Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM...
Transcript of Diffuse Ray Constraints on Annihilating or Decaying DM after Fermi · 2010-02-27 · by DM...
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
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
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
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
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
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
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
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
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
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
ICS Fluxes at Earth from DM Ann/Dec
dΦ
dε=
1
ε
Z∆Ω
dΩ
Zl.o.s.
dsj(ε, r(s))
4π
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
ICS Fluxes at Earth from DM Ann/Dec
dΦ
dε=
1
ε
Z∆Ω
dΩ
Zl.o.s.
dsj(ε, r(s))
4π
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
ICS Fluxes at Earth from DM Ann/Dec
dΦ
dε=
1
ε
Z∆Ω
dΩ
Zl.o.s.
dsj(ε, r(s))
4π
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
ICS Fluxes at Earth from DM Ann/Dec
dΦ
dε=
1
ε
Z∆Ω
dΩ
Zl.o.s.
dsj(ε, r(s))
4π
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
ICS Fluxes at Earth from DM Ann/Dec
dΦ
dε=
1
ε
Z∆Ω
dΩ
Zl.o.s.
dsj(ε, r(s))
4π
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
ICS Fluxes at Earth from DM Ann/Dec
dΦ
dε=
1
ε
Z∆Ω
dΩ
Zl.o.s.
dsj(ε, r(s))
4π
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
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
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
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
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
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
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
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
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
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
4π
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
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
4π
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
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
Draw the Exclusion Lines 〈σannv〉/mχ Plane
Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying DM after Fermi
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
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
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
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
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
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
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
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
mχ
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
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
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
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
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
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
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
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
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