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Antiproton Limits on Decaying Gravitino Dark Matter
Michael GrefeDepartamento de Fı́sica TeóricaInstituto de Fı́sica Teórica UAM/CSICUniversidad Autónoma de Madrid
Particle Theory Journal ClubRudolf Peierls Centre for Theoretical Physics – University of Oxford
13 June 2013
based on T. Delahaye and MG: arXiv:1305.7183
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 1 / 26
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Outline
I Motivation for Decaying Gravitino Dark Matter
I Gravitino Dark Matter with Broken R Parity
I Indirect Detection of Gravitino Dark Matter
I Antiproton Limits on the Lifetime and the Amount of R-Parity Violation
I Conclusions
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 2 / 26
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Motivation for Decaying Gravitino Dark Matter
Motivation forDecaying Gravitino Dark Matter
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 3 / 26
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Motivation for Decaying Gravitino Dark Matter
What Do We Know about Dark Matter?
I Observed on various scales through its gravitational interactionI Contributes significantly to the energy density of the universe
[M. Whittle] [ESA / Planck Collaboration] [NASA / Clowe et al.]
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)• Extremely long-lived but can be unstable!
[ESA / Planck Collaboration]
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 4 / 26
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Motivation for Decaying Gravitino Dark Matter
How Can We Unveil the Nature of Dark Matter?
I Three search strategies for dark matter
• Direct detection in the scattering off matter nuclei• Production of dark matter particles at colliders• Indirect detection in cosmic ray signatures
[Max-Planck-Institut für Kernphysik]
[CERN] [Aprile et al. (2012)] [AMS Collaboration]
A combination will be necessary to identify the nature of particle dark matter!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 5 / 26
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Motivation for Decaying Gravitino Dark Matter
How Can We Unveil the Nature of Dark Matter?
I Three search strategies for dark matter
• Direct detection in the scattering off matter nuclei• Production of dark matter particles at colliders• Indirect detection in cosmic ray signatures
[Max-Planck-Institut für Kernphysik]
[CERN] [Aprile et al. (2012)] [AMS Collaboration]
A combination will be necessary to identify the nature of particle dark matter!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 5 / 26
-
Motivation for Decaying Gravitino Dark Matter
Gravitino Dark Matter: Stable or Unstable?
I Stable Gravitino Dark Matter• Typical in gauge mediation with conserved R-parity• No direct detection signal expected: σN ∼ M−4Pl• No annihilation signal expected: σann ∼ M−4Pl• Collider signals from long-lived NLSP expected• Long-lived NLSP can be in conflict with BBN
[The Particle Zoo]
I Unstable Gravitino Dark Matter• Typical candidate in models with R-parity violation• Lifetime larger than the age of the universe• No direct detection signal expected: σN ∼ M−4Pl• Decays could lead to observable cosmic-ray signals• Collider signals from long-lived NLSP expected
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 6 / 26
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Motivation for Decaying Gravitino Dark Matter
Why Decaying Gravitino Dark Matter?I Smallness of observed neutrino masses motivates seesaw mechanism
I Explains baryon asymmetry via thermal leptogenesis [Fukugita, Yanagida (1986)]• Needs high reheating temperature: TR & 109 GeV [Davidson, Ibarra (2002)]
I Supergravity predicts gravitino as spin-3/2 superpartner of the graviton
I Gravitinos are thermally produced after inflation in the early universe:
ΩTP3/2h2 '
3∑i=1
ωi g2i
(1 +
M2i3 m23/2
)ln(
kigi
)(m3/2
100 GeV
)(TR
1010 GeV
)[Pradler, Steffen (2006)]
I Problem in scenarios with neutralino dark matter:• Gravitino decays suppressed by Planck scale:
τ3/2 ∼M2Pl
m33/2≈ 3 years
(100 GeV
m3/2
)3• Decays with τ & O(1–1000 s) spoil BBN ⇒ Cosmological gravitino problem
Possible solution: Gravitino is the LSP and thus stable!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 7 / 26
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Motivation for Decaying Gravitino Dark Matter
Why Decaying Gravitino Dark Matter?I Smallness of observed neutrino masses motivates seesaw mechanism
I Explains baryon asymmetry via thermal leptogenesis [Fukugita, Yanagida (1986)]• Needs high reheating temperature: TR & 109 GeV [Davidson, Ibarra (2002)]
I Supergravity predicts gravitino as spin-3/2 superpartner of the graviton
I Gravitinos are thermally produced after inflation in the early universe:
ΩTP3/2h2 '
3∑i=1
ωi g2i
(1 +
M2i3 m23/2
)ln(
kigi
)(m3/2
100 GeV
)(TR
1010 GeV
)[Pradler, Steffen (2006)]
I Problem in scenarios with neutralino dark matter:• Gravitino decays suppressed by Planck scale:
τ3/2 ∼M2Pl
m33/2≈ 3 years
(100 GeV
m3/2
)3• Decays with τ & O(1–1000 s) spoil BBN ⇒ Cosmological gravitino problem
Possible solution: Gravitino is the LSP and thus stable!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 7 / 26
-
Motivation for Decaying Gravitino Dark Matter
Why Decaying Gravitino Dark Matter?I Relation between gravitino mass and reheating temperature:
m g =
500Ge
V
m g =
10Te
V
no thermal leptogenesis
Gravitino not LSPexc
luded
by
gluino
search
es
disfav
oured
by
hierar
chypro
blem
Delahaye & Grefe H2013L
1 10 100 1000 10 000
107
108
109
1010
1011
Gravitino Mass m32 HGeVL
Reh
eatin
gT
empe
ratu
reT
RHG
eVL
I With thermal leptogenesis correct relic density possible forO(10) GeV < m3/2 < O(500) GeV ⇒ Gravitino dark matter
[Buchmüller et al. (2008))]
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 8 / 26
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Motivation for Decaying Gravitino Dark Matter
Why Decaying Gravitino Dark Matter?
I Still problematic:• NLSP can only decay to gravitino LSP:
τNLSP '48πM2Plm
23/2
m5NLSP≈ 9 days
(m3/2
10 GeV
)2(150 GeVmNLSP
)5• Late NLSP decays are in conflict with BBN ⇒ Cosmological gravitino problem
Possible solution: R-parity is not exactly conserved!
I 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) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 9 / 26
-
Motivation for Decaying Gravitino Dark Matter
Why Decaying Gravitino Dark Matter?
I Still problematic:• NLSP can only decay to gravitino LSP:
τNLSP '48πM2Plm
23/2
m5NLSP≈ 9 days
(m3/2
10 GeV
)2(150 GeVmNLSP
)5• Late NLSP decays are in conflict with BBN ⇒ Cosmological gravitino problem
Possible solution: R-parity is not exactly conserved!
I 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) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 9 / 26
-
Gravitino Dark Matter with Broken R-Parity
Gravitino Dark Matterwith Broken R-Parity
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 10 / 26
-
Gravitino Dark Matter with Broken R-Parity
Gravitino Dark Matter with Bilinear R-Parity Violation
I Bilinear R-parity violation: W/Rp = µiHuLi , −Lsoft/Rp
= BiHu ˜̀i + m2Hd`i H∗d
˜̀i + h.c.
• Only lepton number violated ⇒ Proton remains stable!
I R-parity violation can be parametrized by sneutrino VEV: ξ =〈ν̃〉v
I Bound from contribution to neutrino masses• Upper bound: Below limit on sum of neutrino masses: ξ . O(10−4–6)
I Cosmological bounds on R-violating couplings• Lower bound: The NLSP must decay before the time of BBN: ξ & O(10−11–14)• Upper bound: No washout of lepton/baryon asymmetry: ξ . O(10−6)
I Tiny bilinear R-parity violation can be related to U(1)B–L breaking[Buchmüller et al. (2007)]
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 11 / 26
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Gravitino Dark Matter with Broken R-Parity
Gravitino Dark Matter with Bilinear R-Parity Violation
I Gravitino decay suppressed by Planck scale and small R-parity violation
• Gravitino decay width: Γ3/2 ∝ξ2 m33/2
M2Pl= 2.6× 10−24 s−1
( m33/210 GeV
)3 (ξ
10−7)2
[Takayama, Yamaguchi (2000)]
• The gravitino lifetime by far exceeds the age of the universe (τ3/2 � 1017 s)
The unstable gravitino is a well-motivated and viable dark matter candidate!
I 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, 2012)]
• Gravitino decays can possibly be observed at indirect detection experiments[Takayama et al. (2000), Buchmüller et al. (2007), Ibarra, Tran (2008), Ishiwata et al. (2008) etc.]
Gravitinos could be observed at colliders and in the spectra of cosmic rays!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 12 / 26
-
Gravitino Dark Matter with Broken R-Parity
Gravitino Dark Matter with Bilinear R-Parity Violation
I Gravitino decay suppressed by Planck scale and small R-parity violation
• Gravitino decay width: Γ3/2 ∝ξ2 m33/2
M2Pl= 2.6× 10−24 s−1
( m33/210 GeV
)3 (ξ
10−7)2
[Takayama, Yamaguchi (2000)]
• The gravitino lifetime by far exceeds the age of the universe (τ3/2 � 1017 s)
The unstable gravitino is a well-motivated and viable dark matter candidate!
I 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, 2012)]
• Gravitino decays can possibly be observed at indirect detection experiments[Takayama et al. (2000), Buchmüller et al. (2007), Ibarra, Tran (2008), Ishiwata et al. (2008) etc.]
Gravitinos could be observed at colliders and in the spectra of cosmic rays!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 12 / 26
-
Gravitino Dark Matter with Broken R-Parity
Gravitino Decay ChannelsI Several two-body decay channels: ψ3/2 → γ νi , Z νi , W `i , h νi
+ ...
• Γγνi 'ξ2i m
33/2
32πM2Pl|Uγ̃Z̃ |
2 ∝ξ2i m
33/2
M2Pl
(M2−M1M1 M2
)2• ΓZνi '
ξ2i m33/2
32πM2Pl
(1− m
2Z
m23/2
)2{U2Z̃ Z̃ f
(m2Z
m23/2
)+ ...
}• ΓW+`−i '
ξ2i m33/2
16πM2Pl
(1− m
2W
m23/2
)2{U2W̃W̃ f
(m2W
m23/2
)+ ...
}• Γhνi '
ξ2i m33/2
192πM2Pl
(1− m
2h
m23/2
)4I Dependence on mass mixings → dependence on gaugino masses
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 13 / 26
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Gravitino Dark Matter with Broken R-Parity
Gravitino Decay Width and Branching Ratios
I Three benchmark models• Bino-like NLSP: M1 = 1.1 m3/2• Wino-like NLSP: M2 = 1.1 m3/2• Higgsino-like NLSP: µ = 1.1 m3/2
I Common asymptotic decay width
Ξ = 10-9
Bino NLSP
Wino NLSP
Higgsino NLSP
asymptotic value: G32 =Ξ
2 m323
48 Π MPl2
Delahaye & Grefe H2013L
10 100 1000 10 000
10-60
10-59
10-58
10-57
Gravitino Mass m32 HGeVL
Gra
vitin
oD
ecay
Wid
thG
32
m3
23
HGeV
-2 L
Bino NLSP
Wino NLSP
Higgsino NLSP
ΓΝ
W{
ZΝ
hΝ
Delahaye & Grefe H2013L
100 1000 10 000
0.001 %
0.01 %
0.1 %
1 %
10 %
100 %
Gravitino Mass m32 HGeVL
Bra
nchi
ngR
atio I Branching ratios are independent
of strength of R-parity violation
I Exact ratio between channels ismodel-dependent, in particular γν
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 14 / 26
-
Gravitino Dark Matter with Broken R-Parity
Final State Particle Spectra
I Gravitino decays produce stable cosmic rays: γ, e, p, d , νe/µ/τ• Proton/antiproton spectra from gravitino decay generated with PYTHIA• No protons from γν; Zν and W ` very similar; a bit more protons from hν
Ψ32 ® ZΝi , pp Spectrum
m32 =100 GeV
1 TeV10 TeV
Delahaye & Grefe H2013L
10-6 10-5 10-4 10-3 0.01 0.1 1
10-6
10-5
10-4
10-3
0.01
0.1
1
Kinetic Energy x = 2 Tm32
Prot
onA
ntip
roto
nSp
ectr
umx
dNd
x
Ψ32 ® W {i , pp Spectrum
m32 =100 GeV
1 TeV10 TeV
Delahaye & Grefe H2013L
10-6 10-5 10-4 10-3 0.01 0.1 1
10-6
10-5
10-4
10-3
0.01
0.1
1
Kinetic Energy x = 2 Tm32
Prot
onA
ntip
roto
nSp
ectr
umx
dNd
x
Ψ32 ® hΝi , pp Spectrum
mh = 125 GeV
m32 =150 GeV
1 TeV10 TeV
Delahaye & Grefe H2013L
10-6 10-5 10-4 10-3 0.01 0.1 1
10-6
10-5
10-4
10-3
0.01
0.1
1
Kinetic Energy x = 2 Tm32
Prot
onA
ntip
roto
nSp
ectr
umx
dNd
x
Basis for phenomenology of indirect gravitino dark matter searches!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 15 / 26
-
Gravitino Dark Matter with Broken R-Parity
Final State Particle Spectra
I Gravitino decays produce stable cosmic rays: γ, e, p, d , νe/µ/τ• Proton/antiproton spectra from gravitino decay generated with PYTHIA• No protons from γν; Zν and W ` very similar; a bit more protons from hν
Ψ32 ® ZΝi , pp Spectrum
m32 =100 GeV
1 TeV10 TeV
Delahaye & Grefe H2013L
10-6 10-5 10-4 10-3 0.01 0.1 1
10-6
10-5
10-4
10-3
0.01
0.1
1
Kinetic Energy x = 2 Tm32
Prot
onA
ntip
roto
nSp
ectr
umx
dNd
x
Ψ32 ® W {i , pp Spectrum
m32 =100 GeV
1 TeV10 TeV
Delahaye & Grefe H2013L
10-6 10-5 10-4 10-3 0.01 0.1 1
10-6
10-5
10-4
10-3
0.01
0.1
1
Kinetic Energy x = 2 Tm32
Prot
onA
ntip
roto
nSp
ectr
umx
dNd
x
Ψ32 ® hΝi , pp Spectrum
mh = 125 GeV
m32 =150 GeV
1 TeV10 TeV
Delahaye & Grefe H2013L
10-6 10-5 10-4 10-3 0.01 0.1 1
10-6
10-5
10-4
10-3
0.01
0.1
1
Kinetic Energy x = 2 Tm32
Prot
onA
ntip
roto
nSp
ectr
umx
dNd
x
Basis for phenomenology of indirect gravitino dark matter searches!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 15 / 26
-
Indirect Detection of Gravitino Dark Matter
Indirect Detection ofGravitino Dark Matter
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 16 / 26
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Indirect Detection of Gravitino Dark Matter
Cosmic-Ray PropagationI Cosmic rays from gravitino decays propagate through the Milky Way
I Experiments observe spectra of cosmic rays at Earth
[NASA E/PO, SSU, Aurore Simonnet] [PAMELA Collaboration] [IceCube Collaboration]
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 17 / 26
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Indirect Detection of Gravitino Dark Matter
Cosmic-Ray PropagationI Diffusion equation for cosmic-ray density ψ:
~∇ · (~Vc ψ − K0 β pδ ~∇ψ) + 2 h δ(z) ∂E (bloss ψ − DEE ∂Eψ)= Qprim + 2 h δ(z)
(Qsec + Qter
)− 2 h δ(z) Γann ψ
+ boundary conditions
• ~Vc : velocity of the convective wind from stars in the Galactic plane• K0 β pδ: spatial diffusion from irregularities of the Galactic magnetic field• bloss: energy losses from interaction with interstellar gas• DEE : coefficient for diffusion in energy• Qsec: antiprotons from collisions of cosmic-ray protons or α with interstellar gas• Qter: antiprotons from inelastic collisions of antiprotons with interstellar gas• Γann: annihilation of antiprotons with cosmic-ray protons
I Gravitino decays are a primary antiproton source in the Galactic halo:
Qprim(T , r) =ρhalo(r)
m3/2 τ3/2dNdT
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 18 / 26
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Indirect Detection of Gravitino Dark Matter
Cosmic-Ray Propagation
I Two approaches to solve diffusion equation:• Numerical: GALPROP, DRAGON• Semi-analytical: Two-zone diffusion model for the Milky Way (USINE)
I Propagation parameters constrained by secondary-to-primary ratios
I Typical approach: 3 parameter sets to estimate uncertainty
L (kpc) K0 (kpc2/Myr) δ ‖~Vc‖ (km/s) Va (km/s)
MIN 1 0.0016 0.85 13.5 22.4MED 4 0.0112 0.70 12 52.9MAX 15 0.0765 0.46 5 117.6
I Our approach: Scan over all allowed propagation parameters• Roughly 1600 parameter sets [Maurin et al. (2001))]• Allows to reliably estimate the uncertainty from cosmic-ray propagation
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 19 / 26
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Indirect Detection of Gravitino Dark Matter
Gravitino Decay Signals in Antiproton Spectra
æ
æ ææ æ æ
ææ æ
æ ææ
æ
æ ææ
æ
æ
æ
æ
æ
æ
æ
ææ PAMELA dataAstrophysical Background
MAXMEDMIN
100 GeV1 TeV10 TeV
Bino NLSP
Τ32 = 1028 s
Delahaye & Grefe H2013L
0.1 1 10 100 1000
10-7
10-6
10-5
10-4
10-3
0.01
0.1
Kinetic Energy T HGeVL
Ant
ipro
ton
Flux
Fp
HGeV
-1
m-
2s-
1sr
-1
L
I Observed antiproton spectrum well described by astrophysical background• No need for contribution from dark matter
I Propagation uncertainty roughly one order of magnitude• Expected to be improved by forthcoming AMS-02 cosmic-ray data
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 20 / 26
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Antiproton Limits on the Lifetime and the Amount of R-Parity Violation
Antiproton Limits on the Lifetimeand the Amount of R-Parity Violation
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 21 / 26
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Antiproton Limits on the Lifetime and the Amount of R-Parity Violation
Limits on the Gravitino Lifetime
I Lifetime limits derived using chi-squared statistics
χ2 =∑
i
(Oi − Ei )2
σ2i
• Oi : Observed flux in energy bin i• Ei : Expected flux in energy bin i (DM signal + astrophysical background)• σi : Data error bar in energy bin i
I Limits at 95 % CL derived from deviation from best fit
χ2(τ95 % CL) = χ2(τbest fit) + ∆χ
2
• χ2(τbest fit)/dof ∼ 0.7 (in general no DM contribution)• ∆χ2 = 4 (corresponding to 2σ exclusion for 1 fit parameter)
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 22 / 26
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Antiproton Limits on the Lifetime and the Amount of R-Parity Violation
Limits on the Gravitino Lifetime
I Bounds on gravitino lifetime derived from PAMELA antiproton data
MAX
MED
MIN
Full range from scan
Bino NLSP
with solar modulation
all PAMELA p data
Delahaye & Grefe H2013L
100 1000 10 000
1026
1027
1028
1029
Gravitino Mass m32 HGeVL
95%
CL
Low
erL
imit
onL
ifet
ime
Τ95
%C
LHsL
I Gravitino lifetimes below a few times 1028 s to 1026 s excluded• Scan over propagation parameters can change highest/lowest limits by ∼ 40 %• Gravitino decay cannot explain rise in positron fraction (PAMELA, AMS-02)
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 23 / 26
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Antiproton Limits on the Lifetime and the Amount of R-Parity Violation
Limits on the Amount of R-Parity Violation
I Gravitino lifetime limits constrain R-parity violation: τ3/2 ∝M2Pl
ξ2 m33/2
MAX
MED
MIN Bino NLSP
Wino NLSP
Higgsino NLSP
Envelope of Antiproton Constraints
excluded by washout
excluded by BinoWino NLSP decay
excluded by Higgsinostau NLSP decay
excluded by neutrinomass
excluded by antiprotons
Delahaye & Grefe H2013L
100 1000 10 00010-15
10-14
10-13
10-12
10-11
10-10
10-9
10-8
10-7
10-6
10-5
10-4
Gravitino Mass m32 HGeVL
R-
Par
ity
Vio
lati
ngP
aram
eter
Ξ
Indirect searches set strong limits on R-parity violation!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 24 / 26
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Antiproton Limits on the Lifetime and the Amount of R-Parity Violation
Limits on the Amount of R-Parity Violation
I Gravitino lifetime limits constrain R-parity violation: τ3/2 ∝M2Pl
ξ2 m33/2
MAX
MED
MIN Bino NLSP
Wino NLSP
Higgsino NLSP
Envelope of Antiproton Constraints
excluded by washout
excluded by BinoWino NLSP decay
excluded by Higgsinostau NLSP decay
excluded by neutrinomass
excluded by antiprotons
Delahaye & Grefe H2013L
100 1000 10 00010-15
10-14
10-13
10-12
10-11
10-10
10-9
10-8
10-7
10-6
10-5
10-4
Gravitino Mass m32 HGeVL
R-
Par
ity
Vio
lati
ngP
aram
eter
Ξ
Indirect searches set strong limits on R-parity violation!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 24 / 26
-
Conclusions
Conclusions
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 25 / 26
-
Conclusions
Conclusions
• Both, stable and unstable gravitinos, are viable dark matter candidates
• Gravitino DM with broken R-parity is well motivated from cosmology
• Decaying gravitino DM can be probed in colliders and cosmic rays
• Strong constraints on the lifetime from PAMELA antiproton data
• Antiproton limits constrain the strength of R-parity violation
Thanks for your attention!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 26 / 26
-
Conclusions
Conclusions
• Both, stable and unstable gravitinos, are viable dark matter candidates
• Gravitino DM with broken R-parity is well motivated from cosmology
• Decaying gravitino DM can be probed in colliders and cosmic rays
• Strong constraints on the lifetime from PAMELA antiproton data
• Antiproton limits constrain the strength of R-parity violation
Thanks for your attention!
Michael Grefe (IFT UAM/CSIC) Antiproton Limits on Decaying Gravitino Dark Matter University of Oxford – 13 June 2013 26 / 26
Motivation for Decaying Gravitino Dark MatterGravitino Dark Matter with Broken R-ParityIndirect Detection of Gravitino Dark MatterAntiproton Limits on the Lifetime and the Amount of R-Parity ViolationConclusions
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