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![Page 1: An explanation to the diffuse gamma-ray emission Fiorenza Donato @ Physics Dept., UN. Torino In collaboration with: M. Ajello, T. Bringmann, F. Calore,](https://reader035.fdocuments.in/reader035/viewer/2022070413/5697bfbc1a28abf838ca1882/html5/thumbnails/1.jpg)
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
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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
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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
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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: νS < 1014 Hz ISP: 1014 Hz < νS < 1015 Hz HSP: νS > 1015 Hz
We work with: 80 HSP, 34 ISP, 34 LSP (68 LISP)
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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
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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
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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, 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)
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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.
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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
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Diffuse γ-ray emission from unresolved misaligned AGN
Best fit MAGN diffuse flux: 20-30% Fermi-LAT IGRB, |b|>10o
Estimated uncertainty band: factor 10
Di Mauro,Calore,FD, Ajello, Latronico ApJ2014
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EGB: sum of astrophysical contributionsDi Mauro et al. 2014
The sum of all the contributions to fits Fermi-LAT (preliminary) EGB data
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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
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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
PRELIM
INARY
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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
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The anisotropy – integrated flux consistency
MAGN contribute the most to the IGRB, being very numerous whilst faintHSP 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
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Q: Which room is left to
Dark Matter annihilation
into gamma-rays
in the halo of the Milky Way?
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Bounds on WIMP annihilation cross section
• 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
Bringmann, Calore, FD, Di Mauro, PRD 2013
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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)
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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
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Testing Lγ-Lr 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
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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)!
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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
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BL Lacs data
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 HSP34 ISP34 LSP (68 LISP)
M. Di Mauro, FD, G. Lamanna, D. Sanchez, P.D. Serpico, ApJ
2014
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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
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Simulated all-sky maps
E=4 GeVmDM=200 GeV<σv>=3×1026 cm3/s
Emission from Einasto profile is more clustered.
Calore, De Romeri, Di Mauro, FD, Herpich, Macciò, Maccione MNRAS 2014
EinastoMoore-Stadel
MS profile shows more extended cores
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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