The ∼200,000 stars observed by the Kepler mission have provided unprecedented constraints across astrophysics. With the advent of modern spectroscopic and photometric surveys, new limits in stellar characterizations are within reach. In this work, we report a compilation of atmospheric parameters (T eff, log ( g ) , and [M/H]) for the Kepler stars

Ground-based radio telescopes are routinely used to search for light dark matter (DM) candidates such as axionlike particles or dark photons. However, these instruments face inherent limitations to push the searches to masses below 10 - 7 eV, due to the effect of the Earth's ionosphere. The extant and planned space- or Moon-based radio telescopes

We present a stellar stream found in images of the nearby, nearly face-on, late-type galaxy, NGC 3938 obtained for the Large Binocular Telescope Imaging of Galactic Halos and Tidal Structures (LIGHTS) survey that is thin, has very low mean surface brightness (<μ g> ≍ 28.7 mag arcsec −2 and <μ r> ≍ 28.1 mag arcsec −2), appears to lie nearly on the

Context. Images recorded with the Tunable Magnetograph (TuMag) instrument on board the SUNRISE III balloon observatory are affected by temporal contrast fluctuations. These variations are related to high-frequency vibrations (jitter) of the platform that cannot be entirely compensated by the image stabilization unit of the telescope. Jitter smooths

We investigate the capability of the J-PAS survey to constrain the primordial power spectrum using a non-parametric Bayesian method. Specifically, we analyze simulated power spectra generated by an oscillatory primordial feature template motivated by non-standard inflation. The feature is placed within the range of scales where the signal-to-noise

Context. Spectroscopic and spectropolarimetric observations, which rely on the Doppler effect, only provide access to the line-of-sight component of the solar plasma velocity (i.e., v z). However, many dynamic processes in the solar atmosphere involve strong horizontal motions (i.e., in the plane perpendicular to the line of sight: v x, v y)