Blazars and Neutrinos C. Dermer (Naval Research Laboratory) Collaborators: A. M. Atoyan (Universite de Montreal) M. Böttcher (Rice University) R. Schlickeiser (Bochum U.) Erice, June 2002 “Transformation Properties of External Radiation Fields, Energy Loss Rates and Scattered Spectra, and a Model for Blazar Variability,” CD and R. Schlickeiser, ApJ, in press, August 20 th, 2002 (astro-ph/020280) “High Energy Neutrinos from Photomeson Processes in Blazars,” A. Atoyan and CD, PRL, 87, 22, 1102 (2001) “An Evolutionary Scenario for Blazar Evolution,” M. Böttcher and CD, ApJ, 564, 86 (2002) “X-ray Synchrotron Spectral Hardenings from Compton and Synchrotron Losses in Extended Chandra Jets” 2002, CD and A. Atoyan, ApJ Letters, 2002, 568, L81

Outline 1.Introduction 1.Radio Galaxies 2.Blazars 3.Standard Blazar Model 2.Leptonic Models 1.Radiation Processes (see Dermer and Schlickeiser 2002) 2.Electron Injection and Energy Losses 3.Model for Blazar Evolution 3.Hadronic Models 1.Photomeson Production 2.Neutrino Detection 3.Neutral Beam Formation 4.Extended Jets

The Evolution of Active Galaxies The nuclear activity in a galaxy evolves in response to the changing environment, which itself imprints its presence on the spectral energy distribution of the galaxy. External Photon field  FSRQs, Intense n,  beam p +  p +  0 |  n +  + |  2     eV  Rays, cascade FR IIs Dilute clouds  BL Lac objects Low luminosity Weak jet  ’s FR Is 

FR I: low luminosity, twin jet sources Cyg A 3C 2963C 465 FR II: high luminosity, lobe dominated Radio Galaxies Fanaroff-Riley (1974) Classification Scheme FR I: separation between the points of peak intensity in the two lobes is smaller than half the largest size of the source – Edge-darkened, twin jet sources FR II: separation between the points of peak intensity in the two lobes is greater than half the largest size of the source. – Edge-brightened hot spots and radio lobes, classical doubles Morphology correlates strongly with radio power at 2x10 25 W/Hz at 178 MHz (  4x10 40 ergs s -1 ), or total radio power of  ergs s -1 Optical emission lines in FR IIs brighter by an order of magnitude than in FR Is for same galaxy host brightness 3C 173.1

Blazars Blazars (see lectures by R. Sambruna for more detail) Class of AGNs which includes optically violently variable quasars; highly polarized quasars, flat spectrum radio sources, superluminal sources BL Lac objects – nearly lineless (equivalent widths < 5 Å:  dilute surrounding gas) Flat Spectrum Radio Quasars (strong emission lines:  dense broad line region clouds) Blazars: radio galaxies where jet is pointed towards us; radio galaxies = misaligned blazars FR Is are parent population of BL Lac objects; FR IIs are parent population of FSRQs L ~5x10 48 x (f/10 -9 ergs cm -2 s -1 ) ergs s -1 L ~10 45 x (f/ ergs cm -2 s -1 ) ergs s -1 Mrk 421, z = C 279, z = (Urry and Padovani 1995)

Blazar SED Sequence E pk of synchrotron and Compton components inversely correlated with L Sambruna et al. 1996; Fossati et al Finding an order in the SEDs of blazars FSRQ BL Lac

Standard Blazar Model Dermer and Schlickeiser 1994  -2 ≡ (  sc /0.01) Nonthermal electron synchrotron and Compton processes Various sources of soft photons Relativistic motion accounts for lack of  attenuation

Multiwavelength Blazar Spectra Leptonic processes: Nonthermal synchrotron radiation Synchrotron self-Compton radiation, Accretion disk radiation Disk radiation scattered by broad-line clouds

Blazar Variability Location of gamma-ray production site can be measured with GLAST

Blazar Sequence Comparison Evolution from FSRQ to BL Lac Objects in terms of a reduction of fuel from surrounding gas and dust FSRQ BL Lac

What about Nonthermal Protons and Ions? Nonthermal particles; Intense photon fields Importance of external radiation field for photomeson production in FSRQs  Strong photomeson production

B and  Photomeson Neutrino Production Calculations   )  640 K 1  0.2  = 380  b K 2   = 120  b     B eq B ob Tavecchio ; Atoyan and Dermer 2001

Nonthermal Proton Spectrum Nonthermal proton power corresponds to average  –ray luminosity measured from 3C 279 Unlikely to produce UHECRs in the inner jets of blazars Proton power based on 3-week average spectral fluxes from 3C 279 in 1996 (Wehrle et al. 1998)

Photomeson production energy-loss timescale Different Doppler factors  = 15  = 10  = 7 photomeson energy- loss timescales in observer frame for properties derived from 3-week average spectral fluxes from 3C 279 in 1996 (Wehrle et al. 1998) t var = 1 day compare case with no external field Atoyan and Dermer 2001

Evolution of the proton distribution  = 7 1 day 3 day, 10 day, 21 day, 30 day

Energy Distributions of Relativistic Protons Different Doppler factors  = 15  = 10  = 7 Proton distribution after 3 weeks, with and without external field Dots: no neutron escape Nonthermal proton accumulation

Neutrino and  -Ray Fluences Different Doppler factors  = 15  = 10  = 7 Neutrino and  -ray fluences from 3C 279 based on 3-week average spectral fluxes observed in 1996 (Wehrle et al. 1998), with t var = 1 day

Evolution of the Neutrino Flux  = 7 1 day 3 day, 10 day, 21 day, 30 day

3-week average Neutrino Fluxes Different Doppler factors Neutrino fluxes from 3C 279 based on 3-week average spectral fluxes observed in 1996 (Wehrle ), with t var = 1 day Compare average  -ray fluxes observed during this time:   5x ergs cm -2 s -1 ~ 10% efficiency in neutrinos compared to  rays what is k pe ?  = 15  = 10  = 7

Astronomy High Energy Neutrino Physics 

X-rays from the Outer Jet Sambruna et al Wilson et al Wilson et al Schwartz et al. 2000; Chartas et al Pictor A Cygnus A 3C 273 PKS Pair halos (Aharonian, Coppi, and V ö lk 1994

Neutrino detection with km 2 exposure Three week average P P   100 TeV    Gaisser, Halzen, and Stanev  No neutron escape No external radiation field

Neutrino detection with km 2 exposure Parameters derived from 2 day flare of 3C 279 in 1996 ; t var = 1 day  No neutron escape No external radiation field Predict FSRQ sources of high energy neutrinos

Electromagnetic Cascade n,  Hot Spot Photons with energies > 100 TeV are attenuated by CMB and DIIRF background and materialize into e + -e - pairs and produces electromagnetic cascade Neutron beam more highly directed than jet plasma; pre-accelerates IGM in FSRQs; Difference between FR I and FR II galaxies Some beam energy is reprocessed into  rays through Compton scattering, forming pair halos around radio-loud AGN (Aharonian, Coppi, & Völk 1994) Rest of beam energy emerges as X-ray synchrotron jet Larger magnetic field in hot spot reprocesses directed electron-positron beam energy into synchrotron radiation ? Blazar energy in TeV range injected into IGM IGM n,  Inner Jet SMBH

Evolution of Luminous and Active Galaxies

Evolution of Blazars

will be tested by Neutrino Telescopes (Neutrinos from FSRQs rather than BL Lacs) and Gamma Ray Telescopes (  -ray halos around FR II galaxies, but not around FR I galaxies; Statistics of BL Lacs and FSRQs) Radio Jet Formation Scenario

Galaxy Evolution Dark matter halos collapse from initial spectrum of density fluctuations Press-Schechter formalism for collapse on different mass scales Hierarchical structure formation (bottom-up) Cluster accretion and subcluster interactions Infrared luminous galaxies Galaxy mergers and fueling: evolution of active galaxies Black Hole/Jet Physics Formation of jets in FR II and FRI radio galaxies: importance of neutral beams Extended X-ray emission from jet sources Neutrino and  -ray test

Sensitivity of High Energy Telescopes Chandra ASCA HESS