dama/libra-phase2 in wimp effective...
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DAMA/LIBRA-phase2 in WIMP effective modelsSUNGHYUN KANG
IN COLLABORATION WITH S . SCOPEL , G. TOMAR, J .H. YOON
SOGANG UNIVERSITY
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Introduction
Many evidences of Dark Matter
CDM(Cold Dark Matter)
Neutrino
WIMP
(Weakly Interacting Massive Particle)
"Content of the Universe - Pie Chart“Wilkinson Microwave Anisotropy Probe.
National Aeronautics and Space Administration. Retrieved 9 January 2018.
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DAMA/LIBRA-phase2 analyses
Bernabei et al. (DAMA Collaboration), 1805.10486
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DAMA/LIBRA-phase2 analyses
A. L. Fitzpatrick, W. Haxton, E. Katz, N. Lubbers, and Y. Xu, The Effective Field Theory of Dark Matter Direct Detection, JCAP 1302 (2013) 004
τ : isospinj : interaction type
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DAMA/LIBRA-phase2 analyses
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon DAMA/LIBRA-phase2 in WIMP effective models, JCAP07(2018)016
𝑅𝑙ττ′: WIMP response function
𝑊𝑙ττ′: nucleus response function: M, Σ’, Σ’’, Δ, φ’’, φ’ (M=SI, , Σ’, Σ’’=SD)
(from Nikhil Anand, A. Liam Fitzpatrick, W. C. Haxton,Model-independent WIMP Scattering Responses and EventRates : A Mathematica Package for Experimental Analysis)
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DAMA/LIBRA-phase2
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon DAMA/LIBRA-phase2 in WIMP effective models, JCAP07(2018)016
Considering one EFT coupling at a time
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DAMA/LIBRA-phase2 analyses
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon DAMA/LIBRA-phase2 in WIMP effective models, JCAP07(2018)016
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DAMA/LIBRA-phase2 analyses
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon DAMA/LIBRA-phase2 in WIMP effective models, JCAP07(2018)016
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DAMA/LIBRA-phase2 analyses
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon DAMA/LIBRA-phase2 in WIMP effective models, JCAP07(2018)016
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DAMA/LIBRA-phase2
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DAMA/LIBRA-phase2
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Anapole Dark Matter(ADM)
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon, P. Gondolo, Anapole Dark Matter after DAMA/LIBRA-phase2, arXiv:1808.04112
Electric, velocity dependent part
Magnetic, velocity independent part
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Anapole Dark Matter(ADM)
Experimental form factorHaxton(blue dot-dash) vs
experimental form factor(purple)
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Anapole Dark Matter(ADM)
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon, P. Gondolo, Anapole Dark Matter after DAMA/LIBRA-phase2, arXiv:1808.04112
Maxwellian velocity distribution Maxwellian velocity distribution
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Anapole Dark Matter(ADM)
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon, P. Gondolo, Anapole Dark Matter after DAMA/LIBRA-phase2, arXiv:1808.04112
Halo independent case
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pSIDM
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon, Proton-philic spin-dependent inelastic Dark Matter (pSIDM) as a viable explanation of DAMA/LIBRA-phase2, arXiv:1810.09674
χ 𝑚χ′ −𝑚χ = δ
Inelastic case : δ ≠ 0
pp
Χ’
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pSIDM
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon, Proton-philic spin-dependent inelastic Dark Matter (pSIDM) as a viable explanation of DAMA/LIBRA-phase2, arXiv:1810.09674
How pSIDM evades constraints
Xe, Ge: spin-dependent WIMP-proton cross section(no interaction with neutron)
F : 𝑣𝑚𝑖𝑛∗𝐹 > 𝑣𝑒𝑠𝑐
DAMA signal is okay since 𝑣𝑚𝑖𝑛∗𝑁𝑎, 𝑣𝑚𝑖𝑛
∗𝐼 < 𝑣𝑒𝑠𝑐
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pSIDM
Sunghyun Kang, S.S., G. Tomar, J.H. Yoon, Proton-philic spin-dependent inelastic Dark Matter (pSIDM) as a viable explanation of DAMA/LIBRA-phase2, arXiv:1810.09674
Halo independent caseMaxwellian velocity distribution
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Conclusions
non-relativistic effective models can fit the DAMA/LIBRA-phase2 data with less fine tuning compared to a standard SI interaction- all model excluded by fluorine&xenon detectors
Anapole Dark Matter could explain DAMA/LIBRA-phase1 in compliance with constraints from other experiments. It is now excluded after DAMA/LIBRA-phase2.
pSIDM could explain DAMA/LIBRA-phase1 in compliance with constraints from other experiments. Still OK after DAMA/LIBRA-phase2 if WIMP velocity distribution departs from a Maxwellian.