Moderator: Mitch Begelman

1
WHERE DO WE GO FROM HERE?

• Moderator Mitch Begelman
• Panelists
• Stefi Baum
• Katherine Blundell
• Greg Madejski
• Paul Nulsen
• Lukasz 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 ? 100s 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? ?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-? 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-? 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
  ?min and ?max - 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??