A reviewon the discoveryreach of directionaldetectionpp · • constraint on DM properties (halo...
Transcript of A reviewon the discoveryreach of directionaldetectionpp · • constraint on DM properties (halo...
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A review on the discovery reach
of directional detection
F. Mayet
LPSC
Université Joseph Fourier
Grenoble, France
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Outline
1. Review of the discovery reach of directional detection
Exclusion
Discovery
Identification
2. Interplay with latest LHC results
Heavy squarks
monophoton/monojet
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WIMP fluxin galactic coordinates
Constellation Cygnus (l = 90°,b = 0°)
Elastic scattering100 GeV/c2 WIMP
Angular distribution of Fluorine recoils [5;50] keV
WIMP signal(recoil map)
Directional detection : expected signal
Background
Unambiguous differencebetween WIMP and
background
for a standard halo(isothermal and isotropic)
• low number of WIMPs(low exposure)
• large residual background• poor angular resolution
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1. Review of the discovery reach of directional detection
Exclusion
Discovery
Identification
Can we exclude a Dark Matter signal ?J. Billard et al., PRD 2010
S. Henderson et al., PRD 2008
0 WIMP + 300 Bckg
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Your preferred detector
Exclusion
Goal : try to be competitive with ongoing/planned direct experimentsdevoted to Spin-dependent interaction (on proton)
Best limit on SD interaction (proton)
Result depends on exposure,
residual background level,
threshold, …
Your preferred SUSY model
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Isotropy rejection
The exposure required to reject isotropy(and hence detect a WIMP signal) at 95% CL in 95% of exp.
Study done for a CS2 target
With ~104 kg.days (CS2) reach ~10-7 pb (SI)
3D without sense recognition
3D with sense recognition
A. M. Green & B. Morgan, Astropart. Phys. 2007
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1. Review of the discovery reach of directional detection
Exclusion
Discovery
Identification
100 WIMPs + 100 Bckg
Can we claim a Dark Matter discovery ?
J. Billard et al., PLB 2010, PRD 2012
A.M. Green & B. Morgan, PRD 2010
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Directional detection may be used to discover Dark Matter
Gal
actic
Latit
ude
Galactic Longitude
• Proof of discovery : signal from Cygnus
Ang
ula
rsi
gnat
ure
Exclusion strategy
Discovery strategy
J. Billard et al., PLB 2010, PRD 2012
Blind likelihood analysis
Estimation of the statistical significance…
Discovery
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Discovery at 3σWith BKG (300)
Without BKG
� Even with a large number of background events, discovery is still possible
� Only low number of WIMP events are required at low masses
� A discovery (>3σσσσ @90%CL) with BKG is possible down to 10-3-10-4 pb
Detector characteristics-10 kg CF4- DAQ : 3 years- Recoil energy range [5, 50] keV
Estimation of the discovery potentialconsidering astrophysical uncertainties=> Profile likelihood method
J. Billard et al., PLB 2010, PRD 2012
Discovery
3σσσσ discovery
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Discovery at 3σWith BKG (300)
Without BKG
� Even with a large number of background events, discovery is still possible
� Only low number of WIMP events are required at low masses
� A discovery (>3σσσσ @90%CL) with BKG is possible down to 10-3-10-4 pb
Estimation of the discovery potentialconsidering astrophysical uncertainties=> Profile likelihood method
detector characteristics-10 kg CF4- DAQ : 3 years- Recoil energy range [5, 50] keV
MSSM and NMSSM
J. Billard et al., PLB 2010, PRD 2012
D. Albornoz-Vasquez et al., PRD 2012
Discovery
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Directional reach in SUSY space
MSSM NMSSM
• (N)MSSM with 11(12) parameters defined at the weak scale• Cosmology and Colliders constraints included (before Higgs discovery)
� low µ and M1 models would not escape a discovery with a large directional detector (30 kg.year).
discovery
exclusion
D. Albornoz-Vasquez et al., PRD 2012
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J. Billard et al., PLB 2013
N-body simulations favor a co-rotating Dark Disk (10%-50% of local DM density)
�for a nul lag velocity, Dark Disk Wimps have an isotropic velocity distribution
Relative Asymmetry(in the mean recoil deviation)
�only extreme Dark Disk parameters may affect the directional signal
�not a threat for directional detection
standard halo (SH)
SH and extreme DD
Discovery : beyond the standard halo
3σσσσ discovery
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1. Review of the discovery reach of directional detection
Exclusion
Discovery
Identification
Can we infer Dark Matter properties from directional detection ?
J. Billard et al., PRD 2011
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Directional detection may be used to identify Dark Matter
i.e. measure WIMP and halo properties
Dark Matter identificationJ. Billard et al., PRD 2011
A Markov Chain Monte Carlo analysis dedicated to direc tional detection (10-3 pb)
• Simulated data : CF4 detector (30 kg.year) + 35% background
• Multivariate gaussian (triaxial halo)
• Eight free parameters constrain with the same set of directional data
• The WIMP mass mΧ
• The WIMP-nucleon cross section σn• The main direction of the signal (lO,bO)• The three velocity dispersions σx, σy et σz• The background rate Rb
WIMP properties
Halo properties
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Mass
Cross section
l
b
σx
σy
σz
Rb
Input parameters
• Isotropic halo σx = σy = σz = 155
km/s
• WIMP mass: 50
GeV/c2
• Cross section 10-3 pb
• Background rate (Rb): 10 evts/kg/an
(35%)
The eight fitting parameters are simultaneously and consistently contrained according to the input values
Dark Matter identification
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WIMP mass Vs cross section WIMP velocity distributionDiscovery proof
The eight parameters are strongly constrained with only one directional data set.
Masse
Section efficace
l
b
σx
σy
σz
J. Billard et al., PRD 2011
Dark Matter identification
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Going further : Dark Matter 3D
D. S. M. Alves et al., arXiv1204.5487
Post-discovery era : the WIMP mass and cross section are supposed to be knownHence, after LHC discovery and/or other DM exp.
• A generic parametrization of DM distribution• 3 integrals of motion decomposedon the basis of special functions
~1000 events are required for a good measurement of the underlying DM distribution
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A priori : no ! SD-neutron versus SD-proton, but…
Is Xenon100 a threat to directional detection ?
2. Interplay with latest LHC results
Heavy squarks
monophoton/monojet
Is LHC a threat to directional detection ?
D. Albornoz-Vasquez et al., PRD 2012
G. Bélanger et al., in preparation
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SD interaction
Proton SD interaction (an=0)
CF4 detectorsNeutron SD interaction (ap=0)
Xenon100, CDMS, Edelweis, ..
First caveat : model independent treatment requires to consider both cross-sectionsD. R. Tovey et al., PLB 2010
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Recent results from LHC
SUPPRESSED
• LHC => Heavy squarks (>TeV)
• Squark exchang diagramm : suppressed
• SD cross section :
�does not depend on quark flavor
�only on the Z-neutralino coupling
SD cross section should be close (and should not depend on SUSY parameters)
(2013)
ATLAS-CONF-2013-047
simplified phenomenological MSSM
(2011)
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MSSM + collider & cosmology contraints MSSM + … + LHC squark result
D. Albornoz-Vasquez et al., PRD 2012
Consequences for Dark Matter
• SD cross-section on p and n can no longer be considered as independent
�All SD results apply to directional detection
e.g. large exposure experiments (Xenon, SuperCDMS, …)
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SD interaction on Nucleon
• All SI experiments have a not so small odd-nuclei fraction (129,131Xe, 73Ge, 29Si)
3% in Si, 7% in Ge, 50% in Xe
We need to consider SD-nucleon cross section
• Upcoming SI results may close the directionnal window
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Other searches : monophoton/monojet @LHC
t-channel
Elastic scatterring
s-channel
DM pair production
golden channel … no signal
� consider ISR
� one photon/jet and missing energy
make it visible…
versus
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ATLAS Col., JHEP 2013, PRL 2013
• Effective theory
4-fermion interaction a la Fermi
Point like interaction = heavypropagator
Question :
Is it really model independent ?
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Conclusion
1) A large directional detector (30 kg.year) could lea d either to a :• constraint on DM properties (halo and particle), ~10-3 pb• conclusive discovery (with a high significance), 10-4-10-5 pb• competitive exclusion, 10-5-10-6 pb
cannot be achieved by non-directional detectors
2) Most other Dark Matter searches seem to be relevant to the SD-neutron space• Large exposure SI detectors • LHC• Neutrino telescope