1. Moderator: Mitch Begelman Panelists: Stefi Baum Katherine Blundell Greg Madejski Paul Nulsen Łukasz Stawarz WHERE DO WE GO FROM HERE?

2. WHERE HAVE WE BEEN? X-RAYS FROM JETS/KNOTS –Close-in: relation to optical (HST), radio, IR (Spitzer!) Variability, proper motions Localized vs. continuous particle acceleration Rotation measures – Distant: kpc → 100’s of kpc One-sided: relativistic flow at large r Radiation mechanism: synchrotron vs. SSC vs. IC-CMB Particle lifetimes X-RAYS FROM LOBES/HOTSPOTS –Equipartition? γ min ? Jet composition? ENVIRONMENTAL IMPACTS –Shocks vs. weak shocks vs. sound waves vs. bubbles –Feedback Cool cores, not cooling flows; excess entropy on large scales Energy budget – BH growth/mass

3. WHERE ARE WE? X-RAYS FROM JETS/KNOTS –Jet energy contents: KE vs. Poynting, pairs vs. baryons –Kinematics: bulk motions vs. pattern speeds –Dissipation: shocks vs. reconnection, KH vs. MHD instabilities X-RAYS FROM LOBES/HOTSPOTS –Acceleration mechanisms, turbulence ENVIRONMENTAL IMPACTS –Microphysics of dissipation and transport processes –Feedback loop

4. SCIENCE QUESTIONS: HOW DO RELATIVISTIC FLOWS BEHAVE? HOW DO BLACK HOLES INTERACT WITH PLASMAS? HOW DO AGN OUTFLOWS AFFECT FORMATION & EVOLUTION OF COSMIC STRUCTURE (GALAXIES, CLUSTERS…) HOW DO MASSIVE BHs FORM AND GROW?

5. WHERE DO WE GO FROM HERE? KINDS OF OBSERVATIONS –Deeper: Better characterization of populations Faint features, e.g., sound waves in clusters Low-luminosity and obscured sources –Surveys: e.g., GPS/CSS, X-jets –Synoptic: Variability, proper motions QPOs in AGN? –Multi-λ: campaigns, follow-ups SYNERGY WITH NEW FACILITIES –w/GLAST, NuSTAR, ALMA, LOFAR, LWA, TeV… STRATEGIES –Key projects (“Legacy”) or continue “free market”? –ToO, follow-up agreements with GLAST, TeV…. UNIQUE CAPABILITIES –High spatial resolution

6. CASE STUDY: GLAST COMPACT, INNER JETS Location of the dissipation region, particle content,... – variability of limited use w/o simultaneous multi-λ obs. GLAST will provide an all-sky survey, follow-up in radio, IR, optical, X-ray - On-going effort of the GLAST collaboration via single snapshots of many objects + intensive campaigns in a few selected objects; need careful determination of cadence, length; some good successes from VLBI + opt, opt polarization + X-ray campaigns (successful examples: Marscher's BL Lac, but before-GLAST; 3C454.3 with Agile) EXTENDED, KPC-SCALE JETS: X-ray emission: X-ray polarization needed for the verification, but data need to be resolved on the relevant angular scale so jet not contaminated by core Particle content: e+/e- vs. e-/p+ - how to get there? - Faraday rotation and other radio observations; broader band observations: IC interaction with the CMB along the lines of "Sikora bump" in the IR... Energetics of jet particles: what broad - band observations are crucial? need to combine with γmin and γmax - how to get those? hard X-ray imaging will provide sensitive data; future - mid-range gamma-rays? Hot spots in local RG may be resolvable with GLAST Jets and hot spots: thermal vs. non-thermal? How much is in the thermal plasma? In clusters, it might be possible to use the interaction of the jet with the cluster gas as a calorimeter (some progress already made!) - what observations would make it easier? (example: spectral features rather than pure continuum would be tell-tales of thermal plasma - possible via spectroscopy with the X-ray calorimeter on NeXT, but poor angular resolution - must be used in conjunction with Chandra by using joint spatial / spectral data analysis, a technique still to be developed, along the lines of Peterson et al. XMM RGS cluster spectroscopy??