We report on the discovery of a transiting Earth-sized (0.95R ⊕) planet around an M3.5 dwarf star at 57 pc, EPIC 249631677. The planet has a period of ∼3.14 days, i.e., ∼π, with an installation of 7.45 S ⊕. The detection was made using publicly available data from K2's Campaign 15. We observed three additional transits with SPECULOOS Southern and

Context. Milky Way globular clusters (GCs) are difficult to identify at low Galactic latitudes because of high differential extinction and heavy star crowding. The new deep near-infrared (IR) images and photometry from the VISTA Variables in the Via Láctea Extended Survey (VVVX) allow us to chart previously unexplored regions. Aims: Our long term

The asteroid explorer Hayabusa2 encountered the Cb-type asteroid 162173 Ryugu between June 2018 and November 2019. The Telescopic Optical Navigation Camera (ONC-T) [1, 2] onboard Hayabusa2 observed Ryugu with 7 bandpass filters ranging in wavelength of 0.40-0.95 mm. On 8 January 2019, ONC-T observed the asteroid in the opposition geometry from ~20

We present cloud-tracking results from Venus nightside images with velocity errors approaching 1 m/s (rms). The cloud-tracking scheme focuses on 1) reducing the errors associated with Venus disk registration and 2) modeling cloud feature trajectories over a succession of images. Venus disk registration errors are reduced to within 0.25 pixels with

We compare Venus dayside cloud top winds from Akatsuki UVI images to contemporaneous winds in the lower clouds retrieved on the night side using IRTF/SpeX 2.3 µm images. From Nov 19 to Dec 6, 2018, we obtained daily images of the night side of Venus with SpeX at 1.74, 2.3 and 5.1 µm, and spectral images cubes of the disk from 0.7 to 2.5 µm. On Nov

Aims: We aim to study the magnetic field in solar spicules using high-resolution spectropolarimetric observations in the Ca II 8542 Å line obtained with the Swedish 1-m Solar Telescope. Methods: The equations that result from the application of the weak field approximation (WFA) to the radiative transfer equations were used to infer the line-of