The atmospheres of low-temperature brown dwarfs and gas giant planets are expected to contain the phosphine molecule, PH 3. However, previous observations have shown much lower abundances of this molecule than predicted with atmospheric chemistry models. We report JWST spectroscopic observations of phosphine in the atmosphere of the brown dwarf

C≡N-bearing species are valuable tracers of nitrogen chemistry in the solar system. Ranging from volatile compounds like HCN and CH 3CN in cometary comae to refractory CN-bearing organics in some micrometeorites and interplanetary dust particles, these species originate in, or are derived from, molecular precursors in the interstellar medium (ISM)

Context. The physical conditions in stellar atmospheres, such as temperature, velocity, and magnetic fields, can be obtained by interpreting solar spectro-polarimetric observations. Traditional inversion codes, while successful, are computationally demanding, however, especially for lines whose formation is complex and dictated by nonlocal

We report the discovery of a new black-widow millisecond pulsar, PSR J1544–2555, associated with the Fermi-Large Area Telescope (LAT) source 4FGL J1544.2–2554. Optical, radio, and gamma-ray observations confirmed its nature as a compact spider binary system. Optical photometry from ULTRACAM revealed a $\sim$2.7-h orbital period, guiding MeerKAT

The Gaia BP/RP spectra provide an excellent opportunity to search for extremely metal-poor (EMP; [M/H] ≤ –3.0) stars. In this study, we assess the potential of our Gaia BP/RP-based candidate catalog, vetting newly identified EMP candidates with higher-resolution follow-up observations. The candidates are selected based on the metallicity derived

We present an independent spectroscopic and radial velocity analysis for nine stars from the Pennsylvania-Toruń Planet Search. For BD+24 4697, we present an updated true companion's mass (0.16±0.02 M☉) as well as evidence of stellar activity. For BD+54 1640 and BD+65 1241 we present true masses of companions, m=0.15±0.04 M☉ and m=0.091± 0.005 M☉