Constraints on spin-independent nucleus scattering with sub-GeV WIMP dark matter from the CDEX-1 B Experiment at CJPL

Z. Z. Liu, Q. Yue, ∗ L. T. Yang, † K. J. Kang, Y. J. Li, H. T. Wong, ‡ M. Agartioglu, 4, ‡ H. P. An, 5 J. P. Chang, J. H. Chen, ‡ Y. H. Chen, J. P. Cheng, 2 Z. Deng, Q. Du, H. Gong, X. Y. Guo, L. He, S. M. He, J. W. Hu, Q. D. Hu, H. X. Huang, L. P. Jia, H. Jiang, H. B. Li, ‡ H. Li, J. M. Li, J. Li, X. Li, X. Q. Li, Y. L. Li, B. Liao, F. K. Lin, ‡ S. T. Lin, S. K. Liu, Y. D. Liu, Y. Y. Liu, H. Ma, § J. L. Ma, 5 J. H. Ning, H. Pan, N. C. Qi, J. Ren, X. C. Ruan, 4 V. Sharma, 11, ‡ Z. She, L. Singh, 11, ‡ M. K. Singh, 11, ‡ T. X. Sun, C. J. Tang, W. Y. Tang, Y. Tian, G. F. Wang, L. Wang, Q. Wang, 5 Y. Wang, 5 S. Y. Wu, Y. C. Wu, H. Y. Xing, Y. Xu, T. Xue, 5 N. Yi, C. X. Yu, H. J. Yu, J. F. Yue, M. Zeng, Z. Zeng, F. S. Zhang, M. G. Zhao, J. F. Zhou, Z. Y. Zhou, and J. J. Zhu (CDEX Collaboration) Key Laboratory of Particle and Radiation Imaging (Ministry of Education) and Department of Engineering Physics, Tsinghua University, Beijing 100084 College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875 Institute of Physics, Academia Sinica, Taipei 11529 Department of Physics, Dokuz Eylül University, İzmir 35160 Department of Physics, Tsinghua University, Beijing 100084 NUCTECH Company, Beijing 100084 YaLong River Hydropower Development Company, Chengdu 610051 College of Physical Science and Technology, Sichuan University, Chengdu 610065 Department of Nuclear Physics, China Institute of Atomic Energy, Beijing 102413 School of Physics, Nankai University, Tianjin 300071 Department of Physics, Banaras Hindu University, Varanasi 221005 Department of Physics, Beijing Normal University, Beijing 100875 (Dated: May 2, 2019)

Introduction. Weakly interacting massive particles (WIMPs, denoted as χ) are the most popular candidates of dark matter, the searches of which are of intense experimental interest [1]. Direct detection experiments such as XENON [2], LUX [3], PandaX [4], CDMSlite [5], DarkSide [6], CDEX [7][8][9][10][11][12] are based on WIMP-nucleus (χ-N) elastic scatterings through spin-independent (SI) and spin-dependent (SD) interactions. However, the nuclear recoil energy and hence the experimental observable rapidly diminishes with decreasing m χ . Detectors with low threshold have to be used to study these light WIMPs. At the lowest achieved threshold of 30.1 eV in nuclear recoil energy, the CRESST [13] experiment extends the reach of m χ to below 0.16 GeV/c 2 , using the conventional χ-N scattering detection channel.
It is recently pointed out that finite amount of electrons or photons are produced in χ-N scattering [14][15][16][17]. Two of the mechanisms that produce electro-magnetic final states in χ-N scatterings are Migdal effect [15,16] and bremsstrahlung emissions [17]. The observable signals due to electron recoils or gamma rays are much larger than those of nuclear recoils at m χ less than several few GeV. Taking these two effects into account, the lower reach of m χ in direct detection experiments can be substantially extended to domains far below 1 GeV/c 2 . P-type point contact germanium (PPCGe) detectors have been adopted by CDEX [7][8][9][10][11][12] in light WIMP searches, exploiting their good energy resolution and ultra-low energy threshold. Located in the China Jinping Underground Laboratory (CJPL) [18], CDEX-1B experiment [11] has for its target a single-element PPCGe detector cooled by a cold finger, with an active mass of 939 g. A NaI(Tl) anti-Compton detector is used as active shielding. The detector has been under stable data taking conditions since March 27, 2014 and limits on χ-N SI-scattering down to m χ ∼2 GeV/c 2 are derived at an energy threshold of 160 eVee ("eVee" represents the electron equivalent energy) with an exposure of 737.1 kg·day [11]. In this letter, taking Migdal effect and bremsstrahlung emissions into account, the CDEX-1B data is re-analyzed to derive new limits on χ-N SIinteractions, cross-section of which denoted by σ SI χN .
Migdal effect and bremsstrahlung emissions. The conventional and simplified treatment of χ-N scattering is that all the kinetic energy is transferred from χ to nuclear recoil via elastic scattering. Complexities arise in real physical systems, since the target nuclei in detectors, being part of the atoms, are coupled also to the electrons. There is finite probability that high-energy electrons are ejected via inelastic processes. The electrons do not follow the motion of the nuclei such that the ionization characteristics to the target medium from the electron recoils are different from those of nuclear recoils where the ionization energy is quenched due to recombinations. The process, called Migdal effect [19][20][21] were recently studied in the context of WIMP detection via χ-N interactions [15,16]. The probability of having two or more electrons ionized or excited in an interaction is much smaller than those with only one electron. Therefore, only single electron excitation and ionization is considered. The total transition rates are the summation of ionization and excitation probabilities and the probability for the recoil atoms to remain in ground state, which is given by Eq. (4.12) in Ref. [15]. According to Ref. [15], the excitation probability is much smaller than ionization probability, especially for inner shell electron, so the excitation is also neglected.
After an electron is ejected via ionization, the ionized atom will de-excite and emit new electrons or photons, whose total energy is the binding energy, denoted as E nl . The total electronic energy, distinctive from the nuclear recoil energy, is given by E EM = E e + E nl , where E e is the kinetic energy of electron after ionization, while the cross section is given by where E R is the nuclear recoil energy, q e is equal to m e q A /m A , m A is the atomic mass approximated to target nucleus mass, and q A is equal to √ 2m A E R , n and l are the principal quantum number and orbital quantum number, respectively.
The maximum energy of electronic energy E EM,max is equal to 1/2µ N v 2 , µ N is the reduced mass, v is the relative velocity between χ and the target nucleus, while the maximum energy of nuclear recoil E R,max is equal to For example, while m χ = 0.05 GeV/c 2 and m N = 67.66 GeV/c 2 (the nucleus mass of Ge), for v max =776 km/s, the resulting E EM,max ≈ 167 eV and E R,max ≈ 1 eV.
As the nucleus acquires kinetic energy from χ-N scattering, the accompanying ejected electron will get accelerated in order to follow the nuclear recoil trajectory, resulting with a finite probability that a photon will be emitted through bremsstrahlung. According to Ref. [17], the photo-emission cross section (σ) is given by where E γ is the energy of photon, α is the fine structure constant, m N is the mass of target nucleus, is the atomic scattering factors documented at the NIST Standard Reference Database [22], and Θ refers to the truncation function.
The χ-N event rates due to both Migdal effect and bremsstrahlung emissions can be expressed as: where N T is the number of target nuclei per unit detector, E x refers to E γ or E EM , ρ χ is the density of dark matter, m χ is the mass of DM particle, v E is Earth's velocity relative Galaxy.
As the CDEX PPCGe detectors do not discriminate nuclear recoils from electron recoils, the observable signals are the summation of nuclear recoil energy and electron recoil energy, denoted as E det = E x +Q nr E R , where Q nr is the quenching factor [23]. In this letter, the Lindhard formula [24] is adopted for the evaluation of Q nr . There is no experiment data for Q nr of Ge below 0.2 keVnr, so the κ value (κ=0.22) in Lindhard formula is derived by fitting of experiment data [25][26][27] under 2 keVnr with a conservative uncertainty of 30% adopted as systematic error. Time-integrated (TI) analysis. The expected energy spectrum of χ-N SI scattering is shown in Fig. 1, where the target nucleus is Ge, m χ = 1 GeV/c 2 , and σ SI χN = 10 −36 cm 2 . The standard WIMP galactic halo assumption and conventional astrophysical models [28] are used, with χ-density ρ χ set to 0.3 GeV/(c 2 cm 3 ), Earth's velocity v E at 232 km/s, χ-velocity distribution assumed to be Maxwellian with the most probable velocity v 0 = 220 km/s, the local Galactic escape velocity at 544 km/s, and the Helm form factor [29,30] is adopted. Smearing due to energy resolution is taken into account in later analysis. Only the ionization spectra from L and M shell (n = 2,3) are considered, while those of K-shell are negligible, and those of the valence electrons (N shell, n=4) are not reliable.
Using Fig. 1 as illustration, the expected rates in complete energy range for χ-N elastic SI-scattering, Migdal effects and bremsstrahlung emissions at m χ =1 GeV/c 2 are in ratio of about 8 × 10 8 : 2 × 10 4 : 1. However, at a threshold of 160 eVee where the χ-N elastic scatterings are no longer observable, the Midgal effect and bremsstrahlung processes can still produce signals above threshold and therefore open the sensitivity windows to lower m χ . Upper limits at 90% confidence level (C.L.) in σ SI χN are derived by Binned Poisson method [35] with the CDEX-1B TI-data [11]. The exclusion curve is shown in Fig. 2, in which several other experiments are superimposed for reference. The sensitivity to σ SI χN contributed by Migdal effect dominates over that by bremsstrahlung emissions by four to five order of magnitude. New limits are achieved for m χ < 0.18 GeV/c 2 , and the lower reach is extended to 0.05 GeV/c 2 . Annual modulation (AM) analysis. Positive observations of AM would provide smoking-gun signatures for WIMPs independent of the astrophysics and background models. The Earth's velocity relative to the galactic WIMP-halo is time-varying with a period of one year, and can be expressed as v E = 232 + 30 × 0.51 cos(2π/T × (t − Φ), where T is set to be 365.25 days, Φ is set to be 152.5 days from January 1 st [36]. The expected measurable spectra at different time of the year are shown in Fig. 3 (a). The AM-amplitudes (summer-winter differece in the spectra) at different m χ are depicted in Fig. 3 (b). It can be seen that the AM-amplitudes from Migdal effect or bremsstrahlung are both enhanced at lower m χ . Consequently, the AM analysis might provide more sensitive probes at low m χ than TI analysis at the same energy threshold.
We adopt in this AM analysis the same data as previously used to study AM effects in the conventional χ-N nuclear recoil channel [37]. There are two datasets, Run-1 with the the NaI(Tl) anti-Compton detector, and Run-2 without NaI(Tl), having 751.3 and 428.1 live days, respectively, and together spanning a total of 1527 calendar days (∼4.2 yr) and a total exposure of 1107.5 kg·day. The background stability and environment parameters have been checked, and the time stability of the candidate χ-N event rates at different energy ranges were demonstrated with Fig. 1 of Ref. [37]. The Model-Dependent AM analysis [37] is adopted in this analysis. The AM-amplitudes (A ik of the i th energy-bin of the k th Run) are related and constrained by a known function (f ) of m χ and σ SI χN , , where E ik and δE ik are the mean energy and its corresponding binsize, respectively. The same analysis threshold of 250 eVee and χ 2 minimization procedures are adopted [37]. Fig. 4 are the 90% C.L. limits from AM analysis with Migdal effects and bremsstrahlung emissions. The only previous AM analysis on bremsstrahlung emissions was performed by XMASS-I [38] where threshold is higher (1 keVee). Its limits are also displayed. Superimposed for comparison are the AM nuclear recoils bounds from CDEX-1B [37] and XMASS-I [38], as well as the AM-allowed regions of CoGeNT [39,40] and DAMA/LIBRA [21,35,41,42]. The lower reach light WIMPs is extended to 0.075 GeV/c 2 .

Depicted in
Summary. In this letter, we incorporate two newly identified mechanisms on χ-N SI-interactions to the analysis of CDEX-1B data. New m χ windows are opened and new limits are derived. The Migdal effect has stronger impact than bremsstrahlung emissions and provides much more stringent bounds in both TI and AM analysis. The exclusion region in m χ can be extended 0.05 GeV/c 2 with an energy threshold of 160 eVee in the TI analysis. The best sensitivity in σ SI χN is achieved for m χ ∼(0.05−0.18) GeV/c 2 via the Migdal effect. About 4.2 years time-span of CDEX-1B data are used in the AM analysis. At an energy threshold of 250 eVee, the best sensitivity of σ SI χN for m χ < 3.0 GeV/c 2 via the Migdal effect is achieved, extending to 0.075 GeV/c 2 .  [37]. The energy threshold of the modulated analysis is 250 eVee, while the reach of the exclusion line (red line and blue line) is extended to 0.075 GeV/c 2 . The nuclear-recoil only limits from the same data set is superimpsed [37]. Constraints [38] and allowed regions [21,35,[39][40][41][42] from AM analysis from other experiment are also shown.