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Gamma Rays, the EBL, the IGMF, and UHECRs

Guillermo Haro 2011 Workshop INAOE, Puebla, Mexico July 5 – 14, 2011. Gamma Rays, the EBL, the IGMF, and UHECRs. Chuck Dermer United States Naval Research Laboratory Washington, DC USA charles.dermer@nrl.navy.mil Justin Finke, Soebur Razzaque, Massimo Cavadini, Benoit Lott, Jim Chiang

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Gamma Rays, the EBL, the IGMF, and UHECRs

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  1. Guillermo Haro 2011 Workshop INAOE, Puebla, Mexico July 5 – 14, 2011 Gamma Rays, the EBL, the IGMF, and UHECRs Chuck Dermer United States Naval Research Laboratory Washington, DC USA charles.dermer@nrl.navy.mil Justin Finke, Soebur Razzaque, Massimo Cavadini, Benoit Lott, Jim Chiang Kohta Murase, Giulia Migliori, Hajime Takami • Outline • Extragalactic Background Light (EBL) • Using Fermi/TeV Measurements to constrain the EBL • Measuring the Intergalactic Magnetic Field (IGMF) • Ultra-high energy cosmic rays and TeV blazar emission Dermer Guillermo Haro Workshop July 12, 2011

  2. Abdo et al. ApJ, 720, 435 (2010) 1. EBL

  3. IR-UV EBL The Extragalactic Background Light (EBL) at IR/UV frequencies from all stars: either directly (UV-optical) , or through absorption and re-radiation by dust (IR) Why is it important? • Evolution of matter in the universe: star formation history, dust extinction, light absorption and re-emission by dust, etc • Knowledge of the absorption effects due to EBL is necessary to infer the intrinsic spectra of extragalactic gamma-ray sources. Measurement • Direct measurements difficult because of foreground subtraction: zodiacal light; Galactic synchrotron radiation • Number counts can give lower limits. • EBL evolves due to star formation, absorption and re-emission of light by dust dust stars Dermer Guillermo Haro Workshop July 12, 2011

  4. EBL and g-ray absorption g 500 GeV g rays  1 eV target photons universe transparent below ~10 GeV Dermer Guillermo Haro Workshop July 12, 2011

  5. Models of the EBL • g-ray horizon: tgg(Eg,z) = 1 (Stecker-Fazio relation) • Empirical method: sum optical/IR emissions from sources at various redshifts using luminosity-dependent galaxy SEDs (Stecker et al., Franceschini et al. 2008) • Model of galaxy formation during mergers of dark matter halos, including supernova feedback, dust attenuation, metal production (Primack et al., Gilmore) • Models based on integrating stellar light with dust absorption absorption (Kneiske, Finke et al.) • Inferring EBL spectrum from TeV observations by scanning over a large grid of possible EBL, deabsorbing TeV observations limited by spectral hardness (0.75 and 1.5) (Mazin & Raue 2007)

  6. Initial Mass Function (IMF) Finke et al. (2010) Model for the EBL Dust absorption Basic ingredients for model building • Direct starlight Star formation rate (SFR) • Reprocessed dust Dust emissivity Values of fn and Q chosen to fit luminosity densitydata Dermer Guillermo Haro Workshop July 12, 2011

  7. EBL for Different SFR and IMF Models 7 Dermer Guillermo Haro Workshop July 12, 2011

  8. Evolution of the EBL Spectral Energy Density Model “C” 8 Dermer Guillermo Haro Workshop July 12, 2011

  9. Comparison with Other Models 9 Dermer Guillermo Haro Workshop July 12, 2011

  10. Comparison with Other Models • = 0.75 G = 1.5 • Mazin & Raue (2007) 10 Dermer Guillermo Haro Workshop July 12, 2011

  11. EBL Model Predictions Dermer Guillermo Haro Workshop July 12, 2011

  12. tgg = 3 2. EBL Studies with Fermi Data tgg = 1 Highest energy photons from blazars and GRBs make energetic demands on source Abdo et al. ApJ, 723, 1082 (2010) Comparison between expected number of high-energy photons from extrapolation of low energy Fermi GeV spectra constrains EBL model Dermer Guillermo Haro Workshop July 12, 2011

  13. Flux Ratio Method • Assuming intrinsic blazar spectra are z-independent, then ratio of high to low energy fluxes decreases with z • Must use blazar subclasses because of multi-GeV softenings in FSRQs/LSPs/ISPs that are at higher redshifts than ISPs and HSPs with known redshift

  14. EBL Model Rejection with Fermi Data 1FGL J0808-0750 = PKS 0805-07 Abdo et al. ApJ, 723, 1082 (2010) Dermer Guillermo Haro Workshop July 12, 2011

  15. Constraints on EBL Models from GRBs Dermer Guillermo Haro Workshop July 12, 2011

  16. EBL Constraints: GRB 090510 Highest energy photon: (0.829 s after LAT trigger in interval c) z = 0.903 Only Stecker et al. model is (marginally) optically thick Compare GRB 080916C: Highest energy photon: 13 GeV But z = 4.35 Dermer Guillermo Haro Workshop July 12, 2011

  17. Redshift Constraints on BL Lacs • Only ~60% of 2LAC BL Lacs have measured redshifts • VHE g rays constrain EBL; provides method for determining redshift of BL Lacs Synchrotron/SSC modeling Abdo et al. ApJ, 708, 1310 (2010) PG 1553+113, z < 0.75 HST: z~0.40-0.43

  18. Just one thing… 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 Essey, Kalashev, Kusenko, Beacom (2010, 2011)

  19. 3. Cascade Halo Radiation, the EBL and the IGMF e+ g e- Magnetic obscuration of charged particle trajectories: UHECR ions; Lepton secondaries ofgge+e- Attenuation by the EBL: what happens to the generated pairs? Pair halos(Aharonian, Coppi, & Völk 1994; Roustazadeh & Böttcher 2011) Temporal delay and Intergalactic Magnetic Field (IGMF) (Plaga 1995) Temporal delay/echoes from bursting sources (Razzaque et al. 2004; Murase et al. 2008) Angular extent 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 (d’Avezac et al. 2007; Neronov & Vovk 2010; Tavecchio et al. 2010) Nondetection by Fermi of TeV blazar sources  BIGMF >~ 10-16 G Ando & Kusenko (2010): ~30 halos in stacked data of 170 hard-spectrum Fermi blazars  BIGMF~10-15 G (lcoh/kpc)-1/2Criticisms: Neronov et al. (2011), Fermi statement and paper in preparation Dermer Guillermo Haro Workshop July 12, 2011 19

  20. Spectral Model of Halo Emission Cooling spectrum nFn n1/2 Compton-scattered spectrum nFn n3/2 Isotropized spectrum nFn n1/2 Tavecchio et al. (2010a,b) z =0.14 1ES 0229+200 20

  21. Limits on IGMF and Correlation Length Origin of the Intergalactic Magnetic Field (BIGMF): Primordial Early universe physics Biermann battery (~10-30 G on Mpc scale) Galaxy dynamo other Recombination inflation Electroweak IES 0229+200 QCD IES 0347-121 21 Neronov & Vovk (2010)

  22. 1ES 0229+200 HESS: Aharonian et al. 2007 VERITAS: Perkins 2010 VERITAS data preliminary E (TeV) VERITAS: October 2009 – Jan 2010 VERITAS data courtesy J. Perkins and VERITAS team HESS: Sept 1, 2005 + 35d, Aug 20, 2006 +121 d

  23. GeV/TeV Data of 1ES 0229+200 Fermi UL: 2008 Aug 4 – 2010 Sept 5

  24. GeV-TeV Data (Orr, Krennrich, Dwek 2011)

  25. Geometry for Compton-gg Cascade Halo photon: q > qpsf Apply to 1ES 0229+200 z = 0.1396  0.14 ~

  26. Semi-analytic Model of Cascade Pair injection from EBL absorption kinematic term cascade g(Dteng): time for electrons to cool to g during activity time Dteng of central engine g at which electrons are deflected out of beam Compton (Thomson) spectrum from cooling electrons Integration over blackbody spectrum

  27. qj = 0.1

  28. qj = 0.3

  29. qj = 1.0

  30. BIGMF = 10-19 G

  31. BIGMF = 10-18 G

  32. Range of BIGMF; tengine = 3 yr

  33. Range of BIGMF; Different Source Spectrum

  34. Lower Limits on the Intergalactic Magnetic Field Use Fermi upper limits or detections at GeV energies to limit BIGMF given TeV data and EBL model e+ g e- ?  BIGMF > 10-15 G ~ (Neronov & Vovk 2010; Tavecchio et al. 2010)  BIGMF > 10-18 G ~ (relaxing assumption of extended TeV emission) (CD, Cavadini, Razzaque, Finke, Chiang, Lott, 2011)

  35. 4. Ultrahigh Energy Cosmic Rays and TeV Emission of Blazars Are TeV blazars plausible source candidates?

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

  37. 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)

  38. z = 0.047 z = 0.044 z = 0.129 z = 0.139 z = 0.186 z = 0.188 variable z = 0.44 z = 0.538

  39. Invalid > 10 TeV

  40. Essey et al. (2011) Origin of Hard TeV Emission Component? • New component could be leptonic or hadronic • Must explain dependence of break energy on z Böttcher et al. 2008: Leptonic Model for 1ES 1101-232

  41. Cascade Spectra Initiated by Photons and Protons Dermer Guillermo Haro Workshop July 12, 2011

  42. Test for Source Photons or UHECR Production of TeV Emission Component (K. Murase, H. Takami, CD, G. Migliori, 2011)

  43. Conclusions • EBL model constraints from GeV-TeV analysis of blazars and GRBs • High EBL models ruled out--provided photons are made at the source • Deconvolved emission spectra reveal hard TeV component for most EBL models • Halo emission likely for large opening angle, persistent TeV jet sources • Large range of primary source spectra match data • All require an emission component with nFn peak >~ 5 TeV • Minimalist model implies BIGMF >~ 10-18 G • Discriminate flux of >>10 TeV source emission from spectrum near 1 TeV-- Spectral shoulder at 1 TeV implies hard primary emission • Question: Origin of this spectral component? • Leptonic or hadronic (UHECR?) • Use next generation CTA or HAWC experiment to determine if TeV blazar spectra show evidence for UHECR proton origin

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