Hello everyone welcome to my lecture Revision of

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Hello everyone, welcome to my lecture Revision of Blazars’ Nature Objects with Binary Supermassive

Hello everyone, welcome to my lecture Revision of Blazars’ Nature Objects with Binary Supermassive Black Hole Bašta, M. Astronomical Institute, Academy of Sciences of the Czech Republic Supervisor: RNDr. R. Hudec, CSc. (ASU AV, CR) Consultant: doc. A. Sillanpaa (Tuorla, Finland) 06/10/2004 Seminar of the Astronomuical Institute

Outline of this lecture I will tell you. . . • • What AGN

Outline of this lecture I will tell you. . . • • What AGN and blazars are What basic properties of blazars are About our blazar sample for which we suggest supermassive binary black hole should be present How we probe the binary nature of blazars and explain the observed behavior At first, let us talk about Active galactic nuclei (=AGN). We will see that blazars are just a class of AGN. 06/10/2004 Seminar of the Astronomuical Institute

Active Galactic Nuclei (= AGN) in pictures Blazar Mkn 421 Quasar 3 C 273

Active Galactic Nuclei (= AGN) in pictures Blazar Mkn 421 Quasar 3 C 273 Seyfert galaxy NGC 5194 Radio galaxy Centaurus A 06/10/2004 Seminar of the Astronomuical Institute

Active Galactic Nuclei (= AGN) Active Galactic Nuclei (AGN) powerful luminosity; non-stellar spectrum; high

Active Galactic Nuclei (= AGN) Active Galactic Nuclei (AGN) powerful luminosity; non-stellar spectrum; high variability; BH engine; differ in luminosity, spectra, variability, morphology; 1 - 10 % of galaxies supposed to be AGN Observational classification of AGN • Quasars Quasi stellar radio sources, powerful, radio loud vs. quiet • Blazars Highly variable • Radio galaxies Powerful in radio, radio lobes, elliptical • Seyfert galaxies Spiral, luminous center, SG I vs. SG II • LINERs, Nuclear HII Regions Specific energy production • Strong IRAS & starburst galaxies Star formation 06/10/2004 Seminar of the Astronomuical Institute

Engine of AGN & AGN Unification I Radio lobes Dusty torus Black hole +

Engine of AGN & AGN Unification I Radio lobes Dusty torus Black hole + Accretion disk Coming closer to AGN Cygnus A Centaurus A Decreasing the angle between observer and jet 06/10/2004 Seminar of the Astronomuical Institute Blazar 3 C 273

Engine of AGN & AGN Unification II Quasar Blazar Radio galaxy Seyfert 2 galaxy

Engine of AGN & AGN Unification II Quasar Blazar Radio galaxy Seyfert 2 galaxy Radio loud (strong jets) Torus vs. Radio quiet (weak jets) 06/10/2004 Black hole + Accretion disk Seminar of the Astronomuical Institute Seyfert 1 galaxy Jet !!! Antonucci, 1993

Blazars & their powerful jet Jet = Beam of energetic particles and magnetic field

Blazars & their powerful jet Jet = Beam of energetic particles and magnetic field moving close to the speed of light!! Line of sight Blazar observer 06/10/2004 Supermassive black hole with accretion disc Effects of the small angle between observer and jet: • Featureless continuum • Relativistic beaming • High luminosity • Superluminal motion • Gamma rays • Rapid variability Seminar of the Astronomuical Institute

Standard model of blazar = one supermassive black hole According to the Unification model

Standard model of blazar = one supermassive black hole According to the Unification model (Antonucci, 1993) there is ONE supermassive black hole in the center of a blazar. “Standard model” = One supermassive black hole 06/10/2004 Seminar of the Astronomuical Institute

Secondary black hole However, there are quite a lot of suggestions that not ONE

Secondary black hole However, there are quite a lot of suggestions that not ONE black hole but TWO Jet are present in several blazars. . . Primary black hole Artist’s conception of a supermassive binary black hole (= BBH) system • Volonteri et al. , 2003 BBHs should be common • There is observational evidence for BBHs Accretion disk 06/10/2004 Seminar of the Astronomuical Institute

Our blazar sample for grant proposal (Part I) 1. ON 231 Possible periodicities: •

Our blazar sample for grant proposal (Part I) 1. ON 231 Possible periodicities: • 13. 6 years in optical (Liu et al. , 1995) We have gathered following suggestions for periodicity in our blazar sample. 2. Mkn 421 Possible periodicities: • 23 years in the optical band (Liu et al. , 1997) • 104 second variations in the X-ray band (Marashi et al. , 1999) 3. 0109+224 Possible periodicities: • Long-term oscillations of the base-level flux on a timescale of about 11. 6 years (Smith & Nair, 1995) 4. Mkn 501 Possible periodicities: • 23 days in the X-ray and Te. V band (Nishikawa et al. , 1999) 06/10/2004 Seminar of the Astronomuical Institute

Our blazar sample for grant proposal (Part II) 5. Mkn 766 Possible periodicities: •

Our blazar sample for grant proposal (Part II) 5. Mkn 766 Possible periodicities: • 4200 seconds in the X-ray band (Boller et al. , 2001) 6. 3 C 345 Possible periodicities: • 5 and 11 years in the optical band (Caproni & Abraham, 2004) 7. AO 0235+16 Possible periodicities: • 5. 7 years in the radio light curve (Raiteri et al. , 2001) • 2. 95 years in the optical light curve (Fan et al. , 2002) 8. 3 C 279 Possible periodicities: • 7. 1 years in the long-term near infrared light curve (Fan, 1999) • 22 -year period from movement of jet components (Abraham & Carrara, 1998) 06/10/2004 Seminar of the Astronomuical Institute

Our blazar sample for grant proposal (Part III) 9. PKS 0420 -014 Possible periodicities:

Our blazar sample for grant proposal (Part III) 9. PKS 0420 -014 Possible periodicities: • 13 -months between optical major outbursts The periodicity in the blazars may be a suggestion of binary black hole systems. (Wagner et al. , 1995) 10. 0716+714 Possible periodicities: • • • 0. 7 -year quasi-periodic ejection of VLBA components (Jorstad et al. , 2001) 12. 5, 2. 5 & 0. 14 -day periodicity of polarization in the optical band (Impey et al. , 2000) 4 -day periodicity in the optical band (Heidt & Wagner, 1996) 11. 3 C 66 a Possible periodicities: • 2. 5 years (Belokon & Babadzhanyants, 2003), 275 and 64 days in the optical band (Marchenko, 1999; Lainela et al. , 1999) 06/10/2004 Seminar of the Astronomuical Institute

Origin of Binary Black Holes (= BBHs) The origin of the binary black hole

Origin of Binary Black Holes (= BBHs) The origin of the binary black hole system is in the merging of galaxies. If each galaxy contains a supermassive black hole a binary black hole system is formed (frequent in clusters) Hibbard & van Gorkom, 1996 06/10/2004 Seminar of the Astronomuical Institute

Observational evidence for BBH systems • NGC 6240 Hubble, optical Chandra, X-ray Komossa et

Observational evidence for BBH systems • NGC 6240 Hubble, optical Chandra, X-ray Komossa et al. , 2003 • High-redshift quasars observed in pairs Q 1343. 4+2640, LBQS 0103 -2753, UM 425, . . . Komossa, 2003 True pairs x Chance alignments x Lensing effect 06/10/2004 Seminar of the Astronomuical Institute

The periods in our “grant proposal” sample of 11 blazars are not confirmed at

The periods in our “grant proposal” sample of 11 blazars are not confirmed at all as their light curves are not well-sampled and do not involve much historical data. We apply the following steps in our work: 1. Gathering of optical data • • • 2. 3. 4. 5. Photographic plate collections • Sonneberg Observatory, Germany (280 000 plates) • Harvard College Observatory, USA (600 000 plates) • UKSTU plate collection ROE Edinburgh, UK (18 000 plates) • Observatory Leiden, NL (40 000 plates) Papers Observational campaigns archives Gathering support data from other energy bands Periodicity analysis of the optical light curve An overall analysis to adopt a BBH model Establishing statistical results based on our sample of 11 blazars 06/10/2004 Seminar of the Astronomuical Institute

Possible origin of periods in blazars It is necessary to watch out for the

Possible origin of periods in blazars It is necessary to watch out for the whole spectrum behavior and for the behavior of colors and flares to be able to distinguish between different origin of periods in blazars. 06/10/2004 Seminar of the Astronomuical Institute

Blazars & support data from other bands Blazar emit their energy from radio to

Blazars & support data from other bands Blazar emit their energy from radio to Te. V band. Data in all wavelength enable to specify the nature of blazars. Spectral energy distribution of blazars 06/10/2004 Seminar of the Astronomuical Institute

Optical data gathering & Periodicity analysis Sextractor processing Sonneberg photographic plate Sextractor screenshot Modified

Optical data gathering & Periodicity analysis Sextractor processing Sonneberg photographic plate Sextractor screenshot Modified Argelander method Thousands of photographic plates ANALYSIS OF THE TIME SERIES • Stellingwerf’s method (folded light curves) • Deeming method • CLEAN algorithm • Wavelets analysis 06/10/2004 Seminar of the Astronomuical Institute Determination of magnitude of a specific object in individual plates

Violent optical variability of BL Lac on a long time scale 06/10/2004 Seminar of

Violent optical variability of BL Lac on a long time scale 06/10/2004 Seminar of the Astronomuical Institute

 • There is wide range of possible interpretations of periods found in the

• There is wide range of possible interpretations of periods found in the light curves (in different bands). We present a short introduction into the interpretation of periods using the supermassive binary black hole scenario and the following designation: q angle between jet and observer M mass of the primary BH Torbital period G Lorenz factor of the jet bapparent b 06/10/2004 m mass of the secondary BH rm separation of black holes b vjet/c z redshift Seminar of the Astronomuical Institute

Periodicity interpretation – origin in jet I Angle q between direction to observer and

Periodicity interpretation – origin in jet I Angle q between direction to observer and jet to n tio ver c e r Di obser the Periods originating in the jet can be drastically shortened due to relativistic effects and small viewing angles: Tobserved is any observed period originating in jet q of ow n l it o utf ec t o r i D e je th 06/10/2004 Time: Dt. (1 -v/c. cosq) Seminar of the Astronomuical Institute

Periodicity interpretation – origin in jet II The Lorenz factor G can be estimated

Periodicity interpretation – origin in jet II The Lorenz factor G can be estimated i. e. from superluminal motion. Apparent speeds higher than c are observed in the jet From optical or VLBI measurements Typical values of G: 10 -15 06/10/2004 Time: Dt. (1 -v/c. cosq) The max. apparent speed can be used as an estimate of G. Seminar of the Astronomuical Institute

Periodicity interpretation – origin in jet III The period observed in the jet may

Periodicity interpretation – origin in jet III The period observed in the jet may be induced i. e. by the tidal effect of the secondary black hole on the accretion disk of the primary. Figure credit: Romero, Fan & Nuza, 2003 06/10/2004 Seminar of the Astronomuical Institute

Periodicity interpretation – origin in jet IV The periods originating in the jet period

Periodicity interpretation – origin in jet IV The periods originating in the jet period may be also caused by: • knots rotating in the jet • emission from jet carried by the secondary BH • components moving in helically distorted jets 06/10/2004 Seminar of the Astronomuical Institute

Periodicity interpretation – origin in the accretion disk • While the secondary is piercing

Periodicity interpretation – origin in the accretion disk • While the secondary is piercing a channel into the accretion disk of the primary the gas gets heated and radiates. • Timing of the outbursts enables the determination of the orbital period. • Color behavior may support or reject the origin of the periodicity in disk!! The secondary BH crosses twice the disk The origin of the period in disk may be the case of blazar OJ 287: “Predicting the next outburst of OJ 287”, Valtonen, M. ; Lehto, H. . Hudec, R. ; Basta, M. . . , in preparation for Ap. J 06/10/2004 Seminar of the Astronomuical Institute

Determination of the mass of the primary via high energy data support Estimates of

Determination of the mass of the primary via high energy data support Estimates of the mass of the primary black hole can be sometimes obtained using the high energy data. g-ray e +, e - X-ray Estimating d and measuring variability timescales in gamma-ray band gives an estimate of the mass of the primary black hole. 06/10/2004 Seminar of the Astronomuical Institute

Determination of the mass of the secondary from periodicity studies Stages of evolution of

Determination of the mass of the secondary from periodicity studies Stages of evolution of a BBH system: Dynamical friction stage Non-hard binary stage Hard-binary stage Gravitational radiation stage: The loss of energy via gravitational radiation results in the orbit decay Time: Dt. (1 -v/c. cosq) Knowing Torbital , M and errors in determination of Torbital, can lead to an estimate of the upper limit of m. 06/10/2004 Seminar of the Astronomuical Institute

Predicting the next outburst of OJ 287 Valtonen, M. ; Lehto, H. ; .

Predicting the next outburst of OJ 287 Valtonen, M. ; Lehto, H. ; . . Hudec, R. ; Basta, M; . . In preparation for Ap. J We participate in a paper in preparation where a specific model was applied to the blazar OJ 287 light curve 06/10/2004 Scalegram for OJ 287 Seminar of the Astronomuical Institute

Conclusion and future plans • It is highly possible that the engine of blazars

Conclusion and future plans • It is highly possible that the engine of blazars and AGN is not associated with one supermassive black hole but with two supermassive black holes. • Periodicity studies supported by data from other energy bands and supported by spectral/color and flare behavior may help to establish a viable model. • Our studies are based on gathering the data for a larger sample of blazars and carrying out the appropriate analysis, results discussion and establishing a new model of blazar. • We have applied our approach fully already to OJ 287. The processing of other blazars is in the stage of data gathering and period analysis. 06/10/2004 Seminar of the Astronomuical Institute

References and acknowledgements Some fundamental papers Antonucci, R. : Unified models for active galactic

References and acknowledgements Some fundamental papers Antonucci, R. : Unified models for active galactic nuclei and quasar, 1993, ARA&A, 31, 473 A Bromm, V. & Loeb, A. : Formation of the first supermassive black holes, 2003, Ap. J, 596, 34 B Conway, J. E. & Murphy, D. W. : Helical jets and the misalignment distribution for core-dominated radio sources, 1993, Ap. J, 411, 89 C Conway, J. E. & Wrobel, J. M. A helical jet in the orthogonally misaligned BL Lacertae object Markarian 501, 1995, Ap. J, 439, 98 De Paolis et al. , F. : Binary black holes in Mkns as sources of gravitational radiation for space based interferometer, 2003, A&A, 410, 741 Faber, S. M. et al. : The centres of early-type galaxies with HST. IV. Central parameter relations, 1997, AJ, 114, 1771 F Fan, MNRAS, 1999, 308, 1032 Hardee. P. E. ; Cooper, M. A. & Clarke, D. A. : On jet response to a driving frequency and the jets in 3 C 449, 1994, Ap. J, 424, 126 H Katz, J. I. : A precessing disk in OJ 287, 1997, Ap. J, 478, 527 Komossa, S. : Observational evidence for supermassive black hole binaries, 2003, AIPC, 686, 161 K Komossa, S. et al. : Discovery of a binary active galactic nucleus in the ultraluminous infrared galaxy NGC 6240 using Chandra, 2003, Ap. J, 582, 15 Lehto, H. & Valtonen, M. : OJ 287 outburst structure and binary black hole model, 1996, Ap. J, 460, 207 Liu et al. , A&A, 1995, 295, 1 Magorrian, J. et al. : The demography of massive dark objects in galaxy centres, 1998, AJ, 115, 2285 M Raiteri, C. M. : Optical and radio variability of the BL Lacertae object AO 0235+16: A possible 5 -6 year periodicity, 2001, A&A, 377, 396 R Rieger, F. M. & Mannheim, K. : Implications of a possible 23 day periodicity for binary black hole models in Mkn 501, 2000, A&A, 359, 948 R Romero, G. E. ; Fan, Jun-Hui & Nuza, S. E. : The binary black hole scenario for the BL Lacertae object AO 0235+16, 2003, Ch. JAA, 3, 513 R Sillanpaa, et al. : OJ 287 – Binary pair of supermassive black holes, 1988, Ap. J, 325, 628 Smith & Nair, 1995, PASP, 107, 863 Valtaoja, E. et al. : Radio Monitoring of OJ 287 and Binary Black Hole Models for Periodic Outbursts; 2000, Ap. J, 531, 744 Villata, M. & Raiteri, C. M. : Helical jets in blazars. I. The case of MKN 501, 1999, A&A, 347, 30 V Villata, M. et al. : A beaming model for the OJ 287 periodic optical outbursts, 1998, MNRAS, 293, L 13 Volonteri, M. et al. , The assembly and merging history of supermassive black holes in hierarchical models of galaxy formation, 2003, Ap. J, 582, 559 Yu, Q. : Evolution of massive binary black holes, 2002, MNRAS, 331, 935 Y Xu, W. et al. : The bimodal distribution of misalignment angle in powerful extragalactic radio sources, 1994, cers. conf, 7 Some web references and photo credits http: //www. gsfc. nasa. gov http: //chandra. harvard. edu http: //users. rowan. edu/~polikar/WAVELETS/WTtutorial. html http: //www-glast. stanford. edu/ 06/10/2004 Seminar of the Astronomuical Institute

Last thought I expect to pass through this world but once; any good thing

Last thought I expect to pass through this world but once; any good thing therefore that I can do, or any kindness that I can show to any fellow creatures, let me do it now; let me not defer or neglect it, for I shall not pass this way again. Ettiene De Grallet My thanks and acknowledgments for the support with my scientific research and this presentation are passed to the following: René Hudec, Aimo Sillanpaa, Harry Lehto, Mauri Valtonen, Adam Hill, Filip Munz, Martin Toast Topinka, Ivana Joanne Stoklasová, Libor “Měkká koza“ Švéda, Petr Skalický, Martin “Matesí Péro” Jelínek, Petr Sobotka 06/10/2004 Seminar of the Astronomuical Institute