1. 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 “Astroparticle Physics” - Amsterdam, June 26, 2014

2. The Fermi-LAT isotropic diffuse emission 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, […] L. Baldini, this conference

3. Active Galactic Nuclei 3 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 Urry & Padovani 1995

4. 1. Diffuse γ-ray emission from unresolved BL Lacs M. 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: ν S < 10 14 Hz ISP: 10 14 Hz < ν S < 10 15 Hz HSP: ν S > 10 15 Hz We work with: 80 HSP, 34 ISP, 34 LSP (68 LISP)

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

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 from Misaligned 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, Bl Lacs 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 Best fit MAGN diffuse flux: 20-30% Fermi-LAT IGRB, |b|>10 o Estimated uncertainty band: factor 10 Di Mauro,Calore,FD, Ajello, Latronico ApJ2014

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

12. 3. Diffuse γ-ray emission from galactic 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 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) Cuoco, Di Mauro, FD, Siegal-Gaskins, in preparation PRELIMINARY

14. AGN angular power and Fermi-LAT data 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 PRELIMINARY Cuoco, Di Mauro, FD, Siegal-Gaskins, in preparation

15. The anisotropy – integrated flux consistency 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 PRELIMINARY Cuoco, Di Mauro, FD, Siegal-Gaskins, in preparation

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

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|>10 o : 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 L γ -L r correlation: upper limits from undetected FRI&FRII GREAT!!! they do not violate the correlation  It looks physical We derive upper limits for FRI and FRII having strong radio core fluxes

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 m DM =1 (10) TeV the constraints on 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 Lacs data BL Lacs can be classified according to their synchrotron peak frequency ν S (low, intermediate, high synchrotron peak): LSP: ν S < 10 14 Hz ISP: 10 14 Hz < ν S < 10 15 Hz HSP: ν S > 10 15 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 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 Calore, De Romeri, Di Mauro, FD, Herpich, Macciò, Maccione MNRAS 2014

25. Simulated all-sky maps E=4 GeV m DM =200 GeV =3×10 26 cm 3 /s Emission from Einasto profile is more clustered. Calore, De Romeri, Di Mauro, FD, Herpich, Macciò, Maccione MNRAS 2014 Einasto Moore-Stadel MS profile shows more extended cores

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