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An explanation to the diffuse gamma- ray emission

An explanation to the diffuse gamma- ray emission. Fiorenza Donato @ Physics Dept., UN. Torino In collaboration with: M. Ajello, T. Bringmann, F. Calore, A. Cuoco, M. Di Mauro, G. Lamanna L. Latronico, D. Sanchez, P.D. Serpico, J. Siegal-Gaskins

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An explanation to the diffuse gamma- ray emission

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  1. An explanation to the diffuse gamma-rayemission Fiorenza Donato @Physics Dept., UN. Torino In collaboration with:M. Ajello, T. Bringmann, F. Calore, A. Cuoco, M. Di Mauro, G. Lamanna L. Latronico, D. Sanchez, P.D. Serpico, J. Siegal-Gaskins “Astroparticle Physics”- Amsterdam, June 26, 2014

  2. The Fermi-LAT isotropic diffuse emission L. Baldini, this conference The origin of the IGRB Undetected sources: AGN (blazars: BL Lacs, FSRQ; mis-aligned AGN) star forming galaxies, (galactic) milli-second pulsars (MSP), […] Diffuse processes: UHECRs interacting with EBL, dark matter annihilation, intergalactic shocks, […]

  3. Active Galactic Nuclei Urry & Padovani 1995 Radio quiet AGN: Quasars, Seyfert, Liners Radio loud AGN: Blazars: BL Lacs (no emission lines, closer, less luminous) FSRQ (stronger emission lines, farther, more luminous) Quasars (SSRQ, FSRQ) Radio Galaxies (FRI, FRII) (decreasing view angle) Fermi-LAT data on |b|>10: 1042 sources, 873 associated out of which 357 are BL Lacs and 318 FSRQs

  4. 1. Diffuse γ-ray emission from unresolved BL LacsM. Di Mauro, FD, G. Lamanna, D. Sanchez, P.D. Serpico ApJ 2014 • Spectral energy distribution (SED) derived from Fermi-LAT data AND TeV catalogs • Luminosity function derived from Fermi-LAT data • EBL absorption included (> 100 GeV) • Blazars studied according • to radio and X-ray classification: • Low (High) synchrotron peaked • LSP: νS < 1014 Hz • ISP: 1014 Hz < νS < 1015 Hz • HSP: νS > 1015 Hz • We work with: • 80 HSP, 34 ISP, 34 LSP (68 LISP)

  5. Observed Spectral Energy Distribution (SED) LSP BL Lac SED HSP BL Lac SED Power-law with exp cut-off provides better fits (huge uncertainties in the cut-off)

  6. Diffuse γ-ray emission from unresolved BL Lacs Di Mauro, FD, Lamanna, Sanchez, Serpico ApJ2014 • Softening at > 100 GeV due to EBL absorption: data are nicely reproduced! • Treating LSP and HSP separately gives non negligible differences

  7. 2. Diffuse γ-ray emission fromMisaligned Active Galactic Nuclei (MAGN) M. Di Mauro, F. Calore, FD, M. Ajello, L. Latronico ApJ 2014 • MAGN: AGN with jet not aligned along the line-of-sight (l.o.s.) • Doppler boosting negligible • Radio galaxies (RG) and steep-spectrum radio quasars (SSRQs) • RG have been classified by Fanaroff&Riley (1974) • FRI edge-darkened, less powerful, BlLacs parent • FRII edge-brightened, more powerful, FSRQs parent • Abundant RADIO data: • total (including lobes) and central compact region (core) • Fermi-LAT observed 15 MAGN between 0.1-100 GeV • (Fermi-LAT ApJ 720, 2010)

  8. γ-ray vs radio luminosity function for MAGN Correlation between luminosity of radio core at 5 GHz and γ-ray luminosity > 0.1 GeV The strength of the correlation has been confirmed by the Spearman test and the modified Kendall τ rank correlation test: chance correlation excluded at 95% C.L.

  9. Constraints from logN-logS The cumulative source number above a given flux: Our assumptions (core radio – γ-ray correlation, link between core and total radio emission, …) are consistent with the Fermi-LAT MAGN number count Consistency also for k=1 (equal number of radio and γ-ray emitters) Trend at lowest fluxes  intensity of diffuse flux

  10. Diffuse γ-ray emission from unresolved misaligned AGN Di Mauro,Calore,FD, Ajello, Latronico ApJ2014 Best fit MAGN diffuse flux: 20-30% Fermi-LAT IGRB, |b|>10o Estimated uncertainty band: factor 10

  11. EGB: sum of astrophysical contributionsDi Mauro et al. 2014 The sum of all the contributions to fits Fermi-LAT (preliminary) EGB data

  12. 3. Diffuse γ-ray emission fromgalactic milli-second pulsars (MSPs) Calore, Di Mauro, FD 1406.2706 Galactic MSPs contribution to the IGRB is negligible at all energies

  13. Anisotropy power spectra from astrophysical sources Cuoco, Di Mauro, FD, Siegal-Gaskins, in preparation We study angular power for classes of AGN: • BL Lacs: LISP and HSP (Low, Intermediate and High Synchrotron Peak) • Misaligned AGN (MAGN) • Flat Spectrum Radio Quasar (FSRQ) PRELIMINARY

  14. AGN angular power and Fermi-LAT data Cuoco, Di Mauro, FD, Siegal-Gaskins, in preparation PRELIMINARY HSP BL Lacs contribute the most to the anisotropy; high energy spectrum MAGN are very numerous by faint, little amount of AP Fermi-LAT data explained by AGN

  15. The anisotropy – integrated flux consistency Cuoco, Di Mauro, FD, Siegal-Gaskins, in preparation PRELIMINARY MAGN contribute the most to the IGRB, being very numerous whilst faint HSP BL Lacs get relevant to the highest energies, but sub-dominant Our emission models for AGN are compatible with Fermi-LAT data on anisotropy AND diffuse emission

  16. Q: Which room is left to Dark Matter annihilation into gamma-rays in the halo of the Milky Way?

  17. Bounds on WIMP annihilation cross section Bringmann, Calore, FD, Di Mauro, PRD 2013 • Standard halo assumptions I(ψ) • Prompt and IC photons • BR=1 at fixe annih. channel • Bkgd= MAGN + ΣBMS • ΣBMS = MSPs (Calore+2012)+ • BL Lac (Abdo+2010) + • FSRQs (Ajello+2012) + • SF galaxies (Ackermann+2012) • DM + bkgd must not exceed • any data point (at 2σ) Effect of MAGN contribution

  18. Constraints to DM from diffuse γ-ray emission • High latitude data: |b|>10: • Bringmann, Calore, Di Mauro, FD 2013 • Negligible the choice for ρ(r) • crucial the backgrounds from • extra-galactic unresolved sources • Halo 5<|b|<15,|l|<80: • Fermi-LAT Coll. 1204.6474 • Models for the diffuse • galactic emission improve the limits • - Important the choice for ρ(r)

  19. Conclusions • The IGRB is studied for |b|>10o: faint, diffuse, isotropic flux • We present new estimations of the diffuse emission from unresolved BL Lacs, MAGN, MSPs: Fermi-LAT data for the IGRB are very well explained by astrophysical sources • Anisotropies for the astrophysical sources compatible with Fermi-LAT data • Dark matter: anisotropies depend on the behavior of the density profile extrapolated at low radii • We show how much the MAGN background reduces the room left to Dark Matter annihilation

  20. Testing Lγ-Lr correlation: upper limits from undetected FRI&FRII We derive upper limits for FRI and FRII having strong radio core fluxes GREAT!!! they do not violate the correlation  It looks physical

  21. Effect of Inverse Compton contribution from e+e- DM annihilation The inclusion of the IC scattering (on CMB, infrared radiation, stellar light) is non-negligible for Wimp Dark Matter masses >~ 100 GeV. At mDM=1 (10) TeV the constraints on <σv> increase by a factor 10 (50)!

  22. Fermi-LAT MAGNs: main radio and gamma properties • Some of Fermi-LAT sources are variable • Radio CORE data taken at 5 GHz, and contemporary to Fermi-LAT data • Up to z~0.7 • 4 FRII and 8 FRI

  23. BL Lacsdata BL Lacs can be classified according to their synchrotron peak frequency νS (low, intermediate, high synchrotron peak): LSP: νS < 1014 Hz ISP: 1014 Hz < νS < 1015 Hz HSP: νS > 1015 Hz We work with:80 HSP 34 ISP 34 LSP (68 LISP) M. Di Mauro, FD, G. Lamanna, D. Sanchez, P.D. Serpico, ApJ 2014

  24. Effect of unresolved (smaller) sub-haloes Calore, De Romeri, Di Mauro, FD, Herpich, Macciò, Maccione MNRAS 2014 • Black lines: Aquarius Aq-A-1 simulated sub-haloes, Einasto profile (Springer+2008) • More massive and cored haloes give a flattening at high l (red line) • The smaller haloes give more power and a Poisson-like trend

  25. Simulated all-sky maps Calore, De Romeri, Di Mauro, FD, Herpich, Macciò, Maccione MNRAS 2014 Moore-Stadel Einasto E=4 GeV mDM=200 GeV <σv>=3×1026 cm3/s Emission from Einasto profile is more clustered. MS profile shows more extended cores

  26. Spatial information: Anisotropies in γ-rays Peculiar DM over-dense regions may imprint spatial signatures in high resolution data Predicted angular power spectrum: galactic and extragalactic Fermi-LAT: detected angular power >3σ in 1-10 GeV range at high l Fornasa et al. 2012 Fermi-Lat Coll. 1202.2856

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