Search for Light Weakly-Interacting-Massive-Particle Dark Matter by Annual Modulation Analysis with a Point-Contact Germanium Detector at the China Jinping Underground Laboratory

We present results on light weakly interacting massive particle (WIMP) searches with annual modulation (AM) analysis on data from a 1-kg mass $p$-type point-contact germanium detector of the CDEX-1B experiment at the China Jinping Underground Laboratory. Datasets with a total live time of 3.2 yr within a 4.2 yr span are analyzed with analysis threshold of 250 eVee. Limits on WIMP-nucleus (${\chi}$-$N$) spin-independent cross sections as function of WIMP mass ($m_{\chi}$) at 90\% confidence level (C.L.) are derived using the dark matter halo model. Within the context of the standard halo model, the 90\% C.L. allowed regions implied by the DAMA/LIBRA and CoGeNT AM-based analysis are excluded at $>$99.99\% and 98\% C.L., respectively. These results correspond to the best sensitivity at $m_{\chi}$$<$6$~{\rm GeV}/c^2$ among WIMP AM measurements to date.

We present results on light weakly interacting massive particle (WIMP) searches with annual modulation (AM) analysis on data from a 1-kg mass p-type point-contact germanium detector of the CDEX-1B experiment at the China Jinping Underground Laboratory. Datasets with a total live time of 3.2 yr within a 4.2 yr span are analyzed with analysis threshold of 250 eVee. Limits on WIMP-nucleus (χ-N ) spin-independent cross sections as function of WIMP mass (mχ) at 90% confidence level (C.L.) are derived using the dark matter halo model. Within the context of the standard halo model, the 90% C.L. allowed regions implied by the DAMA/LIBRA and CoGeNT AM-based analysis are excluded at >99.99% and 98% C.L., respectively. These results correspond to the best sensitivity at mχ<6 GeV/c 2 among WIMP AM measurements to date. PACS numbers: 95. 35.+d, 98.70.Vc Compelling cosmological evidence indicates that about one-quarter of the energy density of the Universe manifests as dark matter [1], a favored candidate of which is the weakly interacting massive particle (WIMP, denoted as χ). In direct laboratory searches of WIMPs conducted with WIMP-nucleus (χ-N ) elastic scattering, positive evidence of WIMPs can only be established by assuming detailed knowledge of the background. The annual modulation (AM) analysis, on the other hand, only requires the background at the relevant energy range is stable with time. It can provide smoking-gun signatures for WIMPs independent of background modeling. Within the astrophysical dark matter halo model [2], the expected χ-N rates have distinctive AM features with maximum intensity in June and a period of 1 yr due to the Earth's motion relative to the galaxy dark matter distribution.
Positive results were concluded at significance of 12.9 σ and 2.2 σ from AM-based analysis of DAMA/LIBRA [3][4][5] and CoGeNT [6][7][8] experiments, respectively. However, these interpretations are challenged by integrated rate experiments with liquid xenon [9][10][11], cryogenic bolometer [12][13][14] and ionization germanium [15][16][17][18][19] detectors, when the data were analyzed in certain scenarios where the dark matter particle properties and distributions in the Milky Way's halo are precisely defined. Comparison of AM data with differnet targets is also model dependent. The AM-allowed regions of DAMA/LIBRA and CoGeNT have been probed and excluded by AM analysis from the XMASS-1 experiment [20,21], which is limited by the diminishing sensitivities of the liquid xenon techniques at light WIMP masses (m χ ) below 6 GeV/c 2 . The ANAIS-112 [22] and COSINE-100 [23] experiments aim to resolve this tension by a model-independent test of DAMA/LIBRA's obser-arXiv:1904.12889v2 [hep-ex] 26 Nov 2019 vation using identical detector target materials. Their latest results are consistent with both the null hypothesis and DAMA/LIBRA's 2−6 keV best-fit value, but at poor confidence levels due to the limited 1.5 yr and 1.7 yr data. The CDEX experiment, located in the China Jinping Underground Laboratory (CJPL) with about 2400 m of rock overburden [24], utilizes p-type point contact germanium detectors (PPCGe) [25][26][27] for dark matter direct detection. The low analysis threshold of about 200 eVee ("eVee" represents electron equivalent energy derived from calibrations with known cosmogenic x-ray peaks) [15][16][17][18][19] implies AM studies with germanium can complement the liquid xenon results. It provides an alternative probe to the allowed parameter space of DAMA/LIBRA [3,4] (with model dependence due to different target isotopes) and CoGeNT [8] (with a model-independent comparison, since both use germanium as target) and extends the reach of AM test to lower m χ .
The CDEX-1B experiment is the second phase of the CDEX experiment and has previously set upper limits for spin-independent (SI) and spin-dependent cross sections by the χ-N recoil spectral analysis [18]. The PPCGe target of mass 1 kg (fiducial mass of 939 g, after corrections due to a 0.88±0.12 mm surface layer) was shielded, from inside out, with 20 cm of copper, 20 cm of borated polyethylene and 20 cm of lead. The whole setup was assembled inside a 6 m (H)×8 m (L)×4 m (W ) polyethylene room with wall thickness of 1 m. The target was enclosed by an NaI(Tl) anti-Compton detector from September 27, 2014 to August 2, 2017 (Run 1), and subsequently without NaI(Tl) (replaced by passive copper shielding) from August 4, 2017 till December 2, 2018 (Run 2). The gaps from December 27, 2014 to March 8, 2015 and from March 16, 2016 to June 2, 2016 were due to calibration with neutron and gammaray sources, respectively. The two runs have 751.3 and 428.1 live days, respectively, and together span a total of 1527 calendar days (∼4.2 yr), with the total exposure of 1107.5 kg d. The Run 1 events were further categorized by AC −(+) corresponding to those without(with) coincidence of NaI(Tl) signals. Candidate χ-N events were therefore AC − in Run 1 and all triggered ones in Run 2, which will also be denoted with AC − in the following text for convenient purpose. The energy calibration during the running period was achieved using the low energy internal x-rays from the cosmogenic nuclides inside the germanium crystal, also showing good stabilities. The nuclear recoil spectral analysis of Run 1 [18] achieved an analysis threshold of 160 eVee, limited by the pedestal of the electronic noise. For AM analysis, good stability of contaminations due to electronic noise is required. Accordingly, a conservative analysis threshold of 250 eVee away from the pedestal noise edge is adopted, such that both the physics event selection efficiency and trigger efficiency are 100%.
At the keVee energy range relevant to this analysis, background events are dominated by Compton scattering of high energy gamma rays and by internal radioactivity from cosmogenic long-lived isotopes, the time variations of which have to be checked and accounted for. The time evolutions of radon contamination show good stabilities by the combined intensities of several radon-related γ lines (295.2 and 351.9 keV from 214 Pb, the daughter of 222 Rn). The stabilities of the relevant background at the low energy are demonstrated in Fig. 1(a), with the count rates at 20−40 and 2.0−4.0 keVee both for AC − and AC + . Time is denoted as the number of days since January 1, 2014. It can be seen from the displayed χ 2 /d.o.f.(degrees of freedom) and p values that the low energy background count rates are stable within the data taking periods.
The 4.2 yr of CDEX-1B data are separated into 35 subdatasets in different time bins, each with about 1 month of live time. WIMP candidate events in the bulk of the detector are selected [18] via some basic cuts and the bulk or surface (B/S) events discrimination. The B/S correction procedure is done by likelihood fitting of the bulk or surface rise-time distribution probability density functions (PDFs) and has no cut efficiency associated, as described in details in Refs. [18,28]. During the B/S procedure, each subdataset was treated independently with its distinct calibration parameters. The inputs of B/S procedure include (i) AC − events in corresponding subdataset; (ii) summation of AC − in the rest of subdatasets; (iii) all AC + in Run 1; and (iv) three calibration samples ( 60 Co, 137 Cs, 241 Am), while 241 Am is a pure surface source and can supply the constrain to surface PDFs. Systematic uncertainties related to the B/S correction are adopted from Ref. [18] and are combined quadratically. The B/S corrections are stable within data taking periods, as checked by the stability of a few control parameters such as rise-time PDFs of background data, the counts of AC + bulk and AC − surface events.
The only requirement for AM analysis is to have stable background with time. The modeling of their origins and spectral shapes, which are sources of uncertainties in the time-integrated spectral analysis, is not involved. Stability of χ-N candidate events with time is further demonstrated in Fig. 1(b) with the bulk event count rates after B/S correction at three energy ranges which are most relevant to the sensitivities at m χ ∼8 GeV/c 2 . The data at low energies show slight time-dependent features. However, those features are not universal to all energy ranges. Based on the physical understanding on the background components, we adopted a scenario of the time-independent background contribution plus an exponentially time-dependent background contribution from the L-shell x rays from cosmogenic isotopes, which is not fitted, but derived from the corresponding K-shell lines intensities behavior. The expected time dependence due to the cosmogenic origin background contributions The B/S corrected bulk event counts versus time at three energy ranges which are most relevant to the sensitivities at mχ∼8 GeV/c 2 , with the overall χ 2 /d.o.f. of 35.5/60 for Run 1 and 24.6/39 for Run 2 in these energy ranges. The uncertainties in these energies are dominated by the systematic uncertainties from B/S correction, in which overestimated upper bound was used [18]. A bin size of 200 eVee is used in this plot, while different bin size is adopted in the analysis.
was observed. It dominated the background in energy ranges of 1.0−1.4 keVee, especially in Run 1. The timeindependent background levels of every energy bin were taken as free parameters and were uncorrelated between Run 1 and Run 2 due to the different shielding configurations. The unmodulated χ-N rates were treated as a component of the constant background in AM analysis. Data at 0.25−5.8 keVee were analyzed, below the region of internal K-shell x rays. The selected energy bin sizes are 50, 100, and 200 eVee for measured energy at <0.8, 0.8−1.6, and >1.8 keVee, respectively, according to the requirements of statistical accuracy in B/S correction. The corrected counts of bulk events are denoted by n ijk corresponding to the respective bin with i, j, k = (energy, time, run). There are in total i = 1 − 40 energy bins, with 35 time bins divided into k = 1 − 2 runs (j = 1 − 21 time bins for k = 1, j = 1 − 14 time bins for k = 2) in this analysis. For each of the ith energy bin, a minimum χ 2 analysis was performed simultaneously, with where φ and T are, respectively, the modulation phase and period. The period is fixed at 365.25 d (one yr) for all scenarios, whereas the phase is either taken as free parameter or fixed at 152.5 d as expected from the standard halo model. P ijk is the time-varying background contributions of the L-shell x rays from cosmogenic longlived isotopes such as 68 Ge, 68 Ga and 65 Zn, the intensities of which are fixed by the measured K shell x rays at 8.5−10.8 keV, B ik is the background level, in which we adopted a time-independent background scenario, and ∆ ijk 2 are the combined statistical and systematic errors dominated by the B/S correction [18]. The modulation amplitude A i is fixed to 0 for the null hypothesis and left unconstrained (positive or negative) for the modulation hypothesis. Summation is performed over all of the jth time bins each at median time t j and the kth run.
The data are first studied with a model-independent analysis without invoking astrophysical models and parameters, i.e., model independently, with the phase φ For the model-dependent analysis, the individual A i are correlated with a known function (f ) of m χ and χ-N cross section, while the function is related to the applied astrophysics models. The data are then analyzed under the standard spherical isothermal galactic halo model [2,30], with a most probable speed of υ 0 = 220 km/s, a galactic escape velocity of υ esc = 544 km/s [31], an Earth's velocity related to dark matter of υ E = {232 + 15cos 2π(t − φ)/T } km/s and local dark matter density of 0.3 GeV/(c 2 cm 3 ) [32,33]. The period and phase are fixed at 365.25 and 152.5 d, respectively. Quenching factor of Ge is derived by the TRIM software package [27,34,35] with a 10% systematic error adopted for the analysis [17]. Possible dark matter contributions which are not time varying are incorporated as part of B ik . The AM amplitudes A i are calculated by integration of f with mean energy of the bin E i and bin size δE i , that is, where σ SI denotes SI χ-N cross section as function of m χ . Best-fit values of σ SI are then evaluated by minimizing χ 2 i of Eq. (1). The unified approach [36] is then used to place the upper bounds of positive definite σ SI at different m χ .
tively. The DAMA/LIBRA high-m χ region (I-recoil) is not probed in this analysis.
Systematic uncertainties on time-dependent background assumption are assessed by replacing constant backgrounds with linear functions, resulting in at most 3.4% deviation of the upper bound and best fit of σ SI for m χ ranging from 2 to 20 GeV. The B/S discrimination contributes less than 8% deviation of σ SI and the uncertainty of K/L ratios [39] is also incorporated in the systematic uncertainty budget.
The analysis is extended by taking the modulation phase φ as a free parameter, and the exclusion contours of the best-fit results on σ SI at m χ =7.9 GeV/c 2 are depicted in Fig. 4, superimposed with the best-fit result from CoGeNT [7,8] at the same m χ and the phase in halo model. The data exclude CoGeNT's 90% C.L. allowed region at its best-fit phase of 102 ± 47 d [8] and the halo model at fixed φ at 93% and 98% C.L., respectively. The analysis at m χ in the range 3.2−17 GeV/c 2 indicates that the data are consistent with the null hypothesis within 1-σ (p value>0.32) at the entire φ range of φ from 0 to 2π.
The CDEX-1B experiment provided unique low threshold (250 eVee) and stable (3. data for sensitive AM analysis results without energydependent background model assumptions. The CDEX dark matter program continues taking data at CJPL, expanding to use Ge-detector arrays immersed in liquid nitrogen acting as cryogenic coolant and shield against ambient radioactivity [19]. R&D efforts on the Ge-detector fabrication, and further radiation background reduction, are being pursued. Scaled-up experiment toward target mass of 100 kg is being prepared at CJPL-II [24].