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Disk-Jet Connection Disk-Jet Connection in the Radio in the Radio

Galaxies 3C 120 and Galaxies 3C 120 and 3C 1113C 111

Ritaban ChatterjeeRitaban Chatterjee

YCAA Seminar, September 22YCAA Seminar, September 22ndnd, , 2009.2009.

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Data SourcesData Sources X-Ray (RXTE-PCA) and VLBA: X-Ray (RXTE-PCA) and VLBA: A. Marscher, S. A. Marscher, S.

JorstadJorstad (BU)(BU) 37 GHz : 37 GHz : Anne Lahteenmaki, Merja Anne Lahteenmaki, Merja

Tornikoski, Talvikki HovattaTornikoski, Talvikki Hovatta (Metsahovi (Metsahovi Observatory, Finland).Observatory, Finland).

R Band: R Band: I. McHardyI. McHardy (U. Southampton), (U. Southampton), Kevin Kevin Marshall, H. Richard Miller, Wesley T. RyleMarshall, H. Richard Miller, Wesley T. Ryle (Georgia State)(Georgia State)

V Band: V Band: Large international team (please see Large international team (please see ApJ paper for details) led by Martin GaskellApJ paper for details) led by Martin Gaskell (U. Texas, Austin, U. Nebraska, Lincoln).(U. Texas, Austin, U. Nebraska, Lincoln).

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“An active galactic nucleus (AGN) is a compact region at the center of a galaxy which has a much higher than normal luminosity over some or all of the electromagnetic spectrum. The radiation from AGN is believed to be a result of accretion on to a super-massive black hole at the centre of the host galaxy.” -Wikipedia

AGN: Definition

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AGN : Unified Picture

Courtesy: C.M. Urry & P. Padovani

BlazarBLRG 3C 120 and 3C 111

are BLRGs

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Mirabel &Rodriguez 1998,Nature, 392, 673.

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OUTLINE

• Why time variability

• 3C 120, 3C 111: Characteristic timescale

• 3C 120, 3C 111: X-ray/optical production mechanism(s) and location

• 3C 120, 3C 111: Accretion disk-jet connection

• Effect of these results on AGN-BHXRB connection

• Future Plans

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Why Time Variability?

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Thesis TitleThesis Title

Multi-Frequency Multi-Frequency Time variabilityTime variability of Active Galactic Nucleiof Active Galactic Nuclei

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Alternative TitlesAlternative Titles

Reliable Information from Reliable Information from Variable EmissionVariable Emission

Variable Emission, Dependable Variable Emission, Dependable ResultsResults

Consistent Information from Consistent Information from Variable Emission: Multi-Variable Emission: Multi-Frequency Time Variability of Frequency Time Variability of Active Galactic NucleiActive Galactic Nuclei

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VLBA (BU blazar group)3C 279Z=0.5361 mas = 6.3 pc

3C 279

Optical (STScI DSS)

Gamma-Ray (CGRO team)

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Use of Time Variability Use of Time Variability AnalysisAnalysis

Upper limit to physical size : Upper limit to physical size : R ≤ cΔt'R ≤ cΔt' Power spectral density (amplitude of Power spectral density (amplitude of

variability as a function of timescale) variability as a function of timescale) => => periodicity, characteristic periodicity, characteristic timescalestimescales

Correlation and light curve Correlation and light curve decomposition (Comparison of flux at decomposition (Comparison of flux at different wavelengths) => different wavelengths) => structure structure and emission mechanism(s)and emission mechanism(s)

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OUTLINE

• Why time variability

• 3C 120, 3C 111: Characteristic timescale

• 3C 120, 3C 111: X-ray/optical production mechanism(s) and location

• 3C 120, 3C 111: Accretion disk-jet connection

• Effect of these results on AGN-BHXRB connection

• Future Plans

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3C 120

1. BLRG2. FR-I3. z=0.033 4. Angle between jet axis and

line of sight ~20o

5 GHz Image: Walker, Benson & Unwin 1987 ApJ, 316, 546

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3C 1111. BLRG2. FR-II3. z=0.048 4. Angle between jet axis and

line of sight ~20o

1.4 GHz Image: Linfield & Perley 1984, ApJ, 279, 60

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Why 3C 120 and 3C 111?

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Variability atdifferent timescales

Power Spectral Density (PSD) => Amplitude of variability as a function of timescale

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X-Ray PSD of Cygnus X-1 : Break

BH Mass vs. Break Time Scale

Uttley et al. 2004, MNRAS

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3C 120 X-Ray Power Spectral Density (PSD)

Break Frequency=10-5 HzBreakTime Scale=2 Days

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Uttley et al. 2004, MNRAS, 348, 783

X-Ray PSD of Cygnus X-1 : Break

BH Mass vs. Break Time Scale

3C 120

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X-Ray PSD of Cygnus X-1 : Break

BH Mass vs. Break Time Scale

3C 120

3C 111

These radio galaxies have characteristic timescales similar to the Galactic BH systems => Accretion processes in alarge range of BH masses (10-108 Msun) have similar properties

Uttley et al. 2004, MNRAS, 348, 783

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Working on 3C 120 ! . . . . . . Are you in Craig Walker’s group?

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OUTLINE

• Why time variability

• 3C 120, 3C 111: Characteristic timescale

• 3C 120, 3C 111: X-ray/optical production mechanism(s) and location

• 3C 120, 3C 111: Accretion disk-jet connection

• Effect of these results on AGN-BHXRB connection

• Future Plans

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X-RAY

OPTICAL

RADIO

Light Curves of 3C 120 between 2002 and 2007

Chatterjee et al. 2009, ApJ, in press

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3C 120: X-ray/Optical Correlation

Chatterjee et al. 2009, ApJ, in press

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X-RAY

OPTICAL

RADIO

Light Curves of 3C 111 between 2002 and 2007

Chatterjee et al. 2009, in preparation

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3C 111: X-ray/Optical Correlation

Chatterjee et al. 2009, in preparation

X-ray leadsOptical by15±5 days

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• Optical emission is blackbody radiation from the accretion disk

• Thermal optical/UV seed photons are inverse-Compton scattered to X-rays by hot electrons in the corona

• Modeling of the accretion disk-corona system

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Chatterjee et al. 2009, ApJ, in press

Model of the Accretion Disk/Corona System

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X-ray and Opticalmodel flares

Disturbance is propagating toward the center

Disturbance is propagating away from the center

Chatterjee et al. 2009, ApJ,in press

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Feedback in Accretion Disk/Corona System

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X-ray and Optical Model Flares (Including Feedback)

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OUTLINE

• Why time variability

• 3C 120, 3C 111: Characteristic timescale

• 3C 120, 3C 111: X-ray/optical production mechanism(s) and location

• 3C 120, 3C 111: Accretion disk-jet connection

• Effect of these results on AGN-BHXRB connection

• Future Plans

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Movie Time!

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Superluminal Ejections Follow X-ray Dips in 3C 111

Chatterjee et al. 2009, in preparation

•X-rays are produced in the accretion disk, radio emission is from the jet•Connection between X-ray and radio emission => Connection between accretion disk and jet

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Possible Explanation of thePossible Explanation of the X-ray Dip and X-ray Dip and Superluminal Ejection CorrelationSuperluminal Ejection Correlation

Change in the magnetic field configuration in Change in the magnetic field configuration in the accretion disk from turbulent to aligned the accretion disk from turbulent to aligned

absence of viscous heating causes dips in X-absence of viscous heating causes dips in X-ray production ray production

aligned B field configuration facilitates shock to aligned B field configuration facilitates shock to move toward the jet (Livio et al. 2003)move toward the jet (Livio et al. 2003)

TurbulentX-ray productionWeaker flow in the jet

AlignedDecrease in X-ray productionIncrease in flow in the jet

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OUTLINE

• Why time variability

• 3C 120, 3C 111: Characteristic timescale

• 3C 120, 3C 111: X-ray/optical production mechanism(s) and location

• 3C 120, 3C 111: Accretion disk-jet connection

• Effect of these results on AGN-BHXRB connection

• Future Plans

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The next three slides are from:Rob Fender, U. Southampton, UK.

The life and times of a black hole X-ray binary…

X-ray hardness

X-r

ay L

um

inosi

ty /

Ed

din

gto

n

<10-6

~0.01

~0.1

~1.0

softspectrum

hardspectrum

Quiescence

after, typically,10+ years ofrelative peace, accretion rateincreases

Outburst

source getsvery bright and ‘softens’

source remainssoft for some time then fadesaway, returningto hard X-rayspectrum

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Faint, hard source have steady, ~1 jets

More powerful, hard sources have more powerful, steady jets…

As source softens, jet velocity increases abruptly, causing internal shock in jet

Subsequently, soft states show no jet

Relation to AGN ?

X-ray hardness

Lum

inosi

ty /

Ed

din

gto

n

<10-6

~0.01

~0.1

~1.0

soft hard

Quiescence<10-9

Sgr A*

LLAGN

Bright,Radio-loudAGN

Bright, radio-quiet AGN (with old lobes?)

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Fundamental Plane of BH Activity (edge-on view)

Merloni, Heinz & Di Matteo 2003, MNRAS, 345, 1057

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ConclusionsConclusions X-ray and optical emission from the X-ray and optical emission from the

accretion disk/corona systemaccretion disk/corona system Corona lies within ~50 gravitational radiiCorona lies within ~50 gravitational radii Similar characteristic timescale in Similar characteristic timescale in

accreting BH systems of masses accreting BH systems of masses 10-1010-1088 M Msunsun

Connection between accretion disk and jetConnection between accretion disk and jet Similarity with galactic black hole X-Ray Similarity with galactic black hole X-Ray

Binaries: Universality of BH systemsBinaries: Universality of BH systems

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Future PlansFuture Plans More detailed theory of the time More detailed theory of the time

variable emission from the accretion variable emission from the accretion disk-corona systemdisk-corona system..

Analysis and interpretation of X-ray Analysis and interpretation of X-ray binary monitoring data from binary monitoring data from SMARTS.SMARTS.

Gamma-ray variability of blazars Gamma-ray variability of blazars using Fermi data. Also related multi-using Fermi data. Also related multi-wavelength data including SMARTS.wavelength data including SMARTS.

More detailed theory of the time More detailed theory of the time variable emission from blazar jets.variable emission from blazar jets.

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Time-Variability of Active Galactic Nuclei

THE END

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3C 120 X-Ray Power Spectral 3C 120 X-Ray Power Spectral Density (PSD)Density (PSD)

Break Frequency=10-5 HzBreakTime Scale=2 Days

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corona

accretion disk BH

X-rays

UV

The Accretion-Disk/Corona The Accretion-Disk/Corona ComplexComplex

Simple modeling of the above system

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Spectral Energy Distribution of 3C 279 : Spanning 16 decades of Frequency

Courtesy: Alan Marscher

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AGN : Schematic Model

Cartoon courtesy:

Prof. Alan Marscher

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X-ray light curve :Sum of model flares & real data

Chatterjee et al. 2008(ApJ, in press)

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Optical light curve :Sum of model flares & real data

Chatterjee et al. 2008(ApJ, in press)

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Light Curve Decomposition

Chatterjee et al. 2008, ApJ, 489, 79

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Superluminal Ejections Follow X-ray Dips in 3C 120

Chatterjee et al. 2009, ApJ,in press

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Superluminal Ejections Follow

X-ray Dips in 3C 120

Chatterjee et al. 2009, ApJ,in press

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X-ray/37 GHz Anti-correlation (X-ray leads 37GHz by 120 days)

Chatterjee et al. 2009, ApJ,in press

5656

Possible Explanation of thePossible Explanation of the X-ray Dip and X-ray Dip and Superluminal Ejection CorrelationSuperluminal Ejection Correlation

Corona is the base of the jet Corona is the base of the jet decrease in the number density of decrease in the number density of

electrons at the base of the jet electrons at the base of the jet causes decrease in X-ray production causes decrease in X-ray production increase in the speed of particles increase in the speed of particles

(continuity eqn.) => shock wave.(continuity eqn.) => shock wave.