MULTIPHASE AGN FEEDING & FEEDBACK II: Linking the Micro to Macro Scales in Galaxies, Groups, and Clusters
LOCATION: Sexten Primary School - Via Panorama 6, Sexten
In the last decade, increasingly strong efforts have been devoted to understand the role of active galactic nuclei (AGN) during the cosmic evolution of galaxies, groups and clusters of galaxies. Chandra, XMM-Newton, and Hitomi have unveiled spectacular interactions of the central supermassive black hole (SMBH) with the host atmosphere in the form of resolved X-ray cavities, shocks, metal uplifts, and turbulence. At the same time, the hot halos of galaxies, groups, and clusters recurrently condense in localized regions forming multiphase filaments and clouds that rain onto the central SMBH and that are detected via optical/IR/radio telescopes (e.g., HST, Magellan, VLT, IRAM, SOFIA).
In the nuclear region, spectroscopical studies of AGN have discovered an amazing diversity of feeding and feedback phenomena, including ultrafast outflows, warm absorbers, massive ionized, neutral and molecular outflows. With the advent of next-generation telescopes (e.g., ALMA, MUSE, JWST, XARM, Athena, LOFAR/SKA), we are starting to learn that multiphase outflows are an ubiquitous phenomenon in cosmic structures of different masses and ages. Linking the macro to micro scales — and vice versa — of feeding and feedback processes is thus vital to advance our knowledge on the (co)evolution of black holes, galaxies, and clusters of galaxies.
The aim of the workshop is to bring together active researchers in the above tightly related — but often disjointed — fields in order to discuss the latest results, confront state-of-the-art simulations/models and observations, as well as promote new collaborations and set the path to future observational and numerical campaigns.
The goal is to dissect the following aspects and open issues of AGN feeding and feedback:
• linking the Mpc scale (macro) to the pc scale (meso) to the Schwarzschild radius (micro scale);
• the mode of accretion onto SMBHs: cold versus hot mode, chaotic versus smooth accretion;
• the formation of multiphase filaments and clouds during the gaseous halo evolution;
• the interplay of key physics as a function of time and environment, e.g., MHD, cooling, heating, turbulence, and rotation;
• the amount of energy released by the AGN feedback and the related duty cycle;
• how AGN feed back the environment, e.g., via massive outflows, relativistic jets, and/or radiation;
• linking the multiphase/multiwavelength AGN feedback channels: ionized, neutral, molecular outflows, and relativistic jets;
• key properties of multiphase outflows: mass loading, velocities, entrainment, energy-/momentum-conserving mode, obscuration, and ionization;
• how, where, and when the AGN energy is deposited, e.g., cavities, shocks, turbulence, and mixing.
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Seniors: 200 Eur - Students: 120 Eur
WORKSHOP CODE FOR PAYMENT 2020MUAG
Massimo Gaspari (Princeton University, USA) — Chair
Francesco Tombesi (University of Rome, Italy)
Massimo Cappi (INAF-IASF Bologna, Italy)