Structure of jet cores in blazars:  -ray observations Greg Madejski Stanford Linear Accelerator Center and Kavli Institute for Particle Astrophysics and Cosmology In collaboration with: Jun Kataoka, Tad Takahashi, Marek Sikora, Rie Sato, Lukasz Stawarz, Masayoshi Ushio, others Context: blazars as active galaxies with dominant relativistic jet Main questions: structure, acceleration, collimation, and content of the jet, -> all inferred from radiative processes via broad-band spectra Recent Suzaku observations of blazars: signature of “bulk-Compton” process in PKS ? X-ray spectral shape of Mkn 421 & distribution of radiating electrons Future: GLAST

Mkn 421; data from Macomb et al Context: extragalactic jets and their  -ray emission Jets are powered by accretion onto a massive black hole – the details of the energy conversion process are still poorly known but  -rays often energetically dominant: blazar phenomenon Gamma-ray emission often extends to the TeV region All inferences hinge on the current ”standard model” – broad-band radiation is due to the synchrotron & inverse Compton processes We gradually are developing a better picture of the jet (content, location of the energy dissipation), but how are the particles accelerated? Where? Protons or electrons? – are still open questions Variability (simultaneous broad-band monitoring) can provide crucial information about the structure and content of the innermost jet, relative power as compared to that dissipated via accretion, … X-ray variability of Mkn 421 (Takahashi et al. 1996)

Another example: archetypal GeV blazar 3C279, ‘96 flare Correlated variability on day time scales is common Variable emission presumably arises in the innermost regions of the jet (but this is arguable…) Variability in X-ray and  -ray bands puts constraints on the minimum relativistic boost (  j ) of the innermost region (via  absorption to e+/e- pair production) Lorentz factors  j of jets inferred from VLBI (multi-parsec scales) can be compared against  j inferred from variability (sub-parsec scales) ->  j as a function of distance from the black hole? - > constraints on acceleration process of the jet Data from Wehrle et al Data from Jorstad et al. 2000

Suzaku observations of PKS : hard power law + “soft excess” Suzaku observed a number of blazars - the list includes many detected by EGRET and TeV observatories Generally, the X-ray spectra of EGRET blazars are very hard power laws (energy indices often < 0.5), extending into the HXD PIN energy range (contrast to TeV blazars) Very difficult to explain such hard spectra! Interesting recent result is for PKS , a blazar at z ~ 0.3 for 120 ks (joint observation of Jun Kataoka & GM; Kataoka+ 2008) Spectrum is a hard power law (energy index  ~ 0.2), but with a soft X-ray “excess” below ~ 1.5 keV, best described as a steep power law or a thermal component with kT ~ 0.2 keV Explanation as a “tail” of the synchrotron emission unlikely – extrapolation does not work Too hot to be the tail of the “blue bump”

Suzaku observations of PKS : possible evidence for “bulk-Compton” bump -> constraints on the jet content? This soft excess might be the tentative evidence for the “Sikora bump” – arising by the inverse Compton scattering of BEL light by the cold electrons comoving in the relativistic jet (E bump ~ E(Ly  ) x  2 ~ 1 keV) Even if it is not “bulk-Compton”… From its isotropic luminosity of L BC < 3 x erg/s - we can set a limit on the energy flux L e,cold carried by the cold electrons and the e+/e- pair content of the jet: -since L BC = (4  T /3m e c 2 ) U BEL r BLR  j 3 L e,cold we have L e,cold < 2.7x10 43 (r BLR /0.1pc) (  j /10) -3 (L BEL /10 45 erg/s) -1 erg/s - Significantly less than the required kinetic luminosity of the jet - Now the total power delivered by the jet must be 8x10 44 erg/s -With more realistic parameters, n e /n p in the jet is < 5 --> Jet contains more pairs than protons, but cannot be dynamically dominated by e+/e- pairs -For details, see Kataoka+ 2008

Another recent example: Mkn 421 observed with Suzaku time [sec] XIS 0.6~10keV PIN 12~40keV count/sec (1day)(0day)(0.5day) Mrk 421 Ushio, GM, + 08 in preparation 6 * Broad-band X-ray spectrum measured by Suzaku cannot be described as a simple power law Instead, the index steepens with increasing energy Assuming constant B field, steepening electron distribution is implied Best fitted with power-law electron distribution (index ~ 2.2), with super-exponential cutoff (as inferred for some SNR; Tanaka et al. 2008) Such a cutoff is predicted in, e.g., radiating relativistic electrons that were accelerated in turbulent B field (see, e.g., Stawarz and Petrosian 2008) Applicable to many blazars where the X-ray band represents the high-energy tail of the synchrotron peak (often the “TeV blazars”)

EGRET All Sky Map (>100 MeV): precursor to GLAST Cygnus Region 3C279 Geminga Vela Cosmic Ray Interactions With ISM LMC PKS PKS Crab PSR B

Rocket Fairing installation around GLAST

GLAST Launch Launch from Cape Canaveral Air Station 11 June 2008 at 16:05PM UTC Circular orbit, 565 km altitude (96 min period), 25.6 deg inclination. Communications: –Science data link via TDRSS

GLAST is in orbit! Schematic principle of operation of the GLAST Large Area Telescope  -rays interact with the hi-z material in the foils, pair-produce, and are tracked with silicon strip detectors * The instrument “looks” simultaneously into ~ 2 steradians of the sky * Energy range is ~ GeV, with the peak effective area of ~ 12,000 cm 2 - allows an overlap with TeV observatories Why SLAC? clear synergy with particle physics: - particle-detector-like tracker/calorimeter - potential of discovery of dark matter particle

GLAST observing strategy & performance: angular resolution, broad-band sensitivity (1 year) 100 s 1 orbit 1 day LAT 1 yr cm -2 s -1 3EG  limit 0.01  0.001

Engineering Data: Single Events in the LAT The green crosses show the detected positions of the charged particles, the blue lines show the reconstructed track trajectories, and the yellow line shows the candidate gamma-ray estimated direction. The red crosses show the detected energy depositions in the calorimeter.

GLAST LAT has much higher sensitivity to weak sources, with much better angular resolution GLAST EGRET

Example of flaring activity of blazars: Recent outburst of 3C454.3 Objects subject to intensive monitoring (=GLAST LAT  -ray flux history will be available, no special repointing): 3C273NRAO 530 3C2791ES PKS OJ 287 3C PKS PKS Mkn 421 PKS BL Lacertae PKS Mkn W Com ( ) … GLAST flux limit for reporting of “major flares”: 2 x photons/cm 2 /s (E>100 MeV)

Clusters of galaxies with GLAST and NuSTAR From Markevitch et al. (X-ray data: 2004, 2005); Clowe et al. NuSTAR schematic: SMEX; (lensing data: 2004), and Bradac et al (S+W lensing)sensitive hard X-ray (10-80 keV) telescope system; launch What are details of formaton of clusters? Non-thermal processes? Jet-cluster interaction? Best studied in hard X-rays or  -rays: inverse Compton of CMB or thermal X-ray photons against cluster’s relativistic particles