Events, Seminars, Talks

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The masses of supermassive black holes (BHs) in active galactic nuclei (AGNs) can be determined by resolving the BH sphere of influence over time using reverberation mapping (RM). The established relationship between the broad-line region (BLR) radius and AGN luminosity serves as a foundation for measuring black hole mass (MBH) across the Universe. For an increasing number of nearby AGNs, high signal-to-noise and high-cadence RM data offer new insights into BLR geometry and kinematics through dynamical modeling. Combining these independent MBH measurements with new spatially resolved host galaxy kinematics allows us to refine MBH-host galaxy scaling relations with unprecedented precision. I will discuss biases arising from varying aperture sizes, host galaxy morphologies, and AGN luminosities, and how they impact the intrinsic scatter in these scaling relations. Finally, I will explain how our findings influence the interpretation of MBH-scaling relations as tests for the co-evolution of black holes and their host galaxies.

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We aim to trace the evolution of eight edge-on star-forming disc galaxies through the analysis of stellar population properties of their (thin and thick) discs. We use Multi-Unit Spectroscopic Explorer (MUSE) observations and full-spectrum fitting to produce spatially resolved maps of ages, metallicities and [Mg/Fe] abundances and extract the star formation histories of stellar discs. Our maps show thick discs that are on average older, more metal-poor and more ?-enhanced than thin discs. However, age differences between thin and thick discs are small (around 2 Gyr) and the thick discs are younger than previously observed in more massive and more quiescent galaxies. Both thin and thick discs show mostly sub-solar metallicities, and the vertical metallicity gradient is milder than previously observed in similar studies. [Mg/Fe] differences between thick and thin discs are not sharp. The star formation histories of thick discs are extended down to recent times, although most of the mass in young stars was formed in the thin discs. Our findings show thick discs that are different from old thick discs previously observed in more massive galaxies or more quiescent galaxies. We propose that thick discs in these galaxies did not form quickly at high redshift, but slowly in an extended time. The thin discs were formed also slowly, but with a larger mass fraction at very recent times.

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