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ANAIS-112 Sensitivity in the Search for Dark Matter Annual Modulation

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ANAIS-112 Sensitivity in the Search for Dark Matter Annual Modulation Eur. Phys. J. C (2019) 79:233 https://doi.org/10.1140/epjc/s10052-019-6733-4 Regular Article - Experimental Physics ANAIS-112 sensitivity in the search for dark matter annual modulation I. Coarasa1,2,a ,J.Amaré1,2, S. Cebrián1,2, C. Cuesta1,2,4, E. García1,2, M. Martínez1,2,3,M.A.Oliván1,5, Y. Ortigoza1,2, A. Ortiz de Solórzano1,2, J. Puimedón1,2, A. Salinas1,2, M. L. Sarsa1,2, P. Villar1,2, J. A. Villar1,2 1 Grupo de Física Nuclear y Astropartículas, Universidad de Zaragoza, Calle Pedro Cerbuna 12, 50009 Zaragoza, Spain 2 Laboratorio Subterráneo de Canfranc, Paseo de los Ayerbe s/n, 22880 Canfranc Estación, Huesca, Spain 3 Fundación Agencia Aragonesa para la Investigación y el Desarrollo, ARAID, Avenida de Ranillas 1-D, 50018 Zaragoza, Spain 4 Present Address: Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, CIEMAT, 28040 Madrid, Spain 5 Present Address: Centro de Investigación de Recursos y Consumos Energéticos, CIRCE, 50018 Zaragoza, Spain Received: 5 December 2018 / Accepted: 28 February 2019 © The Author(s) 2019 Abstract The annual modulation measured by the DAMA/ other target materials and techniques (like those from CDMS LIBRA experiment can be explained by the interaction of [11], CRESST [12], EDELWEISS [13], KIMS [14], LUX dark matter WIMPs in NaI(Tl) scintillator detectors. Other [15], PICO [16], XENON [17] or DarkSide [18,19] collab- experiments, with different targets or techniques, exclude the orations) have been ruling out for years the most plausible region of parameters singled out by DAMA/LIBRA, but compatibility scenarios. Nevertheless, DAMA/LIBRA has the comparison of their results relies on several hypothe- accumulated up to now twenty annual cycles in the [2,6] ses regarding the dark matter model. ANAIS-112 is a dark keVee energy region (keVee for keV electron-equivalent) matter search with 112.5 kg of NaI(Tl) scintillators at with 12.8σ statistical significance (phase and period fixed) the Canfranc Underground Laboratory (LSC) to test the [3–5]. Moreover, DAMA/LIBRA-phase2 has been able to DAMA/LIBRA result in a model independent way. We ana- accumulate six annual cycles in the [1,6] keVee energy region lyze its prospects in terms of the aprioricritical and detection with 9.5σ statistical significance because all the photomul- limits of the experiment. A simple figure of merit has been tipliers (PMTs) were replaced by a second generation PMTs obtained to compare the different experiments looking for Hamamatsu R6233MOD, with higher quantum efficiency the annual modulation observed by DAMA/LIBRA. We and with lower background with respect to those used in conclude that after 5 years of measurement, ANAIS-112 can phase1 [5]. detect the annual modulation in the 3σ region compatible The WIMP interaction counting rate experiences an with the DAMA/LIBRA result. annual modulation as the result of the motion of the Earth around the Sun that can be approximated [20,21] by: − 1 Introduction dR t t0 (E R, t) ≈ S0 (E R) + Sm (E R) · cos 2π · , dER T The ANAIS experiment [1,2] is intended to search for dark (1) matter annual modulation with ultrapure NaI(Tl) scintillators at the Canfranc Underground Laboratory (LSC) in Spain, in where R is the interaction rate, E R is the recoil energy, t0 order to provide a model independent confirmation of the is the expected time of the maximum (or minimum, depend- signal reported by the DAMA/LIBRA collaboration [3–5] ing on the sign of Sm), 152.5 days after 1st January, and using the same target and technique. Projects like DM–Ice T is the expected period of one year. The time-averaged [6], COSINE-100 [7,8], SABRE [9] and PICO–LON [10] differential rate is denoted by S0, whereas the modulation also envisage the use of large masses of NaI(Tl) for dark amplitude is given by Sm [21]. The value of Sm measured . ± . ± . matter searches. Results obtained by other experiments with by DAMA/LIBRA is 0 0102 0 0008 and 0 0105 0 0011 cpd/kg/keVee within [2,6] and [1,6] keVee intervals, respec- J.A. Villar: Deceased. tively (cpd stands for counts per day)[5]. In this paper, we analyze the ANAIS-112 prospects in a e-mail: [email protected] terms of the aprioricritical and detection limits of the exper- 0123456789().: V,-vol 123 233 Page 2 of 8 Eur. Phys. J. C (2019) 79:233 iment and a simple figure of merit has been obtained to com- 1 pare the different experiments looking for the annual modula- detector 0 tion observed by DAMA/LIBRA. The structure of the paper 0.8 is as follows: Sect. 2 describes the ANAIS-112 experimental detector 1 detector 2 layout; Sect. 3 focuses on the procedure to search for a mod- 0.6 detector 3 ulation signal in the [2,6] keVee energy region, considering detector 4 a single energy bin and afterwards the energy binning and Efficiency 0.4 detector 5 segmented detector in nine modules; Sect. 4 focuses on the detector 6 [1,6] keV energy region in view of the last DAMA/LIBRA- 0.2 ee detector 7 phase2 results. Finally, conclusions are presented in Sect. 5. detector 8 0 123456 Energy (keVee) 2 The ANAIS-112 experiment Fig. 1 Total efficiency for every ANAIS-112 detector ANAIS-112 consists of nine modules made by Alpha Spectra (AS), Inc. Colorado and then shipped to Spain along several system) has been also considered [2]. The total efficiency years, arriving at LSC the first of them at the end of 2012 and for the selection of dark matter compatible events in every the last by March, 2017. Each crystal is cylindrical (4.75 ANAIS-112 detector is shown in Fig. 1. diameter and 11.75 length), with a mass of 12.5 kg. NaI(Tl) ANAIS-112 dark matter run started on August 3, 2017. crystals were grown from selected ultrapure NaI powder and The first year of data taking finished on July 31, 2018, having housed in OFE (Oxygen Free Electronic) copper; the encap- accumulated 341.72 days of live time. The low energy data sulation has a mylar window allowing low energy calibra- is blinded except for the multiplicity 2 events that we use to tion. Two Hamamatsu R12669SEL2 PMTs were coupled test the analysis procedures. On the other hand, ∼10% of the through quartz windows to each crystal at LSC clean room. first year of data has been unblinded for background assess- All PMTs have been screened for radiopurity using germa- ment. To do this, one-day time bins have been selected ran- nium detectors in Canfranc. The shielding for the experi- domly distributed throughout the whole year. The low energy ment consists of 10 cm of archaeological lead, 20 cm of low spectra corresponding to the unblinded data for each of the activity lead, 40 cm of neutron moderator, an anti-radon box detectors in anticoincidence (single hit events) after event (continuously flushed with radon-free nitrogen) and an active selection and efficiency correction are shown in Fig. 2.We muon veto system made up of plastic scintillators designed also display in Fig. 3 the total anticoincidence background to cover top and sides of the whole ANAIS set-up. The hut (adding up all 9 detectors) below 10 keVee for the unblinded housing the experiment is at the hall B of LSC under 2450 data. m.w.e. At the region of interest, crystal bulk contamination is the The light output measured for all AS modules is at the level dominant background source. Contributions from 40K, 210Pb 22 3 of ∼ 15 phe/keVee [2], which is 1.5 times larger than that (powder/crystal growing contaminants), Na and H (cos- determined for the best DAMA/LIBRA detectors [5]. This mogenics) are the most relevant [22,23]. In almost all detec- 40 high light collection, possible thanks to the excellent crystal tors the K peak at 3.2 keVee is clearly visible. The back- quality and the use of high quantum efficiency PMTs, has a ground level at 2 keVee ranges from 2 to 5 cpd/kg/keVee, direct impact in energy threshold. Triggering below 1 keVee depending on the detector, and then increases up to 5–8 is confirmed by the identification of bulk 22Na and 40K events cpd/kg/keVee at 1 keVee. A detailed analysis of the back- at 0.9 and 3.2 keVee, respectively, thanks to coincidences ground contributions can be found in [23]. with the corresponding high energy photons following the electron capture decays to excited levels [2]. To remove the PMT origin events, dominating the back- 3 Searching for a modulation signal in the [2,6] keVee ground below 10 keVee, and then reach the 1 keVee threshold, energy interval specific filtering protocols for ANAIS-112 detectors have been designed. Multiparametric cuts based on the number A model independent way to check the DAMA/LIBRA result of photoelectrons in the pulses, the temporal parameters of is looking for a signal not only with the same target and the pulses and the asymmetry in light sharing between PMTs technique but also in the same region where DAMA/LIBRA are considered, and the corresponding acceptance efficien- finds it. First, we search for a modulation in the rate in a cies for such filters have been calculated. The trigger effi- model independent way, i.e. without assumptions about the ciency (probability that an event is triggered by the DAQ origin and characteristics of the signal other than the one- 123 Eur. Phys. J. C (2019) 79:233 Page 3 of 8 233 14 14 14 12 12 12 10 10 10 8 8 8 6 6 6 4 4 4 2 2 2 det 2 (cpd/kg/keVee) 2 det det 0 (cpd/kg/keVee) 0 det 0 (cpd/kg/keVee) 1 det 0 0 12345678910 12345678910 12345678910 Energy (keVee) Energy (keVee) Energy (keVee) 14 14 14 12 12 12 10 10 10 8 8 8 6 6 6 4 4 4 2 2 2 det 3 (cpd/kg/keVee) 3 det 0 (cpd/kg/keVee) 4 det 0 (cpd/kg/keVee) 5 det 0 12345678910 12345678910 12345678910 Energy (keVee) Energy (keVee) Energy (keVee) 14 14 14 12 12 12 10 10 10 8 8 8 6 6 6 4 4 4 2 2 2 det 6 (cpd/kg/keVee) 6 det 0 (cpd/kg/keVee) 7 det 0 (cpd/kg/keVee) 8 det 0 12345678910 12345678910 12345678910 Energy (keVee) Energy (keVee) Energy (keVee) Fig.
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