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UHECRs from the Jets of Black Holes

UHECRs from the Jets of Black Holes. Chuck Dermer Naval Research Laboratory Washington, DC USA charles.dermer@nrl.navy.mil. M87. Centenary Symposium 2012: Discovery of Cosmic Rays University of Denver 26-28 June 2012. Black-Hole Jet Sources and UHECRs.

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UHECRs from the Jets of Black Holes

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  1. UHECRs from the Jets of Black Holes Chuck Dermer Naval Research Laboratory Washington, DC USA charles.dermer@nrl.navy.mil M87 Centenary Symposium 2012: Discovery of Cosmic Rays University of Denver 26-28 June 2012 Black-Hole Jet Sources and UHECRs • UHECR source criteria: Blazars vs. GRBs • Leptonic models for blazars and difficulties • EM signatures of UHECRs in blazars Dermer Denver Cosmic Ray Centenary 27 June 2012

  2. UHECRs sources must have Larmor radius < source size Rules out many classes of potential UHECR sources: • flare stars, • white dwarfs, • “normal” neutron stars • Galactic sources… Hillas 1984 UHECR Size Scale Requirement Larmor radius < size scale of system (Hillas condition)

  3. UHECRs from Black Holes: GRBs and Blazars HiRes Collaboration 2008 The most energetic and powerful radiations in nature are made by particles accelerated through Fermi processes in black-hole jets powered by rotation. Possibilities: Pulsars/magnetars Structure formation shocks Particle physics candidates Radio-quiet AGNs Dormant black holes Lobes/hotspots of radio galaxies Others UHECRs are accelerated in the inner jets of black-hole jet sources

  4. Background Radiation Intensity Extragalactic Background Light (EBL) Puzzle of the origin of the Extragalactic g-ray Background (EGB)

  5. Criteria for UHECR sources: GRBs and blazars • Sources are extragalactic • Can accelerate to ultra-high energies 3. Adequate energy production rate within GZK volume • Sources within GZK radius • UHECR escape Electromagnetic signatures of UHECRs Neutrino signatures of UHECRs Abbasi et al. 2012; IceCube results for GRBs Evidence favors (radio-loud) AGN hypothesis for UHECR origin

  6. L ~1045 x (f/10-10 ergs cm-2 s-1) erg s-1 FR2/FSRQ Cygnus A Radio Galaxies and Blazars 3C 279 FR1/2: radio power/ morphology correlation; dividing line at  1042 ergs s-1(2×1025 W/Hz at 178 MHz) Mrk 421, z = 0.031 BL Lacs: optical emission line equivalent widths < 5 Å 3C 279, z = 0.538 FR1/BL Lac 3C 296 W Comae

  7. 2nd LAT AGN Catalog (2LAC) Ackermann et al. 2011 (2LAC) GeV-TeV connection Cygnus A • 2FGL (1873 sources; 1319 at |b|> 10°) 2LAC: 1017 AGNs at |b|> 10°, TS>25 2LAC Clean: 886 AGNs (46% larger than 1 LAC Clean) 2LAC threshold is ~5×10-12 erg/cm2-s • Probabilistic Association Method • Major Results: 1LAC and 2LAC • Small number of non-blazar AGNs • Redshift distributions and incompleteness • FSRQs: LSP; BL Lacs: LSPs. ISPs, HSPs • HSP BL Lac sources have harder spectra and smaller γ-ray luminosities than FSRQs

  8. Particle Acceleration to Ultra-High Energies in Relativistic Outflows Hillas condition for relativistic wind with Fermi acceleration Proper frame (´) energy density of relativistic wind with apparent power L > Lg R Maximum particle energy G Lorentz contraction:

  9. Minimum UHECR Emissivity

  10. Luminosity Density of UHECR Candidates from Fermi-LAT Data GRBs have adequate energy production rate only if baryon loading large Star-forming galaxies and radio galaxies are too weak Fermi data favors ion acceleration by BL Lacs/FR1 radio galaxies UHECR requirements GRB observations Dermer & Razzaque (2010)

  11. g-ray induced emissions Pair secondaries of g rays formed by gge+e- with photons of the extragalactic background light (EBL) e+ g e- After attenuation by the EBL: what happens to the produced pairs? Pair halos(Aharonian, Coppi, & Völk 1994) Temporal delay of bursting sources InterGalactic Magnetic Field (IGMF) (Plaga 1995,Razzaque et al. 2004; Murase et al. 2008) Angularextent of halos around blazars (Elyiv et al. 2009, Aharonian et al. 2009) Halo extent at GeV energies  measurement of IGMF SpectralTeV/GeV constraints on IGMF (Neronov & Vovk 2010; Tavecchio et al. 2010)Nondetection by Fermi of TeV blazar sources  BIGMF >~ 10-16 G

  12. EBL Effects on Blazar Spectra Dermer et al. 2011 g e+ g 2g e- lgg Measurements of IGMF >~ 10-15 G for persistent jet; >~10-18 G for jet active for observing period Origin of hard component in deabsorbed BL Lac spectra? Halo constraints from Fermi-LAT IRF studies GeV-TeV Spectral index difference DGStecker-Scully (2006, 2010) relation

  13. z = 0.047 z = 0.044 z = 0.129 z = 0.139 z = 0.186 z = 0.188 z = 0.44 z = 0.538 Finke et al. 2010

  14. UHECR-ray Induced emissions g g n,e+ e+ p0, p p g n,p 2g n,e- e- ~100 Mpc ~ Gpc UHECR protons with energies ~1019 eV make ~1016 eV e that cascade in transit and Compton-scatter CMBR to TeV energies UHECRs also deposit energy near source Essey, Kalashev, Kusenko, Beacom 2010, 2011

  15. Spectrum and Jet Physics • FSRQs: synchrotron/SSC + EC 3C 454.3 Abdo et al. 2011a Abdo et al. 2009 Mrk 501 Abdo et al. 2011b 3C 279 Hayashida et al. 2012 Mrk 421 BL Lacs: synchrotron/synchrotron self-Compton (many BL Lacs are well fit with sync/SSC model)

  16. Spectrum and Jet Physics • FSRQs: synchrotron/SSC + EC 3C 454.3 Abdo et al. 2011a Abdo et al. 2009 Mrk 501 Abdo et al. 2011b 3C 279 Hayashida et al. 2012 Mrk 421 BL Lacs: synchrotron/synchrotron self-Compton (many BL Lacs are well fit with sync/SSC model)

  17. Auger Collaboration 2009 Maximum Cosmic Ray energies in BL Lac objects Standard one-zone synchrotron/SSC model Parameters: B, d, R  c d tvar Hillas condition: • Protons accelerated to <~ 1019 eV • Composition change at 1019 eV to heavies (need escape mechanism) • Hadronic models for g rays require much larger magnetic fields Murase, Dermer, Takami, Migliori (2012)

  18. Electromagnetic Signatures of UHECRs UHECR-induced cascade in IGM Photon-induced cascade in IGM Murase, et al. 2012 Polisensky & Ricotti 2011 Predictions for CTA

  19. Location of g-ray Emission Site T. Savolainen • Location of the Emission Region • Radio-g correlations • Optical polarization angle swings: 3C 279, PKS 1510-089, OJ 287 • Rapid variability, large luminosity implies inner jet origin of g rays • The curious case of 4C +21.35 r < c G2 tvar

  20. g-ray Observations of 4C+21.35 Aleksic et al. (2011) PKS 1222+2163 = 4C+21.35, z = 0.432 Flare of 17 June 2010 MAGIC spectrum MAGIC observations • Emission over 30 minutes • Flaring on timescales of 10 minutes • Lg ~ 1047 erg/s (TeV energies) • Lg ~ 1048 erg/s (GeV energies) Black hole mass: 1.5x108 Mo (Wang et al. 2004) => extreme event MAGIC light curve Fermi-LAT and MAGIC spectrum Tanaka et al. (2011) 21

  21. g-ray Observations of 4C+21.35 Aleksic et al. (2011) PKS 1222+2163 = 4C+21.35, z = 0.432 Flare of 17 June 2010 MAGIC spectrum MAGIC observations • Emission over 30 minutes • Flaring on timescales of 10 minutes • Lg ~ 1047 erg/s (TeV energies) • Lg ~ 1048 erg/s (GeV energies) Black hole mass: 1.5x108 Mo (Wang et al. 2004) => extreme event MAGIC light curve Fermi-LAT and MAGIC spectrum Tanaka et al. (2011) 22

  22. Pair Production and Photohadronic Opacity Dermer, Murase, Takami, 2012, in press Detection of 40-700 GeV g rays  x > 3×1018 cm →←

  23. Neutron Production Spectrum from the Acceleration of UHECR Protons in the Inner Jet Warm dust (Spitzer; Malmrose et al. 2011) Cool dust Ly a Scattered accretion-disk radiation Two peaks s=2.1 Neutron decay length

  24. Neutrino Production Spectrum Pion-decay and beta-decay neutrinos Need ~> 10-3 erg/cm2 neutrinos for IceCube detection 1049 erg/s × 3600 s /4pdL2 = 6x10-4 erg/cm2 PeV neutrino sources are flaring g ray FSRQs with VHE emission: 4C +21.35, 3C 279, PKS 1510-089

  25. Cascade Radiation Spectrum γ-ray spectra formed by a neutron beam generated in the inner jet. MAGIC data are also overlaid, which have been deabsorbed using a low intensity model of the EBL (Domınguez et al. 2011). GeV radiation made in BLR Outflowing UHECR neutrons make photopion secondaries Synchrotron emission from ultra-relativistic leptons More rapid variability at higher energies (> 100 GeV) More rapid variability at lower energies (< 1 GeV) New mechanism for ultra-short variability (blast wave vs. directed electrons/particle beam) Variability depends on magnetic field at the pc scale r >> c G2 tvar

  26. Extragalactic g-ray Background (EGB) Ajello et al. 2012 z EGB (PRL 2010) does not include point source fluxes observed during first 10 months of Fermi mission. Anti-hierarchical behavior Seen in radio sources, radio-quiet AGNs, but not BL Lacs Luminosity Downsizing FSRQs make 9.3% +1.6% - 1.0% (+- 3% systematic) of Fermi isotropic emission

  27. Fit EGB to 600 GeV with UHECR-induced emissions Murase, Beacom, Takami 2012 Cascade radiation from UHECR sources with different star formation histories: constant (left), as the Hopkins-Beacom SFR (right)

  28. Conclusions Sources of UHECR sources are radio-loud AGNs/radio galaxies/g-ray blazars Inner jets of blazars accelerate UHECRs, making an escaping neutron/neutrino beam and hadronic contribution to spectrum Helps resolve puzzles in blazar g-ray studies: Deabsorbed spectra of distant (z > 0.1) TeV blazars show unexplained emission component DG = GGeV – GTeV relation violated Location of g-ray emitting regions in blazars puzzling May account for high-energy deficit in extragalactic background light Hadronic cascade scenario can be distinguished from leptonic scenarios by observing g rays above 25 TeV in 1ES 0229+200 with CTA Predict composition change to heavies at ~1019 eV Detection of PeV neutrinos from VHE FSRQs/TeV BL Lacs with IceCube/KM3NeT Dermer Denver Cosmic Ray Centenary 27 June 2012

  29. Limits to the Extreme Universe arXiv:1202.2814

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