Dark Matter in the Universe
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- Brittany Sims
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1 Dark Matter in the Universe NTNU Trondheim []
2 Experimental anomalies: WMAP haze: synchrotron radiation from the GC
3 Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron annihilation line from the Galactic bulge
4 Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron annihilation line from the Galactic bulge EGRET excess, surplus of diffuse γ-rays
5 Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron annihilation line from the Galactic bulge EGRET excess, surplus of diffuse γ-rays PAMELA anomaly: positrons, but no anti-protons
6 Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron annihilation line from the Galactic bulge EGRET excess, surplus of diffuse γ-rays PAMELA anomaly: positrons, but no anti-protons ATIC anomaly: positrons, but no anti-protons
7 Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron annihilation line from the Galactic bulge EGRET excess, surplus of diffuse γ-rays PAMELA anomaly: positrons, but no anti-protons ATIC anomaly: positrons, but no anti-protons HESS: TeV γ-rays from GC
8 Experimental anomalies: WMAP haze: synchrotron radiation from the GC Integral: positron annihilation line from the Galactic bulge EGRET excess, surplus of diffuse γ-rays PAMELA anomaly: positrons, but no anti-protons ATIC anomaly: positrons, but no anti-protons HESS: TeV γ-rays from GC DAMA/Libra modulation signal
![Earlier indirect detection claims: [Elsässer, Mannheim 04 ] Signal](/docs-images/87/95242258/images/9-0.jpg "from extragalactic χχ annihilations in the diffuse photon")
9 Earlier indirect detection claims: [Elsässer, Mannheim 04 ] Signal from extragalactic χχ annihilations in the diffuse photon background:
10 Earlier indirect detection claims: [Elsässer, Mannheim 04 ] Signal from extragalactic χχ annihilations in the diffuse photon background: E 2 x Gamma Ray Intensity / (GeV cm -2 s -1 sr -1 ) EGRET µ = 978GeV m 2 = -1035GeV m A = 1036GeV tan β = 6.6 m S = 1814GeV A t = 0.88 A b = Ωh 2 = 0.1 α = Salamon & Stecker Blazar Model m χ = 520 GeV <σv> χ = 3.1 x cm 3 s -1 Straw Person's Blazar Model: χ 2 /ν =1.05 Dark Matter Scenario (Total) χ 2 /ν =0.74 0, Observed Gamma Ray Energy / GeV
11 Earlier indirect detection claims: [de Boer et al ] Signal from Galactic χχ annihilations in the diffuse photon flux: E 2 * flux [GeV cm -2 s -1 sr -1 ] tot. background Pion decay Inverse Compton Bremsstrahlung EGRET bg sig signal extragalactic m 0 = 1400 GeV m 1/2 = 175 GeV tan β = Dark Matter: E [GeV] Candidates and their properties
12 Earlier indirect detection claims: [de Boer et al ] Signal from Galactic χχ annihilations in the diffuse photon flux: E 2 * flux [GeV cm -2 s -1 sr -1 ] tot. background Pion decay Inverse Compton Bremsstrahlung EGRET bg sig signal extragalactic m 0 = 1400 GeV m 1/2 = 175 GeV tan β = 51 Bump not seen by Fermi Dark Matter: E [GeV] Candidates and their properties
13 PAMELA anomaly - )) )+ φ(e ) / (φ(e Positron fraction φ(e Muller & Tang 1987 MASS 1989 TS93 HEAT94+95 CAPRICE94 AMS98 HEAT00 Clem & Evenson 2007 PAMELA Energy (GeV)
14 PAMELA anomaly: positron-proton identification via de/dx, topology electrons protons
15 ATIC anomaly
16 ATIC anomaly Ballon experiment CR induced background under control?
17 PAMELA and ATIC anomaly - )) )+ φ(e ) / (φ(e Positron fraction φ(e Muller & Tang 1987 MASS 1989 TS93 HEAT94+95 CAPRICE94 AMS98 HEAT00 Clem & Evenson 2007 PAMELA Energy (GeV)
18 Possible explanations for the PAMELA anomaly: Dark matter requires large boost factors Sommerfeld enhancement dense, cold clumps
19 Possible explanations for the PAMELA anomaly: Dark matter requires large boost factors Sommerfeld enhancement dense, cold clumps exclusive coupling to leptons
20 Possible explanations for the PAMELA anomaly: Dark matter requires large boost factors Sommerfeld enhancement dense, cold clumps exclusive coupling to leptons Astrophysics: as primaries from pulsars supernova remanants (SNR)
21 Astrophysical sources for anti-matter: CR secondaries standard secenario for Galactic CRs: sources are SNRs: kinetic energy output of SNe: 10M ejected with v cm/s every 30 yr L SN,kin erg/s explains local energy density of CR ε CR 1 ev/cm 3 for a escape time from disc τ esc yr
22 Astrophysical sources for anti-matter: CR secondaries standard secenario for Galactic CRs: sources are SNRs: kinetic energy output of SNe: 10M ejected with v cm/s every 30 yr L SN,kin erg/s explains local energy density of CR ε CR 1 ev/cm 3 for a escape time from disc τ esc yr 1.order Fermi shock acceleration dn/de E γ with γ = diffusion with D(E) τ esc (E) E δ and δ 0.6 explains observed spectrum E 2.6
23 Astrophysical sources for anti-matter: CR secondaries standard secenario for Galactic CRs: sources are SNRs: kinetic energy output of SNe: 10M ejected with v cm/s every 30 yr L SN,kin erg/s explains local energy density of CR ε CR 1 ev/cm 3 for a escape time from disc τ esc yr 1.order Fermi shock acceleration dn/de E γ with γ = diffusion with D(E) τ esc (E) E δ and δ 0.6 explains observed spectrum E 2.6 electrons, positrons: τ loss τ esc and τ loss 1/E
24 Astrophysical sources for anti-matter: CR secondaries standard secenario for Galactic CRs: sources are SNRs: kinetic energy output of SNe: 10M ejected with v cm/s every 30 yr L SN,kin erg/s explains local energy density of CR ε CR 1 ev/cm 3 for a escape time from disc τ esc yr 1.order Fermi shock acceleration dn/de E γ with γ = diffusion with D(E) τ esc (E) E δ and δ 0.6 explains observed spectrum E 2.6 electrons, positrons: τ loss τ esc and τ loss 1/E electrons dn /de E γ 1 positrons dn + /de E γ δ 1
25 Astrophysical sources for anti-matter: CR secondaries standard secenario for Galactic CRs: sources are SNRs: kinetic energy output of SNe: 10M ejected with v cm/s every 30 yr L SN,kin erg/s explains local energy density of CR ε CR 1 ev/cm 3 for a escape time from disc τ esc yr 1.order Fermi shock acceleration dn/de E γ with γ = diffusion with D(E) τ esc (E) E δ and δ 0.6 explains observed spectrum E 2.6 electrons, positrons: τ loss τ esc and τ loss 1/E electrons dn /de E γ 1 positrons dn + /de E γ δ 1 ratio n + n E δ secondaries cannot expalain increasing positron fraction
26 Astrophysical explanations I: Pulsars Pulsar: (fast) rotating, stronly magnetized neutron star
27 Astrophysical explanations I: Pulsars Pulsar: (fast) rotating, stronly magnetized neutron star suggested as source of CRs up-to ev
28 Astrophysical explanations I: Pulsars Pulsar: (fast) rotating, stronly magnetized neutron star suggested as source of CRs up-to ev produce hard spectrum, dn/de E 1.5
29 Astrophysical explanations I: Pulsars Pulsar: (fast) rotating, stronly magnetized neutron star suggested as source of CRs up-to ev produce hard spectrum, dn/de E 1.5 old pulsars (> 10 5 yr) lost nebula positrons can escape
30 Astrophysical explanations I: Pulsars Pulsar: (fast) rotating, stronly magnetized neutron star suggested as source of CRs up-to ev produce hard spectrum, dn/de E 1.5 old pulsars (> 10 5 yr) lost nebula positrons can escape few sources (Geminga, B ) may dominate HE part anisotropy or peaks possible
31 Astrophysical explanations I: Pulsars
32 Astrophysical explanations I: Pulsars
33 Astrophysical explanations: Pulsars - Geminga+B
34 Astrophysical explanations: Pulsars - Geminga+B
35 Astrophysical explanations: Pulsars if Geminga and B dominate HE part:
36 Astrophysical explanations: Pulsars if Geminga and B dominate HE part: implies anisotropy from Fick s law F a (E) = D ab b n(e,x) anisotropy δ = I max I min = 3D 1 n I max + I min n n z
37 Astrophysical explanations: Pulsars
38 Astrophysical explanations: old SNRs
39 Astrophysical explanations II: SNR [P. Blasi 09 ] N CR (E) N e (E) for energies E m p in acceleration region
40 Astrophysical explanations II: SNR [P. Blasi 09 ] N CR (E) N e (E) for energies E m p in acceleration region significant e ± production even for small τ pp in source
41 Astrophysical explanations II: SNR [P. Blasi 09 ] N CR (E) N e (E) for energies E m p in acceleration region significant e ± production even for small τ pp in source secondary e ± are accelerated, spectra becomes harder
42 Astrophysical explanations II: SNR [P. Blasi 09 ] N CR (E) N e (E) for energies E m p in acceleration region significant e ± production even for small τ pp in source secondary e ± are accelerated, spectra becomes harder several important implications for CR physics predicts also increase of p/p
43 Astrophysical explanations II: SNR [P. Blasi 09 ]
44 Neutralino annihilations CDM velocitities v 2 v p-wave annihilations strongly suppressed
45 Neutralino annihilations CDM velocitities v 2 v p-wave annihilations strongly suppressed for Majorana particles: s-wave σ m 2 f annihilations into b, t quarks and W, Z, h, H, A
46 Neutralino annihilations CDM velocitities v 2 v p-wave annihilations strongly suppressed for Majorana particles: s-wave σ m 2 f annihilations into b, t quarks and W, Z, h, H, A typical hadronization spectra with φ ν (E)/2 φ γ (E) 3φ e (E) 10φ N (E)
47 Neutralino annihilations CDM velocitities v 2 v p-wave annihilations strongly suppressed for Majorana particles: s-wave σ m 2 f annihilations into b, t quarks and W, Z, h, H, A typical hadronization spectra with φ ν (E)/2 φ γ (E) 3φ e (E) 10φ N (E) photon signal I sm (E,ψ) = dn i de Z σv 2m 2 X l.o.s. ds ρ2 [r(s,ψ)], 4π
48 Neutralino annihilations CDM velocitities v 2 v p-wave annihilations strongly suppressed for Majorana particles: s-wave σ m 2 f annihilations into b, t quarks and W, Z, h, H, A typical hadronization spectra with φ ν (E)/2 φ γ (E) 3φ e (E) 10φ N (E) photon signal I sm (E,ψ) = dn i de Z σv 2m 2 X l.o.s. ds ρ2 [r(s,ψ)], 4π main uncertainty: boost factor = enhancement compared to σv = cm 3 /s and ρ = ρ sm
49 DM annihilations and PAMELA/ATIC standard branching ratios and mass: overproduction of anti-protons
50 DM annihilations and PAMELA/ATIC non-standard branching ratios: only leptons best-fit to ATIC boost factor 1000 needed but minimal γ-ray flux from Bremsstrahlung, not seen
51 DM annihilations and PAMELA/ATIC standard branching ratios: hide p above E max of Pamela happy with M = 10 TeV?
52 Boost factor particle physics: σv 1/v allowed by unitarity requires s-channel resonances or bound states
53 Boost factor particle physics: σv 1/v allowed by unitarity requires s-channel resonances or bound states Sommerfeld enhancement in Coulomb limit S 0 = πx 1 exp( πx), x = g2 β
54 Boost factor particle physics: σv 1/v allowed by unitarity requires s-channel resonances or bound states Sommerfeld enhancement in Coulomb limit S 0 = πx 1 exp( πx), x = g2 β for Coulomb limit, add new light boson
55 Boost factor particle physics: σv 1/v allowed by unitarity requires s-channel resonances or bound states Sommerfeld enhancement in Coulomb limit S 0 = πx 1 exp( πx), x = g2 β for Coulomb limit, add new light boson astrophysics: clumpy substructure of DM halo
56 Boost factor particle physics: σv 1/v allowed by unitarity requires s-channel resonances or bound states Sommerfeld enhancement in Coulomb limit S 0 = πx 1 exp( πx), x = g2 β for Coulomb limit, add new light boson astrophysics: clumpy substructure of DM halo Dm in clumps may be colder both effects magnify each other
57 Summary Cosmology probes only generic properties of DM: abundance, cold, dissipation-less
58 Summary Cosmology probes only generic properties of DM: abundance, cold, dissipation-less various candidates with these properties: neutralino, gravitino, axion, axino, SHDM,...
59 Summary Cosmology probes only generic properties of DM: abundance, cold, dissipation-less various candidates with these properties: neutralino, gravitino, axion, axino, SHDM,... only a combination of accelerator, direct and/or indirect searches can identify the DM particle
60 Summary Cosmology probes only generic properties of DM: abundance, cold, dissipation-less various candidates with these properties: neutralino, gravitino, axion, axino, SHDM,... only a combination of accelerator, direct and/or indirect searches can identify the DM particle even in the best-case scenario (SUSY at LHC), confirmation of LSP as DM by (in-) direct searches necessary all sorts of data are coming!
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