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

Massive stars drive the ionization and mechanical feedback within young star-forming regions. The Large Magellanic Cloud (LMC) is an ideal galaxy for studying individual massive stars and quantifying their feedback contribution to the environment. We analyze eight exemplary targets in LMC N11 B from the Hubble UV Legacy Library of Young Stars as

Context. Samples from the asteroid Ryugu provide key information on the initial composition and evolutionary processes of primitive bodies. Aims. This study aims to detect H 2O spectral features associated with inter-layer water in a statistically significant number of Ryugu grains protected from terrestrial contamination. Methods. We analysed

We present seeing-limited (0.8″) near-infrared integral field spectroscopy data of the type-2 quasars, QSO2s, SDSS J135646.10+102609.0 (J1356) and SDSS J143029.89+133912.1 (J1430, the Teacup), both belonging to the Quasar Feedback, QSOFEED, sample. The nuclear K-band spectra (1.95–2.45 μm) of these radio-quiet QSO2s reveal several H 2 emission

Using early data from the Dark Energy Spectroscopic Instrument (DESI) survey, we search for active galactic nuclei (AGN) signatures in 410,757 line-emitting galaxies. By employing the BPT emission-line ratio diagnostic diagram, we identify AGNs in 75,928/296,261 (≈25.6%) high-mass ( 9.5) and 2444/114,496 (≈2.1%) dwarf ( 9.5) galaxies. Of these AGN