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Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Light dark matter properties with neutrinos fromthe Sun
Mattias [email protected]
May 21, 2013, GDR neutrino, ParisCollaborators: J. Edsjo, T. Ohlsson, E. Fernandez-Martinez, O. Mena, S. Agarwalla, M. Carrigan
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
1 Status of Dark Matter
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
1 Status of Dark Matter
2 Dark Matter in the Sun
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
1 Status of Dark Matter
2 Dark Matter in the Sun
3 Using “small” neutrino detectors
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
1 Status of Dark Matter
2 Dark Matter in the Sun
3 Using “small” neutrino detectors
4 Summary and conclusions
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
1 Status of Dark Matter
2 Dark Matter in the Sun
3 Using “small” neutrino detectors
4 Summary and conclusions
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
Beyond the Standard Model
Hints for physics beyond the StandardModel:
Dark Matter (DM)Dark EnergyNeutrino oscillations
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
Beyond the Standard Model
Hints for physics beyond the StandardModel:
Dark Matter (DM)Dark EnergyNeutrino oscillations
Open questions for this talk
What is the nature of DM?How can we detect it?Can we use neutrinos?
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
Comparing Baryonic and Dark Matter
Baryons
Mass:mN ≃ 1 GeVAbundance:nb/nγ = (6.19± 0.15) · 10−10
Density:Ωb ≃ 0.049
Dark Matter
Mass:
Abundance:
Density:
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
Comparing Baryonic and Dark Matter
Baryons
Mass:mN ≃ 1 GeVAbundance:nb/nγ = (6.19± 0.15) · 10−10
Density:Ωb ≃ 0.049
Dark Matter
Mass:mDM = ?Abundance:
Density:
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
Comparing Baryonic and Dark Matter
Baryons
Mass:mN ≃ 1 GeVAbundance:nb/nγ = (6.19± 0.15) · 10−10
Density:Ωb ≃ 0.049
Dark Matter
Mass:mDM = ?Abundance:nDM = ?Density:
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
Comparing Baryonic and Dark Matter
Baryons
Mass:mN ≃ 1 GeVAbundance:nb/nγ = (6.19± 0.15) · 10−10
Density:Ωb ≃ 0.049
Dark Matter
Mass:mDM = ?Abundance:nDM = ?Density:ΩDM ≃ 0.27
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
Comparing Baryonic and Dark Matter
Baryons
Mass:mN ≃ 1 GeVAbundance:nb/nγ = (6.19± 0.15) · 10−10
Density:Ωb ≃ 0.049
Dark Matter
Mass:mDM = ?Abundance:nDM = ?Density:ΩDM ≃ 0.27
ΩDM
Ωb
≃ 5
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
WIMP Dark Matter
Theorists have a (unhealthy)predisposition to expect new physics atthe TeV scale
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
WIMP Dark Matter
Theorists have a (unhealthy)predisposition to expect new physics atthe TeV scale
Assume dark matter at the TeV scale,mDM ≃ 0.1− 1 TeV
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
WIMP Dark Matter
Theorists have a (unhealthy)predisposition to expect new physics atthe TeV scale
Assume dark matter at the TeV scale,mDM ≃ 0.1− 1 TeV
Assume dark matter is produced thermallyin the early Universe
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
WIMP Dark Matter
Theorists have a (unhealthy)predisposition to expect new physics atthe TeV scale
Assume dark matter at the TeV scale,mDM ≃ 0.1− 1 TeV
Assume dark matter is produced thermallyin the early Universe
=⇒ Cross section of weak strength
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
WIMP Dark Matter
Theorists have a (unhealthy)predisposition to expect new physics atthe TeV scale
Assume dark matter at the TeV scale,mDM ≃ 0.1− 1 TeV
Assume dark matter is produced thermallyin the early Universe
=⇒ Cross section of weak strength
Weakly Interacting Massive Particles(WIMPs)
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
WIMP Dark Matter
Theorists have a (unhealthy)predisposition to expect new physics atthe TeV scale
Assume dark matter at the TeV scale,mDM ≃ 0.1− 1 TeV
Assume dark matter is produced thermallyin the early Universe
=⇒ Cross section of weak strength
Weakly Interacting Massive Particles(WIMPs)
Great! Or is it?
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
The WIMP miracle
Baryons
Mass:mN ≃ 1 GeVAbundance:nb/nγ = (6.19± 0.15) · 10−10
Density:Ωb ≃ 0.046
WIMP Dark Matter
Mass:mDM ≃ 1 TeVAbundance:nDM ≃ 10−3nb
Density:ΩDM ≃ 0.23
ΩDM
Ωb
≃ 5
The WIMP miracle!
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Motivation
The WIMP miracle
Baryons
Mass:mN ≃ 1 GeVAbundance:nb/nγ = (6.19± 0.15) · 10−10
NOT thermal production!Density:Ωb ≃ 0.046
WIMP Dark Matter
Mass:mDM ≃ 1 TeVAbundance:nDM ≃ 10−3nbThermal freezoutDensity:ΩDM ≃ 0.23
ΩDM
Ωb
≃ 5
The WIMP miracle!
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Experimental strategies
The three avenues
Directdetection
Indirectdetection
Accelerator(LHC)
Accelerators: LHC
Direct detection: DAMA/LIBRA,COUPP, CoGeNT, XENON
Indirect detection: PAMELA,AMS-02, FERMI/LAT, IceCube
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Experimental strategies
The three avenues
?
SM DM
DMSM
Accelerator
Indirect
Direct
Accelerators: LHC
Direct detection: DAMA/LIBRA,COUPP, CoGeNT, XENON
Indirect detection: PAMELA,AMS-02, FERMI/LAT, IceCube
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Experimental strategies
Direct detection
Signal: Recoils fromDM-SM scattering
Many different experiments
DAMA/LIBRACoGeNTCRESSTCDMSXENONx XENON100, Phys.Rev.Lett. 109 (2012) 181301
Large nuclei → Spin independent cross-sections (scales as A2)
Dependent on local DM distribution
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Experimental strategies
Accelerator searches
Signal: Something missing!
In many ways complementary todirect searches
Typically assume effective theory
At disadvantage for light mediatormasses?
Fox, Harnik, Kopp, TsaiPhys.Rev. D85 (2012) 056011
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Experimental strategies
Indirect detection
Signal: DM annihilation products
Where? Almost everywhere!
Gamma rays (Fermi-LAT)Antimatter excess in cosmicfluxes (PAMELA, AMS-02,Fermi-LAT)Neutrinos from the Sun(IceCube, Super-K, etc)
Scales as DM density squared
Very dependent on assumptions
AMS-02 homepage
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Experimental strategies
The current status (good news!)
We have several DMsignals/hints!
Direct
DAMA/LIBRA, CoGeNT, CRESSTmDM ≃ 10 GeV, σ ≃ 0.1 fb
Indirect
Fermi-LATmDM ≃ 130 GeVPAMELA, Fermi-LAT, AMS-02mDM & 300 GeV
They just dont fit together . . .
. . . or with or with other experiments . . .
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Experimental strategies
The current status (bad news!)
Image from FreeDigitalPhotos.net
All signals seem to be excluded orunlikely to be caused by DM
Direct detection – excluded byothers (most stronglyXENON100)Positron excess – difficult frommodel perspectiveGamma ray excess – is it there ornot?
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
1 Status of Dark Matter
2 Dark Matter in the Sun
3 Using “small” neutrino detectors
4 Summary and conclusions
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
DM capture and annihilation
χ
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
DM capture and annihilation
χ
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
DM capture and annihilation
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
DM capture and annihilation
χχ → . . . → νν
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
DM capture and annihilation
ν
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
Capture
dC⊙,i
dV=
ρχ ρ⊙,i (r)
2mχµ2i
σi
∞∫
0
duf (u)
u
ER,max∫
ER,min
dER |F (ER)|2 (1)
f (u)
u=
1√π v2⊙
(
e−(u−v⊙)2/v2⊙ − e−(u+v⊙)2/v2
⊙
)
(2)
C⊙ = 4π∑
i
R⊙∫
0
dr r2dC⊙,i
dV(3)
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
Capture
Proportional to σp
Proportional to local DMdensity
Depends on the DM mass
Depends on v⊙
We assume:v⊙ = 220 km/sρDM = 0.3 GeV/cm3
0 20 40 60 80
1027
1028
1029
1030
m Χ@GeVDC@s-
1p
bD
sp in-independen t
sp in-dependent
Kappl, Winkler, Nucl.Phys. B850 (2011) 505-521
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
Annihilation
Several different annihilationchannels possible(depending on mDM)
Quarks (qq)Leptons (ℓ+ℓ−, νν)Weak mediators(W+W−, ZZ )Gluons (gg)
10−3 10−2 10−1 1x = Eν / mDM
0
0.05
0.1
0.15
0.2
dN/d
log 1
0 E
ν
νe,µ from DM DM → τ τ
10−3 10−2 10−1 1x = Eν / mDM
0
0.05
0.1
0.15
0.2
dN/d
log 1
0 E
ν
νe,µ from DM DM → t t
10−3 10−2 10−1 1x = Eν / mDM
0
0.1
0.2
0.3
0.4
0.5
0.6
dN/d
log 1
0 E
ν
νe,µ from DM DM → ZZ
10−3 10−2 10−1 1x = Eν / mDM
0
0.1
0.2
0.3
0.4
dN/d
log 1
0 E
ν
νe,µ from DM DM → W+ W−
10−3 10−2 10−1 1x = Eν / mDM
0
0.05
0.1
0.15
0.2
dN/d
log 1
0 E
ν
νe,µ from DM DM → b b
10−3 10−2 10−1 1x = Eν / mDM
0
0.02
0.04
0.06
0.08
0.1
dN/d
log 1
0 E
ν
νe,µ from DM DM → c c
10−3 10−2 10−1 1x = Eν / mDM
0
0.0025
0.005
0.0075
0.01
0.0125
0.015
dN/d
log 1
0 E
ν
νe,µ from DM DM → q q Sun EarthDM massin GeV
10
30
100
300
1000
Cirelli, et al., Nucl.Phys. B727 (2005) 99-138
Some do not give neutrinos
For the others we can compute the spectrum
Not dependent on annihilation cross section(!) but sensitiveto branching ratios
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
Propagation to the Earth
Do we need to consider neutrino oscillations? What is ∆m231L?
Sun-Earth, ∼ 3.5 · 105 GeV
Perhelion-aphelion, ∼ 104 GeV
Day-night, ∼ 30 GeV
On the other hand
Detectors have finite resolution
Typically oscillation effects arewashed out
See:Cirelli, et al., Nucl. Phys. B727, 99 (2005)MB, Edsjo, Ohlsson, JCAP 0801 (2008) 021Esmaili, Farzan, Phys.Rev. D81 (2010) 113010
10-3
10-2
10-1
1
10
0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1
νe (std. osc.)
νe (no osc.)
νµ (std. osc.)
νµ (no osc.)
ντ (std. osc.)
ντ (no osc.)
z = Eν / mχ
dNν/
dz (
ann-1
)
Neutrino yields at 1 AUMass: 250 GeVChannel: τ+τ-
M. Blennow, J. Edsjö and T. Ohlsson, 2007
MB, Edsjo, Ohlsson, JCAP 0801 (2008) 021
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Capture and detection
WimpSim
MonteCarlo for neutrino telescope studies: WimpSimMB, Edsjo, Ohlsson, JCAP 0801 (2008) 021http://copsosx03.physto.se/wimpsim/
Addition to DarkSusy
Dark matter capture
Annihilations
Oscillation and absorbtion
Event based
Gives different types of fluxes at a detector as output
In use in the neutrino telescope community
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Current limits
Current limits (spin independent)
)-2 / GeV cχ
log10 ( m1 2 3 4
)2 /
cmS
I,pσ
log1
0 (
-46
-45
-44
-43
-42
-41
-40
-39
-38MSSM incl. XENON (2012) ATLAS + CMS (2012)DAMA no channeling (2008)CDMS (2010)CDMS 2keV reanalyzed (2011)CoGENT (2010)XENON100 (2012)
)bIceCube 2012 (b♦)
-W+IceCube 2012 (W
)2 = 80.4GeV/cW<mχ for m-τ+τ (♦
IceCube Collaboration, Phys.Rev.Lett. 110 (2013) 131302
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Current limits
Current limits (spin dependent)
)-2 / GeV cχ
log10 ( m1 2 3 4
)2 /
cmS
D,p
σlo
g10
(
-40
-39
-38
-37
-36
-35MSSM incl. XENON (2012) ATLAS + CMS (2012)DAMA no channeling (2008)COUPP (2012)Simple (2011)PICASSO (2012)
)bSUPER-K (2011) (b)
-W+SUPER-K (2011) (W
)bIceCube 2012 (b♦)
-W+IceCube 2012 (W
)2 = 80.4GeV/cW<mχ for m-τ+τ (♦
IceCube Collaboration, Phys.Rev.Lett. 110 (2013) 131302
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Current limits
Low DM mass region (Super-K)
10.05.02.0 20.03.0 15.07.0
10-42
10-41
10-40
10-39
10-38
m Χ@GeVD
Σp@c
m2 D
s-wave
ΥΥ
ΤΤ
4Τbb
ccCDMSCoGeNT
DAMA qNa=0.45DAMA qNa=0.3
2 5 10 20 50
10-40
10-39
10-38
10-37
10-36
10-35
m Χ@GeVD
Σp@c
m2 D
s-wave
ΥΥ
ΤΤ
4Τbb
ccCOUPPPICASSO
DAMA qNa=0.45DAMA qNa=0.3
Kappl, Winkler, Nucl.Phys. B850 (2011) 505-521
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
1 Status of Dark Matter
2 Dark Matter in the Sun
3 Using “small” neutrino detectors
4 Summary and conclusions
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What could we use?
What do we need?
If Super-K works, what about the next generation of neutrinodetectors? What do we need?
Volume!
Not competing with IceCube - different mass regime
Low threshold
We need to see the spectrumPreferably significantly lower than mDM
High resolution
In energy → spectral informationIn angle → background suppression
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What could we use?
Volume
More volume = More statistics
IceCube = 1 km3 = 1 Gton
Future neutrino experiment ≃ 0.1 Mton
Denser instrumentation = lower threshold
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What could we use?
Low threshold
5 10 15 20 25 3010
−3
10−2
10−1
100
101
102
Rat
e [y
ear−1 ]
Energy [GeV]
5 10 15 20 25 30
10−3
10−2
10−1
100
101
102
Rat
e [y
ear−1 ]
5 10 15 20 25 30
10−3
10−2
10−1
100
101
102
Atmo q τ ν
5 10 15 20 25 3010
−3
10−2
10−1
100
101
102
Energy [GeV]
I will get back to this figure
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What could we use?
Resolution
Energy
Would like to do morethan countingMass determinationAnnihilation branchingratios
Angle
Background rejection(atmospheric)Compare to “ordinary”solar ν
Dar, Shaviv, Phys.Rept. 311 (1999) 115-141
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What could we use?
Candidates
Good news: If you can do atmospherics, you (probably) cando this
Consider some detectors discussed for future LBL experiments
Liquid Argon (LAr) TPC – LBNO / LBNEMagnetic Iron Calorimeter (MIND) – INOWater Cherenkov – Hyper-K
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Simulation setup
Results are based on a MarkovChain Monte Carlo study
Consider the following experiment
LAr (34 kton, 100 kton)MIND (100 kton)
Consider the following parameters
mDM, σBrν , σBrτ , σBrq
(σBrx = σSD BR(χχ → xx))
Good convergence, 8 · 105 samples
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Spectra @ detectors
σSD = 1 fb
Background includesangular cut (could berefined)
For details onassumptions, seeoriginal reference
5 10 15 20 25 3010
−3
10−2
10−1
100
101
102
Rat
e [y
ear−1 ]
Energy [GeV]
5 10 15 20 25 30
10−3
10−2
10−1
100
101
102
Rat
e [y
ear−1 ]
5 10 15 20 25 30
10−3
10−2
10−1
100
101
102
Atmo q τ ν
5 10 15 20 25 3010
−3
10−2
10−1
100
101
102
Energy [GeV]
MB, Carrigan, Fernandez-Martinez, arXiv:1303.4530
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Sensitivity (χχ → νν)
5 10 15 20 2510
−3
10−2
10−1
100
mDM
[GeV]
σ B
r ν [fb]
MINDLAr34LAr100
MB, Carrigan, Fernandez-Martinez, arXiv:1303.4530
Gray line,Super-KamiokandefromKappl, Winkler, Nucl.Phys. B850(2011) 505-521
1–2 order ofmagnitudeimprovement
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Sensitivity (χχ → τ+τ−)
5 10 15 20 2510
−2
10−1
100
mDM
[GeV]
σ B
r τ [fb]
MINDLAr34LAr100
MB, Carrigan, Fernandez-Martinez, arXiv:1303.4530
Gray line,Super-KamiokandefromKappl, Winkler, Nucl.Phys. B850(2011) 505-521
1–2 order ofmagnitudeimprovement
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Sensitivity (χχ → qq)
5 10 15 20 2510
−1
100
101
mDM
[GeV]
σ B
r q [fb]
MINDLAr34LAr100
MB, Carrigan, Fernandez-Martinez, arXiv:1303.4530
Gray line,Super-KamiokandefromKappl, Winkler, Nucl.Phys. B850(2011) 505-521
1–2 order ofmagnitudeimprovement
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Branching ratios and mass
χχ → νν, mDM = 25 GeV
Sub-GeV precision inmDM for LAr (solidand dashed)
GeV precision forMIND (dotted)
Precision worse forlower signal(expected) m
DM [GeV]
σ B
r ν [fb]
20 22 24 26 28 300
0.05
0.1
0.15
0.2
MB, Carrigan, Fernandez-Martinez, arXiv:1303.4530
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Branching ratios and mass
χχ → τ+τ−, mDM = 25 GeV
Mass determinationstill fair
Requires largerbranching
First signs ofdegeneracy (MIND)
mDM
[GeV]
σ B
r τ [fb]
10 15 20 25 300
0.2
0.4
0.6
0.8
MB, Carrigan, Fernandez-Martinez, arXiv:1303.4530
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Branching ratios and mass
χχ → qq, mDM = 25 GeV
Bad mass resolution
Very large branching
Degenerate!
mDM
[GeV]
σ B
r q [fb]
5 10 15 20 25 300
1
2
3
4
5
6
7
MB, Carrigan, Fernandez-Martinez, arXiv:1303.4530
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Origin of the degeneracy
mDM
[GeV]
σ B
r τ [fb]
5 10 15 20 25 300
0.05
0.1
0.15
0.2
0.25
mDM
[GeV]
σ B
r q [fb]
5 10 15 20 25 300
1
2
3
4
5
34 kton LAr
σ Brq [fb]
σ B
r τ [fb]
0 1 2 3 40
0.05
0.1
0.15
0.2
0.25
MB, Carrigan, Fernandez-Martinez,arXiv:1303.4530
Lower mass,differentbranching
MainlyσBrq–σBrτdegeneracy
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
What can we do?
Degeneracy as seen in the spectrum
Energy [GeV]
Rat
e [y
ear−1 ]
2 4 6 8 10 12 14 1610
−2
10−1
100
101
a: 25 GeV, σ Brq = 3 fb
b: 14 GeV, σ Brq = 1.3 fb
c: 14 GeV, σ Brτ = 0.15 fb
d: 14 GeV, σ Brν = 0.0009 fb
e: Atmof: (b)+(c)+(d)
MB, Carrigan, Fernandez-Martinez, arXiv:1303.4530
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
1 Status of Dark Matter
2 Dark Matter in the Sun
3 Using “small” neutrino detectors
4 Summary and conclusions
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Summary
Dark Matter, just like neutrinos, point to beyond-SM physics
Detection prospects: Accelerator, Direct, Indirect
Indirect neutrino signals from the Sun
Neutrino telescopes, but “small” detectors can compete atlow masses!
Study for future long baseline detectors
Discussed degeneracy in determination of parameters
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Outline Status of Dark Matter Dark Matter in the Sun Using “small” neutrino detectors Summary and conclusions
Conclusions
Indirect detection of neutrinos from the Sun offers acomplement to direct detection and accelerators
The framework for implementation and analysis is welldeveloped, as is the underlying theory
Can span a wide range of Dark Matter masses
Contstraints can be pushed down in the low mass regime byLBL detectors – or we make a discovery
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Backup slides
5 Backup slides
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
Backup slides
Oscillations in the neutrino channel
mDM
[GeV]
Br ν [f
b]
24 25 26 27 28
0.3
0.4
0.5
0.6
0.7
0.8
Mattias Blennow KTH Theoretical Physics
Light dark matter properties with neutrinos from the Sun
