SLIDE 1
Oren Slone Supervisor - Tomer V
- lansky
Direct Detection of Light Dark Matter
In collaboration with Rouven Essig, Jeremy Mardon
Thursday, July 24, 14
Motivation
u n
- e
x p l
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Thursday, July 24, 14
Direct Detection of Light Dark Matter Oren Slone Supervisor - Tomer - - PowerPoint PPT Presentation
Direct Detection of Light Dark Matter Oren Slone Supervisor - Tomer - - PowerPoint PPT Presentation
Direct Detection of Light Dark Matter Oren Slone Supervisor - Tomer V olansky In collaboration with Rouven Essig, Jeremy Mardon Thursday, July 24, 14 Motivation u n - e x p l o r e d Thursday, July 24, 14 New avenues for light DM
SLIDE 2
SLIDE 3
New avenues for light DM direct detection
Chemical Bond Breaking in Molecules
Low Energy Threshold Systems
Creation of Color Centers q m1 m2 m2 m1 ~ few eV ~ few 10 eV
Thursday, July 24, 14
SLIDE 4
Molecular Detection Rate
V elocity Distribution DM Form Factor Target Form Factor # of Targets DM Density
Thursday, July 24, 14
SLIDE 5
The Molecular Form Factor
Final State W avefunction Initial State W avefunction The FF ~ The W avefunction Overlap
2 3 4 5 6 r @a0D
- 0.4
- 0.2
0.2 0.4 0.6
WaveFunction Overlap for l=90
Thursday, July 24, 14
SLIDE 6
Understanding the Rate
Outgoing Free Radial Waves Classical Picture
240 260 280 300 320 q @keVD 5 10 15 20 †FdisHqL§2
20 eV Molecular Form Factor
q m1 m2 m2 m1
Thursday, July 24, 14
SLIDE 7
Expected Rates for H2
1 10 100 1000 104 Mc @MeVD 1000 104 105 106 107 108
Event Rate @
100 kg yrD
Radial Waves Classical Picture
Thursday, July 24, 14
SLIDE 8
Expected Sensitivity
10 102 103 104 10-45 10-44 10-43 10-42 10-41 10-40 10-39 103 104 105 106 107 108 m c @MeVêc2D sp @cm2D Event Rate Hsp=10-37cm2L
Cross Section Sensitivity and Event Rate for H2
+
Hper 100kg yearL
Thursday, July 24, 14
SLIDE 9
Future Prospects
Understanding Color Centers Solar Neutrinos Experimental Setup
Thursday, July 24, 14
SLIDE 10
Thank You
Thursday, July 24, 14
SLIDE 11
Backup
Thursday, July 24, 14
SLIDE 12
The True Interaction Rate
Form Factor is suppressed because outgoing wavefunction has less overlap. Phase space grows because the momentum grows as the atom leaves the potential well.
Two Competing Effects
Thursday, July 24, 14
SLIDE 13
Backgrounds
Use of annual modulation Slow neutrons: Understand the background from one area of the experiment and extrapolate. Use fiducial volume excluding the outskirts. Energetic neutrons: Remove high energy events. Neutrinos: Understand the Background Electrons / Gamma Rays: Problem for molecules No problem for color centers
Thursday, July 24, 14
SLIDE 14
Other Experiments
Experiment Detection Technique Reported Signal Energy Threshold Remarks XENON 100
Ionization and Scintillation NO ~ 10-100 keV
LUX
Ionization and Scintillation NO ~ 10 keV Currently most sensitive
DAMA/Libra
Scintillation NaI YES (Annual Modulation) Possibly due to muon flux
CDMS (Si / Ge)
Ionization and Phonons YES (for Si) NO (for Ge) ~ 10 keV Only a few events reported
CoGeNT
Ionization YES
CRESST
Phonon Detection YES
Molecules
Flouresence Ion Drifting Polymerization NOT YET ~ 10-100 eV
Thursday, July 24, 14
SLIDE 15
Other Experiments
Thursday, July 24, 14
SLIDE 16
Example Model for LDM
Fermionic DM charged under a new U(1)D AD gauge boson with coupling gD Coupling to SM through kinetic mixing with the photon.
Essig, Mardon, V
- lansky, arXiv: 1108:5383
Thursday, July 24, 14
SLIDE 17
Solar Neutrinos
Thursday, July 24, 14
SLIDE 18
Oren Slone Supervisor - Dr. Tomer Volansky
10 102 103 104 10-42 10-41 10-40 10-39 10-38 102 103 104 105 m c @MeVêc2D sp @cm2D Event Rate Hsp=10-37cm2L
Cross Section Sensitivity and Event Rate for H2
+Hper 100kg yearL
New direct detection techniques for light (sub GeV) DM
Chemical bond breaking in molecules Color centers
Experimental setup
Detection via photons / chemical amplification
Application to detection of solar neutrinos Dynamical RPV with new LHC phenomenology
Thursday, July 24, 14