1. Xray observations of high redshift radio galaxies
Thermal emission:
a. Cluster Atmospheres: Beacons to high z (proto-)clusters,
Constrain Omega_M
b. Hydrodynamic interaction of radio source and ISM/ICM:
Cavities, Bow shocks, constrain source dynamics, probe
pre-existing ICM
Non-thermal emission:
a. Synchrotron emission: constrain high gamma_e and particle
acceleration mechanisms
b. Inverse Compton emission: constrain magnetic fields,
low gamma_e
AGN emission: constrain emission processes (accretion disk,
core-jet, scattering), absorption columns, constrain L_opt, identify cluster member AGN (type-II AGN?)

2. Cygnus A (Wilson, Smith, Arnaud, Young)
200 kpc
L_X = L_R = L_O = 1e45 erg/s
M_grav = 2e14 M_sun, M_gas = 1e13 M_sun

3. Hydrodynamics of a powerful radio jet (Clarke et al 1999)
Xray

4. Cygnus A: hydrodynamics
‘Shocked’ ICM: n=0.01, T=7e7, P = 1e-10 (cgs)
Radio lobe (minE): B = 30 uG, P = 2e-11 (cgs)
=> Departure from minimum energy?

5. Caution: what you CAN see is what you get
Clarke et al 1996

6. IC emission from radio hot spots and lobes
Sync
B_SSC = 150 uG
B_minE = 250 uG
SSC

7. Synchrotron vs. IC (CMB) losses vs. redshift

8. Radio quiet, IC loud jets at very high z?
z=5.99 Schwartz 2002
T_CMB = 2.7(1+z) => nu_CMB = 1.6e11(1+z)
=> Gamma_e (1 keV obs)= 1000 (independent of z!)=> t_e= 9.4e5yrs
U_CMB = aT^4 => off-sets distance losses
Gamma_e (5 GHz obs) = => t_e = 2.5e6 yrs

9. Synchrotron jets: 3C 273 (Marshall et al. 2002)
Merlin HST Chandra/HST
gamma = 2e7 => t_e = 70 yrs

10. Cygnus A nucleus: AGN emission and absorption
nucleus: L_2-10keV = 4e44 erg/s
alpha = -0.8, N(HI) = 2e23 cm^-2
scattered (electron): L_2-10keV = 4e42 erg/s

11. Examples at z = 0.5 3C295 Harris et al. 2002 3C263 3C330 3C351
Hardcastle et al. 2002

12. Xray observations of z > 2 radio galaxies
z=2.2
z=2.0
3c294
z=1.8
z=3.4 4”

13. Massive, virialized clusters at high redshift?
, , : No
Beta = 2.5
R_c = 12”
L_x (cluster) < 1.5e44 erg/s (eg. <40% Cygnus A)

14. M_virial > 1e14 M_sun (T_x > 3keV) => Omega_M < 0.9
3C 294: Yes? (Fabian etal. 2001)
L_x (cluster) = 5e44 erg/s
M_virial > 1e14 M_sun (T_x > 3keV)
=> Omega_M < 0.9 3 5
9kev

15. 1138-262: rich in Xray-loud AGN? (Pentericci et al. 2002)
Xray sources: 15 type-I AGN, 1 type-II, 1 star
Two confirmed at z = 2.2, Four others likely
Overdensity = 2x ‘field’ => AGN in (proto-) cluster?

16. Xray spectra of high z radio galaxy AGN
-1.1
L_2-10keV = 4e45 erg/s
N(HI) = 3e22 cm^-2
Gamma = -1.8
1e45
7e23 -2
N(HI) = 1e23 => A_V = 60

17. AGN: Radio-Xray-Optical correlations
Brinkmann et al. 1997
Obey: L_x – L_R,core for steep spectrum quasars
L_Q ( ) = 1e46 erg/s
L_Q ( ) = 1e47 erg/s

18. Radio-Xray alignment effect
z=2.2
z=2.0
3c294
z=1.8 4”

19. 3C294: West-Barthel/Arnaud effect
Giant elliptical galaxies form from ‘filamentary’ mergers
Radio jets oriented along the major axis of matter distribution are more luminous (ie. higher conversion efficiency) (?)
Dubinski 1998

20. 2036-254: Brunetti mechanism=IC of AGN radiation field
<alpha_rx> = but opposing X/R gradients argue against synchrotron and IC_CMB
Consistent with IC_Q => B_IC = 25 uG vs. B_minE = 75 uG
Counter-lobe brighter: back-scattering + time delay

21. 1138-262: Multiple (all?) mechanisms
Radio-Xray

22. Optical-Xray

23. Ly alpha – Xray

24. Ly alpha - Radio

25. Soft
Medium
Hard

26. 1138-262: Multiple Mechanisms Not:
Scattering: required core luminosity too high + wrong spectrum
Synchrotron: requires spectral flattening and non-detected in optical
Could be:
Two AGN +
IC_Q in jet: B_IC = 30 uG (but offsets in outer source => not IC?) +
Hot Gas: shock-heated, I(proto-)CM:
n_e= 0.05 cm^ M_gas= 2.5e12 M_sun
P_x= 8e P_minE= 6e P_line= 1e-9
=> Xrays reveal the pervasive medium confining radio source and
line clouds?

27. Rees model for proto-Giant elliptical
1. Multiphase medium: clouds/filaments at temperatures ranging from low ff ‘clouds’ at 1e4 K to high ff, virialized gas at 1e6-7 K.
2. Passage of Jet shock =>
High density clouds (>few cm^-2) are induced to form stars in higher pressure environment
Medium density regions (0.5 cm^-2) are shocked but cool on timescales < 1e7yrs, giving rise to Ly alpha emission
Low density regions (<0.1 cm^-2) are shock heated to X-ray emitting temperatures as seen by CHANDRA

28. B. Overdensity of galaxies => will evolve into cluster, but
Multiphase ‘cloudy’ medium: 1e4 – 1e7K
A. Ambient medium into which radio source expands changes significantly with redshift.
B. Overdensity of galaxies => will evolve into cluster, but
lack of X-ray cluster atmosphere => not dynamically relaxed => ‘proto-cluster’

29. Xray observations of high redshift radio galaxies
Thermal emission:
a. Cluster Atmospheres: Beacons to high z (proto-)clusters,
Constrain Omega_matter: Not seen => PROTO-clusters?
b. Hydrodynamic interaction of radio source and ISM/ICM:
Cavities, Bow shocks, constrain source dynamics, probe
pre-existing ICM: Shocked gas confining RS + line clouds
Non-thermal emission:
a. Synchrotron emission: constrain high gamma_e and particle
acceleration mechanisms
b. Inverse Compton emission: constrain magnetic fields,
low gamma_e: Brunetti mechanism at work => L_Q>1e46
AGN emission: constrain emission processes, absorption columns, constrain L_opt: Large N(HI) (but not Compton thick), consistent with steep spectrum Quasars: L_Q>1e46