Xray observations of high redshift radio galaxies

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Xray observations of high redshift radio galaxies
Thermal emission a. Cluster Atmospheres Be
acons 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-t
hermal emission a. Synchrotron emission co
nstrain high gamma_e and particle
acceleration mechanisms
b. Inverse Compton emission constrain
magnetic fields, low gamma_e AGN emis
sion constrain emission processes (accretion
disk, core-jet, scattering), absorption col
umns, 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

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Hydrodynamics of a powerful radio jet (Clarke et
al 1999)
Radio
Xray
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Cygnus A hydrodynamics
Shocked ICM n0.01, T7e7, P 1e-10 (cgs)
Radio lobe (minE) B 30 uG, P 2e-11 (cgs)
Departure from minimum energy?
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Caution what you CAN see is what you get
Clarke et al 1996
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IC emission from radio hot spots and lobes
Sync
B_SSC 150 uG B_minE 250 uG
SSC
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Synchrotron vs. IC (CMB) losses vs. redshift
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Radio quiet, IC loud jets at very high z?
z5.99 Schwartz 2002
T_CMB 2.7(1z) nu_CMB 1.6e11(1z)
Gamma_e (1 keV obs) 1000 (independent of
z!) t_e 9.4e5yrs U_CMB aT4 off-sets
distance losses Gamma_e (5 GHz obs) 7000 t_
e 2.5e6 yrs
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Synchrotron jets 3C 273 (Marshall et al. 2002)
Merlin HST
Chandra/HST
gamma 2e7 t_e 70 yrs
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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
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Examples at z 0.5
3C263
3C330
3C351
3C295 Harris et al. 2002
Hardcastle et al. 2002
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Xray observations of z 2 radio galaxies
1138-262 z2.2
0236-254 z2.0
3c294 z1.8
0902343 z3.4
4
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Massive, virialized clusters at high redshift?
1138-262, 0902343, 2036-254 No
Beta 2.5 R_c 12
L_x (cluster) A)

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3C 294 Yes? (Fabian etal. 2001)
L_x (cluster) 5e44 erg/s M_virial 1e14 M_sun
(T_x 3keV)
Omega_M
3
5
9kev
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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?
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Xray spectra of high z radio galaxy AGN
1138-262 3C294
0902343
3e45 8e22 -1.1
1e45 7e23 -2
L_2-10keV 4e45 erg/s N(HI) 3e22 cm-2 Gamma
-1.8
N(HI) 1e23 A_V 60
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AGN Radio-Xray-Optical correlations
Brinkmann et al. 1997
Obey L_x L_R,core for steep spectrum quasars
L_Q (2036-254) 1e46 erg/s L_Q (1138-262)
1e47 erg/s
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Radio-Xray alignment effect
1138-262 z2.2
0236-254 z2.0
3c294 z1.8
4
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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
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2036-254 Brunetti mechanismIC of AGN
radiation field
-0.92 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-scatte
ring time delay
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1138-262 Multiple (all?) mechanisms
Radio-Xray
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Optical-Xray
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Ly alpha Xray
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Ly alpha - Radio
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Soft
Medium
Hard
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1138-262 Multiple Mechanisms
Not
Scattering required core luminosity too high
wrong spectrum Synchrotron requires spectral fla
ttening 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-2 M_gas 2.5e12
M_sun P_x 8e-10 P_minE 6e-10
P_line 1e-9 Xrays reveal the pervasive me
dium confining radio source and
line clouds?
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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 (
to X-ray emitting temperatures as seen by CHANDRA
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Multiphase cloudy medium 1e4 1e7K
A. Ambient medium into which radio source
expands changes significantly with
redshift. B. Overdensity of galaxies will evol
ve into cluster, but lack of X-ray cluster atmos
phere not dynamically relaxed
proto-cluster
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Xray observations of high redshift radio galaxies
Thermal emission a. Cluster Atmospheres Be
acons to high z (proto-)clusters,
Constrain Omega_matter Not seen
PROTO-clusters? b. Hydrodynamic interaction o
f 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 mechanis
m at work L_Q1e46 AGN emission constrain e
mission processes, absorption columns, constrain
L_opt Large N(HI) (but not Compton thick),
consistent with steep spectrum Quasars L_Q1e46