15 April 2015 University of Oslo Dark Matter Indirect Detection amid hints & constraints Marco Cirelli (CNRS IPhT Saclay) NewDark
15 April 2015 University of Oslo Dark Matter Indirect Detection amid hints & constraints Marco Cirelli (CNRS IPhT Saclay) NewDark
Introduction Introduction
Introduction Introduction DM exists
Introduction DM exists weak lensing (e.g. in clusters) ‘precision cosmology’ (CMB, LSS) galactic rotation curves
Introduction DM exists weak lensing (e.g. in clusters) ‘precision cosmology’ (CMB, LSS) galactic rotation curves DM is a neutral, very long lived, feebly- corpuscle weakly interactingpa rticle.
Introduction DM exists weak lensing (e.g. in clusters) ‘precision cosmology’ (CMB, LSS) galactic rotation curves DM is a neutral, very long lived, weakly interacting particle. Some of us believe in the WIMP miracle. - weak -scale mass (10 GeV - 1 TeV) - weak interactions σ v = 3 · 10 − 26 cm 3 / sec - give automatically correct abundance
DM Candidates A matter of perspective: plausible mass ranges eV (1 TeV)
DM Candidates A matter of perspective: plausible mass ranges ‘only’ 90 orders of magnitude!
DM Candidates A matter of perspective: plausible mass ranges Color code: ID, DD Fermi 135 GeV GeV line gamma PAMELA, excess 3.5 KeV Fermi, at GC line HESS PeV neutrinos excesses Icecube Light DM lots of activity some activity (‘Dama’) recently recently anomaly ‘only’ 90 orders of magnitude!
DM detection direct detection Xenon, CDMS, Edelweiss... (CoGeNT, Dama/Libra...) production at colliders LHC from annihil in galactic center or halo γ and from synchrotron emission Fermi, ICT , radio telescopes... e + indirect from annihil in galactic halo or center PAMELA, Fermi, HESS, AMS, balloons... from annihil in galactic halo or center ¯ p ¯ from annihil in galactic halo or center d GAPS ν , ¯ ν from annihil in massive bodies SK, Icecube , Km3Net
DM detection direct detection production at colliders from annihil in galactic center or halo γ and from synchrotron emission Fermi, ICT , radio telescopes... e + indirect from annihil in galactic halo or center PAMELA, Fermi, HESS, AMS, balloons... from annihil in galactic halo or center ¯ p ¯ from annihil in galactic halo or center d GAPS ν , ¯ ν from annihil in massive bodies SK, Icecube , Km3Net
DM detection direct detection production at colliders from annihil in galactic center or halo γ and from synchrotron emission Fermi, ICT , radio telescopes... e + indirect from annihil in galactic halo or center PAMELA, Fermi, HESS, AMS, balloons... from annihil in galactic halo or center ¯ p ¯ from annihil in galactic halo or center d GAPS ν , ¯ ν from annihil in massive bodies SK, Icecube , Km3Net
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p 8 k p c
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p S N N N S S N S
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p S N V C V C V C V C V C N N S S N S -V C -V C -V C -V C -V C
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p S N V C V C V C V C V C N N S S N S -V C -V C -V C -V C -V C
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p S N V C V C V C V C V C N N S S N S -V C -V C -V C -V C -V C
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p S N V C V C V C V C V C N N 2L S h S N S -V C -V C -V C -V C -V C Salati, Chardonnay, Barrau, spectrum Donato, Taillet, Fornengo, Maurin, Brun... ‘90s, ‘00s ∂ f ∂ t � K ( E ) · ⇤ 2 f � ∂ ∂ E ( b ( E ) f ) + ∂ ∂ z ( V c f ) = Q inj � 2 h δ ( z ) Γ spall f diffusion energy loss convective wind source spallations [uncert]
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p thickness L { diffusion diff. reacc. p index convection solar mod. Cirelli, Gaggero, Giesen, Taoso, Urbano 1407.2173 cfr. Evoli, Cholis, Grasso, Maccione, Ullio, 1108.0664 Donato et al., 2003+
Indirect Detection: charged CRs Solar wind Modulation of cosmic rays: = p 2 d Φ ¯ d Φ ¯ p ⊕ p ⊕ T = T ⊕ + | Ze | φ F dT , p 2 dT ⊕ Fisk spectrum spectrum potential φ F � 500 MV at Earth far from Earth (11 yr) AMS-01 Caprice Caprice PAMELA BESS
Indirect Detection: charged CRs Solar wind Modulation of cosmic rays: = p 2 d Φ ¯ d Φ ¯ p ⊕ p ⊕ T = T ⊕ + | Ze | φ F dT , p 2 dT ⊕ Fisk spectrum spectrum potential φ F � 500 MV at Earth far from Earth E.g. φ F ' 900 MV Boudard, Cirelli, Giesen, Salati, 1412.5696
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p S N V C V C V C V C V C N N 2L S h S N S -V C -V C -V C -V C -V C What sets the overall expected flux? flux ∝ n 2 σ annihilation
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p S N V C V C V C V C V C N N 2L S h S N S -V C -V C -V C -V C -V C What sets the overall expected flux? flux ∝ n 2 σ annihilation particle astro& cosmo
Indirect Detection: charged CRs and from DM annihilations in halo e + ¯ p S N V C V C V C V C V C N N 2L S h S N S -V C -V C -V C -V C -V C What sets the overall expected flux? flux ∝ n 2 σ annihilation particle reference cross section: astro& cosmo σ v = 3 · 10 − 26 cm 3 / sec
DM halo profiles From N-body numerical simulations: ⌅ − 2 r s ⇤ 1 + r ρ s [GeV/cm 3 ] DM halo r s [kpc] α NFW : ρ NFW ( r ) = ρ s r r s ⇧⇤ r NFW 24.42 0.184 − ⌅ α ⌥ − 2 ⌃� Einasto 0.17 28.44 0.033 Einasto : ρ Ein ( r ) = ρ s exp − 1 r s α EinastoB 0.11 35.24 0.021 ρ s Isothermal 4.38 1.387 Isothermal : ρ Iso ( r ) = − 1 + ( r/r s ) 2 Burkert 12.67 0.712 − ρ s Moore 30.28 0.105 Burkert : ρ Bur ( r ) = − (1 + r/r s )(1 + ( r/r s ) 2 ) Angle from the GC � degrees ⇥ ⌅ − 1 . 84 � r s ⇥ 1 . 16 ⇤ 1 + r Moore : ρ Moo ( r ) = ρ s 10 ⇤⇤ 30 ⇤⇤ 1 ⇤ 5 ⇤ 10 ⇤ 30 ⇤ 1 o 2 o 5 o 10 o 20 o 45 o r r s At small r: ρ ( r ) ∝ 1 /r γ 10 4 Moore Cirelli et al., 1012.4515 10 3 NFW ⇥ DM � GeV ⇤ cm 3 ⇥ 6 profiles: Einasto EinastoB 10 2 cuspy: NFW, Moore 10 Iso 1 mild: Einasto Burkert ⇥ � 10 � 1 smooth: isothermal, Burkert r � 10 � 2 EinastoB = steepened Einasto 10 � 3 10 � 2 10 � 1 1 10 10 2 (effect of baryons?) r � kpc ⇥
Indirect Detection: basics ( � ) ( � ) DM p , W � , Z, b, τ � , t, h . . . � e ⇥ , D . . . ( − ) ( − ) W + , Z, ¯ b, τ + , ¯ t, h . . . � e ± , p , D . . . DM
Indirect Detection: basics ( � ) ( � ) DM p , W � , Z, b, τ � , t, h . . . � e ⇥ , D . . . primary channels ( − ) ( − ) W + , Z, ¯ b, τ + , ¯ t, h . . . � e ± , p , D . . . DM
Indirect Detection: basics ( � ) ( � ) DM p , W � , Z, b, τ � , t, h . . . � e ⇥ , D . . . decay primary channels ( − ) ( − ) W + , Z, ¯ b, τ + , ¯ t, h . . . � e ± , p , D . . . DM
Indirect Detection: basics ( � ) ( � ) DM p , W � , Z, b, τ � , t, h . . . � e ⇥ , D . . . final decay primary products channels ( − ) ( − ) W + , Z, ¯ b, τ + , ¯ t, h . . . � e ± , p , D . . . DM spectra spectra spectra e � primary spectra spectra spectra p primary spectra spectra spectra e ⇧ ⌃ 10 M DM ⇥ 1000 GeV M DM ⇤ 1000 GeV q b 10 x x x t W 1 x x dN � d log x dN � d log x x x dN � d log x Z h 115 1 g ⌅ 10 � 1 V ⌥⇧ 10 ⇥ 1 � � � 10 ⇥ 2 10 � 2 10 ⇥ 5 10 ⇥ 4 10 ⇥ 3 10 ⇥ 2 10 ⇥ 1 1 10 � 5 10 � 4 10 � 3 10 � 2 10 � 1 1 x ⇤ K � M DM x ⇥ K � M DM � � � � spectra spectra spectra 10 x x x x � � �
Indirect Detection: basics ( � ) ( � ) DM p , W � , Z, b, τ � , t, h . . . � e ⇥ , D . . . final decay primary products channels ( − ) ( − ) W + , Z, ¯ b, τ + , ¯ t, h . . . � e ± , p , D . . . DM spectra spectra spectra e � primary spectra spectra spectra p primary spectra spectra spectra e ⇧ ⌃ 10 M DM ⇥ 1000 GeV M DM ⇤ 1000 GeV q b 10 x x x t W 1 x x dN � d log x dN � d log x x x dN � d log x Z h 115 1 g ⌅ 10 � 1 V ⌥⇧ 10 ⇥ 1 � � � 10 ⇥ 2 10 � 2 10 ⇥ 5 10 ⇥ 4 10 ⇥ 3 10 ⇥ 2 10 ⇥ 1 1 10 � 5 10 � 4 10 � 3 10 � 2 10 � 1 1 x ⇤ K � M DM x ⇥ K � M DM � � � � spectra spectra spectra ElectroWeak corrections! Sala et al., 1009.0224 Cirelli, Panci, Sala et al., 1012.4515 10 x x x x � � �
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