All B-type subdwarf stars (hereafter sdB) should have low flux of ionizing photons, making them incapable of producing a noticeable circumstellar photoionized shell. However, a few sdB stars have been associated with circumstellar nebulae, resembling in some cases a planetary nebula. These discoveries spark doubts about the nature of the physical

Context. Molecular emission is observed in a wide variety of astrophysical environments, yet a substantial fraction of spectral features detected at millimeter wavelengths remain unidentified. Identifying these features is essential for constraining the inventory of interstellar and circumstellar molecules and for understanding the chemical

In this work, we derive and calibrate the redshift distribution of the MagLim++ lens galaxy sample used in the Dark Energy Survey Year 6 (DES Y6) 3 × 2 pt cosmology analysis. The 3 × 2 pt analysis combines galaxy clustering from the lens galaxy sample and weak gravitational lensing. The redshift distributions are inferred using the SOMPZ method—a

Current and forthcoming galaxy redshift surveys, such as DESI and Euclid, are going to bring cosmological analysis to an unprecedentedly exquisite level of precision in the determination of the cosmological parameters. However, these efforts require a high degree of control over theory and systematics, to obtain unbiased results. In this sense, the

We report a mm-wave search for axion dark matter from SGR 1745─2900, based on 4.8 h of ALMA observations. No candidate features are found between 133.99─135.78, 135.91─137.70, 145.99─147.78, and 147.99─149.78 GHz, corresponding to 0.55─0.62 meV. Interpreting this null result within a state-of-the-art stellar framework, we derive sensitivity to the

We present the morphological, photometric, and spectroscopic properties of a z ∼ 1 galaxy, "lil gal," serendipitously detected in JWST Mid Infrared Instrument (MIRI) images of nearby galaxy VV 340. In the MIRI F560W and F770W images, we identify what appears to be a spiral galaxy with a central bulge. However, in the F1500W image, a second peak