There will be formal discussion time for each session. We encourage participants to bring material (e.g. a slide) and thoughts to present during the discussions.
Cluster outskirts, profiles and mass estimate
Chair: Daisuke Nagai
- what's special about outskirts?
- what are the relative importance of random motion, gas clumping, accretion, electron-proton non-equilibrium, filament, CR, magnetic field… on interpreting the observations at outskirts?
- why mass? what about gravitational potential?
ICM in surveys
Chair: Naoki Yoshida
- cross-correlation studies: what will be possible? what can we learn?
- what will new observations reveal?
Turbulence, bulk motions
Chair: Peng Oh
- simulations: how well do different codes agree on the gas velocity field? how to separate bulk and turbulent motions?
- what are the main sources of turbulence/bulk motions during a cluster's cosmological evolution? what does the current amplitude of turbulence/bulk motions tell us?
- new diagnostic methods?
Chair: Eugene Churazov
- how does AGN feedback work? how to model it?
- what's the sphere of influence of AGN feedback?
Chair: Alex Schekochinhin
- how does ICM turbulence dissipate? to which degree/for what purposes can we trust simulations with different approximations?
- transport coefficients: how & how well do we know their values? Is it important/ possible to get them right in simulations?
- how is non-thermal energy divided among turbulence, magnetic-field and cosmic ray?
Structures in clusters: radio halos, radio relics, cold fronts, ghost cavities, cool cores, buoyant bubbles...
Chair: Torsten Ensslin
- what are their origins, are they stable, how universal are they?
- as dynamical state tracer? e.g. radio - SZ connection
- what do they tell us about ICM microphysics?