GLEAM-X J1627-52 was discovered as a periodic ( $\sim$18 min) radio signal over a duration of three months in 2018. It is an enigmatic example of a growing population of 'long-period radio transients' consistent with Galactic origins. Their nature is uncertain, and leading models invoke magnetic neutron stars or white dwarfs, potentially in close

TOI-836 is a ∼2–3 Gyr K dwarf with an inner super Earth (R = 1.7 R ⊕, P = 3.8 days) and an outer mini-Neptune (R = 2.6 R ⊕, P = 8.6 days). JWST/NIRSpec 2.8–5.2 μm transmission spectra are flat for both planets. We present Keck/NIRSPEC observations of escaping helium for super-Earth b, which shows no excess absorption in the 1083 nm triplet to deep

The present state of cosmology is facing a crisis where there is a fundamental disagreement in measurements of the Hubble constant ( $H_{0}$), with significant tension between the early and late Universe methods. Type Ia supernovae (SNe Ia) are important to measuring $H_{0}$ through the astronomical distance ladder. However, there remains potential

Aims. The United Kingdom Infrared Telescope (UKIRT) microlensing survey was conducted over four years, from 2016 to 2019, with the goal of serving as a precursor to future near-infrared microlensing surveys. Focusing on stars in the Galactic center and utilizing near-infrared passbands, the survey identified approximately one thousand microlensing

We reconstructed the star formation histories of seven massive (M ⋆ ≳ 10 10 M ⊙) early-type galaxies (ETGs) in the Virgo cluster by analysing their spatially resolved stellar population (SP) properties including their ultraviolet (UV) and Hα emission. As part of the Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE), we used Hα

Context. The latest Gaia Focused Product Release (FPR) has provided variability information for ∼1000 long-period red giant binaries, including almost ∼700 ellipsoidal binary candidates, thus providing the largest sample to date of this binary type with both photometric and spectroscopic time series observations. Aims. We aim to characterize both