Tadayuki Takahashi Institute of Space and Astronautical Science (ISAS) Spectral and Temporal Variations of Blazars Hidetoshi Kubo(Kyoto), Jun Kataoka (Tokyo.

Slides:



Advertisements
Similar presentations
Connection between the parsec-scale radio jet and γ-ray flare in the blazar Venkatessh Ramakrishnan Aalto University Metsähovi Radio Observatory,
Advertisements

OBSERVATIONS OF AGNs USING PACT (Pachmarhi Array of Cherenkov Telescopes) Debanjan Bose (On behalf of PACT collaboration) “The Multi-Messenger Approach.
Longterm X-ray observation of Blazars with MAXI Naoki Isobe (Kyoto University; & MAXI
Determining the location of the GeV emitting zone in fast, bright blazars Amanda Dotson, UMBC Markos Georganopoulos (advisor), UMBC/GSFC Eileen Meyer,
Multiwavelenth Observations Of Strong Flares From The Tev Blazar 1ES Reporter: 倪嘉阳 Arthor:H.Krawczynski, S.B. Hughes
Modeling the SED and variability of 3C66A in 2003/2004 Presented By Manasvita Joshi Ohio University, Athens, OH ISCRA, Erice, Italy 2006.
Constraints on Blazar Jet Conditions During Gamma- Ray Flaring from Radiative Transfer Modeling M.F. Aller, P.A. Hughes, H.D. Aller, & T. Hovatta The γ-ray.
1 The Multi-Messenger Approach to Unidentified Gamma-Ray Sources Morphological and spectral studies of the shell-type supernova remnants RX J
Electron thermalization and emission from compact magnetized sources
Naoki Isobe, Yoshihiro Ueda (Kyoto University) Kousuke Sugimori, Nobuyuki Kawai (Tokyo Tech.) Hitishi Negoro (Nihon Univ.) Mutsumi Sugizaki, Masaru Matsuoka.
GRB Afterglow Spectra Daniel Perley Astro September* 2005 * International Talk Like a Pirate Day.
1 Origin of Variability of X-ray and γ-ray Spectra on Daily Scale Radovan Milinčić Astrophysics 711 May 3 rd 2005.
The GLAST Telescope Network Involvement for students and teachers in the science of the GLAST mission.
Astrophysical Jets Robert Laing (ESO). Galactic black-hole binary system Gamma-ray burst Young stellar object Jets are everywhere.
Outflow Residual Collisions and Optical Flashes Zhuo Li (黎卓) Weizmann Inst, Israel moving to Peking Univ, Beijing Li & Waxman 2008, ApJL.
Numerical Modeling of Electromagnetic Radiation from AGN Jets Based on  -ray emission and spectral evolution of pair plasmas in AGN jets Bottcher et al.
Hiroyasu Tajima Stanford Linear Accelerator Center Nov 3–8, 2002 VERTEX2002, Kailua-Kona, Hawaii Gamma-ray Polarimetry ~ Astrophysics Application ~
Extragalactic Jets and GLAST Łukasz Stawarz KIPAC, Stanford University.
Zhang Ningxiao.  Emission of Tycho from Radio to γ-ray.  The γ-ray is mainly accelerated from hadronic processes.
Theory of TeV AGNs (Buckley, Science, 1998) Amir Levinson, Tel Aviv University.
Multi-wavelength AGN spectra and modeling Paolo Giommi ASI.
July 2004, Erice1 The performance of MAGIC Telescope for observation of Gamma Ray Bursts Satoko Mizobuchi for MAGIC collaboration Max-Planck-Institute.
1 Arecibo Synergy with GLAST (and other gamma-ray telescopes) Frontiers of Astronomy with the World’s Largest Radio Telescope 12 September 2007 Dave Thompson.
Astrophysics With the Cherenkov Telescope Array P. Coppi (for F. Aharonian, MPIK, Heidelberg)
ATCA monitoring of Sgr A* at 3 millimeter Juan Li Shanghai Astronomical Observatory 2009/10/22 Collaborators: Z.Q. Shen (Shao.), A. Miyazaki (NAOJ), L.
Long-term monitor on Mrk 421 using ARGO-YBJ experiment S.Z Chen (IHEP/CAS/China, On behalf of the ARGO-YBJ collaboration  1. Introduction.
High energy emission from jets – what can we learn? Amir Levinson, Tel Aviv University Levinson 2006 (IJMPA, review)
Studying emission mechanisms of AGN Dr. Karsten Berger Fermi School, June ©NASA.
The jet of Mrk 501 from millions of Schwarzschild radii down to a few hundreds Marcello Giroletti INAF Istituto di Radioastronomia and G. Giovannini, G.
Blazars and Neutrinos C. Dermer (Naval Research Laboratory) Collaborators: A. M. Atoyan (Universite de Montreal) M. Böttcher (Rice University) R. Schlickeiser.
High energy Astrophysics Mat Page Mullard Space Science Lab, UCL 6. Jets and radio emission.
Time dependent modeling of AGN emission from inhomogeneous jets with Particle diffusion and localized acceleration Extreme-Astrophysics in an Ever-Changing.
STATISTICAL ACCELERATION and SPECTRAL ENERGY DISTRIBUTION in BLAZARS Enrico Massaro Physics Department, Spienza Univ. of Roma and Andrea Tramacere ISOC,
19/02/09ARC Meeting, Colonster The Simbol-X mission and the investigation of hard X-rays from massive stars Michaël De Becker (Groupe d'AstroPhysique des.
Lunch discussion on motivations for studying blazar variability Greg Madejski, SLAC Parts of this presentation use slides by Benoit Lott and Jun Kataoka.
High energy radiation from extragalactic jets and prospects for GLAST Greg Madejski Stanford Linear Accelerator Center and Kavli Institute for Particle.
1 Juri Poutanen University of Oulu, Finland (Stern, Poutanen, 2006, MNRAS, 372, 1217; Stern, Poutanen, 2007, MNRAS, submitted, astro- ph/ ) A new.
Determining the location of the GeV emitting zone in fast, bright blazars Amanda Dotson, UMBC Markos Georganopoulous, UMBC/GSFC Eileen Meyer, STScI MARLAM.
ASTR 113 – 003 Spring 2006 Lecture 11 April 12, 2006 Review (Ch4-5): the Foundation Galaxy (Ch 25-27) Cosmology (Ch28-29) Introduction To Modern Astronomy.
Acceleration and Energy Transport in the AGN jets: from sub-pc to kpc scale Jun Kataoka Tokyo Institute of Technology - Acceleration site in the universe.
Radio galaxy Elliptical Fanaroff-Riley type I “Misaligned” BL Lac (~ 60  ) Distance 3.5 Mpc Parameter Value  (J2000) 201   (J2000) -43 
BL LAC OBJECTS Marco Bondi INAF-IRA, Bologna, Italy.
Probing the Inner Jet of the Quasar PKS 1510  089 with Multi-waveband Monitoring Alan Marscher Boston University Research Web Page:
Multi-Zone Modeling of Spatially Non-uniform Cosmic Ray Sources Armen Atoyan Concordia University, Montreal FAA60 Barcelona, 7 November 2012.
Gamma-rays, neutrinos and cosmic rays from microquasars Gustavo E. Romero (IAR – CONICET & La Plata University, Argentina)
Jets Two classes of jets from X-ray binaries
The Quasar : A Laboratory for Particle Acceleration Svetlana Jorstad IAR, Boston U Alan Marscher IAR, Boston U Jonathan Gelbord U. Durham Herman.
Modeling the Emission Processes in Blazars Markus Böttcher Ohio University Athens, OH.
From the Black Hole to the Telescope: Fundamental Physics of AGN Esko Valtaoja Tuorla Observatory, University of Turku, Finland Metsähovi Radio Observatory,
Structure of jet cores in blazars:  -ray observations Greg Madejski Stanford Linear Accelerator Center and Kavli Institute for Particle Astrophysics and.
Blazars: the gamma-ray view of AGILE on behalf of the AGILE WG-AGN Filippo D’Ammando Università degli Studi di Roma “Tor Vergata” INAF - Istituto di Astrofisica.
The X-ray Universe 2008, Granada, May A Jet-Emitting Disk model for the microquasar broad band emission G. Henri Coll. P.O Petrucci, J. Ferreira,
The hard X-ray Extra-Galactic sky with INTEGRAL/IBIS High-z QSOs A.De Rosa on behalf of the INTEGRAL/AGN survey team.
Gamma-Ray Burst Working Group Co-conveners: Abe Falcone, Penn State, David A. Williams, UCSC,
Multi - emission from large-scale jets Fabrizio Tavecchio INAF – Osservatorio Astronomico di Brera.
QUASAR-MICROQUASAR ANALOGY The scales of length and time are proportional to M BH R sh = 2GM BH /c 2 ;  T  M BH Unique system of equations: The maximum.
Modeling the SED and variability of 3C66A in Authors: Manasvita Joshi and Markus Böttcher (Ohio University) Abstract: An extensive multi-wavelength.
Masaki Yamaguchi, F. Takahara Theoretical Astrophysics Group Osaka University, Japan Workshop on “Variable Galactic Gamma-ray Source” Heidelberg December.
The non-thermal broadband spectral energy distribution of radio galaxies Gustavo E. Romero Instituto Argentino de Radio Astronomía (IAR-CCT La Plata CONICET)
The prompt optical emission in the Naked Eye Burst R. Hascoet with F. Daigne & R. Mochkovitch (Institut d’Astrophysique de Paris) Kyoto − Deciphering then.
Implications of VHE Emission in Gamma-Ray AGN Amir Levinson, Tel Aviv University.
Fermi Several Constraints by Fermi Zhuo Li ( 黎卓 ) Department of Astronomy, Peking University Kavli Institute of Astronomy and Astrophysics 23 August, Xiamen.
Tobias Jogler Max-Planck Institut für Physik IMPRS YSW Ringberg 2007 VHE emission from binary systems Outline Binary systems Microquasar Pulsar binaries.
Radio Loud and Radio Quiet AGN
Gamma Rays from the Radio Galaxy M87
Alessandro Buzzatti Università degli Studi di Torino / SLAC
Observation of Pulsars and Plerions with MAGIC
Junior Research Fellow,
MAXI Status and ISS Science
Extragalactic Jets and GLAST
Presentation transcript:

Tadayuki Takahashi Institute of Space and Astronautical Science (ISAS) Spectral and Temporal Variations of Blazars Hidetoshi Kubo(Kyoto), Jun Kataoka (Tokyo IT), Chiharu Tanihata (ISAS)

Cosmic-ray and Particle Accelerator Where are accelerators? What ’ s the maximum energy? How powerful? “ Black Holes ” are important players? Blazars are ideal objects to study the behavior of particle accelerators at the bottom of Jets 3C46 (1.4 GHz) core (AGN) + inner jet knot lobe hot spot Yes:AGN Cosmic Ray Spectrum

Gamma-ray Blazars Gamma-rays –Direct evidence of the existence of GeV/TeV particles –the emitting source cannot be too compact too close to important sources of X-ray photon (e.g. a hot accretion disk corona close to the black hole) to avoid γγ-> e + e - EGRET sky map of AGNs TeV detection Third EGRET AGN Catalogue

Mrk 421 Takahashi et al. 1996,1999 Macomb et al ASCA Whipple (TeV) EGRET X-Gamma Correlations X and γ-rays are cospatial Takahashi et al Fossatti et al. 2003

Gamma-ray Blazars produced in relativistic jets pointing close to the line of sight observer  BLK  Enhancement by Relativistic Beaming (L obs 〜 L  4 )  BLK  cos  Dominated by non-thermal highly variable broad-band radiation High Power Small Emax Low Power High Emax Kataoka 2002 Fit to Spectral Energy Distribution (SED) -> Parameters of Accelerators b ased on the assumption of –Synchrotron –Inverse Compton Sync. Photon (and External) Peak frequency relations Lumunosity relations

Solve “ Parent ” electron distribution from the spectra Self-consistent analysis can constrain –Size –Magnetic Field –Beaming Factor –Electron Distribution (Kinetic Power) X-ray band is sensitive to γmax and γmin  max = x10 5  min = 1  min = 1000 X-ray

Temporal Variations (TeV Blazars) at the maximum end of electron distribution Takahashi et al time (x 10,000 s) cnts/s 1day 2000 ASCA ’ s Long-look Observation (Still Difficult for XMM/Chandra) Daily Flare Shape : almost symmetric : Light Crossing Effect in the blob (not the effect of cooling/acceleration time constant) Offset Component (pedestal)

Spectral Variations (TeV Blazars) at the maximum end of electron distribution Kataoka et al Tanihata et al Takahashi et al. 2000

Acceleration/Cooling High if shock velocity ( v s) is high or  is high  cool (Obs. Frame) B=0.1 Gauss  = keV … 17,000 s 5 keV … 5,000 s (at X-rays) Flare light curve is symmetric. No energy dependence found in rise/decay.

Time dependent treatment Time dependent modeling is important to study the spectral evolution (but available only very recently) –time scale of Acceleration and Cooling Escape (Kirk et al. 1999, Kataoka et al. 2000, Krawczynski et al. 2002) Predicts characteristic spectral evolution (such as “ soft lag/hard lag ” ), from the balance between  acc and  cool. New Component (ex. with higher γmax) Kataoka 2000 B=0.1 gauss R=10 16 cm 3 … Flare Light Curve Injection escape Solve the time evolution of electrons

t var Characteristic Time Scale 1 day Mrk421 Mrk501 PKS Daily flares are commonly observed -Characteristic time scale : t var 〜 40ks - 100ks - -Both -Structure Function -PSD analysis indicate time variablity <tvar is greatly suppressed for t < t var R 〜 ct var  〜 [cm]

Internal Shocks day variability roughly corresponds to 10 Rg for 10 9 M (Rees 1978 Ghisellini 1999, Spada et al Kataoka et al. 2001) D ~  BLK 2 D 0 ~ [cm] R ~  BLK D 0 ~ [cm] d ~ 2D 0 B.H. shock    BLK  (Kataoka et al. 2001, Iwashimizu et al. 2003) Fast shell catches up the slow shell Link to the Characteristic time scale of the ejection from BH. Variablity

Light Curve Simulation - Blobs mainly collide at D ~ D 0 = [cm] -  m = 10,    D 0 = 3×10 13 [cm] - Only the flares due to collisions at the smallest distance will be appeared as “shots (daily flares)” Day-by-day flares Internal Energy Flare time-scale (ksec) No. of flares offset log D (cm) Time F large  OFFSET smaller  structure function offset component Tanihata et al. 2003

Simulation Observation EUVE 1keV 6.3keV 15keV R fo =0.7, T chr =40 ks ⇒ D 0 =1x10 13 cm  G  =0.015,  =15 (assumed) -> very narrow distribution is required Light Curve (Flare, Energy dependent Amplitudes, SF/PSD are OK. Efficiency <0.01 % Application to Mrk 421 Similar Analysis by Guetta et al provides Efficiency < several % still small assumption Energy carried out by the form of Jet does not go into electron acceleration/radiation

One more issue to tackle with Absorption effect (TeV γ) by Diffuse Extragalactic Background Radiation F. Aharonian 2003 Need to correct TeV spectra for the SED fitting, if the emission exceeds several TeV

Re-visiting SED Analysis D B.H. shock Takahara et al. (Poster 81) 1. IR absorption corrected for TeV spectra (important) 2. Fit quiescent phase to determine parameters. Use higher  for flare, scale other parameters with  3. Collision takes place at longer distance for larger  4. maximum energy is higher for larger  Quiescence δ=12, B=0.12G δ=37, B=0.012G Flare in 2000 for Mrk 421 Flare Change of the parameters of accelerator ? Another approach to fit FLARE

Paradigm Shift Inhomogenious Model (continuous flow) Before CGRO/TeV/ASCA Homogenious One Zone Model After X-Gamma Correlation Time-Dependent One Zone Model After Detections of Flare & Spectral Evolution Time Dependent (Internal Shocks) Multi Zone? After Characteristic Time Scale (Daily Flare)

Future Observations ISAS GLAST 2006 AstroE2 GLAST Kataoka et al GLAST SKY ? poster by Fukazawa et al.

Conclusion We have a fairly good understanding of Blazar Spectra (Parameters of Accelerators); u e >u B X-ray/TeV correlations give strong constraint on the model Low Efficiency in sub-pc jets (Blazar emission) –Most of the energy carried out from BH is transported to kpc- jets and Lobes (See Poster 32 by Kataoka) Shift of Paradigm Time Dependent Model is indispensable Internal Shock Model (Multi Zone?) Need sensible and Detector in hard-X and Gamma

Narrow FOV Compton Telescope for the NeXT mission in Japan –Stack Configuration Low Energy 24 layers of Strip Strip detectors (res. 400μm) and 6 mm thick CdTe Pixel (res. 1mm) –High Energy Resolution of <1 - 3 keV BGO Incident angle of γ-rays are defined by a well-type active collimator (Extremely Low Background) ISAS