Connections between Radio and High Energy

Emission in AGN

1

Geoff BicknellResearch School of Astronomy & Astrophysics

Australian National University

Friday, 27 July 12

COSPAR 2012

Collaborators:

2

• Loredana Bassani, INAF, Bologna

•Nadine Neumayer, ESO, Munchen

• Francesca Panessa, INAF, Roma

• Ralph Sutherland, RSAA

• Andrea Tarchi, INAF, Cagliari

• Alex Wagner, Tsukuba University

Friday, 27 July 12

COSPAR 2012

Motivation:

3

Disk emission

Coronal emission / Advection Dominated Accretion Flows (ADAFs)

Jets and Winds

* Parameters of jets in radio-loud objects close to black hole

* Launching of jets from black holes

* Partition of Black Hole Gravitational Power into:

Friday, 27 July 12

COSPAR 2012

Origin of X-ray emission

4

Two main possible emission mechanisms:

• Comptonization of soft disk photons by hot corona

• Synchrotron or Inverse Compton emission from jet

Radio loud: Predominantly flat spectral index

Radio quiet: Predominantly steepspectral index

Shastri et al. ’93

Friday, 27 July 12

COSPAR 2012

Black Hole Fundamental Plane

5

Merloni & Heinz ’03Falcke ’04

5 GHZ core luminosity vs2-10 keV luminosity

log LR = 1.05 log LX + 0.78 log M + 7.33

Offset in Galactic and Extragalactic correlations due to black hole mass

Friday, 27 July 12

COSPAR 2012

Panessa et al 2007

6

Low luminosityRadio Galaxies

Seyfert galaxies(radio quiet)

Difference of 3 orders of magnitude in radio luminosity but same slope

LX / L0.97R

Friday, 27 July 12

COSPAR 2012

Panessa et al. 2011 - Correlation lost at VLBI resolution

7

VLA core

VLBI core

Suggests correlation with jet power rather than luminosity

Friday, 27 July 12

COSPAR 2012

INTEGRAL Sample

8

INTEGRAL 20-40 keV sample; 88 sources (Malizia et al. ’09)

2-10 keV X-ray data (Malizia et al. + literature)

NVSS radio data (Maiorano et al. in prep.)

20-100 keV

Friday, 27 July 12

COSPAR 2012

Different modes of X-ray and radio emission

9

• Disk and corona dissipate gravitational power rapidly

• Jet Poynting flux-dominated, non dissipative

• Jet power manifest on kpc scales

Corona

Gamma-ray and/or X-ray emission region

Jet

Chaotic magnetic field

Wind

Shock orreconnectionregion

Ordered magneticfield

Friday, 27 July 12

COSPAR 2012

Relationship between radio power and jet power

10

Not simply a conversion of jet power into luminosity

Model-dependent, e.g. Shabala et al. ’05: Expansion of radio source into 2-component background medium

Model for Seyferts motivated by observations of NGC 4051

Friday, 27 July 12

COSPAR 2012

NGC 4051: Giroletti & Panessa ’09

11

~ 19 kpc bubble on large scales fed by jet on small scales

Friday, 27 July 12

COSPAR 2012

Jet – Interstellar Medium interaction

12

Density Powerful 1045 ergs s-1 jet in 1 kpc fractal medium

Friday, 27 July 12

COSPAR 2012

Luminosity of bubble

13

j⌫ = Numerical Factors⇥ K B(a+1)/2 ⌫�(a�1)/2

N(�) = K��a

Emissivity

Friday, 27 July 12

COSPAR 2012

Luminosity of bubble

13

j⌫ = Numerical Factors⇥ K B(a+1)/2 ⌫�(a�1)/2

N(�) = K��a

Emissivity

Friday, 27 July 12

COSPAR 2012

Luminosity of bubble

13

j⌫ = Numerical Factors⇥ K B(a+1)/2 ⌫�(a�1)/2

N(�) = K��a

Emissivity

K estimated from electron pressure

K ⇡ 3ptot

mec2

✓pe

ptot

◆�(a�2)

1

Friday, 27 July 12

COSPAR 2012

Luminosity of bubble

13

j⌫ = Numerical Factors⇥ K B(a+1)/2 ⌫�(a�1)/2

N(�) = K��a

Emissivity

K estimated from electron pressure

K ⇡ 3ptot

mec2

✓pe

ptot

◆�(a�2)

1

Lower cutoff

Friday, 27 July 12

COSPAR 2012

Luminosity of bubble

13

Radius and pressure of bubble

R = At3/5

ptot

=1225

⇢aA2t�4/5

A =

125384⇡

FE

⇢a

�1/5

j⌫ = Numerical Factors⇥ K B(a+1)/2 ⌫�(a�1)/2

N(�) = K��a

Emissivity

K estimated from electron pressure

K ⇡ 3ptot

mec2

✓pe

ptot

◆�(a�2)

1

Lower cutoff

Friday, 27 July 12

COSPAR 2012

Luminosity of bubble

13

Radius and pressure of bubble

R = At3/5

ptot

=1225

⇢aA2t�4/5

A =

125384⇡

FE

⇢a

�1/5

Ambient density

j⌫ = Numerical Factors⇥ K B(a+1)/2 ⌫�(a�1)/2

N(�) = K��a

Emissivity

K estimated from electron pressure

K ⇡ 3ptot

mec2

✓pe

ptot

◆�(a�2)

1

Lower cutoff

Friday, 27 July 12

COSPAR 2012

Luminosity of bubble

13

Radius and pressure of bubble

R = At3/5

ptot

=1225

⇢aA2t�4/5

A =

125384⇡

FE

⇢a

�1/5

Ambient density

Jet energy flux

j⌫ = Numerical Factors⇥ K B(a+1)/2 ⌫�(a�1)/2

N(�) = K��a

Emissivity

K estimated from electron pressure

K ⇡ 3ptot

mec2

✓pe

ptot

◆�(a�2)

1

Lower cutoff

Friday, 27 July 12

COSPAR 2012

Luminosity - Jet Power relation

14

P⌫ = j⌫ ⇥Volume

B = Equipartition with total pressure

Friday, 27 July 12

COSPAR 2012

Luminosity - Jet Power relation

14

P⌫ = j⌫ ⇥Volume

B = Equipartition with total pressure

P⌫ ⇡ Numerical Factor⇥ ⇢3(a+1)/20a F (a+11)/10

E t(4�a)/5⌫(3�a)/2

Friday, 27 July 12

COSPAR 2012

Luminosity - Jet Power relation

14

P⌫ = j⌫ ⇥Volume

B = Equipartition with total pressure

P⌫ ⇡ Numerical Factor⇥ ⇢3(a+1)/20a F (a+11)/10

E t(4�a)/5⌫(3�a)/2

na ⇠ 1 cm�3

Friday, 27 July 12

COSPAR 2012

Luminosity - Jet Power relation

14

P⌫ = j⌫ ⇥Volume

B = Equipartition with total pressure

P⌫ ⇡ Numerical Factor⇥ ⇢3(a+1)/20a F (a+11)/10

E t(4�a)/5⌫(3�a)/2

t ⇠ 3⇥ 108 yrna ⇠ 1 cm�3

Friday, 27 July 12

COSPAR 2012

Luminosity - Jet Power relation

14

P⌫ = j⌫ ⇥Volume

B = Equipartition with total pressure

P⌫ ⇡ Numerical Factor⇥ ⇢3(a+1)/20a F (a+11)/10

E t(4�a)/5⌫(3�a)/2

t ⇠ 3⇥ 108 yrna ⇠ 1 cm�3

INTEGRAL sample: ⌫ = 1.4 GHz

Friday, 27 July 12

COSPAR 2012

Radio power -> Luminosity

15

Strongest dependence is on energy flux

P⌫ / F (a+11)/10E

) FE / P 10/(a+11)⌫ = P 0.76

⌫ for a = 2.2

Friday, 27 July 12

COSPAR 2012

Energy flux – X-ray Luminosity

16

38

40

42

44

46

48

41 42 43 44 45 46 47 48

y = -4.1059 + 1.0389x R= 0.78609

log

F E (e

rgs

s-1)

log L(20-100 keV) (ergs s-1)

Almost linear correlation between jet power and X-ray luminosity

FE ∝ LX1.04

Jet power ~ 0.5% of X-ray luminosity – with large deviations from mean

Somewhat misleading since alternative regression =>

LX ∝ FE0.6

Friday, 27 July 12

COSPAR 2012

Main points on disk-dominated X-ray AGN

17

• Need to understand better the relationship between radio and X-ray emission in both radio-loud and radio quiet sources where the X-ray emission is clearly disk coronal emission

• Important to focus on jet power rather than radio luminosity when considering the partition of gravitational power among various modes

• Consideration of the large scale source structure and dynamics useful way of estimating jet power

Friday, 27 July 12

COSPAR 2012

X-ray jet emission in the Radio-Loud Galaxy Centaurus A

18

Extended synchrotronemission

SED of core from Lenain et al ’09

Friday, 27 July 12

COSPAR 2012

Interaction of jet with ISM

192

Radio and X-ray Images from Hardcastle et al 2003 and 2007

Approaching side

Receding side

Friday, 27 July 12

COSPAR 2012

Interaction of jet with ISM

192

Radio and X-ray Images from Hardcastle et al 2003 and 2007

Approaching side

Receding side

Friday, 27 July 12

COSPAR 2012

Interaction of jet with ISM

192

Radio knot SW of nucleus

Radio and X-ray Images from Hardcastle et al 2003 and 2007

Approaching side

Receding side

Friday, 27 July 12

COSPAR 2012

Velocity of [SiVI] – 0.12” SINFONI – VLT

204

Corrected for rotation:

Neumayer et al. 2007

Friday, 27 July 12

COSPAR 2012

Why is [SiVI] blue-shifted?

215

Redshifted emission on approaching side and blueshifted on receding side at first counterintuitive

Expect entrained clouds to be moving with jet

Knot SJ1

Friday, 27 July 12

COSPAR 2012

Geometry

226

z

x

yJet

Counter –Jet

obs

cl

Cloud

Observervcl

x’(W)

y’(N)

SJ1

z-y plane definedby jet and observer

Friday, 27 July 12

COSPAR 2012

Shock models (MAPPINGS)

23

-0.5 0.0 0.5 1.0

-3.0

-2.0

-1.0

0.0

Blue Cloud

Total

precursor

shock + precursor

shock + precursor

shock only

shock only ß=10

ß = 0.1ß = 1ß = 10

1000 km/s

170 km/s

220 km/s

750

1000

1000 ß=11000

ß=10

1000 ß=0.1

750

500

350km/s

Log[ SiVI/Bra ]

Log[

CaV

III/B

ra ]

Friday, 27 July 12

COSPAR 2012

High energy emission from the core

248

Synchrotron + Inverse Compton model fits to the high energy emission from the core of Cen A – Lenain et al. 2009

Model Lorentz factor = 15Inclination ~ 25o

Estimates from VLBIobservations (Tingay et al. 01)

Lorentz factor > 1.12Inclination between450 and 80o

Extended synchrotronemission

Friday, 27 July 12

COSPAR 2012

Parameters of photoionization models

259

U =

No. density of ionising photons

Atomic no. density

=

nph

n↵ = Spectral slope of flux density

Flux density F⌫ / ⌫�↵

Typically ↵ ⇡ 1.4

and log U ⇡ �2

Lenain et al. models of X-ray synchrotron => ↵ ⇡ 0.39

Friday, 27 July 12

COSPAR 2012

Flux of ionizing photons

26

z

x

yJet

Counter –Jet

obs

cl

Cloud

Observervcl

x’(W)

y’(N)

SJ1

�obs

=

1

�(1� � cos ✓obs

)

�cl

=

1

�(1� � cos ✓cl

)

Doppler factors:

Lorentz factor

Friday, 27 July 12

COSPAR 2012

Ionizing flux (cont.)

2712

Nph

=Z 1

⌫0

Nph

(⌫) d⌫

=1c

✓DA

Dcl

◆2

✓�cl

�obs

◆3

Z 1

�obs

��1

cl

⌫0

Fobs

(⌫obs

)h⌫

obs

d⌫obs

z

x

yJet

Counter –Jet

obs

cl

Cloud

Observervcl

x’(W)

y’(N)

SJ1

DA

Dcl

=

Distance to Cen A

Distance of cloud from core

=

sin(✓obs

+ ✓cl

)

cl

Projected angular distance ofcloud from core

Friday, 27 July 12

COSPAR 2012

Results of photoionization calculations

2813

-0.5 0.0 0.5 1.0

-3.0

-2.0

-1.0

0.0

Log[ SiVI/Bra ]

Log[

CaV

III/B

ra ]

Blue Cloud

Total

Log U = -2.0

Log U = -1.0

Log U = +0.0

_ = +0.0

_ = -1.0

-0.8-0.6-0.4

-0.2

Optimal MAPPINGSmodel very close to the slope derived from high energy models

and .....

quite different from standard AGN models

log U = -1.9 typical of dusty photoionization models (Dopita et al. 2002)

Friday, 27 July 12

COSPAR 2012

Density and filling factor

29

Indicates modest Lorentz factors < 5

Friday, 27 July 12

COSPAR 2012

Density and filling factor

29

Typical filling factors for entire NarrowLine Region in AGN ~ few x 10-2 – 10-4

Indicates modest Lorentz factors < 5

Friday, 27 July 12

COSPAR 2012

Conclusions for Centaurus A

30

• Blue-shifted cloud in the core of Centaurus A photoionized by high energy emission from base of jet

• But ... beamed emission from jet consistent with low Lorentz factor not 15 as claimed by high energy model

• Greater consistency with deductions from VLBI data

• Need for substantial revision of models for high energy emission

Friday, 27 July 12