On Dichotomies in Active Galaxies

or

The Jet-Accretion Connection

Annalisa Celotti - S.I.S.S.A. [celotti@sissa.it]

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