We report the discovery and validation of two long-period giant exoplanets orbiting the early K dwarf TOI-4600 (V = 12.6, T = 11.9), first detected using observations from the Transiting Exoplanet Survey Satellite (TESS) by the TESS Single Transit Planet Candidate Working Group. The inner planet, TOI-4600 b, has a radius of 6.80 ± 0.31 R ⊕ and an
TOI-4600 b and c: Two Long-period Giant Planets Orbiting an Early K DwarfMireles, Ismael et al.92023Citations0
Sub-second infrared variability from the archetypal accreting neutron star 4U 1728-34
We report on the first simultaneous high-time resolution X-ray and infrared (IR) observations of a neutron star low mass X-ray binary in its hard state. We performed $\approx 2\,$ h of simultaneous observations of 4U 1728-34 using HAWK-I@VLT, XMM-Newton, and NuSTAR. The source displayed significant X-ray and IR variability down to sub-second timeVincentelli, F. M. et al.
The extended 'stellar halo' of the Ursa Minor dwarf galaxy
Stellar candidates in the Ursa Minor (UMi) dwarf galaxy have been found using a new Bayesian algorithm applied to Gaia EDR3 data. Five of these targets are located in the extreme outskirts of UMi, from ~5 to 12 elliptical half-light radii (rh), where rh(UMi) = 17.32 ± 0.11 arcmin, and have been observed with the high-resolution Gemini Remote AccessSestito, Federico et al.
This is a bug release mostly concerning the checkpointing. Check the changelog for more details.Koposov, Sergey et al.
A 5.3-min-period pulsing white dwarf in a binary detected from radio to X-rays
White dwarf stars are the most common stellar fossils. When in binaries, they make up the dominant form of compact object binary within the Galaxy and can offer insight into different aspects of binary formation and evolution. One of the most remarkable white dwarf binary systems identified to date is AR Scorpii (AR Sco). AR Sco is composed of an MPelisoli, Ingrid et al.
A Bayesian estimation of the Milky Way's circular velocity curve using Gaia DR3
Aims: Our goal is to calculate the circular velocity curve of the Milky Way, along with corresponding uncertainties that quantify various sources of systematic uncertainty in a self-consistent manner. Methods: The observed rotational velocities are described as circular velocities minus the asymmetric drift. The latter is described by the radialPõder, Sven et al.