Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi - - PowerPoint PPT Presentation

Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Paolo Panci

Supported by Marie Curie Early Stage Research Training (MRTN-CT-2006-035863 - UniverseNet) UNIVERSIT` A DEGLI STUDI DE L’AQUILA & UNIVERSIT´ E PARIS 7

21th July 2010, Institut d’Astrophysique de Paris (IAP)

arXiv:0912.0663 in collaboration with M. Cirelli and P.D. Serpico

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Plan of the Talk

Dark Matter Indirect Detection with γ rays

Inverse Compton γ rays Prompt γ rays

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Plan of the Talk

Dark Matter Indirect Detection with γ rays

Inverse Compton γ rays Prompt γ rays

Constraints on Annihilating or Decaying Dark Matter by using the diffuse γ rays measured by the FERMI satellite

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Indirect Detection (γ Ray Constraints)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Indirect Detection (γ Ray Constraints)

1 Prompt γ rays from DM annihilations/decays in the Galactic Center, in

Dwarf Galaxies and Satellites

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Indirect Detection (γ Ray Constraints)

1 Prompt γ rays from DM annihilations/decays in the Galactic Center, in

Dwarf Galaxies and Satellites

2 Radio wave from synchrotron radiation of e+e− produced by DM

annihilations/decays in the GC (very large magnetic field)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Indirect Detection (γ Ray Constraints)

1 Prompt γ rays from DM annihilations/decays in the Galactic Center, in

Dwarf Galaxies and Satellites

2 Radio wave from synchrotron radiation of e+e− produced by DM

annihilations/decays in the GC (very large magnetic field)

3 γ rays from the Inverse Compton Scattering (ICS) of the e+e−, produced

by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Indirect Detection (γ Ray Constraints)

1 Prompt γ rays from DM annihilations/decays in the Galactic Center, in

Dwarf Galaxies and Satellites

2 Radio wave from synchrotron radiation of e+e− produced by DM

annihilations/decays in the GC (very large magnetic field)

3 γ rays from the Inverse Compton Scattering (ICS) of the e+e−, produced

by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons

1 10 100 1000 104 0.001 0.01 0.1 1 10 Λ Μm Λ uΛ eV cm3

ISRF from GC

SL IR CMB

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Diffuse γ Ray Emission (Fermi Data Points)

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

3°lat 3°lon

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

5°lat 30°lon

Talk by S. Digel Talk by S. Digel

Fermi Data (FermiSymposium) 2 regions that surround the GC 3o latitude × 3o longitude 5o latitude × 30o longitude

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Diffuse γ Ray Emission (Fermi Data Points)

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

3°lat 3°lon

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

5°lat 30°lon

Talk by S. Digel Talk by S. Digel

Fermi Data (FermiSymposium) 2 regions that surround the GC 3o latitude × 3o longitude 5o latitude × 30o longitude

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

10°lat 20°lat 180°lon

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

60°lat 90°lat 180°lon

Talk by T. Porter Talk by M. Ackerman

Fermi Data (FermiSymposium) 2 regions outside the Galactic Plane 10o-20o latitude × 180o longitude 60o-90o latitude × 180o longitude

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Diffuse γ Ray Emission (Fermi Data Points)

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

3°lat 3°lon

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

5°lat 30°lon

Talk by S. Digel Talk by S. Digel

Fermi Data (FermiSymposium) 2 regions that surround the GC 3o latitude × 3o longitude 5o latitude × 30o longitude

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

10°lat 20°lat 180°lon

102 103 104 105 106 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

60°lat 90°lat 180°lon

Talk by T. Porter Talk by M. Ackerman

Fermi Data (FermiSymposium) 2 regions outside the Galactic Plane 10o-20o latitude × 180o longitude 60o-90o latitude × 180o longitude The DM signals do not exceed more than 3σ the data

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦ dǫ = 1 ǫ Z

∆Ω

dΩ Z

l.o.s.

ds jtot(ǫ, r(s)) 4π

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦ dǫ = 1 ǫ Z

∆Ω

dΩ Z

l.o.s.

ds jtot(ǫ, r(s)) 4π ǫ is the energy of the photon that we detect at Earth

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦ dǫ = 1 ǫ Z

∆Ω

dΩ Z

l.o.s.

ds jtot(ǫ, r(s)) 4π ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦ dǫ = 1 ǫ Z

∆Ω

dΩ Z

l.o.s.

ds jtot(ǫ, r(s)) 4π ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s) jtot(ǫ, r) = jpγ(ǫ, r) + jIC(ǫ, r): is the total emissivity of a cell located at distance r from the GC

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦ dǫ = 1 ǫ Z

∆Ω

dΩ Z

l.o.s.

ds jtot(ǫ, r(s)) 4π ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s) jtot(ǫ, r) = jpγ(ǫ, r) + jIC(ǫ, r): is the total emissivity of a cell located at distance r from the GC jpγ(ǫ, r) = ǫ Qγ(ǫ, r) DM Annihilation Qann

γ

(ǫ, r) = 1 2σv n2

χ(r) dNann γ

dǫ (ǫ) DM Decay Qdec

γ

(ǫ, r) = Γdec nχ(r) dNdec

γ

dǫ (ǫ) dNγ/dǫ computed by using the PYTHIA MonteCarlo code

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦ dǫ = 1 ǫ Z

∆Ω

dΩ Z

l.o.s.

ds jtot(ǫ, r(s)) 4π ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s) jtot(ǫ, r) = jpγ(ǫ, r) + jIC(ǫ, r): is the total emissivity of a cell located at distance r from the GC jIC(ǫ, r) = 2 Z mχ

me

dEe P(ǫ, Ee, r) ne(Ee, r) Differential Power The derivation is straightforward in terms of the well-known IC kinematics

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦ dǫ = 1 ǫ Z

∆Ω

dΩ Z

l.o.s.

ds jtot(ǫ, r(s)) 4π ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s) jtot(ǫ, r) = jpγ(ǫ, r) + jIC(ǫ, r): is the total emissivity of a cell located at distance r from the GC jIC(ǫ, r) = 2 Z mχ

me

dEe P(ǫ, Ee, r) ne(Ee, r) Differential Power The derivation is straightforward in terms of the well-known IC kinematics Electrons Number Density The derivation can be done by solving the diffusion-loss equation

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

− 1 r 2 ∂ ∂r » r 2D ∂f ∂r – | {z }

diffusion

+ v ∂f ∂r |{z}

advection

− 1 3r 2 ∂ ∂r (r 2v)p ∂f ∂p | {z }

convection

+ 1 p2 ∂ ∂p h ˙ pp2f i | {z }

radiative losses

= Qe(E, r) 4πp2 | {z }

source f = ne(Ee, r)/(4πp2) with p electron momentum Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

− 1 r 2 ∂ ∂r » r 2D ∂f ∂r – | {z }

diffusion

+ v ∂f ∂r |{z}

advection

− 1 3r 2 ∂ ∂r (r 2v)p ∂f ∂p | {z }

convection

+ 1 p2 ∂ ∂p h ˙ pp2f i | {z }

radiative losses

= Qe(E, r) 4πp2 | {z }

source f = ne(Ee, r)/(4πp2) with p electron momentum

Fermi Regions Big Regions of the sky, well outside the GC θ = 1o⇒λo = r⊙θ ≃ 0.15 kpc

1 0.45 kpc × 0.45 kpc 2 0.74 kpc × 4.44 kpc 3 1.48 kpc - 2.96 kpc × 26.65 kpc 4 8.88 kpc - 13.33 kpc × 26.65 kpc

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

− 1 r 2 ∂ ∂r » r 2D ∂f ∂r – | {z }

diffusion

+ v ∂f ∂r |{z}

advection

− 1 3r 2 ∂ ∂r (r 2v)p ∂f ∂p | {z }

convection

+ 1 p2 ∂ ∂p h ˙ pp2f i | {z }

radiative losses

= Qe(E, r) 4πp2 | {z }

source f = ne(Ee, r)/(4πp2) with p electron momentum

Fermi Regions Big Regions of the sky, well outside the GC θ = 1o⇒λo = r⊙θ ≃ 0.15 kpc

1 0.45 kpc × 0.45 kpc 2 0.74 kpc × 4.44 kpc 3 1.48 kpc - 2.96 kpc × 26.65 kpc 4 8.88 kpc - 13.33 kpc × 26.65 kpc

Are only important in a region close to the BH accretion disk (racc ≃ 0.04 pc)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

− 1 r 2 ∂ ∂r » r 2D ∂f ∂r – | {z }

diffusion

+ v ∂f ∂r |{z}

advection

− 1 3r 2 ∂ ∂r (r 2v)p ∂f ∂p | {z }

convection

+ 1 p2 ∂ ∂p h ˙ pp2f i | {z }

radiative losses

= Qe(E, r) 4πp2 | {z }

source f = ne(Ee, r)/(4πp2) with p electron momentum

Fermi Regions Big Regions of the sky, well outside the GC θ = 1o⇒λo = r⊙θ ≃ 0.15 kpc

1 0.45 kpc × 0.45 kpc 2 0.74 kpc × 4.44 kpc 3 1.48 kpc - 2.96 kpc × 26.65 kpc 4 8.88 kpc - 13.33 kpc × 26.65 kpc

Are only important in a region close to the BH accretion disk (racc ≃ 0.04 pc) Approximation for the inner part

• f our Galaxy (τdiff ∼ τrad)

True outside the Galactic Plane (τdiff ≫ τrad)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

− 1 r 2 ∂ ∂r » r 2D ∂f ∂r – | {z }

diffusion

+ v ∂f ∂r |{z}

advection

− 1 3r 2 ∂ ∂r (r 2v)p ∂f ∂p | {z }

convection

+ 1 p2 ∂ ∂p h ˙ pp2f i | {z }

radiative losses

= Qe(E, r) 4πp2 | {z }

source f = ne(Ee, r)/(4πp2) with p electron momentum

Fermi Regions Big Regions of the sky, well outside the GC θ = 1o⇒λo = r⊙θ ≃ 0.15 kpc

1 0.45 kpc × 0.45 kpc 2 0.74 kpc × 4.44 kpc 3 1.48 kpc - 2.96 kpc × 26.65 kpc 4 8.88 kpc - 13.33 kpc × 26.65 kpc

Are only important in a region close to the BH accretion disk (racc ≃ 0.04 pc) Approximation for the inner part

• f our Galaxy (τdiff ∼ τrad)

True outside the Galactic Plane (τdiff ≫ τrad) Turn out to be dominated by the ICS radiative process

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

ne(Ee, r) = 1 btot(Ee, r) Z mχ

Ee

d ˜ Ee Qe(˜ Ee, r)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

ne(Ee, r) = 1 btot(Ee, r) Z mχ

Ee

d ˜ Ee Qe(˜ Ee, r) btot(Ee, r) = bCMB(Ee) + bIR(Ee, r) + bSL(Ee, r)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

ne(Ee, r) = 1 btot(Ee, r) Z mχ

Ee

d ˜ Ee Qe(˜ Ee, r) btot(Ee, r) = bCMB(Ee) + bIR(Ee, r) + bSL(Ee, r) Qe(Ee, r): Source term in the diffusion-loss differential equation

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

ne(Ee, r) = 1 btot(Ee, r) Z mχ

Ee

d ˜ Ee Qe(˜ Ee, r) btot(Ee, r) = bCMB(Ee) + bIR(Ee, r) + bSL(Ee, r) Qe(Ee, r): Source term in the diffusion-loss differential equation DM Annihilation Qann

e

(Ee, r) = 1 2σv n2

χ(r) dNann e

dEe (Ee) σv: Annihilation cross section nχ = ρ/mχ: DM number density dNann

e

/dEe: Electron spectrum produced by DM annihilation DM Decay Qdec

e

(Ee, r) = Γdec nχ(r) dNdec

e

dEe (Ee) Γdec = 1/τdec: Decay rate nχ = ρ/mχ: DM number density dNdec

e

/dEe: Electron spectrum produced by DM decay dNe/dEe computed by using the PYTHIA MonteCarlo code

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Derivation of the Electrons Number Density

ni

e(Ee, r) ≃

1 bi

tot(Ee)

Z mχ

Ee

d ˜ Ee Qe(˜ Ee, r) Constant btot over each of the observation regions that we consider btot(Ee, r) ≃ bi

tot(Ee)

103 102 101 1 10 102 103 104 105 1023 1022 1021 1020 1019 1018 1017 1016 1015 1014 1013 1012 1011 1010 109 108 107 Electron Energy EeGeV ICS Energy Loss GeV sec1

3° 3° & 5° 30° Regions

Thompson Limit Ee

2

bCMB bIR bSL btot 103 102 101 1 10 102 103 104 105 1023 1022 1021 1020 1019 1018 1017 1016 1015 1014 1013 1012 1011 1010 109 108 107 Electron Energy EeGeV ICS Energy Loss GeV sec1

10° 20° 180° Region

Thompson Limit Ee

2

bCMB bIR bSL btot 103 102 101 1 10 102 103 104 105 1022 1021 1020 1019 1018 1017 1016 1015 1014 1013 1012 1011 1010 109 108 107 Electron Energy EeGeV ICS Energy Loss GeV sec1

60° 90° 180° Region

Thompson Limit Ee

2

bIR 0 bSL 0 btot bCMB

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦi dǫ ∆Ω = 8 > > > > > < > > > > > : ¯ Jann

i

1 2 σv 4π ρ2

⊙

m2

χ

r⊙ " dNann

i

dǫ ˛ ˛ ˛ ˛

IC

+ dNann dǫ ˛ ˛ ˛ ˛

pγ

# (annihilation) ¯ Jdec

i

Γdec 4π ρ⊙ mχ r⊙ " dNdec

i

dǫ ˛ ˛ ˛ ˛

IC

+ dNdec dǫ ˛ ˛ ˛ ˛

pγ

# (decay)

dNann/dec

i

dǫ ˛ ˛ ˛ ˛ ˛ ˛

IC

= 2 ǫ Z mχ

me

dEe Pi (Ee, ǫ) bi

tot(Ee)

Z mχ

Ee

d ˜ Ee dNann/dec

e

d ˜ Ee , dNann/dec dǫ ˛ ˛ ˛ ˛ ˛

pγ

= dNann/dec

γ

dǫ . Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

ICS Fluxes at Earth from DM Ann/Dec

dΦi dǫ ∆Ω = 8 > > > > > < > > > > > : ¯ Jann

i

1 2 σv 4π ρ2

⊙

m2

χ

r⊙ " dNann

i

dǫ ˛ ˛ ˛ ˛

IC

+ dNann dǫ ˛ ˛ ˛ ˛

pγ

# (annihilation) ¯ Jdec

i

Γdec 4π ρ⊙ mχ r⊙ " dNdec

i

dǫ ˛ ˛ ˛ ˛

IC

+ dNdec dǫ ˛ ˛ ˛ ˛

pγ

# (decay)

dNann/dec

i

dǫ ˛ ˛ ˛ ˛ ˛ ˛

IC

= 2 ǫ Z mχ

me

dEe Pi (Ee, ǫ) bi

tot(Ee)

Z mχ

Ee

d ˜ Ee dNann/dec

e

d ˜ Ee , dNann/dec dǫ ˛ ˛ ˛ ˛ ˛

pγ

= dNann/dec

γ

dǫ .

Annihilation Scenario ¯ Jann

i

= Z ds r⊙ ρ2[r(s, b, l)] ρ2

⊙

b → Galactic latitude l → Galactic longitude Decay Scenario ¯ Jdec

i

= Z ds r⊙ ρ[r(s, b, l)] ρ⊙ b → Galactic latitude l → Galactic longitude

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Boost Factors in our Regions

Region latitude b & ¯ Jann

i

¯ Jdec

i

longitude l IsoT NFW Einasto IsoT NFW Einasto ‘3×3’ 0.25◦ < |b| < 2.75◦ 35.1 325 595 8.20 14.6 18.5 357.25◦ < l < 359.75◦ 0.25◦ < l < 2.75◦ ‘5×30’ 0.25◦ < |b| < 4.75◦ 20.9 51.1 85.9 6.56 7.53 8.72 330.25◦ < l < 359.75◦ 0.25◦ < l < 29.75◦ ‘10−20’ 10◦ < |b| < 20◦ 3.35 3.46 4.23 2.45 2.38 2.47 0◦ < l < 360◦ ‘Gal Poles’ 60◦ < |b| < 90◦ 0.92 0.96 0.94 1.74 1.69 1.67 0◦ < l < 360◦

In the DM annihilation scenario the signals from the inner part of our Galaxy are boosted compare to the decay one More competitive γ ray constraints in the DM annihilation scenario

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Summary & Results (DM Annihilation)

102 103 104 105 106 104 103 102 101 1 10 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1 FERMI 3° 3° NFW Profile DM DM ΜΜ mΧ 1.5 TeV Σv 31023 cm3sec CMB IR SL Prompt Γ Total 102 103 104 105 106 104 103 102 101 1 10 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1 FERMI 5° 30° Einasto Profile DM DM ΜΜ mΧ 1.5 TeV Σv 31023 cm3sec CMB IR SL Prompt Γ Total 102 103 104 105 106 106 105 104 103 102 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1 F E R M I G a l a c t i c P

• l

e s IsoT Profile DM DM ΜΜ mΧ 1.5 TeV Σv 31023 cm3sec CMB Prompt Γ T

• t

a l 102 103 104 105 106 104 103 102 101 1 10 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1 FERMI 3° 3° IsoThermal Profile DM DM ΤΤ mΧ 3 TeV Σv 21022 cm3sec CMB IR SL Prompt Γ Total 102 103 104 105 106 104 103 102 101 1 10 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1 FERMI 5° 30° IsoThermal Profile DM DM ΤΤ mΧ 3 TeV Σv 21022 cm3sec CMB IR SL Prompt Γ Total 102 103 104 105 106 105 104 103 102 101 1 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1 FERMI 10° 20° IsoThermal Profile DM DM ΤΤ mΧ 3 TeV Σv 21022 cm3sec CMB IR SL P r

• m

p t Γ Total

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines σannv/mχ Plane

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines σannv/mχ Plane

Recent Numerical Simulations (Einasto profile): ρEin(r) = ρs exp » − 2 α „„ r rs «α − 1 «– , α = 0.17. Previously standard choices (NFW & IsoT): ρNFW(r) = ρs rs r „ 1 + r rs «−2 , ρisoT(r) = ρs 1 + (r/rs)2 DM halo model rs in kpc ρs in GeV/cm3 NFW 20.0 0.26 Einasto 21.8 0.05 Isothermal 3.20 2.31

102 101 1 10 102 103 102 101 1 10 102 103 r in kpc ΡDM in GeVcm3 NFW Iso Einasto

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines σannv/mχ Plane

Consider a Benchmark DM Halo profile Calculate the ICS signal and the prompt signal in each given primary annihilation channel spanning the DM mass in a range between 100 GeV up to 10 TeV

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines σannv/mχ Plane

Consider a Benchmark DM Halo profile Calculate the ICS signal and the prompt signal in each given primary annihilation channel spanning the DM mass in a range between 100 GeV up to 10 TeV Require that the DM signals do not exceed more than 3σ the FERMI experimental data

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

IC + Prompt γ Constraints (DM Annihilation)

102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ΤΤ, Einasto profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles P.P., M. Cirelli, P.D. Serpico

The PAMELA allowed region (green 95% C.L. and yellow 99.999% C.L.) FERMI + HESS + PAMELA allowed region (red 95% C.L. and orange 99.999% C.L.) are completely excluded by the IC + Prompt γ constraints !!!

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

IC + Prompt γ Constraints (DM Annihilation)

102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ee, Einasto profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ΜΜ, Einasto profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ΤΤ, Einasto profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ee, NFW profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ΜΜ, NFW profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ΤΤ, NFW profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles

P.P., M. Cirelli, P.D. Serpico Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

IC + Prompt γ Constraints (DM Annihilation)

102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ee, Iso profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ΜΜ, Iso profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM ΤΤ, Iso profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles

P.P., M. Cirelli, P.D. Serpico

For the smooth isothermal profile, regions of the parameters space seem to be reopened. The FERMI + HESS + PAMELA allowed region in the case of annihilation into muons is not excluded yet

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Hadronic Mode Constraints

10 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM bb, Einasto profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 10 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM tt, Einasto profile

mt 180 GeV FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 10 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM WW, Einasto profile

mW 80 GeV FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 10 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM bb, NFW profile

FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 10 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM tt, NFW profile

mt 180 GeV FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles 10 102 103 104 1026 1025 1024 1023 1022 1021 1020 mΧ GeV Σv cm3s

DM DM WW, NFW profile

mW 80 GeV FERMI 3° 3° FERMI 5° 30° FERMI 10° 20° FERMI Gal. Poles

P.P., M. Cirelli, P.D. Serpico Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines τdec/mχ Plane

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from our Galaxy

102 103 104 1023 1024 1025 1026 1027 mΧ GeV Τdec sec

DM ee, Iso profile

FERMI 10° 20° FERMI Gal. Poles 102 103 104 1023 1024 1025 1026 1027 mΧ GeV Τdec sec

DM ΜΜ, Iso profile

FERMI 10° 20° FERMI Gal. Poles 102 103 104 1023 1024 1025 1026 1027 mΧ GeV Τdec sec

DM ΤΤ, Iso profile

FERMI 10° 20° FERMI Gal. Poles

P.P., M. Cirelli, P.D. Serpico

The exclusion lines lie below the FERMI+HESS+PAMELA allowed region The constraints from our Galaxy are not so strong

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from the residual ”Isotropic radiation”

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from the residual ”Isotropic radiation” dΦdec

cosm

dǫ = Γdec Ωχρc,0 mχ 1 H0 Z ∞ dz e−τ(ǫ,z) p ΩM(1 + z)3 + ΩΛ " dNdec dǫ ˛ ˛ ˛ ˛

IC

+ dNdec dǫ ˛ ˛ ˛ ˛

pγ

#

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from the residual ”Isotropic radiation” dΦdec

isotropic

dǫ = dΦdec

cosm

dǫ + 4π dΦdec

halo

dǫ dΩ ˛ ˛ ˛ ˛

Anti−GC Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from the residual ”Isotropic radiation” dΦdec

isotropic

dǫ = dΦdec

cosm

dǫ + 4π dΦdec

halo

dǫ dΩ ˛ ˛ ˛ ˛

Anti−GC

102 103 104 105 106 105 104 103 102 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

AntiGC

Talk by M. Ackerman, FermiSymposium

The ”Isotropic Signal” does not exceed more than 3σ the FERMI data in the Anti-GC

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from the residual ”Isotropic radiation” dΦdec

isotropic

dǫ = dΦdec

cosm

dǫ + 4π dΦdec

halo

dǫ dΩ ˛ ˛ ˛ ˛

Anti−GC

102 103 104 105 106 105 104 103 102 Photon energy Ε MeV Ε2 ddΕ MeV cm2s1sr1

AntiGC

Talk by M. Ackerman, FermiSymposium

The ”Isotropic Signal” does not exceed more than 3σ the FERMI data in the Anti-GC Annihilation Scenario Stronger dependence on the angular distance from the GC is introduced in the galactic flux (no longer ”Isotropic signal”) Dependence on the DM profiles and the clumpiness of DM halos is introduced in the cosmological flux (strong dependence on MHalo

min , cvir) see e.g. Zaharijas et al. JCAP 1004:014,2010 Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

IC + Prompt γ Constraints (DM Decay)

102 103 104 1023 1024 1025 1026 1027 mΧ GeV Τdec sec

DM ee, Iso profile

FERMI 10° 20° FERMI Gal. Poles Extra Gal. Gal. 102 103 104 1023 1024 1025 1026 1027 mΧ GeV Τdec sec

DM ΜΜ, Iso profile

FERMI 10° 20° FERMI Gal. Poles Extra Gal. Gal. 102 103 104 1023 1024 1025 1026 1027 mΧ GeV Τdec sec

DM ΤΤ, Iso profile

FERMI 10° 20° FERMI Gal. Poles Extra Gal. Gal.

P.P., M. Cirelli, P.D. Serpico

The residual ”Isotropic radiation” measured by FERMI imposes the strongest contraints It excludes the decay explanation of the FERMI+HESS+PAMELA anomalies for the ττ channel and starts to exclude the decay explanation for the µµ channel

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Conclusions

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Conclusions

Leptonic Annihilation modes: For the NFW or Einasto profiles, the current data exclude not only DM scenarios explaining the FERMI+HESS+PAMELA allowed regions, but also PAMELA regions alone to hight confidence level For ”cored” profiles, regions of the parameters space seem to be reopened (The annihilation into muons is not excluded yet)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Conclusions

Leptonic Annihilation modes: For the NFW or Einasto profiles, the current data exclude not only DM scenarios explaining the FERMI+HESS+PAMELA allowed regions, but also PAMELA regions alone to hight confidence level For ”cored” profiles, regions of the parameters space seem to be reopened (The annihilation into muons is not excluded yet) Leptonic Decay modes: The residual isotropic radiation measured by Fermi imposes the strongest constraint and it is independent on the DM halo profiles It excludes the decay explanation of the FERMI+HESS+PAMELA anomalies for the ττ channel and starts to exclude the decay explanation for the µµ channel

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Conclusions

Leptonic Annihilation modes: For the NFW or Einasto profiles, the current data exclude not only DM scenarios explaining the FERMI+HESS+PAMELA allowed regions, but also PAMELA regions alone to hight confidence level For ”cored” profiles, regions of the parameters space seem to be reopened (The annihilation into muons is not excluded yet) Leptonic Decay modes: The residual isotropic radiation measured by Fermi imposes the strongest constraint and it is independent on the DM halo profiles It excludes the decay explanation of the FERMI+HESS+PAMELA anomalies for the ττ channel and starts to exclude the decay explanation for the µµ channel Tensions with other Constraints: Constraints from Synchrotron radiation

(Bertone et al. arXiv:0811.3744)

Constraints from Ionization and Heating of the InterGalactic Medium

(Cirelli, Iocco, Panci arXiv:0907.0719), (Huetsi et al. arXiv:0906.4550), (Galli et al. arXiv:0905.0003) Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying