the HS 1700+64 protocluster at $z=2.30$, characterized by two prominent linear filaments traced by spatially extended ${\rm Ly} \, \alpha$ blobs. We conducted a wide area mapping of emission line galaxies across the protocluster using the unique combination of three matched narrow-band filters, corresponding to

A crucial chemical link between stars and their orbiting exoplanets is thought to exist. If universal, this connection could affect the formation and evolution of all planets. Therefore, this potential vital link needs testing by characterizing exoplanets around chemically-diverse stars. We present the discovery of two planets orbiting the metal

We combine near-infrared imaging in two bands from the Hubble Space Telescope with archival observations of molecular gas to study SDSS J160705.16+533558.6 (J1607), an extremely luminous broad-line quasar at z = 3.65 that is also bright in the submillimeter. Via subtraction of the quasar point-spread function, we show that its host galaxy is

Cherenkov Telescope Array Observatory (CTAO) is the next-generation ground-based $\gamma$-ray observatory operating in the energy range from $20\, \mathrm{GeV}$ up to $300\, \mathrm{TeV}$, with two sites in La Palma (Spain) and Paranal (Chile). It will consist of telescopes of three sizes, covering different parts of the large energy range. We

V Sge is a peculiar, highly luminous long-period (12.34 h) binary star that can display a supersoft X-ray emitting component when in the faint phase of its $V \approx 10-13$ mag variability range. Apparently undergoing Eddington-limited accretion from its more massive secondary, it is in a very rare, short-lived evolutionary phase towards the

Context. Super-Earths and mini-Neptunes are missing from our Solar System, yet they appear to be the most abundant planetary types in our Galaxy. A detailed characterization of key planets within this population is important for understanding the formation mechanisms of rocky and gas giant planets and the diversity of planetary interior structures