The WEAVE-Apertif (WA) survey on the William Herschel Telescope will perform dedicated large integral field unit (LIFU; 90") optical spectroscopy follow-up of 400 HI resolved galaxies from the Apertif HI survey. The LIFU observations will provide an unprecedented study of galaxy evolution and dynamics with 3-6x the physical resolution and 2-3x the

Several recent studies have shown that the Vela OB2 region hosts a complex constellation of sub-populations with ages in the range 10 to 50 Myr. Such populations might represent the best example of the outcome of clustered star formation in giant molecular clouds (GMCs). We use Gaia DR2 data over an area of 40 deg radius around the open cluster

Aims: Our objective is to identify analogues of gas giant planets, but located as companions at wide separations of very young stars. The main purpose is to characterise the binarity frequency and the properties of these substellar objects, and to elucidate their early evolutionary stages. Methods: To identify these objects, we cross correlated the

Time series observations of a single dithered field centred on the diffuse dwarf satellite galaxy Crater II were obtained with the Dark Energy Camera (DECam) at the 4m Blanco Telescope at Cerro Tololo Inter-American Observatory, Chile, uniformly covering up to two half-light radii. Analysis of the g and i time series results in the identification

Context. It has recently been proposed that LB-1 is a binary system at 4 kpc consisting of a B-type star of 8 M ☉ and a massive stellar black hole (BH) of 70 M ☉. This finding challenges our current theories of massive star evolution and formation of BHs at solar metallicity. Aims: Our objective is to derive the effective temperature, surface

Measures of exoplanet bulk densities indicate that small exoplanets with radius less than 3 Earth radii (R ⊕) range from low-density sub-Neptunes containing volatile elements 1 to higher-density rocky planets with Earth-like 2 or iron-rich 3 (Mercury-like) compositions. Such astonishing diversity in observed small exoplanet compositions may be the