The Whirlpool Galaxy is a well-studied grand design galaxy with two major spiral arms, and a large satellite NGC 5195. The arms both show long uniform sections with perturbations ("kinks" or sharp turns) in specific regions. Comparing the two arms shows a small radial offset between the main kinked regions. We analyzed the morphology and also the

In recent years, about 150 low-mass white dwarfs (WDs), typically with masses below 0.4 M ⊙, have been discovered. The majority of these low-mass WDs are observed in binary systems as they cannot be formed through single-star evolution within Hubble time. In this work, we present a comprehensive analysis of the double low-mass WD eclipsing binary

We study the ionized gas kinematics of 293 Active Galactic Nucleus (AGN) hosts as compared to that of 485 control galaxies from the MaNGA-SDSS survey using measurements of the [O III]$\lambda$5007 Å emission-line profiles, presenting flux, velocity, and W$_{80}$ maps. In 45 per cent of the AGN, a broad component was needed to fit the line profiles

The oldest stars in the Milky Way (born in the first few billion years) are expected to have a high density in the inner few kpc, spatially overlapping with the Galactic bulge. We use spectroscopic data from the Pristine Inner Galaxy Survey (PIGS) to study the dynamical properties of ancient, metal-poor inner Galaxy stars. We compute distances

WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, saw first light in late 2022. WEAVE comprises a new 2-deg field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU

We present the detection of three exoplanets orbiting the early M dwarf TOI-663 (TIC 54962195; V = 13.7 mag, J = 10.4 mag, R ★ = 0.512 ± 0.015 R ⊙, M ★ = 0.514 ± 0.012 M ⊙, d = 64 pc). TOI-663 b, c, and d, with respective radii of 2.27 ± 0.10 R ⊕, 2.26 ± 0.10 R ⊕, and 1.92 ± 0.13 R ⊕ and masses of 4.45 ± 0.65 M ⊕, 3.65 ± 0.97 M ⊕, and <5.2 M ⊕ at