Comparison between DAMA/LIBRA and COSINE-100 in the light of Quenching Factors. (arXiv:1907.04963v1 [hep-ex])

Comparison between DAMA/LIBRA and COSINE-100 in the light of Quenching Factors. (arXiv:1907.04963v1 [hep-ex])
<a href="http://arxiv.org/find/hep-ex/1/au:+Ko_Y/0/1/0/all/0/1">Y. J. Ko</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kim_K/0/1/0/all/0/1">K. W. Kim</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Adhikari_G/0/1/0/all/0/1">G. Adhikari</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Adhikari_P/0/1/0/all/0/1">P. Adhikari</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Souza_E/0/1/0/all/0/1">E. Barbosa de Souza</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Carlin_N/0/1/0/all/0/1">N. Carlin</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Choi_J/0/1/0/all/0/1">J. J. Choi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Choi_S/0/1/0/all/0/1">S. Choi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Djamal_M/0/1/0/all/0/1">M. Djamal</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Ezeribe_A/0/1/0/all/0/1">A. C. Ezeribe</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Ha_C/0/1/0/all/0/1">C. Ha</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Hahn_I/0/1/0/all/0/1">I. S. Hahn</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Jeon_E/0/1/0/all/0/1">E. J. Jeon</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Jo_J/0/1/0/all/0/1">J. H. Jo</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kang_W/0/1/0/all/0/1">W. G. Kang</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kauer_M/0/1/0/all/0/1">M. Kauer</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kim_G/0/1/0/all/0/1">G. S. Kim</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kim_H/0/1/0/all/0/1">H. Kim</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kim_H/0/1/0/all/0/1">H. J. Kim</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kim_N/0/1/0/all/0/1">N. Y. Kim</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kim_S/0/1/0/all/0/1">S. K. Kim</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kim_Y/0/1/0/all/0/1">Y. D. Kim</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Kim_Y/0/1/0/all/0/1">Y. H. Kim</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lee_E/0/1/0/all/0/1">E. K. Lee</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lee_H/0/1/0/all/0/1">H. S. Lee</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lee_J/0/1/0/all/0/1">J. Lee</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lee_J/0/1/0/all/0/1">J. Y. Lee</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lee_M/0/1/0/all/0/1">M. H. Lee</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lee_S/0/1/0/all/0/1">S. H. Lee</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Leonard_D/0/1/0/all/0/1">D. S. Leonard</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Lynch_W/0/1/0/all/0/1">W. A. Lynch</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Manzato_B/0/1/0/all/0/1">B. B. Manzato</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Maruyama_R/0/1/0/all/0/1">R. H. Maruyama</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Neal_R/0/1/0/all/0/1">R. J. Neal</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Olsen_S/0/1/0/all/0/1">S. L. Olsen</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Park_B/0/1/0/all/0/1">B. J. Park</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Park_H/0/1/0/all/0/1">H. K. Park</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Park_H/0/1/0/all/0/1">H. S. Park</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Park_K/0/1/0/all/0/1">K. S. Park</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Pitta_R/0/1/0/all/0/1">R. L. C. Pitta</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Prihtiadi_H/0/1/0/all/0/1">H. Prihtiadi</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Ra_S/0/1/0/all/0/1">S. J. Ra</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Rott_C/0/1/0/all/0/1">C. Rott</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Shin_K/0/1/0/all/0/1">K. A. Shin</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Scarff_A/0/1/0/all/0/1">A. Scarff</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Spooner_N/0/1/0/all/0/1">N. J. C. Spooner</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Thompson_W/0/1/0/all/0/1">W. G. Thompson</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Yang_L/0/1/0/all/0/1">L. Yang</a>, <a href="http://arxiv.org/find/hep-ex/1/au:+Yu_G/0/1/0/all/0/1">G. H. Yu</a> (COSINE-100 Collaboration)

There is a long standing debate about whether or not the annual modulation
signal reported by the DAMA/LIBRA collaboration is induced by Weakly
Interacting Massive Particles (WIMP) in the galaxy’s dark matter halo
scattering from nuclides in their NaI(Tl) crystal target/detector. This is
because regions of WIMP-mass vs. WIMP-nucleon cross-section parameter space
that can accommodate the DAMA/LIBRA-phase1 modulation signal in the context of
the standard WIMP dark matter galactic halo and isospin-conserving (canonical),
spin-independent (SI) WIMP-nucleon interactions have been excluded by the
COSINE-100 experiment that uses the same NaI(Tl) target/detector material.
Moreover, the recently released DAMA/LIBRA-phase2 results are inconsistent with
an interpretation as WIMP-nuclide scattering via the canonical SI interaction
and prefer, instead, isospin-violating or spin-dependent interactions. Dark
matter interpretations of the DAMA/LIBRA signal are sensitive to the NaI(Tl)
scintillation efficiency for nuclear recoils, which is characterized by
so-called quenching factors (QF), and the QF values used in previous studies
differ significantly from recently reported measurements, which may have led to
incorrect characterizations of the DAMA/LIBRA signal. In this article, the
compatibility of the DAMA/LIBRA and COSINE-100 results, in light of the new QF
measurements is examined for different possible types of WIMP-nucleon
interactions. The resulting allowed parameter space regions associated with the
DAMA/LIBRA signal are explicitly compared with 90% confidence level upper
limits from the initial 59.5 day COSINE-100 exposure. With the newly measured
QF values, the allowed 3$sigma$ regions from the DAMA/LIBRA data are still
generally excluded by the COSINE-100 data.

There is a long standing debate about whether or not the annual modulation
signal reported by the DAMA/LIBRA collaboration is induced by Weakly
Interacting Massive Particles (WIMP) in the galaxy’s dark matter halo
scattering from nuclides in their NaI(Tl) crystal target/detector. This is
because regions of WIMP-mass vs. WIMP-nucleon cross-section parameter space
that can accommodate the DAMA/LIBRA-phase1 modulation signal in the context of
the standard WIMP dark matter galactic halo and isospin-conserving (canonical),
spin-independent (SI) WIMP-nucleon interactions have been excluded by the
COSINE-100 experiment that uses the same NaI(Tl) target/detector material.
Moreover, the recently released DAMA/LIBRA-phase2 results are inconsistent with
an interpretation as WIMP-nuclide scattering via the canonical SI interaction
and prefer, instead, isospin-violating or spin-dependent interactions. Dark
matter interpretations of the DAMA/LIBRA signal are sensitive to the NaI(Tl)
scintillation efficiency for nuclear recoils, which is characterized by
so-called quenching factors (QF), and the QF values used in previous studies
differ significantly from recently reported measurements, which may have led to
incorrect characterizations of the DAMA/LIBRA signal. In this article, the
compatibility of the DAMA/LIBRA and COSINE-100 results, in light of the new QF
measurements is examined for different possible types of WIMP-nucleon
interactions. The resulting allowed parameter space regions associated with the
DAMA/LIBRA signal are explicitly compared with 90% confidence level upper
limits from the initial 59.5 day COSINE-100 exposure. With the newly measured
QF values, the allowed 3$sigma$ regions from the DAMA/LIBRA data are still
generally excluded by the COSINE-100 data.

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