New signals in dark matter detectors · signals in dark matter detectors Joachim Kopp (based on...
Transcript of New signals in dark matter detectors · signals in dark matter detectors Joachim Kopp (based on...
New signals in dark matter detectors
Joachim Kopp(based on work done in collaboration with
Roni Harnik and Pedro Machado, arXiv:1202.6073)
Kaffeepalaver @ MPIK, November 08, 2012
Joachim Kopp New signals in dark matter detectors 1
ν signals in dark matter detectors
Joachim Kopp(based on work done in collaboration with
Roni Harnik and Pedro Machado, arXiv:1202.6073)
Kaffeepalaver @ MPIK, November 08, 2012
Joachim Kopp ν signals in dark matter detectors 2
Outline
1 Direct Dark Matter detection
2 Standard Model neutrino backgrounds in DM detectors
3 Enhanced neutrino scattering from new physics
4 Temporal modulation of ν signals
5 Constraints on hidden photons and sterile neutrinos
6 Conclusions
Joachim Kopp ν signals in dark matter detectors 3
Outline
1 Direct Dark Matter detection
2 Standard Model neutrino backgrounds in DM detectors
3 Enhanced neutrino scattering from new physics
4 Temporal modulation of ν signals
5 Constraints on hidden photons and sterile neutrinos
6 Conclusions
Joachim Kopp ν signals in dark matter detectors 4
Direct Dark Matter detectionIdea: A WIMP (Weakly Interacting Massive Particle) can scatteron an atomic nucleus.
t
f
χ
f
χ
Strategy: Look for feeble nuclear recoil
Problem: Many background processes can mimic the signal:Radioactive decaysCosmic raysNeutrinos→ this talk. . .
Joachim Kopp ν signals in dark matter detectors 5
Direct DM detection — The experimental challenge
background
suppression
Joachim Kopp ν signals in dark matter detectors 6
Direct DM detection — The experimental challenge
background
suppression
Joachim Kopp ν signals in dark matter detectors 6
Direct detection results — Current status
101 102 10310- 45
10- 44
10- 43
10- 42
10- 41
10- 40
10-39
WIMP mass m Χ @GeV D
WIM
P-
nu
cleo
ncr
oss
sect
ion
ΣSI
@cm2
D
í
Limits: 90%Countours: 90%, 3Σ
v0 = 220 km� s
vesc = 550 km� s
CRESST
CDM
S H lowthr .L
CDMS-II H2009L
Xe-100 H2012L
Xe-
10 H lowthr .L
DAMA Hq ± 10%Lscattering on Na
DAMA Hq ± 10%Lscattering on I
CoGeNT H2011L
updated version of plot from JK Schwetz Zupan 1110.2721see also Freese Lisanti Savage 1209.3339
Assumptions here:
Elastic DM scattering ∝ target mass
Joachim Kopp ν signals in dark matter detectors 7
Outline
1 Direct Dark Matter detection
2 Standard Model neutrino backgrounds in DM detectors
3 Enhanced neutrino scattering from new physics
4 Temporal modulation of ν signals
5 Constraints on hidden photons and sterile neutrinos
6 Conclusions
Joachim Kopp ν signals in dark matter detectors 8
Standard Model neutrino backgrounds in DM detectorsSolar neutrinos are a well-known background to future direct DM searches:
see e.g. Gütlein et al. arXiv:1003.5530
dσSM(νN → νN)
dEr=
G2F mNF 2(Er )
2πE2ν
[A2E2
ν + 2AZ (2E2ν (s2
w − 1)− Er mNs2w )
+ 4Z 2(E2ν + s4
w (2E2ν + E2
r − Er (2Eν + mN)) + s2w (Er mN − 2E2
ν ))],
Joachim Kopp ν signals in dark matter detectors 9
Standard Model neutrino backgrounds in DM detectorsSolar neutrinos are a well-known background to future direct DM searches:
see e.g. Gütlein et al. arXiv:1003.5530
dσSM(νN → νN)
dEr=
G2F mNF 2(Er )
2πE2ν
[A2E2
ν + 2AZ (2E2ν (s2
w − 1)− Er mNs2w )
+ 4Z 2(E2ν + s4
w (2E2ν + E2
r − Er (2Eν + mN)) + s2w (Er mN − 2E2
ν ))],
ææ
æ
ææææææææææææææææææææææææææææææææææ
10-1 100 101 102 103 10410-1410-1310-1210-1110-1010-910-810-710-610-510-410-310-210-1100101102
Erec HkeVL
coun
ts�N
A�k
eV�y
ear
electron recoil
DAMA
Borexino
XENON100 e-
CoGeNT
pp7Be
13N 15Opep
8B17F
hepSM total rateComponents
10-4 10-3 10-2 10-1 100 10110-2
10-1
100
101
102
103
104
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Erec HkeVL
coun
ts�to
n�ke
V�y
ear
Nuclear recoil - Ge
pp7Be
13N 15Opep
8B
17F
hep
CoGeNT
CDMS-II
SM total rateComponents
Harnik JK Machado 1202.6073
Joachim Kopp ν signals in dark matter detectors 9
Standard Model neutrino backgrounds in DM detectorsSolar neutrinos are a well-known background to future direct DM searches:
see e.g. Gütlein et al. arXiv:1003.5530
dσSM(νN → νN)
dEr=
G2F mNF 2(Er )
2πE2ν
[A2E2
ν + 2AZ (2E2ν (s2
w − 1)− Er mNs2w )
+ 4Z 2(E2ν + s4
w (2E2ν + E2
r − Er (2Eν + mN)) + s2w (Er mN − 2E2
ν ))],
SM signal will only become sizeable in multi-ton detectors
But: New physics can enhance the rate
Joachim Kopp ν signals in dark matter detectors 9
Outline
1 Direct Dark Matter detection
2 Standard Model neutrino backgrounds in DM detectors
3 Enhanced neutrino scattering from new physics
4 Temporal modulation of ν signals
5 Constraints on hidden photons and sterile neutrinos
6 Conclusions
Joachim Kopp ν signals in dark matter detectors 10
Enhanced neutrino scattering from new physicsQuestion:
Can neutrino scattering be relevant already in the current generation ofDM detectors?Can it explain some of the anomalous signals (CoGeNT, DAMA, CRESST)?
Conditions for large scattering cross sections:Large scattering rate at low energies, low scattering rate at high energies
I High-E neutrino scattering well studied experimentally, consistent with SMI Possible realization: Scattering through a light (or massless) force carrier
φ(mφ ≪ 1 GeV)
ν
ν
f
f
Typically also: Existence sterile neutrinosI Active neutrinos in the same SU(2) doublets as charged leptonsI New physics in the charged lepton sector tightly constrained
Joachim Kopp ν signals in dark matter detectors 11
Light force carriers: MotivationWe know they exist! In particular the photon in electromagnetism.Top-down approaches to particle physics (Grand Unified Theories (GUTs),string theory, . . . ) usually have extra gauge groupsU(1) factors are often left over when gauge symmetries are broken
I Example: SU(2)× U(1)Y → U(1)em
No preferred mass scale for new gauge bosons(depending on BSM symmetry breaking mechanism)Couplings and masses naturally suppressed in extra-dimensional worlds
see talks by Jörg JäckelSlight cosmological preference for extra “radiation” (light particles)
Hamann Hannestad Raffelt Tamborra Wong 1006.5276
Joachim Kopp ν signals in dark matter detectors 12
Light force carriers: Motivation (2)
L = LSM −14
F ′µνF ′µν − 12εF ′µνFµν
10-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 110-16
10-14
10-12
10-10
10-8
10-6
10-4
10-210-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 1
10-16
10-14
10-12
10-10
10-8
10-6
10-4
10-2
Dark Photon Mass MA'HGeVL
Kin
etic
mix
ing
Ε
Fixedtarget
Kinetically Mixed Gauge Boson
Hg-2LΜ
Hg-2Le
U
SN1987A
Atomic PhysicsAtomic Physics
CMB
Glo
bula
rC
lust
ers
Sun�Globular Clusters, energy loss via Νs
Hin models with d 10 keV sterile neutrinosL
Sun
A' capture in SunHpartly allowedL
CASTCMB
LSW
gΝ2 sin22Θ=10-4
gΝ2 sin22Θ=10-12
Borexino Hin models with UH1L'-charged sterile ΝL
Plot from Harnik JK Machado 1202.6073based in part on works by Jaeckel Redondo Ringwald
Lots of open parameter space . . . more on this laterJoachim Kopp ν signals in dark matter detectors 13
Sterile neutrinos: Theoretical motivationStandard Model singlet fermions are a very generic feature of “newphysics” models
I Leftovers of extended gauge multiplets (e.g. GUT multiplets) (typically heavy)I Dark matter (keV . . . TeV or above)
Neutrino–singlet mixing is one of the allowed “portals” between the SMand a hidden sector.SM singlet fermions can live at any mass scaleTypical Lagrangian:
Lmass ⊃ Yν L̄H∗NR + ms ν̄sNR +12
M NcRNR + h.c.
⇒ mass mixing between active and sterile neutrinos
Joachim Kopp ν signals in dark matter detectors 14
Sterile neutrinos: Experimental motivationSeveral experiments have seen hints for sterile neutrinosin
(_ )ν µ → (_ )
ν e appearance and(_ )ν e → (_ )
ν e disappearance oscillations. . . but tension with other experiments (
(_ )ν µ → (_ )
ν e,(_ )ν e → (_ )
ν e,(_ )ν µ → (_ )
ν µ)
10-4 10- 3 10- 2 10-110-1
100
101
sin 2 2 Θ Μe
Dm
2
LSND + react. + Ga+ MB all channels
null resultsappearance
null resultsdisappearancenull results
combined
99% CL, 2 dof
JK Maltoni Schwetz 1103.4570 and work in progresssee also Giunti Laveder 1107.1452 and 1109.4033; Mention et al. 1101.2755; Karagiorgi et al. 0906.1997 and 1110.3735
appearance: E776, ICARUS, KARMEN (ν̄e), LSND (ν̄e), MiniBooNE (νe, ν̄e), NOMADdisappearance: Atmospheric Neutrinos, CDHS, KARMEN νe–12C, LSND νe–12C,
MiniBooNE (νµ, ν̄µ), MINOS, Reactor Neutrinos, Solar NeutrinosJoachim Kopp ν signals in dark matter detectors 15
... back to ν signals in dark matter detectors
Model 1: Neutrino magnetic momentsAssume neutrinos carry an enhanced magnetic moment(e.g. for composite neutrinos)
Lµν⊃ µν ν̄σαβ∂βAαν , µν,SM = 3.2× 10−19
Cross section large at low energies due to photon propagator ∝ q−2
dσµ(νe→ νe)
dEr= µ2
να
(1Er− 1
Eν
),
10 1 100 101 102 10310 -8
10 -7
10 -6
10 -5
10 -4
10 -3
10 -2
10 -1
100
101
102
Erec keVee
coun
tsNA
keV
eeye
ar
electron recoil
DAMA
Borexino
XENON100 e
CoGeNT
Standard model
A
A ΜΝ = 0.32 x 10-10ΜB
10 -4 10 -3 10 -2 10 -1 100 10110 -2
10 -1
100
101
102
103
104
105
106
107
108
E /rec keVnr
coun
ts/t
on/k
eV
/nr
year
Nuclear recoil – Ge
CoGeNT
CDMS II
A
Standard model
A ΜΝ = 0.32 x 10 -10 ΜB
Harnik JK Machado 1202.6073Joachim Kopp ν signals in dark matter detectors 17
Model 2: A hidden photon + sterile neutrinosIntroduce a hidden photon A′ and a sterile neutrino νs
Related model with gauged U(1)B first discussed in Pospelov 1103.3261detailed studies in Harnik JK Machado 1202:6073 and Pospelov Pradler 1203.0545
νs charged under U(1)′ → direct coupling to A′
SM particles couple to A′ only through kinetic mixing
L ⊃ −14
F ′µνF ′µν − 14
FµνFµν − 12εF ′µνFµν + ν̄s i /∂νs + g′ν̄sγ
µνsA′µ
− (νL)cmνLνL − (νs)cmνsνs − (νL)cmmixνs
A small fraction of solar neutrinos can oscillate into νs
νs scattering cross section in the detector given by
dσA′(νse→ νse)
dEr=
ε2e2g′2me
4πp2ν(M2
A′ + 2Er me)2
[2E2
ν + E2r − 2Er Eν − Er me −m2
ν
]Joachim Kopp ν signals in dark matter detectors 18
Model 2: A hidden photon + sterile neutrinos
æ
æ
æ
æ æææææææææææææææææææææææææææææææææ
10-1 100 101 102 10310-8
10-7
10-6
10-5
10-4
10-3
10-2
10-1
100
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102
Erec HkeVeeL
coun
ts�N
A�k
eVee
�yea
r
electron recoil
DAMA
Borexino
XENON100 e-
CoGeNT
Standard model
B
C
DA
Line MA¢ gegΝ
A ΜΝ = 0.32 ´ 10-10ΜB
B 10 keV 4 ´ 10-12
C 50 keV 4 ´ 10-12
D 250 keV 6 ´ 10-12
10-4 10-3 10-2 10-1 100 10110-2
10-1
100
101
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Erec HkeVnrLco
unts
�ton�
keV
nr�y
ear
Nuclear recoil –Ge
CoGeNT
CDMS-II
D
C
B
A
Standard model
Line MA¢ gNgΝ sin2Θ24
A ΜΝ = 0.32 ´ 10-10ΜB activeB 100 MeV 9 ´ 10-8 activeC 100 MeV 8 ´ 10-7 0.02D 10 MeV 10-6 0.02
A: ν magnetic moment A: ν magnetic momentB, C, D: kinetically mixed A′ + sterile νs B: U(1)B−L boson
C: kinetically mixed U(1)′ + sterile νD: U(1)B + sterile ν charged under U(1)Bproposed in Pospelov 1103.3261, details in Pospelov Pradler 1203.0545Enhanced scattering at low Er for light A′
Negligible compared to SM scattering (∼ g4mT /M4W ) at energies probed in dedicated
neutrino experimentsHarnik JK Machado 1202.6073
Joachim Kopp ν signals in dark matter detectors 19
Heavier sterile neutrinosSterile neutrinos with mass close to a kinematic threshold in the Sun lead todifferent recoil spectra
Example: mνs ∼ 861 keV (energy of solar Be-7 line: 7Be + e− → 7Li + ν)
æ
æ
æ
æ æææææææææææææææææææææææææææææææææ
10-1 100 101 102 10310-8
10-7
10-6
10-5
10-4
10-3
10-2
10-1
100
101
102
Erec HkeVeeL
coun
ts�N
A�k
eVee
�yea
r
electron recoil
DAMA
Borexino
XENON100 e-
CoGeNT
Standard model
Line mΝs allA 860 keV MA¢ = 10 keVB 850 keV ge gΝ sinΘ24 = 10-11
C 700 keV
Plot from Harnik JK Machado 1202.6073
Joachim Kopp ν signals in dark matter detectors 20
Outline
1 Direct Dark Matter detection
2 Standard Model neutrino backgrounds in DM detectors
3 Enhanced neutrino scattering from new physics
4 Temporal modulation of ν signals
5 Constraints on hidden photons and sterile neutrinos
6 Conclusions
Joachim Kopp ν signals in dark matter detectors 21
Annual modulation as a “smoking gun” DM signatureAn annually modulation signal is considered very robust evidence for DM.
Freese Frieman Gould 1988
Earth’s velocity relative to the Milky Way’s DM halo is different in summerand in winter
I Expect annually modulating scattering ratesI Low recoil energy, heavy DM: Peak in summer
High recoil energy, light DM: Peak in winter
The DAMA signalI Highly controversial evidence for annual modulation in nuclear or electron
recoils from NaI detectors2-4 keV
Time (day)
Res
idua
ls (
cpd/
kg/k
eV)
DAMA/LIBRA ≈ 250 kg (0.87 ton×yr)
DAMA collaboration, Bernabei et al. 1002.1028
Joachim Kopp ν signals in dark matter detectors 22
Annual modulation as a “smoking gun” DM signatureAn annually modulation signal is considered very robust evidence for DM.
Freese Frieman Gould 1988
Earth’s velocity relative to the Milky Way’s DM halo is different in summerand in winter
I Expect annually modulating scattering ratesI Low recoil energy, heavy DM: Peak in summer
High recoil energy, light DM: Peak in winter
0 200 400 600 800
v @km�sD
ÙdHc
osΘL
vfH
v®L@
A.U
.D
700 720 740 760 780 800
t = Jun 01
t = Sep 01
t = Dec 01
DM scattering rate:
dRdEr∝∫
vmin
d3vf (~v + ~v⊕)
v
vmin =mN + mχ
mNmχ
√Er mN
2
The DAMA signalI Highly controversial evidence for annual modulation in nuclear or electron
recoils from NaI detectors2-4 keV
Time (day)
Res
idua
ls (
cpd/
kg/k
eV)
DAMA/LIBRA ≈ 250 kg (0.87 ton×yr)
DAMA collaboration, Bernabei et al. 1002.1028
Joachim Kopp ν signals in dark matter detectors 22
Annual modulation as a “smoking gun” DM signatureAn annually modulation signal is considered very robust evidence for DM.
Freese Frieman Gould 1988
Earth’s velocity relative to the Milky Way’s DM halo is different in summerand in winter
I Expect annually modulating scattering ratesI Low recoil energy, heavy DM: Peak in summer
High recoil energy, light DM: Peak in winter
The DAMA signalI Highly controversial evidence for annual modulation in nuclear or electron
recoils from NaI detectors2-4 keV
Time (day)
Res
idua
ls (
cpd/
kg/k
eV)
DAMA/LIBRA ≈ 250 kg (0.87 ton×yr)
DAMA collaboration, Bernabei et al. 1002.1028
Joachim Kopp ν signals in dark matter detectors 22
Annual modulation from ellipticity of the Earth orbitEarth–Sun distance is 3.4% larger in summer than in winterThus, the solar neutrino count rate is generically ∼ 7% larger in winterthan in summerThis modulation is opposite to the DAMA modulation . . .. . . but can mimic signals of O(100 GeV) dark matter Freese Frieman Gould 1988
Joachim Kopp ν signals in dark matter detectors 23
Annual modulation from active–sterile oscillationsFor active–sterile oscillations with oscillation lengths . 1 AU, sterile neutrinoappearance depends on the time of year.
Pospelov 1103.3261, Harnik JK Machado 1202.6073, Pospelov Pradler 1203.0545
This does not require extreme fine-tuningJoachim Kopp ν signals in dark matter detectors 24
More modulation mechanismsSterile neutrino absorption: For strong νs–A′ couplings and not-too-weakA′–SM couplings, sterile neutrino cannot traverse the Earth.→ lower flux at night. And nights are longer in winter.
Earth matter effects: An MSW-type resonance can lead to modified fluxof certain neutrino flavors at night. And nights are longer in winter.Direction-dependent detection efficiencies: If channeling effects arenon-negligible, detection rates depend on the position of the Sun.
Joachim Kopp ν signals in dark matter detectors 25
More modulation mechanismsSterile neutrino absorption: For strong νs–A′ couplings and not-too-weakA′–SM couplings, sterile neutrino cannot traverse the Earth.→ lower flux at night. And nights are longer in winter.Earth matter effects: An MSW-type resonance can lead to modified fluxof certain neutrino flavors at night. And nights are longer in winter.
Direction-dependent detection efficiencies: If channeling effects arenon-negligible, detection rates depend on the position of the Sun.
Joachim Kopp ν signals in dark matter detectors 25
More modulation mechanismsSterile neutrino absorption: For strong νs–A′ couplings and not-too-weakA′–SM couplings, sterile neutrino cannot traverse the Earth.→ lower flux at night. And nights are longer in winter.Earth matter effects: An MSW-type resonance can lead to modified fluxof certain neutrino flavors at night. And nights are longer in winter.
I A special case: Oscillation lengths comparable to 2R⊕or ∼ 1 km (thickness of rock overburden)
1 10 100 1000 1040.00
0.05
0.10
0.15
0.20
Distance L travelled in matter @kmD
Fra
ctio
no
fti
me
Solar Ν baselines at Gran Sasso
Winter HOct-MarLSummer HApr-SepL
Direction-dependent detection efficiencies: If channeling effects arenon-negligible, detection rates depend on the position of the Sun.
Joachim Kopp ν signals in dark matter detectors 25
More modulation mechanismsSterile neutrino absorption: For strong νs–A′ couplings and not-too-weakA′–SM couplings, sterile neutrino cannot traverse the Earth.→ lower flux at night. And nights are longer in winter.Earth matter effects: An MSW-type resonance can lead to modified fluxof certain neutrino flavors at night. And nights are longer in winter.Direction-dependent detection efficiencies: If channeling effects arenon-negligible, detection rates depend on the position of the Sun.
Joachim Kopp ν signals in dark matter detectors 25
Outline
1 Direct Dark Matter detection
2 Standard Model neutrino backgrounds in DM detectors
3 Enhanced neutrino scattering from new physics
4 Temporal modulation of ν signals
5 Constraints on hidden photons and sterile neutrinos
6 Conclusions
Joachim Kopp ν signals in dark matter detectors 26
Hidden photons
L ⊃ −14
F ′µνF ′µν − 14
FµνFµν − 12εF ′µνFµν + ν̄s i /∂νs + g′ν̄sγ
µνsA′µ
10-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 110-16
10-14
10-12
10-10
10-8
10-6
10-4
10-210-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 1
10-16
10-14
10-12
10-10
10-8
10-6
10-4
10-2
Dark Photon Mass MA'HGeVL
Kin
etic
mix
ing
Ε
Fixedtarget
Kinetically Mixed Gauge Boson
Hg-2LΜ
Hg-2Le
U
SN1987A
Atomic PhysicsAtomic Physics
CMB
Glo
bula
rC
lust
ers
Sun�Globular Clusters, energy loss via Νs
Hin models with d 10 keV sterile neutrinosL
Sun
A' capture in SunHpartly allowedL
CASTCMB
LSW
gΝ2 sin22Θ=10-4
gΝ2 sin22Θ=10-12
Borexino Hin models with UH1L'-charged sterile ΝL
Constraints from Jaeckel Ringwald 1002.0329, Redondo 0801.1527,Bjorken Essig Schuster Toro 0906.0580, Dent Ferrer Krauss 1201.2683, Harnik JK Machado 1202.6073
Joachim Kopp ν signals in dark matter detectors 27
Anomalous energy loss in stars and supernovaeA′ bosons can be produced by plasmon oscillations in stars + supernovae
see e.g. Redondo 0801.1527 and references therein
L ⊃ −14
F ′µνF ′µν − 14
FµνFµν − 12εF ′µνFµν +
12
m2A′A′µA′µ + Aµjµ
= −14
F ′µνF ′µν − 14
FµνFµν
+12
m2A′A′µA′µ − εm2
A′A′µAµ +12ε2m2
A′AµAµ + Aµjµ
Equations of motion:
(k2gµν − Πµν(k)− ε2m2A′)Aν + εm2
A′A′µ = 0
(k2gµν −m2A′)A′µ + εm2
A′Aµ = 0
(Πµν(k) = polarization tensor, depends on plasma frequency ωP
and on the inverse bremsstrahlung and Compton scattering rates)
Three regimesI Low mA′ : A′ production suppressed by small effective mixing ∼ m4
A′/ω4P
I mA′ ∼ ωP : Resonant A′ productionI High mA′ : Thermal A′ production
Interesting features:
I Resonant enhancement when MA′ ∼ plasmon massI In general: Non-resonant A′ production everywhere in the star
(not just in the outer photosphere)I But: For very large ε, small optical depth even for A′
→ reduced production, weaker limit
Limit based on requirement Pinvisible < Pvisible (P = energy loss rate)
Joachim Kopp ν signals in dark matter detectors 28
Anomalous energy loss in stars and supernovaeA′ bosons can be produced by plasmon oscillations in stars + supernovae
see e.g. Redondo 0801.1527 and references therein
Interesting features:I Resonant enhancement when MA′ ∼ plasmon massI In general: Non-resonant A′ production everywhere in the star
(not just in the outer photosphere)I But: For very large ε, small optical depth even for A′
→ reduced production, weaker limitLimit based on requirement Pinvisible < Pvisible (P = energy loss rate)
10-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 110-16
10-14
10-12
10-10
10-8
10-6
10-4
10-210-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 1
10-16
10-14
10-12
10-10
10-8
10-6
10-4
10-2
Dark Photon Mass MA'HGeVL
Kin
etic
mix
ing
Ε
Fixedtarget
Kinetically Mixed Gauge Boson
Hg-2LΜ
Hg-2Le
U
SN1987A
Atomic PhysicsAtomic Physics
CMB
Glo
bula
rC
lust
ers
Sun�Globular Clusters, energy loss via Νs
Hin models with d 10 keV sterile neutrinosL
Sun
A' capture in SunHpartly allowedL
CASTCMB
LSW
gΝ2 sin22Θ=10-4
gΝ2 sin22Θ=10-12
Borexino Hin models with UH1L'-charged sterile ΝL
Joachim Kopp ν signals in dark matter detectors 28
Anomalous energy loss in stars and supernovaeA′ bosons can be produced by plasmon oscillations in stars + supernovae
see e.g. Redondo 0801.1527 and references therein
Interesting features:I Resonant enhancement when MA′ ∼ plasmon massI In general: Non-resonant A′ production everywhere in the star
(not just in the outer photosphere)I But: For very large ε, small optical depth even for A′
→ reduced production, weaker limitLimit based on requirement Pinvisible < Pvisible (P = energy loss rate)
10-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 110-16
10-14
10-12
10-10
10-8
10-6
10-4
10-210-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 1
10-16
10-14
10-12
10-10
10-8
10-6
10-4
10-2
Dark Photon Mass MA'HGeVL
Kin
etic
mix
ing
Ε
Fixedtarget
Kinetically Mixed Gauge Boson
Hg-2LΜ
Hg-2Le
U
SN1987A
Atomic PhysicsAtomic Physics
CMB
Glo
bula
rC
lust
ers
Sun�Globular Clusters, energy loss via Νs
Hin models with d 10 keV sterile neutrinosL
Sun
A' capture in SunHpartly allowedL
CASTCMB
LSW
gΝ2 sin22Θ=10-4
gΝ2 sin22Θ=10-12
Borexino Hin models with UH1L'-charged sterile ΝL
Joachim Kopp ν signals in dark matter detectors 2810-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 110-16
10-14
10-12
10-10
10-8
10-6
10-4
10-210-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 1
10-16
10-14
10-12
10-10
10-8
10-6
10-4
10-2
Dark Photon Mass MA'HGeVL
Kin
etic
mix
ing
Ε
Fixedtarget
Kinetically Mixed Gauge Boson
Hg-2LΜ
Hg-2Le
U
SN1987A
Atomic PhysicsAtomic Physics
CMB
Glo
bula
rC
lust
ers
Sun�Globular Clusters, energy loss via Νs
Hin models with d 10 keV sterile neutrinosL
Sun
A' capture in SunHpartly allowedL
CASTCMB
LSW
gΝ2 sin22Θ=10-4
gΝ2 sin22Θ=10-12
Borexino Hin models with UH1L'-charged sterile ΝL
Other constraints (1)
10-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 110-16
10-14
10-12
10-10
10-8
10-6
10-4
10-210-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 1
10-16
10-14
10-12
10-10
10-8
10-6
10-4
10-2
Dark Photon Mass MA'HGeVL
Kin
etic
mix
ing
Ε
Fixedtarget
Kinetically Mixed Gauge Boson
Hg-2LΜ
Hg-2Le
U
SN1987A
Atomic PhysicsAtomic Physics
CMB
Glo
bula
rC
lust
ers
Sun�Globular Clusters, energy loss via Νs
Hin models with d 10 keV sterile neutrinosL
Sun
A' capture in SunHpartly allowedL
CASTCMB
LSW
gΝ2 sin22Θ=10-4
gΝ2 sin22Θ=10-12
Borexino Hin models with UH1L'-charged sterile ΝL
Muon and electron g − 2Atomic physics: Test 1/r2 scaling of electromagnetic forceLight shining through wallsFixed target experiments: A′ production in beam dump, decay to SM
I Expect significant improvement from APEX
Joachim Kopp ν signals in dark matter detectors 29
Other constraints (2)
10-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 110-16
10-14
10-12
10-10
10-8
10-6
10-4
10-210-24 10-21 10-18 10-15 10-12 10-9 10-6 10-3 1
10-16
10-14
10-12
10-10
10-8
10-6
10-4
10-2
Dark Photon Mass MA'HGeVL
Kin
etic
mix
ing
Ε
Fixedtarget
Kinetically Mixed Gauge Boson
Hg-2LΜ
Hg-2Le
U
SN1987A
Atomic PhysicsAtomic Physics
CMB
Glo
bula
rC
lust
ers
Sun�Globular Clusters, energy loss via Νs
Hin models with d 10 keV sterile neutrinosL
Sun
A' capture in SunHpartly allowedL
CASTCMB
LSW
gΝ2 sin22Θ=10-4
gΝ2 sin22Θ=10-12
Borexino Hin models with UH1L'-charged sterile ΝL
CMB: Distortions to the black body spectrumAxion telescopes (e.g. CAST): Look for A′ from the Sun oscillating to AB-factories: e+e− → A′ + something,A′ detected as /E or via its decay productsIn models with light sterile neutrinos:
I νs production in stars + supernovaeI νse scattering in Borexino
Joachim Kopp ν signals in dark matter detectors 30
Outline
1 Direct Dark Matter detection
2 Standard Model neutrino backgrounds in DM detectors
3 Enhanced neutrino scattering from new physics
4 Temporal modulation of ν signals
5 Constraints on hidden photons and sterile neutrinos
6 Conclusions
Joachim Kopp ν signals in dark matter detectors 31
ConclusionsNeutrino detection and DM detection are closely related(experimentally and theoretically)Low-E solar neutrino spectrum only accessible in DM detectorsWell-motivated new physics could show up at low E .Models with hidden photons and sterile neutrinos can lead to interestingphenomena in dark matter detectors
I Enhanced neutrino–electron scatteringI Enhanced neutrino–nucleus scatteringI Possibility of annual and daily modulation
Joachim Kopp ν signals in dark matter detectors 32
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