Aims. Coronal lines (CLs) may be a reliable proxy of supermassive black hole (SMBH) mass in active galactic nuclei (AGNs) because the production of these high ionisation potential (IP) lines is sensitive to the shape of the ionising continuum, which for a thin accretion disc relies on the black hole mass. In this work we study the connection

Under the collisionless cold dark matter (CDM) paradigm, galaxies with stellar masses below 10 5--6M ⊙ are expected to preserve primordial cuspy dark matter (DM) profiles. Because baryonic feedback should be too weak to transform cusps into cores at these masses, such galaxies provide especially sensitive tests of DM physics. If cores are observed

Context. Phylogenetic trees offer a hierarchical representation of chemical similarities among stars, from which their evolutionary histories can, in principle, be reconstructed. Simulation-based work suggests that phylogenetic trees built under different chemical evolution scenarios carry distinguishable structural imprints, but whether existing

We present a new age determination of 24 globular clusters (GCs) dynamically associated with the main accretion events experienced by the Milky Way (MW), as part of the Cluster Ages to Reconstruct the Milky Way Assembly (CARMA) project's effort to trace the Galaxy's assembly history. We used deep and homogeneous archival Hubble Space Telescope data

Context. QUIJOTE is a cosmic microwave background (CMB) experiment composed of two telescopes, QT1 and QT2, located at the Teide Observatory (OT) in Tenerife, Spain. The multifrequency instrument (MFI) (2012--2018), installed on QT1, observed the sky at four frequency bands, namely 11, 13, 17, and 19 GHz, with an angular resolution of one degree

Aims. We revisit the carbon abundance in the primitive iron-poor star J0815+4729 ([Fe/H] = -5.49). J0815+4729 is so enhanced in carbon and rich in oxygen that, in addition to the CH and C 2 molecular lines, weaker neutral atomic transitions are measurable in its spectrum. This provides a unique opportunity to explore the line formation of C I and O