The near-infrared calcium II triplet (CaT), around 850 nm, is a key metallicity indicator for red giant stars. We present a revised [Fe/H] calibration as a function of CaT line strengths and four luminosity indicators, including the Gaia G band, together with the classical V, I, and $K_s$ bandpasses. For this purpose, we used a sample of 366 red

Owing to hot and inflated envelopes that facilitate atmospheric studies, ultrahot Jupiters (UHJs) have attracted much attention. Significant progress has been achieved, from enlarging the sample size to broadening the studies to encompass diverse stellar types and ages. Here, we present a transmission spectroscopy study of HAT-P-70b, a UHJ orbiting

Dust in the circumgalactic medium (CGM) has been detected statistically, using tens of thousands of background galaxies or quasars to measure average attenuation. However, variations in dust properties among galaxies, and the causes of those variations, are lost when stacking. To achieve a sufficient level of precision that enables spatially

In order to test the robustness and reliability of the new generation spectral-line identifier PyEMILI, as initially introduced in Paper I, in line identification and establish a reference/benchmark dataset for future spectroscopic studies, we run the code on the line lists of a selected sample of emission-line nebulae, including planetary nebulae

The search for sources of high-energy astrophysical neutrinos can be significantly advanced through a multimessenger approach, which seeks to detect the γ-rays that accompany neutrinos as they are produced at their sources. Multimessenger observations have so far provided the first evidence for a neutrino source, illustrated by the joint detection

We present here the preliminary modeling results for the close binary central star of the planetary nebula Pa 164. While parameter models for about 20-25 close binaries within planetary nebulae exist, this number is far too low to perform significant statistical analysis. To increase this number, we used the Phoebe modelling software to begin the