We present, for the first time, model spectra of single-age, single-metallicity stellar populations computed with the E-MILES evolutionary synthesis code incorporating an environment-dependent, variable galaxy-wide initial mass function (gwIMF). This gwIMF, calculated using the GalIMF code, is rooted in the integrated galactic initial mass function (IGIMF) theory, which predicts IMF variations as a function of the star formation rate and the metallicity. By coupling these two codes, we generated a comprehensive library of single-burst stellar population spectra uniquely sensitive to gwIMF

The solar corona—the outermost layer of the Sun’s atmosphere—is extremely hot and very low in density. One of the main challenges in solar physics is understanding why the corona reaches temperatures of over a million degrees. This heating is believed to be closely related to the Sun’s magnetic field. However, quantifying the coronal magnetic field is difficult because the light emitted by the corona is extremely faint, and its polarization signals, which encode the information on the magnetic field, are subtle. Thanks to recent advances in technology, telescopes like the Daniel K. Inouye

The rocky planet GJ 1132 b, with Earth-like mass and radius, is a prime candidate for atmospheric studies. Previous observations with Hubble and JWST yielded conflicting results about its atmosphere. This study used three transit observations with the CRIRES+ instrument to search for He i, HCN, CH₄, and H₂O in GJ 1132 b's atmosphere. No clear atmospheric signals were detected, but upper limits for CH₄, HCN, and H₂O were established. The results suggest that if GJ 1132 b has an atmosphere, it is not dominated by hydrogen. The work highlights the challenges of detecting high molecular weight