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 21 th 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 ISRF from GC 10 Λ u Λ � eV cm � 3 � 1 0.1 0.01 SL IR CMB 0.001 1 10 100 1000 10 4 Λ � Μ m � Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying
Diffuse γ Ray Emission (Fermi Data Points) 3 ° lat � 3 ° lon 5 ° lat � 30 ° lon Fermi Data (FermiSymposium) 1 1 Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � 2 regions that surround the GC 10 � 1 10 � 1 3 o latitude × 3 o longitude 10 � 2 10 � 2 5 o latitude × 30 o longitude 10 � 3 10 � 3 10 � 4 10 � 4 10 2 10 3 10 4 10 5 10 6 10 2 10 3 10 4 10 5 10 6 Photon energy Ε � MeV � Photon energy Ε � MeV � Talk by S. Digel Talk by S. Digel Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying
Diffuse γ Ray Emission (Fermi Data Points) 3 ° lat � 3 ° lon 5 ° lat � 30 ° lon Fermi Data (FermiSymposium) 1 1 Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � 2 regions that surround the GC 10 � 1 10 � 1 3 o latitude × 3 o longitude 10 � 2 10 � 2 5 o latitude × 30 o longitude 10 � 3 10 � 3 10 � 4 10 � 4 10 2 10 3 10 4 10 5 10 6 10 2 10 3 10 4 10 5 10 6 Photon energy Ε � MeV � Photon energy Ε � MeV � Talk by S. Digel Talk by S. Digel 10 ° lat � 20 ° lat � 180 ° lon 60 ° lat � 90 ° lat � 180 ° lon Fermi Data (FermiSymposium) 1 1 Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � 2 regions outside the Galactic Plane 10 � 1 10 � 1 10 o -20 o latitude × 180 o longitude 10 � 2 10 � 2 60 o -90 o latitude × 180 o longitude 10 � 3 10 � 3 10 � 4 10 � 4 10 2 10 3 10 4 10 5 10 6 10 2 10 3 10 4 10 5 10 6 Photon energy Ε � MeV � Photon energy Ε � MeV � Talk by T. Porter Talk by M. Ackerman Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying
Diffuse γ Ray Emission (Fermi Data Points) 3 ° lat � 3 ° lon 5 ° lat � 30 ° lon Fermi Data (FermiSymposium) 1 1 Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � 2 regions that surround the GC 10 � 1 10 � 1 3 o latitude × 3 o longitude 10 � 2 10 � 2 5 o latitude × 30 o longitude 10 � 3 10 � 3 10 � 4 10 � 4 10 2 10 3 10 4 10 5 10 6 10 2 10 3 10 4 10 5 10 6 Photon energy Ε � MeV � Photon energy Ε � MeV � Talk by S. Digel Talk by S. Digel 10 ° lat � 20 ° lat � 180 ° lon 60 ° lat � 90 ° lat � 180 ° lon Fermi Data (FermiSymposium) 1 1 Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � Ε 2 d � �� d Ε �� � � MeV cm � 2 s � 1 sr � 1 � 2 regions outside the Galactic Plane 10 � 1 10 � 1 10 o -20 o latitude × 180 o longitude 10 � 2 10 � 2 60 o -90 o latitude × 180 o longitude 10 � 3 10 � 3 10 � 4 10 � 4 10 2 10 3 10 4 10 5 10 6 10 2 10 3 10 4 10 5 10 6 Photon energy Ε � MeV � Photon energy Ε � MeV � The DM signals do not exceed more Talk by T. Porter Talk by M. Ackerman than 3 σ the data Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying
ICS Fluxes at Earth from DM Ann/Dec Z Z d Φ d ǫ = 1 ds j tot ( ǫ, r ( s )) d Ω ǫ 4 π ∆Ω l . o . s . Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying
ICS Fluxes at Earth from DM Ann/Dec Z Z d Φ d ǫ = 1 ds j tot ( ǫ, r ( s )) d Ω ǫ 4 π ∆Ω l . o . s . 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 Z Z d Φ d ǫ = 1 ds j tot ( ǫ, r ( s )) d Ω ǫ 4 π ∆Ω l . o . s . 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 Z Z d Φ d ǫ = 1 ds j tot ( ǫ, r ( s )) d Ω ǫ 4 π ∆Ω l . o . s . ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s) j tot ( ǫ, r ) = j p γ ( ǫ, r ) + j IC ( 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 Z Z d Φ d ǫ = 1 ds j tot ( ǫ, r ( s )) d Ω ǫ 4 π ∆Ω l . o . s . ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s) j tot ( ǫ, r ) = j p γ ( ǫ, r ) + j IC ( ǫ, r ): is the total emissivity of a cell located at distance r from the GC j p γ ( ǫ, r ) = ǫ Q γ ( ǫ, r ) DM Annihilation DM Decay χ ( r ) dN ann ( ǫ, r ) = 1 ( ǫ, r ) = Γ dec n χ ( r ) dN dec Q ann 2 � σ v � n 2 γ γ ( ǫ ) Q dec ( ǫ ) γ γ d ǫ d ǫ dN γ / d ǫ 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 Z Z d Φ d ǫ = 1 ds j tot ( ǫ, r ( s )) d Ω ǫ 4 π ∆Ω l . o . s . ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s) j tot ( ǫ, r ) = j p γ ( ǫ, r ) + j IC ( ǫ, r ): is the total emissivity of a cell located at distance r from the GC Z m χ j IC ( ǫ, r ) = 2 dE e P ( ǫ, E e , r ) n e ( E e , r ) m e 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 Z Z d Φ d ǫ = 1 ds j tot ( ǫ, r ( s )) d Ω ǫ 4 π ∆Ω l . o . s . ǫ is the energy of the photon that we detect at Earth s is the coordinate along the line of sight (l.o.s) j tot ( ǫ, r ) = j p γ ( ǫ, r ) + j IC ( ǫ, r ): is the total emissivity of a cell located at distance r from the GC Z m χ j IC ( ǫ, r ) = 2 dE e P ( ǫ, E e , r ) n e ( E e , r ) m e Differential Power Electrons Number Density The derivation is straightforward in The derivation can be done by solving terms of the well-known IC kinematics the diffusion-loss equation Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying
Derivation of the Electrons Number Density » – h i − 1 ∂ r 2 D ∂ f v ∂ f − 1 ∂ r ( r 2 v ) p ∂ f ∂ + 1 ∂ = Q e ( E , r ) pp 2 f + ˙ r 2 ∂ r ∂ r ∂ r 3 r 2 ∂ p p 2 ∂ p 4 π p 2 |{z} | {z } | {z } | {z } | {z } advection convection radiative losses source diffusion f = n e ( E e , r ) / (4 π p 2 ) with p electron momentum Paolo Panci Diffuse γ Ray Constraints on Annihilating or Decaying
Recommend
More recommend
