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The Strange Case of the Blazar 4C +21.35 (aka PKS 1222+216)

The Strange Case of the Blazar 4C +21.35 (aka PKS 1222+216). Paris Observatory Meudon, France 27 March 2012. Charles Dermer Naval Research Laboratory Washington, DC USA charles.dermer@nrl.navy.mil. Blazar Physics: Black Holes and UHECRs. VHE from FSRQs (third after 3C 279, PKS 1510-089)

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The Strange Case of the Blazar 4C +21.35 (aka PKS 1222+216)

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  1. The Strange Case of the Blazar4C +21.35 (aka PKS 1222+216) Paris Observatory Meudon, France 27 March 2012 Charles Dermer Naval Research Laboratory Washington, DC USA charles.dermer@nrl.navy.mil Blazar Physics: Black Holes and UHECRs • VHE from FSRQs (third after 3C 279, PKS 1510-089) • Rapid variability of GeV/VHE emission • VHE g-ray emission must be made on the pc scale • Requires radical departure from standard blazar model • UHECR model Paper with Kohta Murase (OSU), Hajime Takami (MPI)

  2. Hard X-ray: Swift, RXTE, Suzaku, NuStar, Astro-H • X-ray/g-ray INTEGRAL INTErnational Gamma • Ray Astrophysics Laboratory • AGILE Astrorivelatore Gamma ad Immagini • ultra LEggero • Ground-Based g-ray Telescopes • HESS High Energy Stereoscopic System • VERITAS Very Energetic Radiation • Imaging Telescope Array System • MAGIC Major Atmospheric Gamma-ray • Imaging Cherenkov Telescope • HAWCHigh Altitude Water Cherenkov • Pierre Auger Cosmic Ray Observatory • IceCube: South Pole neutrino telescope • Cherenkov Telescope Array (CTA) Swift IceCube Astrophysics at High Energies Auger VERITAS and Fermi INTEGRAL

  3. Fermi 3 year > 1 GeV Sky Map

  4. Galactic Center RegionMass within 0.015 pc  4106 MNearby bright EGRET unID sourceNonvariable HESS point-source + ridge emission R. Genzel et al. (2004)

  5. ~100 kpc × 500 kpc lobes Centaurus A Cen A power: Bolometric radio luminosity: 1041 erg s-1 Gamma-ray power (from Fermi): 5×1041 erg s-1 Hard X-ray/soft g-ray power: 5×1042 erg s-1

  6. Ultra-high Energy Cosmic Rays Radiation flux in space

  7. Auger Data: 2009 58 events: July, 2009 (with Swift-BAT AGN density map) 27 events as of November 2007

  8. 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 L ~1045 x (f/10-10 ergs cm-2 s-1) erg s-1 3C 279, z = 0.538 FR1/BL Lac 3C 296 W Comae

  9. Observer Energy Sources: Accretion vs. Black Hole Rotation q BLR clouds Two Component Synchrotron/ Compton Leptonic Jet Model Accretion disk spectra Location of g-ray Emission Region Far (>pc scale)—Finnish group; Boston U. group Near (sub-pc) scale—most theorists G Relativistically Collimated Plasma Outlfows Blazars and Black Holes Dusty Torus W Accretion Disk BL Lac Objects: Synchrotron/SSC model FSRQs: External Compton model Soft Photon Sources: Accretion Disk Radiation scattered by BLR Dusty Torus Failure of the One-Zone Model Decelerating Jet Emission Sheath and Spine SMBH G Ambient Radiation Fields

  10. MAGIC Observations of 4C+21.35 PKS 1222+2163 = 4C+21.35, z = 0.432, G = 3.7, 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) => hyper-variable MAGIC light curve Fermi-LAT and MAGIC spectrum Aleksic et al. (2011) Tanaka et al. (2011)

  11. Fermi Observations of 4C+21.35 PKS 1222+2163 = 4C+21.35, z = 0.432 Fermi-LAT spectrum • Fermi LAT observations • Major flares 2010 April and June • sub-day scale variability • hour-scale variability (Foschini et al. 2011) • nFn peak at 1 – 10 GeV 11

  12. IR Emission from 4C +21.35 Epoch 2 (August 2008) Epoch 1 (June 2007) Malmrose et al. (2011) • Model Spitzer (5 – 35μ), SDSS, 2MASS, and Swift UVOT data of 4C +21.35 • Decompose spectrum into nonthermal power-law and • two-temperature dust model. • Hot dust with T ≈ 1200 • K radiates ≈ 8 × 1045 erg s−1 from ~pc scale • Second warm dust component radiates ≈ 1045 erg s−1 at T ≈ 660 K, also on pc scale • BLR radiation Ghisellini and Tavecchio (2008)

  13. Variability and Source Location G 1/G x Variability timescale implies engine size scale, comoving size scale factor G larger and emission location ~G2 larger than values inferred for stationary region tvar103 s, G = 100  x < 2×1017 cm

  14. Pair Production and Photohadronic Opacity Detection of 40-700 GeV g rays  x > 3×1018 cm →← 14

  15. Neutron-Beam Model for High Energy Radiation from 4C +21.35 g B n,e+ e+ p0, p n,p 2g g n,e- e- ~ pc ~1017 cm • Activity in inner jet accelerates UHECR protons with energies ~1019 – 1020 eV • Photohadronic interactions with radiation fields makes UHECR neutrals (Atoyan & Dermer 2003) • Highly collimated neutron beam escape inner jet and undergoesn + g  n + po, p + p+with IR photons • Secondary electrons and positrons make GeV  TeV synchrotron radiation • Beaming factor ~ 5th power of Doppler factor 15

  16. Neutron-Beam Model for High Energy Radiation from 4C +21.35 g B n,e+ e+ p0, p n,p 2g g n,e- e- ~ pc ~1017 cm • Activity in inner jet accelerates UHECR protons with energies ~1019 – 1020 eV • Photohadronic interactions with radiation fields makes UHECR neutrals (Atoyan & Dermer 2003) • Highly collimated neutron beam escape inner jet and undergoesn + g  n + po, p + p+with IR photons • Secondary electrons and positrons make GeV  TeV synchrotron radiation • Beaming factor ~ 5th power of Doppler factor 16

  17. Neutron-Beam Model for High Energy Radiation from 4C +21.35 g B n,e+ e+ p0, p n,p 2g g n,e- e- ~ pc ~1017 cm • Activity in inner jet accelerates UHECR protons with energies ~1019 – 1020 eV • Photohadronic interactions with radiation fields makes UHECR neutrals (Atoyan & Dermer 2003) • Highly collimated neutron beam escape inner jet and undergoesn + g  n + po, p + p+with IR photons • Secondary electrons and positrons make GeV  TeV synchrotron radiation • Beaming factor ~ 5th power of Doppler factor 17

  18. Variability from Synchrotron Radiation Leptons as photohadronic secondaries formed with 1011 < γe < 1013 Hyper-relativistic electrons Synchrotron losses dominate of electron with Lorentz factor γe if magnetic field > 1 μG Energy engine variability preserved if B > 3 mG by comparing synchrotron cooling time and deflection time Synchrotron radiation formed from 10’s of GeV to PeV energies if B < few mG The cross-hatched region represents range of γeand magnetic fields where 10 minute variability can be preserved T 18

  19. Cascade Radiation Spectrum GeV radiationmade in BLR Outflowing UHECRs make TeV radiation as Synchrotron emission due to ultra-relativistic leptons Obtain few percent efficiency for g-ray production; therefore require ~1049 erg/s apparent isotropic luminosity in UHECRs More rapid variability at higher energies

  20. 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). Cascade Radiation Spectrum GeV radiationmade in BLR Outflowing UHECRs make TeV radiation as Synchrotron emission due to ultra-relativistic leptons Obtain few percent efficiency for g-ray production; therefore require ~1049 erg/s apparent isotropic luminosity in UHECRs More rapid variability at higher energies

  21. 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). Cascade Radiation Spectrum GeV radiationmade in BLR Outflowing UHECRs make TeV radiation as Synchrotron emission due to ultra-relativistic leptons Obtain few percent efficiency for g-ray production; therefore require ~1049 erg/s apparent isotropic luminosity in UHECRs More rapid variability at higher energies

  22. Other Models Two-zone model Tavecchio et al. 2011 Magnetic recollimation Marscher 1980 Reconfinement shocks Nalewajko & Sikora 2009 Bromberg & Levinson 2009 Stawarz 2006 Embedded compact regions Giannios 2009, Marscher & Jorstad 2010, Ghisellini & Tavecchio 2008 Poynting-flux dominated models Nalewajko et al. 2012 Axion-photon conversion Tavecchio et al. 2012 Tavecchio et al. 2011 22

  23. Other Models Two-zone model Tavecchio et al. 2011 Magnetic recollimation Marscher 1980 Reconfinement shocks Nalewajko & Sikora 2009 Bromberg & Levinson 2009 Stawarz 2006 Embedded compact regions Giannios 2009, Marscher & Jorstad 2010, Ghisellini & Tavecchio 2008 Poynting-flux dominated models Nalewajko et al. 2012 Axion-photon conversion Tavecchio et al. 2012 Tavecchio et al. 2011 23

  24. Other Models Two-zone model Tavecchio et al. 2011 Magnetic recollimation Marscher 1980 Reconfinement shocks Nalewajko & Sikora 2009 Bromberg & Levinson 2009 Stawarz 2006 Embedded compact regions Giannios 2009, Marscher & Jorstad 2010, Ghisellini & Tavecchio 2008 Poynting-flux dominated models Nalewajko et al. 2012 Axion-photon conversion Tavecchio et al. 2012 Tavecchio et al. 2011 24

  25. Other Models Two-zone model Tavecchio et al. 2011 Magnetic recollimation Marscher 1980 Reconfinement shocks Nalewajko & Sikora 2009 Bromberg & Levinson 2009 Stawarz 2006 Embedded compact regions Giannios 2009, Marscher & Jorstad 2010, Ghisellini & Tavecchio 2008 Poynting-flux dominated models Nalewajko et al. 2012 Axion-photon conversion Tavecchio et al. 2012 Finke calculations 25

  26. Cascading g rays from blazars: a test for UHECR origin • rays from photopair production by UHECR protons Essey et al. 2010, 2011 • Distinguish hadronic and photonic origin from spectrum at 20 – 30 TeV • CTA tests for UHECR production from multi-TeV emissions (TeV BL Lac) UHECRs g ray injection Murase, Dermer, Takami, Migliori 2012

  27. Conclusions • 70 GeV – 400 GeV radiation from PKS 1222 highly attenuated if made in the sub-pc scale: trigger of VHE telescopes/CTA with Fermi • Rapid VHE variability is inconsistent with formation at the pc scale: variability at different wavebands/single or multiple GeV/VHE spectrum • Propose model where activity in the central engine accelerates UHECR protons, making an escaping neutron beam/hadronic SED contribution • Photohadronic production of neutrons on IR emission makes highly relativistic electrons and positrons, and synchrotron emission of these secondaries makes highly variable VHE radiation/strong GeV polarization • UHECR production complicates question of location of emission region • Hadronic cascade scenario can be distinguished from leptonic scenarios by observing gamma-ray above 25 TeV in 1ES 0229+200; confirmed by neutrino observations

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