]>PLB34477S0370-2693(19)30149-210.1016/j.physletb.2019.02.043The Author(s)ExperimentsFig. 1Recoil energy spectra for the scattering of spin-12 WIMPs on xenon nuclei, for WIMP masses of 40 GeV/c2 and 400 GeV/c2, and unit isoscalar (di0=1, di1=0) and isovector (di0=0, di1=1) coupling. Top panel: dimension-four V-A interactions. Bottom panel: higher dimension magnetic and electric dipole interactions.Fig. 1Fig. 2Exclusion limits on the coefficients of dimension-four (top panel) and higher dimension (bottom panel) operators.Fig. 2Fig. 3Recoil energy spectra for the scattering of spin-12 WIMPs on xenon nuclei, for WIMP masses of 40 GeV/c2 and 400 GeV/c2, for SD and tensor interactions. The top (bottom) panel corresponds to neutron-only (proton-only) coupling.Fig. 3Fig. 4PandaX-II exclusion limits on the WIMP-nucleon cross section for the standard SD interaction assuming neutron-only (top panel) and proton-only (bottom panel) coupling. The 1σ sensitivity bands are shown in green. Also shown are recent results from LUX [5], XENON100 [9], ATLAS [31], CMS [32], PICO-2L [33], PICO-60 [34,35], IceCube [36] and Super-K [37]. The dashed line (top panel) gives PandaX-II limits on tensor WIMP-neutron couplings.Fig. 4PandaX-II constraints on spin-dependent WIMP-nucleon effective interactionsJingkaiXiaaAbdusalamAbdukerimbWeiChenaXunChenaYunhuaChencXiangyiCuiaDeqingFangdChangboFuaKarlGiboniaFrancoGiulianiaLinhuiGuaXuyuanGuocZhifanGuoeKeHanaChangdaHeaShengmingHecDiHuangaXingtaoHuangfZhouHuangaPengJigXiangdongJiah1xdji@sjtu.edu.cnYonglinJueShaoliLiaHengLinaHuaxuanLiueJianglaiLiuahYugangMadYajunMaoiKaixiangNiaJinhuaNingcXiangxiangRenaFangShiaAndiTanjAnqingWangfChengWangeHongweiWangdMengWangfQiuhongWangdSiguangWangiXiuliWangeXumingWangaZhouWangeMengmengWugShiyongWucMengjiaoXiaojkPengweiXiehBinbinYanfJijunYangaYongYangaChunxuYugJuminYuanfJianfengYuecDanZhangjHongguangZhangaTaoZhangaLiZhaoaQibinZhenglJifangZhoucNingZhoua⁎nzhou@sjtu.edu.cnXiaopengZhouiWick C.Haxtonmn⁎⁎haxton@berkeley.eduaSchool of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai 200240, ChinaSchool of Physics and AstronomyShanghai Jiao Tong UniversityShanghai Key Laboratory for Particle Physics and CosmologyShanghai200240ChinabSchool of Physics and Technology, Xinjiang University, Ürümqi 830046, ChinaSchool of Physics and TechnologyXinjiang UniversityÜrümqi830046ChinacYalong River Hydropower Development Company, Ltd., 288 Shuanglin Road, Chengdu 610051, ChinaYalong River Hydropower Development Company, Ltd.288 Shuanglin RoadChengdu610051ChinadShanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, ChinaShanghai Institute of Applied PhysicsChinese Academy of SciencesShanghai201800ChinaeSchool of Mechanical Engineering, Shanghai Jiao Tong University, Shanghai 200240, ChinaSchool of Mechanical EngineeringShanghai Jiao Tong UniversityShanghai200240ChinafSchool of Physics and Key Laboratory of Particle Physics and Particle Irradiation (MOE), Shandong University, Jinan 250100, ChinaSchool of PhysicsKey Laboratory of Particle Physics and Particle Irradiation (MOE)Shandong UniversityJinan250100ChinagSchool of Physics, Nankai University, Tianjin 300071, ChinaSchool of PhysicsNankai UniversityTianjin300071ChinahTsung-Dao Lee Institute, Shanghai 200240, ChinaTsung-Dao Lee InstituteShanghai200240ChinaiSchool of Physics, Peking University, Beijing 100871, ChinaSchool of PhysicsPeking UniversityBeijing100871ChinajDepartment of Physics, University of Maryland, College Park, MD 20742, USADepartment of PhysicsUniversity of MarylandCollege ParkMD20742USAkCenter of High Energy Physics, Peking University, Beijing 100871, ChinaCenter of High Energy PhysicsPeking UniversityBeijing100871ChinalSchool of Medical Instrument and Food Engineering, University of Shanghai for Science and Technology, Shanghai 200093, ChinaSchool of Medical Instrument and Food EngineeringUniversity of Shanghai for Science and TechnologyShanghai200093ChinamDepartment of Physics, University of California, Berkeley, CA 94720, USADepartment of PhysicsUniversity of CaliforniaBerkeleyCA94720USAnLawrence Berkeley National Laboratory, Berkeley, CA 94720, USALawrence Berkeley National LaboratoryBerkeleyCA94720USA⁎Corresponding author.⁎⁎Corresponding author at: Department of Physics, University of California, Berkeley, CA 94720, USA.Department of PhysicsUniversity of CaliforniaBerkeleyCA94720USA1Spokesperson of PandaX Collaboration.Editor: M. TroddenAbstractWe present PandaX-II constraints on candidate WIMP-nucleon effective interactions involving the nucleon or WIMP spin, including, in addition to standard axial spin-dependent (SD) scattering, various couplings among vector and axial currents, magnetic and electric dipole moments, and tensor interactions. The data set corresponding to a total exposure of 54-ton-days is reanalyzed to determine constraints as a function of the WIMP mass and isospin coupling. We obtain WIMP-nucleon cross section bounds of 1.6×10−41 cm2 and 9.0×10−42 cm2 (90% c.l.) for neutron-only SD and tensor coupling, respectively, for a mass MWIMP∼40GeV/c2. The SD limits are the best currently available for MWIMP>40GeV/c2. We show that PandaX-II has reached a sensitivity sufficient to probe a variety of other candidate spin-dependent interactions at the weak scale.KeywordsPandaX-II experimentWIMP dark matterSpin-dependent effective interactionsAstrophysical and cosmological observations indicate that a large amount of non-luminous dark matter (DM) exists in our universe, constituting ∼27% of the closure density. However, the exact nature of DM remains a mystery. One intriguing DM candidate, a weakly-interacting massive particle (WIMP), arises naturally in many extensions of the standard model [1,2]. Many WIMP searches have been performed, including direct detection of their scattering off target nuclei, indirect detection of their decay or annihilation, and their production in collider experiments. In the analysis of direct detection experiments, frequently it is assumed that the scattering arises from the light-quark-level (u, s, d) effective interaction(1)L∼GF2∑q[χ¯γμχcqVVq¯γμq+χ¯γμγ5χcqAAq¯γμγ5q] which can be reduced to a nucleon-level operator useful in analyzing the nuclear response to WIMP scattering [3]. Limits on the vector spin-independent (SI) and axial spin-dependent (SD) WIMP-proton and WIMP-neutron cross sections σp,nSI,SD can then be derived. The recent stringent direct detection null results obtained successively by LUX [4,5], PandaX [6,7] and XENON [8–10] have significantly tighten the bounds on σp,nSI,SD [11].The interaction of Eq. (1) was motivated by supersymmetric DM candidates, like the neutralino, that can naturally account for the DM relic density. The motivation to focus exclusively on such candidates has weakened due in particular to collider constraints [12]. An alternative approach, effective field theory (EFT) [13–15], has gained favor because it allows one to do an analysis [16–19] free of theory assumptions. One selects an EFT scale – e.g., the light-quark or a nucleon scale – and constructs a complete basis of effective operators to a given order, taking into account all general symmetries limiting that basis. The underlying UV theory of DM will reduce at that scale to some definite combination of the basis operators, regardless of its nature. Experimentalists can explore the sensitivities of their detectors to the basis operators, to make sure they are probing all possibilities. The EFT approach has shown 1) relative experimental sensitivities depend on the operator choice, and 2) direct detection is potentially more powerful than might appear from SI/SD analyses, as six (not two) independent constraints on DM can be obtained, in principle [15].The PandaX-II detector, located in the China Jinping Underground Laboratory (CJPL), is a dual-phase xenon time-projection chamber with 580 kg of liquid xenon in the sensitive target volume. When the incoming WIMP scatters off a xenon nucleus, both the prompt scintillation photons (S1) in the liquid and the delayed proportional scintillation photons (S2) in the gas are collected by 55 top and 55 bottom Hamamatsu R11410-20 3-inch photomultiplier tubes. The experiment has an accumulated exposure of 54-ton-days [6]. The previously reported analysis for the standard (isoscalar) SI interaction yielded a 90% exclusion limit on σSI of 8.6×10−47 cm2 for a WIMP mass of 40GeV/c2. (These bounds were recently superseded by XENON1T results [10].) In this paper we present PandaX-II constraints a variety of candidate interactions that depend on nucleon or WIMP spin.Spin-dependent interactions other than SD can arise from WIMP magnetic and electric dipole moments, vector-axial interference terms, tensor interactions, etc. While the associated nucleon-level effective operators are conventionally expressed in covariant form, they can be rewritten in terms of the Galilean-invariant EFT basis used here, convenient for nonrelativistic shell model (SM) treatments of the nuclear physics. This basis consists of fourteen operators generated at next-to-next-to-leading-order from the nucleon-WIMP perpendicular relative velocity operator v→⊥, the momentum transfer q→, and the WIMP and nucleon spins, S→χ and S→N [15].We specialize to the scattering of a spin-1/2 WIMPs off a natural xenon target, exploring four dimension-four and three higher dimension effective interactions, selected from Table 1 of Ref. [15]. The operator dimension is defined as 4 + number of powers of mM in the denominator, where mM is a scale that governs the strength of the WIMP and nucleon moments being coupled. The dimension-four operators are the V-A interactionsLint5≡χ¯γμχN¯γμN→O1Lint7≡χ¯γμχN¯γμγ5N→−2O7+2mNmχO9Lint13≡χ¯γμγ5χN¯γμN→2O8+2O9(2)Lint15≡χ¯γμγ5χN¯γμγ5N→−4O4 with mN the nucleon mass and O1=1χ1N, O4=S→χ⋅S→N, O7=S→N⋅v→⊥, O8=S→χ⋅v→⊥, and O9=i(S→χ×S→N)⋅q→mN the nonrelativistic operators of [14,15]. While Lint5 generates the standard SI interaction, the other interactions involve an axial coupling and thus depend on spin.One can equally well start with a basis of light-quark effective operators, reducing these via chiral EFT to their nonrelativistic nucleon equivalents [20,21]. The spin-dependent nucleon-level operators arising from the axial part of Eq. (1) (the standard SD interaction) and from the light-quark tensor interaction will be considered here.The dimension-five operators coupling the WIMP magnetic or electric dipole moments with the nucleon's vector current, and the dimension-six operator coupling WIMP and nucleon magnetic moments, are examples of other potential sources of spin-dependent scattering,Lint9≡χ¯iσμνqνmMχN¯γμN→−q→22mχmMO1+2mNmMO5−2mNmM(q→2mN2O4−O6)Lint17≡iχ¯iσμνqνmMγ5χN¯γμN→2mNmMO11(3)Lint10≡χ¯iσμνqνmMχN¯iσμαqαmMN→4(q→2mM2O4−mN2mM2O6) Here O5=iS→χ⋅(q→mN×v→⊥), O6=(S→χ⋅q→mN)(S→N⋅q→mN), and O11=iS→χ⋅q→mN. The dependence on q→ implies nuclear form factors that peak at larger momentum transfers, influencing experimental strategies for optimally constraining such interactions. We set mM≡mN, normalizing both WIMP and nucleon moments to the nucleon scale.Each operator Linti can have independent couplings to protons and neutrons, or equivalently to isospin [15],(4)di0mV2+di1mV2τ3=dipmV21+τ32+dinmV21−τ32 where τ3 is the Pauli isospin operator. The couplings di are dimensionless, defined relative to the weak scalemV≡〈v〉=(2GF)−12=246.2GeV with 〈v〉 the Higgs vacuum expectation value. We will consider isoscalar (di1=0) and isovector (di0=0) interactions, for which dip=din and −dip=din, respectively; as well as couplings only to protons (di1=di0) or neutrons (di1=−di0). For our higher-dimension operators, the di's also encode information about the absolute size of the WIMP electric and dipole moments, given that we have normalized to nucleonic values (mM≡mN).As the spin response of Xe is largely governed by the unpaired neutrons in 129,131Xe, one expects the 1−τ3 projection of nucleon-spin operators to dominate.The differential cross section for elastic scattering is(5)dσ(v,ER)dER=2mTdσ(v,q→2)dq→2=2mT4πv2[12Jχ+112J+1∑spins|M|2] where the square of the Galilean invariant amplitude M is a product of WIMP and nuclear matrix elements and is a function of initial WIMP velocity v (dimensionless, in units of c) and the three-momentum transfer q→ [15]. Here Jχ is the WIMP spin and J the nuclear ground state angular momentum. In the long wavelength limit the nuclear response functions corresponding to matrix elements of simple operators familiar from weak interactions, such as 1(i), σ→(i), ℓ→(i), and σ→(i)⋅ℓ→(i). The differential event rate with respect to nuclear recoil energy is(6)dRdER=ρχmχ∫dσ(v,ER)dERvf(v→)d3v, where the f(v→) is the normalized velocity distribution of the WIMP particles. We calculate WIMP signal rates by evaluating Eq. (6) for a local WIMP mass density of ρχ=0.3GeV/c2/cm3, assuming a Maxwellian WIMP velocity distribution peaked at v0=220km/s and truncated at the galactic escape velocity vesc=544km/s.The nuclear response functions for DM elastic scattering must be calculated before experimental limits can be converted to bounds on the operator coefficients of Eq. (4). For each contributing Xe isotope and needed operator, we performed full-basis shell-model calculations using the GCN5082 [22] interaction (so named because the SM valence space resides between the shell closures at nucleon numbers 50 and 82). The calculations were done without truncation, using the SM code BIGSTICK to treat bases that ranged to 9 billion Slater determinants [23]. Full GCN5082 Xe isotopes response functions are used in the Mathematica script of [24], an update of [15]. This script and the associated library of one-body nuclear density matrices are available on request from the authors of [24]. The scripts of [24] and [15] were carefully cross-checked against one another, to verify their consistency.Fig. 1 shows computed recoil energy spectra. The upper panels include the coherent isoscalar (N+Z) and isovector (N-Z) SI responses (operator Lint5), which we show for normalization. Though we used SM results, simple phenomenological forms [25] also work well, below the diffraction minimum, as the form factor is governed by its known q=0 value and the nuclear radius.The remaining curves corresponding to interactions with nucleon spin (Lint7), WIMP spin (Lint13), or both (Lint15), at two WIMP masses. All curves correspond to weak-scale interactions: with dip=din≡1 (dip=−din≡1) for isoscalar (isovector) coupling. The lower panels show the corresponding results for the magnetic and electric dipole moment interactions, Lint9, Lint10, and Lint17.The WIMP couplings di are constrained by PandaX-II rate limits. We use data from two low-background physics runs with a total exposure of 54-ton-days, Run 9 with 79.6 live days in 2016 and Run 10 with 77.1 live days in 2017. Calibration data from an AmBe source outside the cryogenic vessel and tritium decays from CH3T injected into the Xe provided tests of the detector response to the nuclear (NR) and electron (ER) recoil events, respectively [6]. A NEST-based Monte Carlo (MC) simulation (Ref. [26] for ER, Ref. [27] for NR) of the data in the (S1, S2) distribution is optimized by adjusting the initial excitation-to-ionization ratio and the recombination fluctuation. A reliable tuned NEST model for PandaX-II is obtained for S1 up to 50 photoelectrons (PEs). The S1 and S2 signal distributions for a given EFT interaction are simulated using the tuned NEST model and PandaX-II detector response parameters [6].Our event selection criteria follow Ref. [6]: S1 from 3 to 45 PEs, S2 from 100 (raw, not corrected for electron lifetime) to 10000 PEs, events lying within the 99.99% NR acceptance, and the total fiducial target of 329±16 kg. The backgrounds in Run 9 and Run 10, estimated in Ref. [6], are dominated by Xe127, tritium, other flat ER background (85Kr, radon and detector gamma background), accidental, and neutron contributions.This search window can include nuclear recoil event energies up to 100keVnr (NR energy) due to the smearing of S1 and S2, although the efficiency drops below 50% above 35keVnr on average. For dimension-four operators, the majority of signal events have nuclear recoil energy below 35 keVnr. The overall signal selection efficiency is between 40% and 50%, very similar to that for the SI analysis in Ref. [6]. For dimension-five or dimension-six operators, the analysis is more complicated due to the sharper form factor momentum dependence. For instance, the signal efficiency for the isovector Lint9 operator decreases from 65% to 6.5% as the WIMP mass increases from 40 to 400 GeV. Thus efficiencies can be improved by adjusting search windows according to operator type and WIMP mass, as LUX has described [28]. Such strategies will be explored in future PandaX analyses: detector calibration studies for S1 above 50 PE will be needed to implement such window adjustments.We constrain the WIMP-nucleon EFT couplings di as a function of the WIMP mass, following the likelihood analysis of Ref. [6]. A standard profile likelihood test statistic was determined as a function of WIMP mass and cross section, and compared with that from a large number of toy MC calculations to derive the upper limits of the signal yields at 90% confidence level (C.L.) [29,30].The upper panel of Fig. 2 gives PandaX-II bounds on the coherent SI interaction Lint5 as well as the spin-spin interaction Lint15, related to the traditional SD interaction discussed below. They are well below the nominal weak scale d∼1 over all or almost all WIMP mass range illustrated. The isoscalar coupling limit |d50|<5.6⋅10−5 at maximum sensitivity (∼ 40 GeV WIMP) corresponds to the PandaX-II cross section bound σp,nSI<8.6⋅10−47 cm2. But limits on the axial (WIMP) – vector (nucleus) coupling d130,1 are also at the weak scale, illustrating the power of current-generation experiments to probe momentum- or velocity-dependent interactions. The lower panel gives the corresponding bounds for interaction involving WIMP magnetic and electric dipole moments. The bounds are near and in one case (the WIMP electric dipole moment coupling to the nucleon vector current Lint17) below the nominal weak scale. Bounds given in the lower panel also include an implicit dimensionless factor representing any needed rescaling of the WIMP moments to their physical values, relative to the nucleon scale we adopted via mM∼mN.An often-used measure of experimental sensitivity to spin-dependent WIMP scattering is provided by the SD axial nucleon-level operator obtained from Eq. (1),(7)OSD≡gA(q2)gA(0)O4−mNgP(q2)2gA(0)O6 with the specific combination of nucleon-level axial and induced pseudoscalar operators dependent on isospin through the CqAA. The pseudoscalar coupling is enhanced in the isovector channel by pion-pole dominance. Comparisons are typically made by selecting proton-only (p) or neutron-only (n) couplings. The nuclear cross section σp,nSD A is related to the nucleon cross section σp,nSD by(8)σp,nSD A(q2)=4π3(2J+1)(μAμp,n)2Sp,nA(q2)σp,nSD where μA (μp,n) is the reduced mass for scattering off the nucleus (nucleon), and Sp,nA(q2) is the nuclear spin structure function that we take from [3], including exchange current corrections. Fig. 3 shows recoil spectra for the SD and tensor cross sections.The 90% C.L. cross section limits are shown in Fig. 4. The optimal bounds, obtained at MWIMP∼40GeV/c2, limit σnSD (neutron-only) and σpSD (proton-only) to 1.6×10−41 cm2 and 4.4×10−40 cm2, respectively. The results modestly improve existing LUX bounds [4] for MWIMP>40GeV/c2.Models of asymmetric dark matter favor Dirac fermion WIMPs, where candidate dimension-4 effective operators include the SD and tensor χ¯σμνχq¯σμνq operators. Constraints from direct detection are particularly competitive for the latter [38]. The tensor interaction generates, after a leading-order chiral reduction [21], the nucleon-level operator 8O4. The dashed curve in the top panel of Fig. 4 shows the neutron-only PandaX-II limits. Bounds on σnT and σpT of 9.0×10−42cm2 and 2.2×10−38cm2, respectively, are found at MWIMP∼40 GeV.In conclusion, we have presented new limits on a candidate spin-dependent WIMP interactions, using PandaX-II Run 9 and Run 10 data with an exposure of 54-ton-days. In addition to the standard SD interaction, we considered vector-axial vector interferences, interactions generated by WIMP magnetic and electric dipole moments, and tensor interactions. We showed that PandaX-II has achieved sufficient sensitivity to probe certain velocity- and momentum-dependent interactions at the weak scale. We obtained the most stringent upper limits to date on σnSD for MWIMP above 40GeV/c2, with a lowest excluded value of 1.6×10−41cm2 at 40 GeV/c2, 90% c.l. The corresponding proton and tensor interaction constraints are σpSD<4.4×10−40cm2, σnT<9.0×10−42cm2, and σpT<2.2×10−38cm2.AcknowledgementsThis project has been supported by a 985-III grant from Shanghai Jiao Tong University, grants from National Science Foundation of China (Nos. 11435008, 11455001, 11505112, 11525522, 11775141 and 11755001), a grant from the Ministry of Science and Technology of China (No. 2016YFA0400301). We thank the Office of Science and Technology, Shanghai Municipal Government (No. 11DZ2260700, No. 16DZ2260200, No. 18JC1410200) and the Key Laboratory for Particle Physics, Astrophysics and Cosmology, Ministry of Education, for important support. This work is supported in part by the Chinese Academy of Sciences Center for Excellence in Particle Physics (CCEPP) and Hongwen Foundation in Hong Kong. WH is supported by the US Department of Energy (DE-SC00046548 and DE-AC02-05CH11231) and the National Science Foundation (PHY-1630782). We would like to thank Dr. Yue-Lin Sming Tsai and Dr. Zuowei Liu for the useful discussions on the EFT models in direct detection experiment. Finally, we thank the CJPL administration and the Yalong River Hydropower Development Company Ltd. for indispensable logistical support and other help.References[1]J.L.FengDark matter candidates from particle physics and methods of detectionAnnu. Rev. Astron. Astrophys.48201049554510.1146/annurev-astro-0082708-101659[2]G.BertoneD.HooperJ.SilkParticle dark matter: evidence, candidates and constraintsPhys. Rep.405200527910.1016/j.physrep.2004.08.031[3]P.KlosJ.MenendezD.GazitA.SchwenkLarge-scale nuclear structure calculations for spin-dependent WIMP scattering with chiral effective field theory currentsPhys. Rev. D88201308351610.1103/PhysRevD.88.083516See alsoJ.EngelS.PittelP.VogelInt. J. Mod. Phys. E119921[4]D.AkeribResults from a search for dark matter in the complete LUX exposurePhys. Rev. Lett.118201702130310.1103/PhysRevLett.118.021303[5]D.S.AkeribLimits on spin-dependent WIMP-nucleon cross section obtained from the complete LUX exposurePhys. Rev. Lett.118201725130210.1103/PhysRevLett.118.251302[6]X.CuiDark matter results from 54-ton-day exposure of PandaX-II experimentPhys. Rev. Lett.119201718130210.1103/PhysRevLett.119.181302[7]C.FuSpin-dependent weakly-interacting-massive-particle–nucleon cross section limits from first data of PandaX-II experimentPhys. Rev. Lett.118201707130110.1103/PhysRevLett.118.071301[8]E.AprileFirst dark matter search results from the XENON1T experimentPhys. Rev. Lett.119201718130110.1103/PhysRevLett.119.181301[9]E.AprileXENON100 dark matter results from a combination of 477 live daysPhys. Rev. D94201612200110.1103/PhysRevD.94.122001[10]E.AprileDark matter search results from a one tonne×year exposure of XENON1TPhys. Rev. Lett.121201811130210.1103/PhysRevLett.121.111302[11]J.LiuX.ChenX.JiCurrent status of direct dark matter detection experimentsNat. Phys.13201721210.1038/NPHYS4039[12]M.E.PeskinSupersymmetric dark matter in the harsh light of the large hadron colliderProc. Natl. Acad. Sci. USA112201512256[13]J.FanM.ReeceL.-T.WangNon-relativistic effective theory of dark matter direct detectionJ. Cosmol. Astropart. Phys.1011201004210.1088/1475-7516/2010/11/042[14]A.L.FitzpatrickW.C.HaxtonE.KatzN.LubbersY.XuThe effective theory of dark matter detectionJ. Cosmol. Astropart. Phys.022013004[15]N.AnandA.L.FitzpatrickW.C.HaxtonWeakly interacting massive particle-nucleus elastic scattering responsePhys. Rev. C89201406550110.1103/PhysRevC.89.065501[16]K.SchneckDark matter effective field theory scattering in direct detection experimentsPhys. Rev. D91201509200410.1103/PhysRevD.91.092004[17]E.AprileEffective field theory search for high-energy nuclear recoils using the XENON100 dark matter detectorPhys. Rev. D96201704200410.1103/PhysRevD.96.042004[18]Z.LiuY.SuY.S.TsaiB.YuQ.YuanA combined analysis of PandaX, LUX and XENON1T experiments within the framework of dark matter effective theoryJ. High Energy Phys.11201702410.1007/JHEP11(2017)024[19]S.KangS.ScopelG.TomarJ.-H.YoonPresent and projected sensitivities of dark matter direct detection experiments to effective WIMP-nucleus couplingsarXiv:1805.06113[20]M.HoeferichterP.KlosA.SchwenkChiral power counting of one- and two-body currents in direct detection of dark matterPhys. Lett. B7462015410[21]F.BisharaJ.BrodB.GrinsteinJ.ZupanFrom quarks to nucleons in dark matter direct detectionJ. High Energy Phys.17112017059[22]J.MenendezA.PovesE.CaurierF.NowackiDisassembling the nuclear matrix elements of the neutrinoless ββ decayNucl. Phys. A818200913910.1016/j.nuclphysa.2008.12.005See alsoL.VietzePhys. Rev. D912015043520for a comparison of GCN5082 Xe isotope spectroscopic predictions to experiment and for full-space calculations of certain isotopes (132Xe, 134Xe, 136Xe) that provide valuable numerical cross checks on present work; in other cases Vietze et al. had to make truncations, which are avoided in the present work[23]C.W.JohnsonCurrent status of very-large-basis Hamiltonian diagonalizations for nuclear physicsarXiv:1809.07869to be published in the Proc. of CIPANP18C.W.JohnsonarXiv:1801.08432[24]A.L.FitzpatrickW.C.HaxtonC.JohnsonK.S.McElvainAnnu. Rev. Nucl. Part. Sci.2019in preparation[25]J.D.LewinP.F.SmithReview of mathematics, numerical factors, and corrections for dark matter experiments based on elastic nuclear recoilAstropart. Phys.619968710.1016/S0927-6505(96)00047-3[26]M.SzydagisA.FyhrieD.ThorngrenM.TripathiEnhancement of NEST capabilities for simulating low-energy recoils in liquid xenonJ. Instrum.82013C1000310.1088/1748-0221/8/10/C10003[27]B.LenardoK.KazkazA.ManalaysayJ.MockM.SzydagisM.TripathiA global analysis of light and charge yields in liquid xenonIEEE Trans. Nucl. Sci.622015338710.1109/TNS.2015.2481322[28]N.Larsenthe LUX CollaborationLux sensitivity to effective field theory interactionsProceedings of CIPANP18CIPANP182018to be published by SLAC eConf[29]A.L.ReadPresentation of search results: the cls techniqueJ. Phys. G282002269310.1088/0954-3899/28/10/313[30]T.JunkConfidence level computation for combining searches with small statisticsNucl. Instrum. Methods Phys. Res., Sect. A, Accel. Spectrom. Detect. Assoc. Equip.434199943510.1016/S0168-9002(99)00498-2[31]M.AaboundSearch for dark matter and other new phenomena in events with an energetic jet and large missing transverse momentum using the ATLAS detectorJ. High Energy Phys.01201812610.1007/JHEP01(2018)126[32]A.M.SirunyanSearch for dark matter produced with an energetic jet or a hadronically decaying W or Z boson at s=13TeVJ. High Energy Phys.07201701410.1007/JHEP07(2017)014[33]C.AmoleImproved dark matter search results from PICO-2L Run 2Phys. Rev. D93201606110110.1103/PhysRevD.93.061101[34]C.AmoleDark matter search results from the PICO-60 CF3I bubble chamberPhys. Rev. D93201605201410.1103/PhysRevD.93.052014[35]C.AmoleDark matter search results from the PICO-60 C3F8 bubble chamberPhys. Rev. Lett.25201725130110.1103/PhysRevLett.118.251301[36]M.G.AartsenImproved limits on dark matter annihilation in the sun with the 79-string icecube detector and implications for supersymmetryJ. Cosmol. Astropart. Phys.04201602210.1088/1475-7516/2016/04/022[37]K.ChoiSearch for neutrinos from annihilation of captured low-mass dark matter particles in the Sun by Super-KamiokandePhys. Rev. Lett.114201514130110.1103/PhysRevLett.114.141301[38]M.A.BuckleyAsymmetric dark matter and effective operatorsPhys. Rev. D84201104351010.1103/PhysRevD.84.043510