Direct Detection of Strongly Interacting Sub-GeV Dark Matter via Electron Recoils
Mukul Sholapurkar
C.N. Yang Institute for Theoretical Physics, Stony Brook
Invisibles’19 Workshop
*in collaboration with Rouven Essig, Chris Kouvaris and Timon Emken
arXiv:1905.06348*
Direct Detection of strongly interacting DM
* Essig, Volansky and Yu (1703.00910)
•
Dark matter can scatter off the nuclei and the electrons in the overburden (earth, atmosphere or experiment shielding)
•
Can become invisible to the detector above a critical cross section
What happens as we
increase the cross section ?
The Model
• Dark Photon:
• Electric Dipole Moment:
Electron Interaction
Nuclear Interaction
Stopping Power
• Total stopping power:
Elastic Nuclear
Recoils
Inelastic Electronic
Recoils
Elastic Electronic
(Atomic) Recoil
• Nuclear stopping power:
• Atomic stopping power:
Calculating Constraints
• Monte Carlo simulations :
o Simulate the DM particles traveling through the Earth’s crust or the atmosphere.
(Reference: Emken and Kouvaris 1706.02249) o Analysis includes deflections in the trajectory.
• Analytic method :
o Calculate the final velocity distribution of the DM particles after passing through the crust or the atmosphere.
o Analysis assumes no deflections in the trajectory.
0 200 400 600 800
10-10 10-8 10-6 10-4 10-2
v[km/sec]
f(v)[sec/km]
FDM=(αme/q)2 mχ=100 MeV
vmin
10-32cm2
10-
30cm2 10-29cm2
10-28cm2 3⨯10-28cm2
2⨯10-27cm2 3⨯10-27cm2 4⨯10-27cm2
5⨯10-27cm2 6⨯10-27cm2 8⨯10-27cm2
10-26cm2 no shielding crust shielding(MC)
10-36 10-34 10-32 10-30 10-28 10-26 10-2
100 102 104 106 108 1010 1012
σe[cm2] Nevents
FDM=(αme/q)2 mχ=100 MeV
Si semiconductor target exposure: 0.1 gram yr threshold: 1 e-h+pair underground depth: 1000m
Constraints
100 101 102 103
10-38 10-36 10-34 10-32 10-30 10-28 10-26 10-24 10-22 10-20 10-18
mχ[MeV]
σe[cm2 ]
FDM=1
protoSENSEI@surface CDMS-HVeV protoSENSEI@MINOS XENON10 XE
NON100 DS-50
100 101 102 1000
10-36 10-34 10-32 10-30 10-28 10-26 10-24 10-22 10-20
mχ[MeV]
σe[cm2 ]
FDM=(αme/q)2
protoSENSEI@surface
protoSECDMSNSEI-HVeV@MINOS XENON10 XENON100
DS-50
100 101 102 1000 104
10-36 10-34 10-32 10-30 10-28 10-26 10-24 10-22 10-20 10-18
mχ[MeV]
σe[cm2 ]
FDM=αme/q
protoSENSEI@surface
XENON10
CDMS-HVeV protoSENSEI@MINOS
DS-50 XENON100
Prospects for Balloon/Satellite Experiment
• Balloon/Satellite experiments have very little overburden and have a potential of probing high cross section parameter space
• Also have a modulation signal !
Balloon ISS halo
0 200 400 600 800
0.
0.5 1.
1.5 2.
2.5 3.
v[km/sec]
f(v)[10-3 sec/km]
Balloon ISS
0 200 400 600 800 1000 1200 1400
0 0.5 1 1.5 2
UT [min]
eventrate[105 gr-1 sec-1 ]
mχ=100 MeV, σe=10-23cm2, FDM=(αme/q)2, Ωχ=0.01ΩDM no shadowing
Conclusions
•
Terrestrial effects limit the sensitivity of direct detection experiments to high cross sections•
We calculated constraints and projections for several direct detectionexperiments like SENSEI, XENON10/100 etc. for the dark photon model and an electric dipole moment interaction.
