1. Astrophysical Jets Robert Laing (ESO)

2. Galactic black-hole binary system Gamma-ray burst Young stellar object Jets are everywhere

3. Jets in Active Galaxies … with an emphasis on the nearby Well-collimated, bulk relativistic flows with Γ > 5 Powered by accretion onto black holes M  10 6 - 10 10 M SUN Powers can be as high as 10 41 W Major effects on galaxy formation and cluster evolution Efficient accelerators: electrons 10 14 eV; ? protons >10 20 eV

4. Jets in radio galaxies – up to Mpc scales FRI – low power Deceleration Morphological Classification Correlates with radio luminosity FRII – high power Relativistic and supersonic until hot-spots

5. Key topics Where are the emission sites? What are the radiation mechanisms? Jet velocity fields Effects on galaxy formation and cluster evolution Composition, power thrust Formation and collimation mechanism

6. Emission from jets: broad-band and on many scales Radio - TeV Gamma ray Synchrotron and inverse Compton → broad electron energy distribution + B Protons? Auger Cen A - X-ray synchrotron

7. Relativistic effects in jets Energy spectrum Doppler boosting Doppler factor Jet/counter-jet ratio Aberration v app = 30c Superluminal motion Blazars (θ  0) are bright, and rapidly-varying Low-power radio galaxies are side-on TeV blazars

8. M87 TeV - core or HST-1 Look for correlated variability with both core and HST-1

9. Jet velocity fields Limb-brightening and slow component speeds: gradual acceleration or fast spine + slow shear layer? Kovalev et al. 2007

10. Acceleration → deceleration? NGC315 Cotton et al. 1999 RL et al. 2006 Hardcastle et al. 2003 Tingay et al. TeV results require very high Γ - where are jets accelerated?

11. Velocity fields on large scales VLA data θ = 58 o Model

12. Velocity β = v/c: deceleration and transverse gradients 3C 31 B2 0326+39 NGC 315 3C296

13. shock 380 kpc Hydra A Wise et al. 07 10 61 erg Environmental Impact

14. Radio: Lane et al. 04/Taylor Low Radio Frequency Traces Energy 74 MHz Wise et al. 07 Feedback from jets halts cooling in cores of galaxy clusters Quenching of star formation → major influence on galaxy formation (“downsizing”)

15. Composition? Electromagnetic Leptonic (pair plasma) - not near black hole Hadronic (electron-proton plasma; relativistic protons?) Composition must change along the jet. EM → particles Entrainment of external medium Faraday rotation? Bulk Comptonization Mass, energy, momentum budget

16. Sunyaev-Zeldovich Effect and Radio Lobe Composition Pfrommer, Ensslin & Sarazin (2005) Perseus cluster (NGC1275/3C84) Contours: radio Colour: X-ray Extra pressure component Simulation of ALMA observation of SZ decrement in Perseus cluster Bubble profiles for different lobe compositions

17. Pressure and density 3C31 0326+39 3C296

18. Mach number and entrainment rate Stars Jets must be very light: consistent with electron-positron plasma

19. Power estimates from cavities

20. Krichbaum et al. 2006 174 R s Limits on collimation from mm VLBI Jet base 70 x 20 R S M87 86GHz

21. Magnetic collimation?

22. Coming shortly.... we hope LWA, eLOFAR mm VLBI ALMA GLAST VSOP-2 EVLA eMERLIN