WHERE DO WE GO FROM HERE?

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

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? γmin? 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??