On Dichotomies in Active Galaxies
or
The Jet-Accretion Connection
Annalisa Celotti - S.I.S.S.A. [[email protected]]
Jets/outflows in accreting systems
Active Galactic Nuclei ~10% AGN 'radio-loud' extended / compact jets aligned up to 108 decades < few degrees ~ 10 L ~ 1043- 1048 erg/s SMBH + disc
X-ray Binaries up to ~ 20% (?) a few SL ~ few - >> 1 (?) L ~ 1038- 1040 erg /s BH / NS + disc
Gamma-ray Bursts 102 < < 104 ~ ? L ~ 1052 erg /s
BH + torus
And…
RQ Quasars + Sey 1 ~30% (?) outflows radio
BAL outflows: ~10% QSO
Tb > 108 K + compact (< pc) SMHB + disc
Bl und ell et a l. 0 3
PG
140
7 +
26
3
z=0
.94
Low Luminosity AGN ~20-60%
unresolved radio + Tb > 108 K
SMHB + discYoung Stellar Objects
v ~ vesc ~ 100- 400 km /s
L ~ 10-2 - 10-1 Lstar
protostar + disc
HS
T archive
CrabPulsars
Chandra jets (e.g. Crab)
= ? v =0.5 c (HST)
magnetized rotating NS
no disc ?
Jets/outflows are easy to form
How/Why jets form?
Qs:
- How/where/why are they formed, accelerated and collimated?
- How do they relate to gas inflow?
- In which form is energy extracted and transported?
- How/where/why do they dissipate?
JETS energetically important
COMPACT OBJECT required? v~v esc potential, i.e.
BH necessary for relativistic jets?
DISC necessary? different accretion regimes?
OUTFLOWS: necessary?
Possible answers
Hydromagnetic
B provides link jet-disc/hole
(rotational) power + symmetry from :
spinning BH: low barion loading - no radiation drag
disc: more power (depending on accretion regime) ?
are jets needed?
both?: relativistic el.m./pair core + collimating e-p `slow’ MHD flow
BH vs DISC ? Jet content (pairs, el.m.,e-p)
MBH, accretion mode, relative power
The jet – disc connection
Mi rabel et al 98
Jet-disc connection in AGN
Which is the connection between
accretion rate/accretion regime and jets?
1. Jetted vs non jetted AGN with similar accretion properties RL-RQ quasars
2. Jetted AGN with different accretion properties FRI-FRII Radio Galaxies
3. Non-jetted AGN with different accretion properties LINERS and Seyfert galaxies
RQ
RL
Elvis et al. ‘94
Optical
1 - Radio loudness of quasars
RL ~ 10% AGN (opt. surveys) : dichotomy?
RQ
RL
Elvis et al. ‘94
Optical
Radio Power
Radio-to-optical ratio:
R* Lr / Lo
1 - Evidence for RQ/RL dichotomy
R*5 GHz ~ 10
Pado
vani
199
3
Log10 P5 GHz ~ 25
Mi l ler et al . 19 90
1- Is the RQ/RL dichotomy real ?
New large complete samples FIRST + 2dF Quasar Redshift Survey
FIRST + Large Bright Quasar Survey
The fraction of radio detected quasars depends on apparent and absolute optical magnitudes
2dF + LBQS
Large spread between optical and radio luminosities
Cir
asuo
lo e
t al.
02
Lr vs L opt
No evidence for a gap
2dF + LBQS
Hew
it t et al. 00
R
1- Bypass selection effects: A new approach
* Optical Luminosity Function: Lopt,z
* Monte Carlo simulations + Observational cuts * Comparison with data (KS and 2)Distributions of radio-to-optical ratios and radio powers
Dependence of the fraction on apparent/absolute magnitude
Number counts: radio and optical band
Redshift and absolute magnitude distributions
PG
LBQS2dF
N
R
Shapes Log10 R*1.4 or Log10 Pradio
distributions:
* Radio properties Lr
Radio and optical luminosities
related and unrelated
1 - Result: No dichotomy
Uniqueness of the solution using only a simple prescription for R*
1.4
Radio luminosity depends on optical one, even though with a large scatter.
The dependence of the fraction of RL quasars on apparent and absolute magnitude results from selection effects.
Continuity in jet formation mechanism(s) ?
X1 = -0.5 ± 0.31 = 0.75 ± 0.3
X2 = 2.7 ± 0.22 = 0.7 ± 0.2
97±2 %
Monotonic distribution: no gap
Cir as uo lo e t a l.
0 2
R
Lr
1- What about SLOAN results?Ivezic et al 02, 03
Radio
R
Optical
Ivez
ic e
t al 0
2
Optical
R
R
Ivezic et al 03
See also Jester & Kron: SDSS+FIRST
Cirasuolo et al
2 - Phenomenology of radio galaxies: FRI - FRII
3c31
Imag
es c
ourt
esy
of N
RA
O/A
UI Fanaroff & Riley 74;
Ledlow & Owen 96
Cyg A
Morphology radio power
2- Transition FRI-FRII
MB - MBH [McLure & Dunlop 01]
Lr - LNLR - Lacc [Willott et al 01]
+
Transition FRI-FRII : ~ const ~ 6 10-2 / 0.1 m
Ghisel li ni &
Celott i 01
2 - Estimate of nuclear luminosity - I
Radio gal: direct look at nucleus at HST resolution
3CR RG (z<0.3)
* Compact core (< tens-hundreds pc) in majority of sources
* In FRI optical luminosity correlates with radio
Lopt vs Lr
FRI
Chi
aber
ge, C
apet
ti &
Cel
otti
99, 0
1, 0
2; V
erdo
es K
leijn
ea
01
Lopt
FRI + FRII
Lradio
2 - Estimate of nuclear luminosity II
BLRG + QSO
Unification RL AGN
Relativistic beaming Radio gal vs blazar
Obscuring ‘torus’ Broad vs Narrow lines
BRLG (Broad Line Galaxy) QUASAR LIKE
HEG (High-Excitation Galaxy) OBSCURED OBJECTS
LEG (Low-Excitaton Galaxy) FRI LIKEFRII
2 - Nuclear optical emission
FRI + FRII/LEG: no optically and geometrically thick torus
FRII/HEG: obscured
FRII/BLRG + QSO: ‘’extra’ thermal/disc emission
* Nuclear transition for: continuum + lines + torus
* Nuclear properties do not match extended radio: on-off episodes/evolution?
OPT IR OPT IR
Marchesini, C
apetti & C
elotti 04
2 - Accretion properties
MBH from MB-MBH
LBOL from Lopt (HST) + bolometric correction (caveat RG)
Main sample, is complete and not selected on nuclear properties
m in Eddington units = L / LEdd (log ) ~ 0.45mm
Marchesini, C
elotti & F
errarese 04
FRII/HEG absorbed
= 1
m
2 - MBH and Accretion rate
MBH
FRI
•
10-3
Indication for bimodal
accretion rate distribution
m
QSO
FRII/LEG FRII/BLRG
2 - Why ? Speculations
•m
Complete 3CR subsample (at same z): two peaks ~ equally populated
Continuos distribution, all possible* Unstable flow at intermediate rates : radiation pressure dominated
accretion regime ?
* Gap due to inhibition of jet formation: spin energy via Blandford & Znajek –
efficient for rates >> 1 and << 1 (H~R)?
* Transition due to a change in : e.g transition to radiatively-
inefficient, geom thick, optically thin flow?
* Decrease in the effective mass accretion: mass loss ?
m
Discontinuous distribution in * On-off switching of the nuclear accretion?
* Evolutionary sequence from FRII to FRI-like regime?
m