Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM...

44
Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi Paolo Panci UNIVERSIT ` A DEGLI STUDI DE L’AQUILA Italian Supervisor: Zurab Berezhiani UNIVERSIT ´ E PARIS DENIS DIDEROT-PARIS 7 French Supervisor: Marco Cirelli 02 nd March 2010, Padova Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying

Transcript of Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM...

Page 1: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Diffuse γ Ray Constraints on

Annihilating or Decaying DM afterFermi

Paolo Panci

UNIVERSITA DEGLI STUDI DE L’AQUILAItalian Supervisor: Zurab Berezhiani

UNIVERSITE PARIS DENIS DIDEROT-PARIS 7French Supervisor: Marco Cirelli

02nd March 2010, Padova

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 2: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Indirect Detection (γ Ray Constraints)

1 γ rays annihilations/decays in the Galactic Center (GC)

2 γ rays annihilations/decays in Dwarf Galaxies (DG)

3 Radio wave from synchrotron radiation of e+e− produced by DMannihilations/decays in the GC (very large magnetic field)

4 γ rays from the Inverse Compton Scattering (ICS) of the e+e−, producedby DM annihilations/decays in the Galactic Halo (GH), with the ISRFphotons

1 10 100 1000 1040.001

0.01

0.1

1

10

Λ @ΜmD

Λu Λ

@eV

cm-

3D

ISRF from GC

SL IR CMB

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 3: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Indirect Detection (γ Ray Constraints)

1 γ rays annihilations/decays in the Galactic Center (GC)

2 γ rays annihilations/decays in Dwarf Galaxies (DG)

3 Radio wave from synchrotron radiation of e+e− produced by DMannihilations/decays in the GC (very large magnetic field)

4 γ rays from the Inverse Compton Scattering (ICS) of the e+e−, producedby DM annihilations/decays in the Galactic Halo (GH), with the ISRFphotons

1 10 100 1000 1040.001

0.01

0.1

1

10

Λ @ΜmD

Λu Λ

@eV

cm-

3D

ISRF from GC

SL IR CMB

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 4: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Indirect Detection (γ Ray Constraints)

1 γ rays annihilations/decays in the Galactic Center (GC)

2 γ rays annihilations/decays in Dwarf Galaxies (DG)

3 Radio wave from synchrotron radiation of e+e− produced by DMannihilations/decays in the GC (very large magnetic field)

4 γ rays from the Inverse Compton Scattering (ICS) of the e+e−, producedby DM annihilations/decays in the Galactic Halo (GH), with the ISRFphotons

1 10 100 1000 1040.001

0.01

0.1

1

10

Λ @ΜmD

Λu Λ

@eV

cm-

3D

ISRF from GC

SL IR CMB

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 5: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Indirect Detection (γ Ray Constraints)

1 γ rays annihilations/decays in the Galactic Center (GC)

2 γ rays annihilations/decays in Dwarf Galaxies (DG)

3 Radio wave from synchrotron radiation of e+e− produced by DMannihilations/decays in the GC (very large magnetic field)

4 γ rays from the Inverse Compton Scattering (ICS) of the e+e−, producedby DM annihilations/decays in the Galactic Halo (GH), with the ISRFphotons

1 10 100 1000 1040.001

0.01

0.1

1

10

Λ @ΜmD

Λu Λ

@eV

cm-

3D

ISRF from GC

SL IR CMB

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 6: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Indirect Detection (γ Ray Constraints)

1 γ rays annihilations/decays in the Galactic Center (GC)

2 γ rays annihilations/decays in Dwarf Galaxies (DG)

3 Radio wave from synchrotron radiation of e+e− produced by DMannihilations/decays in the GC (very large magnetic field)

4 γ rays from the Inverse Compton Scattering (ICS) of the e+e−, producedby DM annihilations/decays in the Galactic Halo (GH), with the ISRFphotons

1 10 100 1000 1040.001

0.01

0.1

1

10

Λ @ΜmD

Λu Λ

@eV

cm-

3D

ISRF from GC

SL IR CMB

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 7: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Indirect Detection (γ Ray Constraints)

1 γ rays annihilations/decays in the Galactic Center (GC)

2 γ rays annihilations/decays in Dwarf Galaxies (DG)

3 Radio wave from synchrotron radiation of e+e− produced by DMannihilations/decays in the GC (very large magnetic field)

4 γ rays from the Inverse Compton Scattering (ICS) of the e+e−, producedby DM annihilations/decays in the Galactic Halo (GH), with the ISRFphotons

1 10 100 1000 1040.001

0.01

0.1

1

10

Λ @ΜmD

Λu Λ

@eV

cm-

3D

ISRF from GC

SL IR CMB

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 8: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Diffuse γ Ray Emission (Fermi Data Points)

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

3°lat 3°lon

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

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 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

10°lat - 20°lat 180°lon

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

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 morethan 3σ the data

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 9: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Diffuse γ Ray Emission (Fermi Data Points)

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

3°lat 3°lon

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

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 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

10°lat - 20°lat 180°lon

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

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 morethan 3σ the data

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 10: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Diffuse γ Ray Emission (Fermi Data Points)

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

3°lat 3°lon

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

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 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

10°lat - 20°lat 180°lon

102 103 104 105 10610-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

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 morethan 3σ the data

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 11: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

ICS Fluxes at Earth from DM Ann/Dec

dε=

1

ε

Z∆Ω

Zl.o.s.

dsj(ε, r(s))

ε is the energy of the upscattered photon

s is the coordinate along the line of sight (l.o.s)

j(ε, r(s)) is the emissivity of a cell located at distance r from the GC

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 12: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

ICS Fluxes at Earth from DM Ann/Dec

dε=

1

ε

Z∆Ω

Zl.o.s.

dsj(ε, r(s))

ε is the energy of the upscattered photon

s is the coordinate along the line of sight (l.o.s)

j(ε, r(s)) is the emissivity of a cell located at distance r from the GC

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 13: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

ICS Fluxes at Earth from DM Ann/Dec

dε=

1

ε

Z∆Ω

Zl.o.s.

dsj(ε, r(s))

ε is the energy of the upscattered photon

s is the coordinate along the line of sight (l.o.s)

j(ε, r(s)) is the emissivity of a cell located at distance r from the GC

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 14: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

ICS Fluxes at Earth from DM Ann/Dec

dε=

1

ε

Z∆Ω

Zl.o.s.

dsj(ε, r(s))

ε is the energy of the upscattered photon

s is the coordinate along the line of sight (l.o.s)

j(ε, r(s)) is the emissivity of a cell located at distance r from the GC

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 15: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

ICS Fluxes at Earth from DM Ann/Dec

dε=

1

ε

Z∆Ω

Zl.o.s.

dsj(ε, r(s))

ε is the energy of the upscattered photon

s is the coordinate along the line of sight (l.o.s)

j(ε, r(s)) is the emissivity of a cell located at distance r from the GC

j(ε, r) = 2

Z mχ

me

dEe P(ε, Ee, r) ne(Ee, r)

Differential Power

The derivation is straightforward interms of the well-known IC kinematics

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 16: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

ICS Fluxes at Earth from DM Ann/Dec

dε=

1

ε

Z∆Ω

Zl.o.s.

dsj(ε, r(s))

ε is the energy of the upscattered photon

s is the coordinate along the line of sight (l.o.s)

j(ε, r(s)) is the emissivity of a cell located at distance r from the GC

j(ε, r) = 2

Z mχ

me

dEe P(ε, Ee, r) ne(Ee, r)

Differential Power

The derivation is straightforward interms of the well-known IC kinematics

Electrons Number Density

The derivation can be done by solvingthe diffusion-loss equation

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 17: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Derivation of the Electrons Number Density

− 1

r 2

∂r

»r 2D

∂f

∂r

–| z

diffusion

+ v∂f

∂r|zadvection

− 1

3r 2

∂r(r 2v)p

∂f

∂p| z convection

+1

p2

∂p

hpp2f

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 theGC

θ = 1o⇒λo = rθ ' 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 DM after Fermi

Page 18: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Derivation of the Electrons Number Density

− 1

r 2

∂r

»r 2D

∂f

∂r

–| z

diffusion

+ v∂f

∂r|zadvection

− 1

3r 2

∂r(r 2v)p

∂f

∂p| z convection

+1

p2

∂p

hpp2f

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 theGC

θ = 1o⇒λo = rθ ' 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 DM after Fermi

Page 19: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Derivation of the Electrons Number Density

− 1

r 2

∂r

»r 2D

∂f

∂r

–| z

diffusion

+ v∂f

∂r|zadvection

− 1

3r 2

∂r(r 2v)p

∂f

∂p| z convection

+1

p2

∂p

hpp2f

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 theGC

θ = 1o⇒λo = rθ ' 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 regionclose to the BH accretion disk(racc ' 0.04 pc)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 20: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Derivation of the Electrons Number Density

− 1

r 2

∂r

»r 2D

∂f

∂r

–| z

diffusion

+ v∂f

∂r|zadvection

− 1

3r 2

∂r(r 2v)p

∂f

∂p| z convection

+1

p2

∂p

hpp2f

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 theGC

θ = 1o⇒λo = rθ ' 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 regionclose to the BH accretion disk(racc ' 0.04 pc)

The typical diffusion time isgreater than the characteristictime due to radiative losses(τdiff > τrad)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 21: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Derivation of the Electrons Number Density

− 1

r 2

∂r

»r 2D

∂f

∂r

–| z

diffusion

+ v∂f

∂r|zadvection

− 1

3r 2

∂r(r 2v)p

∂f

∂p| z convection

+1

p2

∂p

hpp2f

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 theGC

θ = 1o⇒λo = rθ ' 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 regionclose to the BH accretion disk(racc ' 0.04 pc)

The typical diffusion time isgreater than the characteristictime due to radiative losses(τdiff > τrad)

Turn out to be dominated by theICS radiative process

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 22: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Derivation of the Electrons Number Density

ne(Ee, r) =1

E(Ee, r)

Z mχ

Ee

dEe Qe(Ee, r)

E(Ee, r): Total power radiates into photon by an electron on energy Ee

Qe(Ee, r): Source term in the diffusion-loss equation

DM Annihilation

Qanne (Ee, r) =

1

2〈σv〉 n2

χ(r)dNann

e

dEe(Ee)

〈σv〉: Annihilation cross section

nχ = ρ/mχ: DM number density

dNanne /dEe: Electron spectrum

produced by DM annihilation

DM Decay

Qdece (Ee, r) = Γdec nχ(r)

dNdece

dEe(Ee)

Γdec = 1/τdec: Decay rate

nχ = ρ/mχ: DM number density

dNdece /dEe: Electron spectrum

produced by DM decay

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 23: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Derivation of the Electrons Number Density

ne(Ee, r) =1

E(Ee, r)

Z mχ

Ee

dEe Qe(Ee, r)

E(Ee, r): Total power radiates into photon by an electron on energy Ee

Qe(Ee, r): Source term in the diffusion-loss equation

DM Annihilation

Qanne (Ee, r) =

1

2〈σv〉 n2

χ(r)dNann

e

dEe(Ee)

〈σv〉: Annihilation cross section

nχ = ρ/mχ: DM number density

dNanne /dEe: Electron spectrum

produced by DM annihilation

DM Decay

Qdece (Ee, r) = Γdec nχ(r)

dNdece

dEe(Ee)

Γdec = 1/τdec: Decay rate

nχ = ρ/mχ: DM number density

dNdece /dEe: Electron spectrum

produced by DM decay

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 24: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Derivation of the Electrons Number Density

ne(Ee, r) =1

E(Ee, r)

Z mχ

Ee

dEe Qe(Ee, r)

E(Ee, r): Total power radiates into photon by an electron on energy Ee

Qe(Ee, r): Source term in the diffusion-loss equation

DM Annihilation

Qanne (Ee, r) =

1

2〈σv〉 n2

χ(r)dNann

e

dEe(Ee)

〈σv〉: Annihilation cross section

nχ = ρ/mχ: DM number density

dNanne /dEe: Electron spectrum

produced by DM annihilation

DM Decay

Qdece (Ee, r) = Γdec nχ(r)

dNdece

dEe(Ee)

Γdec = 1/τdec: Decay rate

nχ = ρ/mχ: DM number density

dNdece /dEe: Electron spectrum

produced by DM decay

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 25: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

ICS Fluxes at Earth from DM Ann/Dec

dΦanni

dε=

1

2

〈σv〉4π

ρ2

m2χ

rJanni ∆Ω

dNann

dε,

dNann

dε= 2

1

ε

Z mχ

me

dEeP(Ee, ε)

E(Ee)Y ann(Ee)

dΦdeci

dε=

Γdec

ρmχ

rJdeci ∆Ω

dNdec

dε,

dNdec

dε= 2

1

ε

Z mχ

me

dEeP(Ee, ε)

E(Ee)Y dec(Ee)

Canonical Geometrical Factors

Annihilation Scenario

Janni ∆Ω =

Z∆Ω

dΩ(b, l)

Zds

r

ρ2[r(s, b, l)]

ρ2

b → Galactic latitudel → Galactic longitude

Decay Scenario

Jdeci ∆Ω =

Z∆Ω

dΩ(b, l)

Zds

r

ρ[r(s, b, l)]

ρ

b → Galactic latitudel → Galactic longitude

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 26: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

ICS Fluxes at Earth from DM Ann/Dec

dΦanni

dε=

1

2

〈σv〉4π

ρ2

m2χ

rJanni ∆Ω

dNann

dε,

dNann

dε= 2

1

ε

Z mχ

me

dEeP(Ee, ε)

E(Ee)Y ann(Ee)

dΦdeci

dε=

Γdec

ρmχ

rJdeci ∆Ω

dNdec

dε,

dNdec

dε= 2

1

ε

Z mχ

me

dEeP(Ee, ε)

E(Ee)Y dec(Ee)

Canonical Geometrical Factors

Annihilation Scenario

Janni ∆Ω =

Z∆Ω

dΩ(b, l)

Zds

r

ρ2[r(s, b, l)]

ρ2

b → Galactic latitudel → Galactic longitude

Decay Scenario

Jdeci ∆Ω =

Z∆Ω

dΩ(b, l)

Zds

r

ρ[r(s, b, l)]

ρ

b → Galactic latitudel → Galactic longitude

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 27: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Summary & Results (DM Annihilation)

102 103 104 105 10610-4

10-3

10-2

10-1

1

10

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

FERMI 3° 3°

NFW Profile

DM DM ® Μ+ Μ-

mΧ= 1.5 TeV

Σv= 310-23 cm3sec

CMB

IR

SL

Prompt Γ

Total

102 103 104 105 10610-4

10-3

10-2

10-1

1

10

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

FERMI 5° 30°

Einasto Profile

DM DM ® Μ+ Μ-

mΧ= 1.5 TeV

Σv= 310-23 cm3sec

CMB

IR

SL

Prompt Γ

Total

102 103 104 105 10610-6

10-5

10-4

10-3

10-2

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

FERMI Galactic Poles

IsoT Profile

DM DM ® Μ+ Μ-

mΧ= 1.5 TeV

Σv= 310-23 cm3sec

CMB

Prompt Γ

Total

102 103 104 105 10610-4

10-3

10-2

10-1

1

10

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

FERMI 3° 3°

IsoThermal Profile

DM DM ® Τ+Τ-

mΧ= 3 TeV

Σv= 210-22 cm3sec

CMB IR

SL

Prom

ptΓ

Total

102 103 104 105 10610-4

10-3

10-2

10-1

1

10

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

FERMI 5° 30°

IsoThermal Profile

DM DM ® Τ+Τ-

mΧ= 3 TeV

Σv= 210-22 cm3sec

CMB IR

SL

Prom

ptΓ

Total

102 103 104 105 10610-5

10-4

10-3

10-2

10-1

1

Photon energy Ε @MeVD

Ε2dF

HdΕ

DW

L@M

eVcm

-2s-

1sr

-1

D

FERMI 10°- 20°

IsoThermal Profile

DM DM ® Τ+Τ-

mΧ= 3 TeV

Σv= 210-22 cm3sec

CMB IR

SL

Prom

ptΓ

Total

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 28: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Draw the Exclusion Lines 〈σannv〉/mχ Plane

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 29: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

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) = ρsrsr

„1 +

r

rs

«−2

, ρisoT(r) =ρs

1 + (r/rs)2

DM halo model rs in kpc ρs in GeV/cm3

NFW 20.0 0.26Einasto 21.8 0.05Isothermal 3.20 2.31

10-2 10-1 1 10 10210-3

10-2

10-1

1

10

102

103

r in kpc

ΡD

Min

GeV

cm

3

NFW

Iso

Einasto

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 30: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Draw the Exclusion Lines 〈σannv〉/mχ Plane

Consider a Benchmark DM Halo profile

Calculate the ICS signal and the prompt signal in each given primaryannihilation channel spanning the DM mass in a range between100 GeV up to 10 TeV

Require that the DM signals do not exceed more than 3σ the FERMIexperimental data

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 31: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Draw the Exclusion Lines 〈σannv〉/mχ Plane

Consider a Benchmark DM Halo profile

Calculate the ICS signal and the prompt signal in each given primaryannihilation channel spanning the DM mass in a range between100 GeV up to 10 TeV

Require that the DM signals do not exceed more than 3σ the FERMIexperimental data

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 32: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

IC + Prompt γ Constraints (DM Annihilation)

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

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 (green95% C.L. and yellow 99.999% C.L.)

FERMI + HESS + PAMELA allowedregion (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 DM after Fermi

Page 33: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

IC + Prompt γ Constraints (DM Annihilation)

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

DM DM ® ee, Einasto profile

FERMI 3° 3°

FERMI 5° 30°

FERMI 10°- 20°

FERMI Gal. Poles

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

DM DM ® ΜΜ, Einasto profile

FERMI 3° 3°

FERMI 5° 30°

FERMI 10°- 20°

FERMI Gal. Poles

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

DM DM ® ΤΤ, Einasto profile

FERMI 3° 3°

FERMI 5° 30°

FERMI 10°- 20°

FERMI Gal. Poles

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

DM DM ® ee, NFW profile

FERMI 3° 3°

FERMI 5° 30°

FERMI 10°- 20°

FERMI Gal. Poles

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

DM DM ® ΜΜ, NFW profile

FERMI 3° 3°

FERMI 5° 30°

FERMI 10°- 20°

FERMI Gal. Poles

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

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 DM after Fermi

Page 34: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

IC + Prompt γ Constraints (DM Annihilation)

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

DM DM ® ee, Iso profile

FERMI 3° 3°

FERMI 5° 30°

FERMI 10°- 20°

FERMI Gal. Poles

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

DM DM ® ΜΜ, Iso profile

FERMI 3° 3°

FERMI 5° 30°

FERMI 10°- 20°

FERMI Gal. Poles

102 103 104

10-26

10-25

10-24

10-23

10-22

10-21

10-20

mΧ @GeVD

Σv

@cm

3s

D

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 bereopened.

The FERMI + HESS + PAMELA allowed region in the case of annihilationinto muons is not excluded yet

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 35: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from our Galaxy

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

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 36: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from our Galaxy

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

dΦdeccosm

dε= Γdec

Ωχρc,0

1

H0

Z ∞

0

dze−τ(ε,z)p

ΩM(1 + z)3 + ΩΛ

dN

dε(ε(1 + z))

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 37: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from our Galaxy

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

dΦdecisotropic

dε=

dΦdeccosm

dε+ 4π

dΦdechalo

dε dΩ

˛Anti−GC

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 38: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from our Galaxy

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

dΦdecisotropic

dε=

dΦdeccosm

dε+ 4π

dΦdechalo

dε dΩ

˛Anti−GC

102 103 104 105 10610-5

10-4

10-3

10-2

Photon energy Ε @MeVD

Ε2

dFHd

ΕD

WL@

MeV

cm-

2s-

1sr

-1

D

Anti-GC

Talk by M. Ackerman, FermiSymposium

The ”Isotropic Signal” does not exceedmore than 3σ the FERMI data

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 39: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Draw the Exclusion Lines τdec/mχ Plane

IC + Prompt γ Constraints from our Galaxy

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

dΦdecisotropic

dε=

dΦdeccosm

dε+ 4π

dΦdechalo

dε dΩ

˛Anti−GC

102 103 104 105 10610-5

10-4

10-3

10-2

Photon energy Ε @MeVD

Ε2

dFHd

ΕD

WL@

MeV

cm-

2s-

1sr

-1

D

Anti-GC

Talk by M. Ackerman, FermiSymposium

The ”Isotropic Signal” does not exceedmore than 3σ the FERMI data in theAnti-GC

Annihilation Scenario

Stronger dependence on theangular distance from the GC isintroduced in the galactic flux(no longer ”Isotropic signal”)

Dependence on the DM profilesand the clumpiness of DM halosis introduced in the cosmologicalflux (not well understand)

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 40: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

IC + Prompt γ Constraints (DM Decay)

102 103 104

1023

1024

1025

1026

1027

mΧ @GeVD

Τde

c@s

ecD

DM ® ee, Iso profile

FERMI 10°- 20°

FERMI Gal. Poles

Extra Gal. + Gal.

102 103 104

1023

1024

1025

1026

1027

mΧ @GeVD

Τde

c@s

ecD

DM ® ΜΜ, Iso profile

FERMI 10°- 20°

FERMI Gal. Poles

Extra Gal. + Gal.

102 103 104

1023

1024

1025

1026

1027

mΧ @GeVD

Τde

c@s

ecD

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 strongestcontraints

It excludes the decay explanation of the FERMI+HESS+PAMELA anomaliesfor the ττ channel and starts to exclude the decay explanation for the µµ

channel

Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi

Page 41: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Conclusions

Leptonic Annihilation modes:

For the NFW or Einasto profiles, the current data exclude not only DMscenarios explaining the FERMI+HESS+PAMELA allowed regions, butalso 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 strongestconstraint and it is independent on the DM halo profiles

It excludes the decay explanation of the FERMI+HESS+PAMELAanomalies for the ττ channel and starts to exclude the decay explanationfor 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 DM after Fermi

Page 42: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Conclusions

Leptonic Annihilation modes:

For the NFW or Einasto profiles, the current data exclude not only DMscenarios explaining the FERMI+HESS+PAMELA allowed regions, butalso 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 strongestconstraint and it is independent on the DM halo profiles

It excludes the decay explanation of the FERMI+HESS+PAMELAanomalies for the ττ channel and starts to exclude the decay explanationfor 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 DM after Fermi

Page 43: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Conclusions

Leptonic Annihilation modes:

For the NFW or Einasto profiles, the current data exclude not only DMscenarios explaining the FERMI+HESS+PAMELA allowed regions, butalso 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 strongestconstraint and it is independent on the DM halo profiles

It excludes the decay explanation of the FERMI+HESS+PAMELAanomalies for the ττ channel and starts to exclude the decay explanationfor 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 DM after Fermi

Page 44: Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM annihilations/decays in the Galactic Halo (GH), with the ISRF photons 1 10 100 1000 104

Conclusions

Leptonic Annihilation modes:

For the NFW or Einasto profiles, the current data exclude not only DMscenarios explaining the FERMI+HESS+PAMELA allowed regions, butalso 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 strongestconstraint and it is independent on the DM halo profiles

It excludes the decay explanation of the FERMI+HESS+PAMELAanomalies for the ττ channel and starts to exclude the decay explanationfor 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 DM after Fermi