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Disk-Jet Connection in the Radio Galaxies 3C 120 and 3C 111 Ritaban Chatterjee YCAA Seminar, September 22nd, 2009. 1 Data Sources X-Ray (RXTE-PCA) and VLBA: A. Marscher, S. Jorstad (BU) 37 GHz : Anne Lahteenmaki, Merja Tornikoski, Talvikki Hovatta (Metsahovi Observatory, Finland). R Band: I. McHardy (U. Southampton), Kevin Marshall, H. Richard Miller, Wesley T. Ryle (Georgia State) V Band: Large international team (please see ApJ paper for details) led by Martin Gaskell (U. Texas, Austin, U. Nebraska, Lincoln). 2 AGN: Definition “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 3 AGN : Unified Picture Blazar BLRG 3C 120 and 3C 111 are BLRGs Courtesy: C.M. Urry & P. Padovani 4 Mirabel & Rodriguez 1998, Nature, 392, 673. 5 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 6 Why Time Variability? 7 Thesis Title Multi-Frequency Time variability of Active Galactic Nuclei 8 Alternative Titles Reliable Information from Variable Emission Variable Emission, Dependable Results Consistent Information from Variable Emission: Multi-Frequency Time Variability of Active Galactic Nuclei 9 3C 279 Optical (STScI DSS) VLBA (BU blazar group) 3C 279 Z=0.536 1 mas = 6.3 pc Gamma-Ray (CGRO team) 10 Use of Time Variability Analysis Upper limit to physical size : R ≤ cΔt' Power spectral density (amplitude of variability as a function of timescale) => periodicity, characteristic timescales Correlation and light curve decomposition (Comparison of flux at different wavelengths) => structure and emission mechanism(s) 11 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 12 3C 120 1. BLRG 2. FR-I 3. z=0.033 4. Angle between jet axis and line of sight ~20o 5 GHz Image: Walker, Benson & Unwin 1987 ApJ, 316, 546 13 3C 111 1. BLRG 2. FR-II 3. z=0.048 4. Angle between jet axis and line of sight ~20o 1.4 GHz Image: Linfield & Perley 1984, ApJ, 279, 60 14 Why 3C 120 and 3C 111? 15 Variability at different timescales Power Spectral Density (PSD) => Amplitude of variability as a function of timescale 16 X-Ray PSD of Cygnus X-1 : Break BH Mass vs. Break Time Scale Uttley et al. 2004, MNRAS 17 3C 120 X-Ray Power Spectral Density (PSD) Break Frequency =10-5 Hz Break Time Scale =2 Days 18 X-Ray PSD of Cygnus X-1 : Break BH Mass vs. Break Time Scale 3C 120 Uttley et al. 2004, MNRAS, 348, 783 19 X-Ray PSD of Cygnus X-1 : Break BH Mass vs. Break Time Scale 3C 111 3C 120 These radio galaxies have characteristic timescales similar to the Galactic BH systems => Accretion processes in a large range of BH masses (10-108 Msun) have similar properties Uttley et al. 2004, MNRAS, 348, 783 20 Working on 3C 120 ! . . . . . . Are you in Craig Walker’s group? 21 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 22 Light Curves of 3C 120 between 2002 and 2007 X-RAY OPTICAL RADIO Chatterjee et al. 2009, ApJ, in press 23 3C 120: X-ray/Optical Correlation Chatterjee et al. 2009, ApJ, in press 24 Light Curves of 3C 111 between 2002 and 2007 X-RAY OPTICAL RADIO Chatterjee et al. 2009, in preparation 25 3C 111: X-ray/Optical Correlation X-ray leads Optical by 15±5 days Chatterjee et al. 2009, in preparation 26 • Optical emission is blackbody radiation from the accretion disk • Thermal optical/UV seed photons are inverseCompton scattered to X-rays by hot electrons in the corona • Modeling of the accretion disk-corona system 27 Model of the Accretion Disk/Corona System Chatterjee et al. 2009, ApJ, in press 28 X-ray and Optical model flares Disturbance is propagating toward the center Disturbance is propagating away from the center Chatterjee et al. 2009, ApJ, in press 29 Feedback in Accretion Disk/Corona System 30 X-ray and Optical Model Flares (Including Feedback) 31 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 32 Movie Time! 33 Superluminal Ejections Follow X-ray Dips in 3C 111 •X-rays are produced in the accretion disk, radio emission is from the jet •Connection between Xray and radio emission => Connection between accretion disk and jet Chatterjee et al. 2009, in preparation 34 Possible Explanation of the X-ray Dip and Superluminal Ejection Correlation Change in the magnetic field configuration in the accretion disk from turbulent to aligned absence of viscous heating causes dips in Xray production aligned B field configuration facilitates shock to move toward the jet (Livio et al. 2003) Turbulent Aligned X-ray production Weaker flow in the jet Decrease in X-ray production Increase in flow in the jet 35 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 36 The next three slides are from: Rob Fender, U. Southampton, UK. 37 The life and times of a black hole X-ray binary… X-ray Luminosity / Eddington ~1.0 source gets very bright and ‘softens’ Outburst ~0.1 ~0.01 source remains soft for some time then fades away, returning to hard X-ray spectrum <10-6 X-ray soft spectrum hard spectrum after, typically, 10+ years of relative peace, accretion rate increases Quiescence hardness As source softens, jet velocity increases abruptly, causing internal shock in jet Subsequently, soft states show no jet More powerful, hard sources have more powerful, steady jets… Faint, hard source have steady, ~1 jets 39 Luminosity / Eddington Relation to AGN ? Bright, radioquiet AGN (with old lobes?) ~1.0 Bright, Radio-loud AGN ~0.1 ~0.01 LLAGN <10-6 <10-9 X-ray Sgr A* soft hard Quiescence hardness Fundamental Plane of BH Activity (edge-on view) Merloni, Heinz & Di Matteo 2003, MNRAS, 345, 1057 41 Conclusions X-ray and optical emission from the accretion disk/corona system Corona lies within ~50 gravitational radii Similar characteristic timescale in accreting BH systems of masses 10-108 Msun Connection between accretion disk and jet Similarity with galactic black hole X-Ray Binaries: Universality of BH systems 42 Future Plans More detailed theory of the time variable emission from the accretion disk-corona system. Analysis and interpretation of X-ray binary monitoring data from SMARTS. Gamma-ray variability of blazars using Fermi data. Also related multi-wavelength data including SMARTS. More detailed theory of the time variable emission from blazar jets. 43 Time-Variability of Active Galactic Nuclei THE END 44 3C 120 X-Ray Power Spectral Density (PSD) Break Frequency =10-5 Hz Break Time Scale =2 Days 45 46 The Accretion-Disk/Corona Complex X-rays corona UV accretion disk BH Simple modeling of the above system 47 Spectral Energy Distribution of 3C 279 : Spanning 16 decades of Frequency Courtesy: Alan Marscher 48 AGN : Schematic Model Cartoon courtesy: Prof. Alan Marscher 49 X-ray light curve : Sum of model flares & real data Chatterjee et al. 2008 (ApJ, in press) 50 Optical light curve : Sum of model flares & real data Chatterjee et al. 2008 (ApJ, in press) 51 Light Curve Decomposition Chatterjee et al. 2008, ApJ, 489, 79 52 Superluminal Ejections Follow X-ray Dips in 3C 120 Chatterjee et al. 2009, ApJ, in press 53 Superluminal Ejections Follow X-ray Dips in 3C 120 Chatterjee et al. 2009, ApJ, in press 54 X-ray/37 GHz Anti-correlation (X-ray leads 37GHz by 120 days) Chatterjee et al. 2009, ApJ, in press 55 Possible Explanation of the X-ray Dip and Superluminal Ejection Correlation Corona is the base of the jet decrease in the number density of electrons at the base of the jet causes decrease in X-ray production increase in the speed of particles (continuity eqn.) => shock wave. 56