Scientific data analysis pipelines commonly use high-level technologies that were popular when they were created, only providing an immediate solution which is unlikely to be sustainable or reproducible in the future. We have implemented "Maneage" (Managing data Lineage), a solution which stores the project in machine-actionable and human-readable

Lockman-SpReSO is a deep optical spectroscopic survey of a complete sample of galaxies previously observed at the greatest depth in X-ray, far infrared, and sub-millimeter, using, respectively, XMM-Newton, Spitzer, Herschel, and radio observations covering the central 24 x 24 arcmin 2 of the Lockman Hole field. The main scientific objective is to

We present the first results of application of the MANCHA3D code (Felipe 2010; Khomenko et al. 2017, 2018) to a K0V cool star. Initially we run the code solving purely hydrodynamic equations until the stationary convection is reached. Then we produce the magnetic field generation and amplification by Biermann's battery seed and local dynamo. We

We use IFS data of four galaxies from the TIMER survey to explore the kinematics measured in different spectral regions that are sensitive to distinct stellar populations. We derive the velocity and velocity dispersion of both a young and an old stellar population and several stellar parameters. We report a correlation of the mean luminosity

We present a comparison of the spin parameter λ R, measured in a region dominated by the galaxy disc, between 20 pairs of nearby (0.005 < z < 0.03) seemingly isolated twin galaxies differing in nuclear activity. We find that 80-82% of the active galaxies show higher values of λ R than their corresponding non-active twin(s), indicating larger

We present an independent discovery and detailed characterization of K2-280 b, a transiting low density warm sub-Saturn in a 19.9-d moderately eccentric orbit (e = $0.35_{-0.04}^{+0.05}$ ) from K2 campaign 7. A joint analysis of high precision HARPS, HARPS-N, and FIES radial velocity measurements and K2 photometric data indicates that K2-280 b has