Gravitino Dark Matter with Broken R-Parity
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- Austen Carson
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![017, arxiv:1111.6779 [hep-ph] and ongoing work.](/docs-images/78/77324609/images/1-3.jpg "Collaborators: L. Covi, T. Delahaye, A. Ibarra, D.")
1 Gravitino Dark Matter with Broken R-Parity Michael Grefe Departamento de Física Teórica Instituto de Física Teórica UAM/CSIC Universidad Autónoma de Madrid Instituto de Física Corpuscular CSIC/Universitat de València València 21 June 2012 Based on JCAP 0901 (2009) 029, JCAP 1004 (2010) 017, arxiv: [hep-ph] and ongoing work. Collaborators: L. Covi, T. Delahaye, A. Ibarra, D. Tran, G. Vertongen Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
2 Outline Motivation for Unstable Gravitino Dark Matter Gravitino Dark Matter with Broken R Parity Indirect Detection of Gravitino Dark Matter Implications for the LHC Limits on the Amount of R-Parity Violation Conclusions and Outlook Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
3 Motivation for Unstable Gravitino Dark Matter Motivation for Unstable Gravitino Dark Matter Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
![significantly to the energy density of the universe [van Albada et al. (1985)] [Clowe et al.](/docs-images/78/77324609/images/4-2.jpg "(2006)] [NASA / WMAP Science Team] I Dark matter properties known from observations: No electromagnetic and strong")
4 Motivation for Unstable Gravitino Dark Matter What Do We Know about Dark Matter? I Dark matter is observed on various scales through its gravitational interaction I Dark matter contributes significantly to the energy density of the universe [van Albada et al. (1985)] [Clowe et al. (2006)] [NASA / WMAP Science Team] I Dark matter properties known from observations: No electromagnetic and strong interactions At least gravitational and at most weak-scale interactions Non-baryonic Cold (maybe warm) Long-lived on cosmological time scales but not necessarily stable! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity [NASA / WMAP Science Team] IFIC Vale ncia 21 June / 32
5 Motivation for Unstable Gravitino Dark Matter What Do We Know about Dark Matter? I Dark matter is observed on various scales through its gravitational interaction I Dark matter contributes significantly to the energy density of the universe [van Albada et al. (1985)] [Clowe et al. (2006)] [NASA / WMAP Science Team] I Dark matter properties known from observations: No electromagnetic and strong interactions At least gravitational and at most weak-scale interactions Non-baryonic Cold (maybe warm) Long-lived on cosmological time scales but not necessarily stable! [NASA / WMAP Science Team] Particle dark matter could be a (super)wimp with lifetime age of the universe! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC Vale ncia 21 June / 32
6 Motivation for Unstable Gravitino Dark Matter How Can We Unveil the Nature of Dark Matter? I There are three main search strategies for dark matter: Direct detection of dark matter in the scattering off matter nuclei Production of dark matter particles at colliders Indirect detection of dark matter in cosmic ray signatures [Max-Planck-Institut fu r Kernphysik] WIMP-Nucleon Cross Section [cm2] DAMA/Na CoGeNT DAMA/I CDMS EDELWEISS XENON100 (2010) XENON100 (2011) [CERN] Michael Grefe (IFT UAM/CSIC) Buchmueller et al WIMP Mass [GeV/c2] [Aprile et al. (2011)] Gravitino Dark Matter with Broken R-Parity 1000 [AMS collaboration] IFIC Vale ncia 21 June / 32
7 Motivation for Unstable Gravitino Dark Matter How Can We Unveil the Nature of Dark Matter? I There are three main search strategies for dark matter: Direct detection of dark matter in the scattering off matter nuclei Production of dark matter particles at colliders Indirect detection of dark matter in cosmic ray signatures [Max-Planck-Institut fu r Kernphysik] WIMP-Nucleon Cross Section [cm2] DAMA/Na CoGeNT DAMA/I CDMS EDELWEISS XENON100 (2010) XENON100 (2011) [CERN] Buchmueller et al WIMP Mass [GeV/c2] [Aprile et al. (2011)] 1000 [AMS collaboration] A combination will be necessary to identify the nature of particle dark matter! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC Vale ncia 21 June / 32
8 Motivation for Unstable Gravitino Dark Matter Why Are We Interested in Unstable Gravitino Dark Matter? Smallness of observed neutrino masses motivates seesaw mechanism Can explain baryon asymmetry via thermal leptogenesis [Fukugita, Yanagida (1986)] Requires high reheating temperature after inflation: T R 10 9 GeV [Davidson, Ibarra (2002)] Supergravity predicts the gravitino as the spin-3/2 superpartner of the graviton Gravitinos are abundantly produced in thermal scatterings: ( Ω 3/2 h 2 T R GeV ) ( 100 GeV m 3/2 ) ( ) 2 m g 1 TeV [Bolz et al. (2001)] Problem in scenarios with neutralino dark matter: Gravitino decays suppressed by Planck scale: τ 3/2 M2 Pl m 3 3 years 3/2 ( ) GeV m 3/2 Late decays with τ O( s) in conflict with BBN Cosmological gravitino problem Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
9 Motivation for Unstable Gravitino Dark Matter Why Are We Interested in Unstable Gravitino Dark Matter? Smallness of observed neutrino masses motivates seesaw mechanism Can explain baryon asymmetry via thermal leptogenesis [Fukugita, Yanagida (1986)] Requires high reheating temperature after inflation: T R 10 9 GeV [Davidson, Ibarra (2002)] Supergravity predicts the gravitino as the spin-3/2 superpartner of the graviton Gravitinos are abundantly produced in thermal scatterings: ( Ω 3/2 h 2 T R GeV ) ( 100 GeV m 3/2 ) ( ) 2 m g 1 TeV [Bolz et al. (2001)] Problem in scenarios with neutralino dark matter: Gravitino decays suppressed by Planck scale: τ 3/2 M2 Pl m 3 3 years 3/2 ( ) GeV m 3/2 Late decays with τ O( s) in conflict with BBN Cosmological gravitino problem Possible solution: Gravitino is the LSP and thus stable! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
10 Motivation for Unstable Gravitino Dark Matter Why Are We Interested in Unstable Gravitino Dark Matter? Gravitino relic density: ( Ω 3/2 h 2 T R GeV ) ( 100 GeV m 3/2 ) ( ) 2 m g 1 TeV Correct relic density possible for m 3/2 > O(10) GeV Gravitino dark matter Still problematic: NLSP can only decay to gravitino LSP: τ NLSP 48πM2 Pl m2 3/2 m 5 NLSP ( ) m3/2 2 ( 150 GeV 9 days 10 GeV m NLSP ) 5 Late NLSP decays are in conflict with BBN Cosmological gravitino problem Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
11 Motivation for Unstable Gravitino Dark Matter Why Are We Interested in Unstable Gravitino Dark Matter? Gravitino relic density: ( Ω 3/2 h 2 T R GeV ) ( 100 GeV m 3/2 ) ( ) 2 m g 1 TeV Correct relic density possible for m 3/2 > O(10) GeV Gravitino dark matter Still problematic: NLSP can only decay to gravitino LSP: τ NLSP 48πM2 Pl m2 3/2 m 5 NLSP ( ) m3/2 2 ( 150 GeV 9 days 10 GeV m NLSP ) 5 Late NLSP decays are in conflict with BBN Cosmological gravitino problem Possible solution: R-parity is not exactly conserved! Other options: Choose harmless NLSP like sneutrino [Covi, Kraml (2007)] Dilute NLSP density by late entropy production [Buchmüller et al. (2006)] Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
12 Gravitino Dark Matter with Broken R-Parity Gravitino Dark Matter with Broken R-Parity Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
13 Gravitino Dark Matter with Broken R-Parity Gravitino Dark Matter with Bilinear R-Parity Violation Bilinear R-parity violation: W /Rp = µ i H ul i, L soft /R p = B i H u li + m 2 H d l i H d l i + h.c. Only lepton number violated Proton remains stable! R-parity violation parametrized by non-vanishing sneutrino VEV: Cosmological bounds on R-violating couplings ξ = ν v Lower bound: The NLSP must decay fast enough to evade BBN constraints: ξ O(10 11 ) Upper bound: No washout of the lepton/baryon asymmetry: ξ O(10 7 ) Tiny bilinear R-parity violation can be related to U(1) B L breaking [Buchmüller et al. (2007)] Gravitino decay suppressed by Planck scale and small R-parity violation Gravitino decay width: Γ 3/2 ξ2 m 3 3/2 M 2 Pl [Takayama, Yamaguchi (2000)] The gravitino lifetime by far exceeds the age of the universe (τ 3/ s) Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
14 Gravitino Dark Matter with Broken R-Parity Gravitino Dark Matter with Bilinear R-Parity Violation Bilinear R-parity violation: W /Rp = µ i H ul i, L soft /R p = B i H u li + m 2 H d l i H d l i + h.c. Only lepton number violated Proton remains stable! R-parity violation parametrized by non-vanishing sneutrino VEV: Cosmological bounds on R-violating couplings ξ = ν v Lower bound: The NLSP must decay fast enough to evade BBN constraints: ξ O(10 11 ) Upper bound: No washout of the lepton/baryon asymmetry: ξ O(10 7 ) Tiny bilinear R-parity violation can be related to U(1) B L breaking [Buchmüller et al. (2007)] Gravitino decay suppressed by Planck scale and small R-parity violation Gravitino decay width: Γ 3/2 ξ2 m 3 3/2 M 2 Pl [Takayama, Yamaguchi (2000)] The gravitino lifetime by far exceeds the age of the universe (τ 3/ s) The unstable gravitino is a well-motivated and viable dark matter candidate! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
15 Gravitino Dark Matter with Broken R-Parity Phenomenology of Unstable Gravitino Dark Matter Rich phenomenology instead of elusive gravitinos: A long-lived NLSP could be observed at the LHC [Buchmüller et al. (2007), Bobrovskyi et al. (2010, 2011)] Gravitino decays lead to possibly observable signals at indirect detection experiments [Takayama, Yamaguchi (2000), Buchmüller et al. (2007), Bertone et al. (2007), Ibarra, Tran (2008), Ishiwata et al. (2008) etc.] Gravitinos could be indirectly observed at colliders and in the spectra of cosmic rays! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
16 Gravitino Dark Matter with Broken R-Parity Bilinear R-Parity Violation: Neutralino Neutrino Mixing Bilinear R-parity violation extends neutralino mass matrix to include neutrinos 7 7 matrix with basis ψi 0 = ( i γ, i Z, H u 0, H d 0, ν i ) T M 1 cw 2 + M 2 sw 2 (M 2 M 1 ) s W c W (M 2 M 1 ) s W c W M 1 s MN 7 W 2 + M 2 cw 2 m Z s β m Z c β m Z ξ j = 0 m Z s β 0 µ 0 0 m Z c β µ m Z ξ i Diagonalized by unitary matrix N 7 Mixing to neutrinos via neutrino zino coupling: Nν 7 i X ξ i U X Z Analytical approximation shows dependence on SUSY parameters U γ Z m Z sin θ W cos θ W M 2 M 1 M 1 M 2 U Z Z m Z ( sin 2 θ W M 1 ) + cos2 θ W M 2 Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
17 Gravitino Dark Matter with Broken R-Parity Bilinear R-Parity Violation: Chargino Charged Lepton Mixing Bilinear R-parity violation extends chargino mass matrix to include charged leptons 5 5 matrix with basis vectors ψ = ( i W, H d, l i ) T and ψ + = ( i W +, H u +, e c + i ) T M 5 M 2 2 mw s β 0 C = 2 2 mw c β µ m lij ξ i c β mw ξ i 0 m lij Diagonalized by unitary matrices U 5 and V 5 Mixing to left-handed leptons via lepton wino coupling: Ul 5 i X 2 ξ i U X W Mixing to right-handed leptons suppressed and negligible Analytical approximation shows dependence on SUSY parameters U W W m W M2 Bilinear R-parity also induces mass mixing in the scalar sector Mixing between SM-like Higgs and sneutrino proportional to sneutrino VEV Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
18 Gravitino Dark Matter with Broken R-Parity Gravitino Decay Channels: 2-body Decays Several two-body decay channels: ψ 3/2 γ ν i, Z ν i, W l i, h ν i +... Γ γνi ξ2 i m 3/ π M Pl 2 U γ Z 2 ξ2 i m 3/2 3 ( ) M2 M 2 1 M Pl 2 M 1 M 2 Γ Z νi ξ2 i m 3/2 3 ( ) 1 m2 2 { ( 32 π M Pl 2 Z U 2 Z m 2 ) } f Z +... m 3/2 2 Z m 3/2 2 Γ W + l ξ2 i m 3 ( ) 3/2 1 m2 2 { ( i 32 π M Pl 2 W U 2 W m 2 ) } f W +... m 3/2 2 W m 3/2 2 Γ hνi ξ2 i m 3/2 3 ( ) 1 m π M Pl 2 h m 3/2 2 Dependence on mass mixings dependence on gaugino masses Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
19 Gravitino Dark Matter with Broken R-Parity Gravitino Decay Channels: 3-body Decays For m 3/2 < m W also three-body decays can play an important role [Choi et al. (2010)] +... dγ Z ν i ds dγ W + l i ds dγ h ν i ds ξi 2 m 3/2 3 ( ) 2 { ( ) } M Pl 2 ((s m2 Z )2 +m Z 2 Γ2 ) 1 s s U 2 Z f s +... m Z 3/2 2 Z m 3/2 2 ξi 2 m 3 ( ) 3/2 2 { ( ) } M Pl 2 ((s m2 W )2 +m W 2 Γ2 ) 1 s s U 2 W f s +... m W 3/2 2 W m 3/2 2 ξi 2 m 3/2 3 m2 f s ( ) 4 M Pl 2 v2 ((s m h 2)2 +m h 2Γ2) 1 s m h 3/2 2 I will concentrate on 2-body dacays in this talk Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
20 Gravitino Dark Matter with Broken R-Parity Gravitino Branching Ratios and Final State Particle Spectra Branching ratios are independent of strength of R-parity violation Ratio between γ ν i and other channels is model-dependent Ψ32ZΝi, m GeV Branching Ratio Γ Z Νi W i Wi ZΝi hνi Gravitino MassGeV ΓΝ i Νe Γ ΝΜ d 10 3 ΝΤ p Kinetic EnergyGeV Gravitino decays produce spectra of stable cosmic rays: γ, e, p, ν e/µ/τ, d Two-body decay spectra generated with PYTHIA Deuteron coalescence treated on event-by-event basis in PYTHIA [Kadastik et al. (2009)] Spectrum dndlog 10 T e Νi Ν e Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
21 Gravitino Dark Matter with Broken R-Parity Gravitino Branching Ratios and Final State Particle Spectra Branching ratios are independent of strength of R-parity violation Ratio between γ ν i and other channels is model-dependent Ψ32ZΝi, m GeV Branching Ratio Γ Z Νi W i Wi ZΝi hνi Gravitino MassGeV ΓΝ i Νe Γ ΝΜ d 10 3 ΝΤ p Kinetic EnergyGeV Gravitino decays produce spectra of stable cosmic rays: γ, e, p, ν e/µ/τ, d Two-body decay spectra generated with PYTHIA Deuteron coalescence treated on event-by-event basis in PYTHIA [Kadastik et al. (2009)] Basis for phenomenology of indirect gravitino dark matter searches! Spectrum dndlog 10 T e Νi Ν e Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
22 Indirect Detection of Gravitino Dark Matter Indirect Detection of Gravitino Dark Matter Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
![(IFT UAM/CSIC) [AMS-02 Collaboration] Gravitino Dark Matter with](/docs-images/78/77324609/images/23-3.jpg "Broken R-Parity [IceCube Collaboration] IFIC Vale ncia 21 June")
23 Indirect Detection of Gravitino Dark Matter Cosmic-Ray Propagation I Cosmic rays from gravitino decays propagate through the Milky Way I Experiments observe spectra of gamma rays, charged cosmic rays and neutrinos [NASA E/PO, SSU, Aurore Simonnet] Michael Grefe (IFT UAM/CSIC) [AMS-02 Collaboration] Gravitino Dark Matter with Broken R-Parity [IceCube Collaboration] IFIC Vale ncia 21 June / 32
24 Indirect Detection of Gravitino Dark Matter What Is the Difference of Dark Matter Annihilations and Decays? Different angular distribution of the gamma-ray/neutrino flux from the galactic halo: Dark Matter Annihilation dj halo de = σv DM dn ρ 2 halo( 8π mdm 2 de l) d l l.o.s. particle physics astrophysics Dark Matter Decay dj halo de = 1 dn ρ halo ( 4π τ DM m DM de l) d l l.o.s. particle physics astrophysics NFW 100 Einasto Isothermal annihilation 10 decay 1 value at galactic anticenter Annihilation (e.g. WIMP dark matter) Annihilation cross section related to relic density Strong signal from peaked structures Uncertainties from choice of halo profile Decay (e.g. unstable gravitino dark matter) Lifetime unrelated to production in the early universe Less anisotropic signal Less sensitive to the halo model Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
25 Indirect Detection of Gravitino Dark Matter What Is the Difference of Dark Matter Annihilations and Decays? Different angular distribution of the gamma-ray/neutrino flux from the galactic halo: Dark Matter Annihilation dj halo de = σv DM dn ρ 2 halo( 8π mdm 2 de l) d l l.o.s. particle physics astrophysics Dark Matter Decay dj halo de = 1 dn ρ halo ( 4π τ DM m DM de l) d l l.o.s. particle physics astrophysics NFW 100 Einasto Isothermal annihilation 10 decay 1 value at galactic anticenter Annihilation (e.g. WIMP dark matter) Annihilation cross section related to relic density Strong signal from peaked structures Uncertainties from choice of halo profile Decay (e.g. unstable gravitino dark matter) Lifetime unrelated to production in the early universe Less anisotropic signal Less sensitive to the halo model Directional detection can distinguish unstable gravitino from standard WIMPs! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
26 Indirect Detection of Gravitino Dark Matter Gravitino Decay Signals in Cosmic-Ray Spectra T 3 Antiproton FluxGeV 2 m 2 s 1 sr antiproton flux background PAMELA AMS01 IMAX Τ s m GeV 1 TeV 10 TeV Kinetic EnergyGeV CAPRICE98 CAPRICE94 MASS91 BESSPolar II BESSPolar BESS 00 BESS 99 BESS 98 BESS 9597 E 2 GammaRay FluxGeV m 2 s 1 sr isotropic diffuse gamma-ray flux Τ s m GeV 1 TeV 10 TeV EnergyGeV Observed antiproton spectrum well described by astrophysical background No need for contribution from dark matter Isotropic diffuse gamma-ray spectrum exhibits power-law behaviour Fermi LAT EGRETStrong et al. EGRETSreekumar et al. Source not completely understood, but no sign of spectral features of a particle decay Even without astrophysical backgrounds lifetimes below O( ) s excluded Gravitino decay cannot be the origin of the PAMELA and Fermi LAT cosmic-ray anomalies Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
27 Indirect Detection of Gravitino Dark Matter Gravitino Decay Signals in Cosmic-Ray Spectra T 3 Antiproton FluxGeV 2 m 2 s 1 sr antiproton flux background PAMELA AMS01 IMAX Τ s m GeV 1 TeV 10 TeV Kinetic EnergyGeV CAPRICE98 CAPRICE94 MASS91 BESSPolar II BESSPolar BESS 00 BESS 99 BESS 98 BESS 9597 E 2 GammaRay FluxGeV m 2 s 1 sr isotropic diffuse gamma-ray flux Τ s m GeV 1 TeV 10 TeV EnergyGeV Observed antiproton spectrum well described by astrophysical background No need for contribution from dark matter Isotropic diffuse gamma-ray spectrum exhibits power-law behaviour Fermi LAT EGRETStrong et al. EGRETSreekumar et al. Source not completely understood, but no sign of spectral features of a particle decay Even without astrophysical backgrounds lifetimes below O( ) s excluded Gravitino decay cannot be the origin of the PAMELA and Fermi LAT cosmic-ray anomalies Astrophysical sources like pulsars required to explain cosmic-ray excesses! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
28 Indirect Detection of Gravitino Dark Matter Antideuteron Signals from Gravitino Decays In particular sensitive at low energies due to small astrophysical background AMS-02 and GAPS will be able to put strong constraints on light gravitinos TnAntideuteron Fluxm 2 s 1 sr BESS 9700 ΦF 500 MV GAPSULDB GAPSLDB AMS02 AMS02 background Τ s m GeV 1 TeV 10 TeV Kinetic Energy per NucleonGeVn Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
29 Indirect Detection of Gravitino Dark Matter Antideuteron Signals from Gravitino Decays In particular sensitive at low energies due to small astrophysical background AMS-02 and GAPS will be able to put strong constraints on light gravitinos TnAntideuteron Fluxm 2 s 1 sr BESS 9700 ΦF 500 MV GAPSULDB GAPSLDB AMS02 AMS02 background Τ s m GeV 1 TeV 10 TeV Kinetic Energy per NucleonGeVn Antideuterons are a valuable channel for light gravitino searches! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
30 Indirect Detection of Gravitino Dark Matter Neutrino Signals from Gravitino Decays Neutrinos provide directional information like gamma rays Gravitino signal features neutrino line at the end of the spectrum Atmospheric neutrinos are the dominant background for the gravitino signal Discrimination of neutrino flavours would allow to reduce the background Signal-to-background ratio best at the end of the spectrum and for large gravitino masses E 2 Neutrino FluxGeV m 2 s 1 sr Τ s ΝΤ ΝΜ Νe m GeV 1 TeV 10 TeV EnergyGeV IceCube40 UnfoldingΝΜ IceCube40ΝΜ AMANDAII UnfoldingΝΜ AMANDAII ForwardΝΜ SuperKamiokandeΝΜ FréjusΝΜ FréjusΝe Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
31 Indirect Detection of Gravitino Dark Matter Neutrino Signals from Gravitino Decays Neutrinos provide directional information like gamma rays Gravitino signal features neutrino line at the end of the spectrum Atmospheric neutrinos are the dominant background for the gravitino signal Discrimination of neutrino flavours would allow to reduce the background Signal-to-background ratio best at the end of the spectrum and for large gravitino masses E 2 Neutrino FluxGeV m 2 s 1 sr Τ s ΝΤ ΝΜ Νe m GeV 1 TeV 10 TeV EnergyGeV IceCube40 UnfoldingΝΜ IceCube40ΝΜ AMANDAII UnfoldingΝΜ AMANDAII ForwardΝΜ SuperKamiokandeΝΜ FréjusΝΜ FréjusΝe Neutrinos are a valuable channel for heavy gravitino searches! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
32 Indirect Detection of Gravitino Dark Matter Neutrino Detection with Upward Through-Going Muons Muon tracks from charged current DIS of muon neutrinos off nuclei outside the detector Advantages Muon track reconstruction is well-understood at neutrino telescopes Disadvantages Neutrino nucleon DIS and propagation energy losses shift muon spectrum to lower energies Bad energy resolution (0.3 in log 10 E) smears out cut-off energy Muon Fluxkm 2 yr Upward ThroughGoing Muons 10 atmospheric background Statistical Significance m GeV 1 TeV 10 TeV 0.01 Τ s EnergyGeV Upward ThroughGoingMuons Τ s m GeV 1 TeV 10 TeV EnergyGeV Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
33 Indirect Detection of Gravitino Dark Matter Neutrino Detection Improvements Using Showers Hadronic and electromagnetic showers from charged current DIS of electron and tau neutrinos and neutral current interactions of all neutrino flavours inside the detector Disadvantages TeV-scale showers are difficult to discriminate from short muon tracks Advantages 3 larger signal and 3 lower background compared to other channels Better energy resolution (0.18 in log 10 E) helps to distinguish spectral features 10 6 Shower Events 100 Shower Events Shower Ratekm 3 yr atmospheric background Τ s m GeV 1 TeV 10 TeV EnergyGeV Statistical Significance Τ s m GeV 1 TeV 10 TeV EnergyGeV Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
34 Indirect Detection of Gravitino Dark Matter Neutrino Detection Improvements Using Showers Hadronic and electromagnetic showers from charged current DIS of electron and tau neutrinos and neutral current interactions of all neutrino flavours inside the detector Disadvantages TeV-scale showers are difficult to discriminate from short muon tracks Advantages 3 larger signal and 3 lower background compared to other channels Better energy resolution (0.18 in log 10 E) helps to distinguish spectral features 10 6 Shower Events 100 Shower Events Shower Ratekm 3 yr atmospheric background Τ s m GeV 1 TeV 10 TeV EnergyGeV Statistical Significance Τ s 0.01 m GeV 1 TeV 10 TeV EnergyGeV Showers are potentially the best channel for dark matter searches in neutrinos! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
35 Indirect Detection of Gravitino Dark Matter Limits on the Gravitino Lifetime Gravitino Lifetimes excluded by line searches excluded by diffuse flux Gravitino MassGeV Fermi LAT photon line Vertongen et al. photon line Fermi LAT diffuse flux Cosmic-ray data give bounds on gravitino lifetime Photon line bounds very strong for low gravitino masses Uncertainties from charged cosmic-ray propagation Background subtraction will improve bounds Antideuterons can be complementary to photon line searches for low gravitino masses Neutrino bounds are competitive for heavy gravitinos Wide range of bounds from multi-messenger approach! Gravitino Lifetimes antideuteron sensitivity excluded by electronpositron flux excluded by antiproton flux excluded by positron fraction Gravitino Lifetimes Gravitino MassGeV Fermi LATH.E.S.S. e e PAMELA p exclusion from PAMELA e e e throughgoing muons after 1 year at IceCubeDeepCore Gravitino MassGeV Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
36 Implications for the LHC Implications for the LHC Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
37 Implications for the LHC Implications for the LHC: Stau NLSP NLSP decays before BBN but may be metastable on collider scales Stau decay channels: τ R τ ν µ, µ ν τ and τ L t R b L Characteristic signatures: Slow particle with long ionising charged track Displaced vertex with missing energy and muon track or jet Minimal decay length from washout limit: 4 mm 10 3 Stau NLSP: Minimal allowed decay length c 1 [m] [GeV] m 1 Min O.P. O.P. in scenario (B) m 3/2 >m EWPT m 3/2 [GeV] [Huang et al. (2011)] Gamma-ray limits from galaxy clusters constrain decay length [Huang et al. (2011)] Minimal decay lengths from current limits: O(100) m O(10) km Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
38 Implications for the LHC 1 Implications for the LHC: Neutralino NLSP Neutralino decay channels: χ 0 1 Z ν i, W + l i, h ν i Bino decay length is directly related to gravitino decay width Characteristic signatures: Displaced vertices far from the interaction point For too small R-parity violation indistinguishable from stable neutralino decay chain with secondary vertices 10 3 Neutralino NLSP: Minimal allowed decay length χ [m] [GeV] m 0 Min O.P. O.P. in scenario (A) m 3/2>m EWPT m 3/2 [GeV] [Bobrovskyi et al. (2011)] [Huang et al. (2011)] Gamma-ray limits from galaxy clusters constrain decay length [Huang et al. (2011)] Minimal decay lengths from current limits: O(100) m O(10) km Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
39 Limits on the Amount of R-Parity Violation Limits on the Amount of R-Parity Violation Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
40 Limits on the Amount of R-Parity Violation Limits on the Amount of R-Parity Violation Limits on gravitino lifetime constrain the strength of R-parity violation: τ 3/2 Limits from photon line searches dominate for small gravitino masses For heavier gravitino bounds from all cosmic-ray channels are comparable M2 Pl ξ 2 m 3 3/2 cosmic-ray limits LHC sensitivity for bino-like NLSP decays 10 7 Ξ 10 7 RParity Violating ParameterΞ Fermi LAT Γ line Fermi LAT diffuse Γ PAMELA p GAPSAMS02 d prospects SuperKamiokandeΝΜ IceCube ΝΜ prospects Ξ Gravitino MassGeV [Bobrovskyi et al. (2011)] The LHC has the potential to detect NLSP decays beyond cosmic-ray constraints Good sensitivity with clean decay chain: χ 0 1 Z ν i and Z µ + µ Taking all channels can improve sensitivity another order of magnitude [Bobrovskyi et al. (2011)] Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
41 Limits on the Amount of R-Parity Violation Limits on the Amount of R-Parity Violation Limits on gravitino lifetime constrain the strength of R-parity violation: τ 3/2 Limits from photon line searches dominate for small gravitino masses For heavier gravitino bounds from all cosmic-ray channels are comparable M2 Pl ξ 2 m 3 3/2 cosmic-ray limits LHC sensitivity for bino-like NLSP decays 10 7 Ξ 10 7 RParity Violating ParameterΞ Fermi LAT Γ line Fermi LAT diffuse Γ PAMELA p GAPSAMS02 d prospects SuperKamiokandeΝΜ IceCube ΝΜ prospects Ξ Gravitino MassGeV [Bobrovskyi et al. (2011)] The LHC has the potential to detect NLSP decays beyond cosmic-ray constraints Good sensitivity with clean decay chain: χ 0 1 Z ν i and Z µ + µ Taking all channels can improve sensitivity another order of magnitude [Bobrovskyi et al. (2011)] Indirect and collider searches probe interesting range of R-parity violation! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
42 Conclusions and Outlook Conclusions and Outlook Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
43 Conclusions and Outlook Conclusions Gravitino dark matter with broken R-parity is well motivated from cosmology Consistent with thermal leptogenesis and big bang nucleosynthesis The Gravitino lifetime is naturally in the range of indirect detection experiments Cannot explain the PAMELA and Fermi LAT excesses due to constraints from gamma rays and antiprotons Multi-messenger approach constrains gravitino lifetime and strength of R-parity violation Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
44 Conclusions and Outlook Outlook Forthcoming experiments like AMS-02 will greatly improve cosmic-ray data Antideuteron searches will probe light gravitino dark matter Neutrino experiments like IceCube will probe heavy gravitino dark matter LHC may discover decays of metastable NLSPs beyond cosmic-ray constraints on R-parity violation We are living in interesting times for dark matter searches! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
45 Conclusions and Outlook Outlook Forthcoming experiments like AMS-02 will greatly improve cosmic-ray data Antideuteron searches will probe light gravitino dark matter Neutrino experiments like IceCube will probe heavy gravitino dark matter LHC may discover decays of metastable NLSPs beyond cosmic-ray constraints on R-parity violation We are living in interesting times for dark matter searches! Thanks for your attention! Michael Grefe (IFT UAM/CSIC) Gravitino Dark Matter with Broken R-Parity IFIC València 21 June / 32
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