-
Andrea Merloni (MPE)28/10/2025, 10:35
The statistical properties of Supermassive Black Holes in the local Universe provide both direct and indirect constraints on theoretical models of BH formation, growth and co-evolution with their host galaxies. In this talk, I will present studies of the local distribution of X-ray selected AGN carried out thanks to the largest survey of the kind, the eROSITA All-Sky Survey. I will focus in...
Go to contribution page -
Catarina Aydar (Max Planck Institute for Extraterrestrial Physics)28/10/2025, 11:00
Unraveling the mysteries of supermassive black holes and their relationship with their host galaxies is challenging and requires a proper disentanglement of the emission from the Active Galactic Nucleus (AGN) and the stellar populations. When observing the same AGN in different phases of its activity, some properties obtained from its optical spectra should be consistent, as the mass of the...
Go to contribution page -
Ms Khushboo - (LMU)28/10/2025, 11:15
Recent JWST mid-infrared observations of the central ~50pc region of the Seyfert 2 nucleus in the galaxy NGC 7582 have revealed prominent ice absorption features. Such icy bands have not been included in existing AGN or starburst dust radiative transfer models. In particular, template spectra from AGN model libraries severely underestimate the mid-infrared flux when compared with the JWST...
Go to contribution page -
Almudena Prieto (IAC & Munich Observatory)28/10/2025, 11:30
I discuss the relevance of high ionisation coronal lines as genuine tracers of the ionising continuum in galactic nuclei, and in turn of the spectral shape and temperature of the accretion disk, hence of the BH mass. On the basis of bona-fide BH masses from reverberation mapping and the strong infrared coronal line [Si VI] 1.96 um, a tight correlation between the excitation of the gas and...
Go to contribution page -
Taro Shimizu (MPE)28/10/2025, 11:45
We present the first sample of cosmic noon quasars with spatially resolved broad-line regions (BLRs) and dynamical black hole mass measurements using GRAVITY+. Through deep integrations with GRAVITY+, we detect the differential phase signal across the H$\alpha$ broad emission line which allows for detailed kinematic modeling of the BLR. We find BLR sizes systematically smaller by a factor of...
Go to contribution page -
Lazaros Souvaitzis (Max Planck Institute for Astrophysics)28/10/2025, 13:10
The most massive galaxies in the Universe also host the largest black holes, with masses of $10^9 \: \mathrm{M_{\odot}}$ and above (SMBHs). During their hierarchical assembly, these galaxies accreted many low-mass galaxies across cosmic time, possibly hosting IMBHs. They have experienced only a few major mergers at low redshift. If some of these IMBHs migrate to the galactic center, they may...
Go to contribution page -
Stefano de Nicola28/10/2025, 13:25
Ultramassive black holes, with masses > 10^10 solar masses, sit at the very top of the black hole mass spectrum. These objects are rare and can’t be identified using standard scaling relations like the classic BH-sigma relation, which underestimate black hole masses at the high-mass end. Instead, the size of the core — a light-deficient central region compared to an inward extrapolation of the...
Go to contribution page -
Justo Gonzalez (European Southern Observatory)28/10/2025, 13:40
AGN feedback has become a standard ingredient in cosmological simulations to help regulate the development of cooling flows and star formation from the scales of galaxies to groups and clusters. However, it is difficult to fine-tune the feedback efficiency to reproduce the observed cool-core fractions at all scales. In the paper "How the cool-core population transitions from galaxy groups to...
Go to contribution page -
Luca Sala (C2PAP/LMU/USM)28/10/2025, 13:55
The mass and spin of massive black holes (BHs) at the centre of galaxies evolve due to gas accretion and mergers with other BHs. Besides affecting the evolution of relativistic jets, the BH spin determines the efficiency with which the BH radiates energy.
Go to contribution page
I implemented a sub-resolution prescription for cosmological, hydrodynamical simulations that models the evolution of the BH spin,... -
Volker Springel (MPA)28/10/2025, 14:30
-
Jelena Ritter (Max Planck Institute for Astrophysics)28/10/2025, 14:55
Extended Ly-alpha nebulae observed around quasars trace the cool gas
Go to contribution page
within the multiphase circumgalactic medium and can provide key insights
into the complex interplay between gas dynamics and active galactic
nuclei (AGN) feedback. However, the connection between this cool phase
and the cold molecular gas around the host galaxies remains largely
unexplored. In this talk, I leverage ALMA... -
Raquel Ruiz Valença (Universidade de São Paulo)28/10/2025, 15:10
Quasars are the most luminous type of AGN currently known, detectable across a vast range of redshifts extending beyond $z=7$. Thus, increasing the number of known quasars is essential for studying the accretion mechanisms of supermassive black holes, the evolution of galaxies, and the large-scale structure of the Universe, among others.
Go to contribution page
Over the last four decades, spectroscopic surveys have... -
Ric Davies (MPE)28/10/2025, 15:25
We present the first near-infrared interferometric data of the broad line region of a QSO at z=4. GRAVITY+ detects a differential phase signal tracing the spatially resolved kinematics for both the H$\beta$ and H$\gamma$ lines. Fitting these lines simultaneously shows that 80% of the HI line emission in the broad line region originates in an outflow with a velocity up to $10^4$ km/s, oriented...
Go to contribution page -
Sunmyon Chon (MPA)28/10/2025, 15:40
The formation of supermassive black holes (SMBHs) is one of the biggest challenges in astrophysics. The Direct Collapse (DC) model provides seed BHs with a mass of 10^5 Msun and explains the origin of high-redshift SMBHs. It has been assumed that these seed BHs can only form in primordial gas, a restrictive condition that yields too few seeds to explain the observed population. We investigate...
Go to contribution page -
Ruancun Li (Max-Planck-Institute for Extraterrestrial Physics)28/10/2025, 16:15
The early growth of high-redshift quasars and their host galaxies raises critical questions about their cosmic evolution. We exploit the angular resolution and sensitivity of NIRCam to investigate the host galaxies of 31 quasars at $4 < z <7$ drawn from multiple JWST surveys. Using a new multi-band forward-modeling code (\textsc{GalfitS}) that incorporates physically motivated priors, we...
Go to contribution page -
Dr Irham Taufik Andika (Ludwig-Maximilians-University Munich)28/10/2025, 16:30
The formation channels of the first supermassive black holes (SMBHs) at z > 6 remain elusive, as current observations are dominated by the most luminous quasars, representing only the tip of the population. To uncover fainter quasars, gravitational lensing provides a uniquely effective natural telescope, extending the accessible luminosity range and offering essential probes of black hole...
Go to contribution page -
Seok-Jun Chang (Max Planck Institut für Astrophysik)28/10/2025, 16:45
Little Red Dots (LRDs), compact galaxies at z > 5 discovered by JWST, show hydrogen Balmer lines with broad wings (>1000 km/s), absorption features, and asymmetric profiles, indicating extremely dense hydrogen gas. When the broad components of Balmer lines are analyzed using standard AGN methods, they imply supermassive black holes with unusually high black hole–to–stellar mass ratios....
Go to contribution page -
Hannah Übler (MPE)28/10/2025, 17:00
JWST has discovered an unexpected ubiquity of massive, active black holes at high redshift. Understanding their formation and the properties of their host galaxies is an ongoing endeavour. I will present first results from BlackTHUNDER, a JWST/NIRSpec-IFS Large Program to study broad-line AGN and their immediate surroundings during the first few billion years of cosmic history. Specifically, I...
Go to contribution page
Choose timezone
Your profile timezone: