Understanding internal backgrounds in NaI(Tl) crystals toward a 200 kg array for the KIMS-NaI experiment

Abstract

(ProQuest: ... denotes formulae and/or non-USASCII text omitted; see image)

The Korea Invisible Mass Search (KIMS) collaboration has developed low-background NaI(Tl) crystals that are suitable for the direct detection of WIMP dark matter. Building on experience accumulated during the KIMS-CsI programs, the KIMS-NaI experiment will consist of a 200 kg NaI(Tl) crystal array surrounded by layers of shielding structures and will be operated at the Yangyang underground laboratory. The goal is to provide an unambiguous test of the DAMA/LIBRA annual modulation signature. Measurements of six prototype crystals show progress in the reduction of internal contamination from radioisotopes. Based on our understanding of these measurements, we expect to achieve a background level in the final detector configuration that is less than 1 count/day/keV/kg for recoil energies around 2 keV. The annual modulation sensitivity for the KIMS-NaI experiment shows that an unambiguous 7...... test of the DAMA/LIBRA signature would be possible with a 600 kg year exposure with this system.

Eur. Phys. J. C (2016) 76:185DOI 10.1140/epjc/s10052-016-4030-z

Regular Article - Experimental Physics

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Web End = Understanding internal backgrounds in NaI(Tl) crystals toward a 200 kg array for the KIMS-NaI experiment

P. Adhikari1, G. Adhikari1, S. Choi2, C. Ha3,a, I. S. Hahn4, E. J. Jeon3, H. W. Joo2, W. G. Kang3, H. J. Kim5,H. O. Kim3, K. W. Kim2, N. Y. Kim3, S. K. Kim2, Y. D. Kim1,3, Y. H. Kim3,6, H. S. Lee3,b, J. H. Lee3, M. H. Lee3,D. S. Leonard3, J. Li3, S. Y. Oh1, S. L. Olsen3, H. K. Park3, H. S. Park6, K. S. Park3, J. H. So3, Y. S. Yoon3

1 Department of Physics, Sejong University, Seoul 05006, Korea

2 Department of Physics and Astronomy, Seoul National University, Seoul 08826, Korea

3 Center for Underground Physics, Institute for Basic Science, Daejeon 34047, Korea

4 Department of Science Education, Ewha Womans University, Seoul 03760, Korea

5 Department of Physics, Kyungpook National University, Daegu 41566, Korea

6 Korea Research Institute of Standards and Science, Daejeon 34113, Korea Received: 28 January 2016 / Accepted: 17 March 2016 The Author(s) 2016. This article is published with open access at Springerlink.com

Abstract The Korea Invisible Mass Search (KIMS) collaboration has developed low-background NaI(Tl) crystals that are suitable for the direct detection of WIMP dark matter.Building on experience accumulated during the KIMS-CsI programs, the KIMS-NaI experiment will consist of a 200 kg NaI(Tl) crystal array surrounded by layers of shielding structures and will be operated at the Yangyang underground laboratory. The goal is to provide an unambiguous test of the DAMA/LIBRA annual modulation signature. Measurements of six prototype crystals show progress in the reduction of internal contamination from radioisotopes. Based on our understanding of these measurements, we expect to achieve a background level in the nal detector conguration that is less than 1 count/day/keV/kg for recoil energies around 2 keV. The annual modulation sensitivity for the KIMS-NaI experiment shows that an unambiguous 7 test of the DAMA/LIBRA signature would be possible with a 600kgyear exposure with this system.

1 Introduction

The detection of light signals from scintillation crystals is a well established technology for searching for extremely rare events such as weakly interacting massive particles (WIMPs) [6,12,16,22,23,28], a strongly motivated particle dark matter candidate. A WIMP can elastically scatter off a nucleus and a portion of the recoil energy that is deposited in the crystal is transformed into scintillation light. For these

a e-mail: mailto:[email protected]

Web End [email protected]

b e-mail: mailto:[email protected]

Web End [email protected]

searches, it is essential to produce ultra low-background crystals by reducing internal radioisotope contaminations to extremely low levels. Among various crystal scintillators, NaI(Tl) is particularly interesting because of the positive signal reported by the DAMA/LIBRA collaboration for an annual modulation in the rate for low-energy events in an array of NaI(Tl) crystals [13,15,16]. This modulation signal has been the subject of a continuing debate because other experiments observe no modulation [1,10] and because the WIMPnucleon or WIMPelectron cross sections inferred from the DAMA/LIBRA modulation are in conict with limits from other experiments, such as LUX [2], Super-CDMS [3], CRESST-II Phase 2 [7], and XENON100 [8,9]. However, it is possible to explain all of the direct search experimental results in terms of non-trivial systematic differences in detector responses and possible modications of the commonly used halo model for the galactic distribution of dark matter [11,17].

The Korea Invisible Mass Search (KIMS) experiment searched for WIMP dark matter using ultra low-background CsI(Tl) crystal detectors [2426,29]. Null results from the KIMS-CsI experiment establish stringent constraints on the interpretation of the DAMA/LIBRA annual modulation signal as being due to WIMPiodine interactions [22,28]. However, an alternative interpretation of the DAMA/LIBRA result that attributes it to being primarily due to WIMP sodium nuclei interactions, as would be the case for low-mass WIMPs, cannot be ruled out. Therefore, it remains necessary to try to reproduce the DAMA/LIBRA observations with crystal detectors of the same NaI(Tl) composition. Efforts by various groups such as DM-Ice [19], ANAIS [5],

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Fig. 1 Schematic drawings of test setups for NaI(Tl) crystals (circles) with CsI(Tl) crystal array (squares). The rst two crystals (NaI-001 and NaI-002) were rst tested with conguration A. In the B conguration,

we tested NaI-003 and NaI-004 crystals together with NaI-001 and NaI-002. Subsequently, NaI-003 and NaI-004 were replaced with NaI-005 and NaI-006

and SABRE [32] to test DAMA/LIBRA signals using the same NaI(Tl) crystals have been initiated. Recently, the KIMS collaboration engaged in R&D to produce ultra low-background NaI(Tl) crystals [21]. The successful growth of crystals with background levels at or below those measured in the DAMA/LIBRA experiment (1 count/day/keV/kg) is required to achieve a stringent and unambiguous test of the DAMA/LIBRA annual modulation observation.

In this article, we describe internal background measurements of NaI(Tl) crystals at the Yangyang underground laboratory (Y2L). Six R&D stage crystals were grown by Alpha Spectra Inc.1 and Beijing Hamamatsu2 using a variety of NaI powders. Background levels measured in the six crystals permitted us to understand the dominant contributions to the WIMP signal region and provided guidance for the further reduction of these backgrounds. Based on our best understanding of the background, the ultimate sensitivity of a 200 kg array of the KIMS-NaI experiment is determined.

2 Background measurements of NaI(Tl) crystals

2.1 The experimental setup

To evaluate the background contamination levels in the NaI(Tl) crystals, we used the same experimental apparatus that was used for the KIMS-CsI experiment at Y2L [21,22]. This includes a 12-module array of CsI(Tl) crystals inside a shield that includes 10 cm of copper, 5 cm of polyethylene, 15 cm of lead, and 30 cm of liquid-scintillator-loaded mineral oil. The shielding stops external neutrons and gamma rays, and vetoes cosmic-ray muons. The availability of the

1 http://www.alphaspectra.com

Web End =http://www.alphaspectra.com .

2 http://www.bhphoton.com

Web End =http://www.bhphoton.com .

already-established setup has been advantageous for a timely evaluation of new crystals.

So far, six R&D stage NaI(Tl) crystals have been tested inside the CsI(Tl) detector array. From February 2014 to September 2014, two NaI(Tl) crystals (NaI-001 and NaI-002) were tested in the A conguration (see Fig. 1). Results from

this test were previously reported in Ref. [21]. In September 2014, two NaI(Tl) crystals (NaI-003 and NaI-004) were delivered and promptly used to replace two CsI(Tl) crystals as shown in the B conguration of Fig. 1. In December

2014 and January 2015, we replaced NaI-003 and NaI-004 with the newly-arrived NaI-005 and NaI-006 crystals. Crystals that arrive hereafter will also be evaluated in this setup.

2.2 NaI(Tl) crystals

The low background NaI(Tl) crystals were grown from highly puried powders. To reach the required background level in the crystal form, it is necessary to study the powder purication procedure and understand the crystal growth environment.

Of the six crystals tested, the rst ve crystals were produced by Alpha-Spectra (AS). The sixth one was produced by Beijing Hamamatsu (BH). Sigma-Aldrich (SA) and AS applied several purication procedures to the powders to reduce levels of radionuclides. NaI-001 and NaI-002 were produced by AS from their own powders. The details of the rst two crystals are discussed in Ref. [21]. The NaI-003 crystal, grown from SA Astro-Grade (AG) powder, is known to contain less contamination from potassium. NaI-004 and NaI-006 were made of SA Crystal-Growth (CG) grade powder but were grown separately by two different crystal growers. For the NaI-005 production, AS developed additional background reduction methods, especially aimed at reduc-

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Table 1 Specication of the NaI(Tl) crystals. The second column species the cylinder diameters and length in inches. The Powder acronyms are AS-B (AS-C): Alpha Spectra puried powder, SAAG: Sigma-Aldrich Astro-Grade powder (reduced K content), SA-CG:

Sigma-Aldrich Crystal-Growth powder, and AS-WSII: Alpha Spectra WIMPScint-II grade powder. The names of the crystal growers are AS: Alpha-Spectra and BH: Beijing-Hamamatsu. The last two columns are the year and month the crystals were grown and transported to Y2L

Crystal Size (D L) Mass (kg) Powder Crystal grower T (growth) T (Y2L) NaI-001 5 7 8.3 AS-B AS 2011.9 2013.9

NaI-002 4.2 11 9.2 AS-C AS 2013.4 2014.1

NaI-003 4.5 3.5 3.3 SA-AG AS 2014.4 2014.9

NaI-004 4.5 3.5 3.3 SA-CG AS 2014.3 2014.9

NaI-005 4.2 11 9.2 AS-WSII AS 2014.7 2014.12

NaI-006 4.8 8.8 11.4 SA-CG BH 2014.10 2015.1

Table 2 Background rates from internal radioactive contaminants in the NaI(Tl) crystals. For the Rate, each alpha particle is counted as one decay. The light yields are measured using 59.6 keV gamma events

from 241Am calibration source. Chain equilibrium is assumed in the interpretation of radioactivity measurements related to 238U and 232Th, with the exception of 210Pb

Crystal natK (40K ) natK (ICP-MS) 238U 232Th Rate Light yield(unit) (ppb) powder (ppb) (ppt) (ppt) (mBq/kg) (Photoelectrons/keV)

NaI-001 40.4 2.9 <0.02 <3.2 3.29 0.01 15.6 1.4

NaI-002 48.1 2.3 <0.12 0.5 0.3 1.77 0.01 15.5 1.4

NaI-003 25.3 3.6 25 <0.14 0.5 0.1 2.43 0.01 13.3 1.3

NaI-004 >116.7 100400 3.9 0.4

NaI-005 40.1 4.2 50 <0.04 0.2 0.1 0.48 0.01 12.1 1.1

NaI-006 >127.1 100400 <0.05 8.9 0.1 1.53 0.01 4.4 0.4

ing 210Pb contamination in the powder and crystal growing process.

The crystals are cylindrical in shape and were cut from large ingots. After the crystals were polished in a pure nitrogen environment by a proprietary process they were wrapped with a Teon reector and inserted into an oxygen-free copper case. The circular plane of the crystal was light-coupled with a quartz window via a gel-type optical pad. Each end of the encapsulated cylinder was attached to a 3-inch. diameter, glass window R12669 photomultiplier tube (PMT) manufactured by Hamamatsu Photonics.3 The specications of the crystals are summarized in Table 1.

2.3 Internal natural backgrounds

To produce ultra low-background NaI(Tl) crystals, one should understand internal contamination of natural radioisotopes. Table 2 lists the contamination levels for the six crystals as measured with the test congurations described above.

2.3.1 40K background

One of the most dangerous sources of background for WIMP searches with NaI(Tl) crystals is contamination from 40K.

3 http://www.hamamatsu.com

Web End =http://www.hamamatsu.com .

Its natural abundance is roughly 0.012 % of the total amount of potassium (natK). About 10 % of 40K decays produce a 1460 keV -ray in coincidence with a 3 keV X-ray. If the 1460 keV -ray escapes the crystal and only the 3 keV X-ray is detected, an event is produced that is similar in energy to that expected for a WIMPnuclei interaction [30]. The

natK contents in the DAMA crystals are in the 1020 ppb range [14].

In our apparatus, 40K decays can be identied by coincidence signals between 1460 keV -rays in the CsI(Tl) detectors and 3 keV X-rays in the NaI(Tl). The 40K background level in each crystal is determined by comparing the measured coincidence rate with a Geant4-simulated rate using the method described in Ref. [21]. To understand the origin of the 40K background, natK contents in powders used in the crystal production are measured by inductively coupled plasma mass spectrometry (ICP-MS) and the results are compared to the crystal measurements.

In three of the crystals (NaI-001, NaI-002, and NaI-005) produced by the AS company, the coincidence analysis results show natK levels in the range of 4050 ppb. For the AS WIMPScint-II grade (AS-WSII) powder, which was used to grow the NaI-005 crystal, ICP-MS measurements similarly show natK contamination of about 50 ppb.

The SA powder comes in two varieties, each with different levels of natK contamination. The SA-CG powder is com-

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monly used for commercial NaI(Tl) crystals while the SAAG powder developed for rare event searches shows reduced contamination of radioisotopes. Using its ICP-MS measurements, the SA company reported that the SA-CG powders contain natK levels of approximately 100400 ppb depending on the batch, while the SA-AG powders have batch-to-batch variation natK levels, all in the range of 330 ppb. The NaI-003 crystal that was grown from the SA-AG powder has a measured natK level of 25.33.6 ppb. This is the lowest natK

contamination of the six tested crystals, and is in good agreement with the vendors ICP-MS measurement of 25 ppb for this batch. Due to lower light yield from NaI-004 and NaI-006, which were made with SA-CG powder, our measurements could only establish a limit on the natK contamination level. The natK level in these crystals was measured to be more than 100 ppb, consistent with contamination levels in the SA-CG powder.

Based on these measurements, we conclude that the source of 40K contamination in the NaI(Tl) crystals originates mostly from contamination in the NaI powder, and that no signicant additional contamination is introduced during the crystal growing procedure. The natK measurements for the six crystals are listed in Table 2.

For further reduction of the 40K contamination, several approaches are currently under development. First, WIMPScint-III grade powder is produced by the AS company with lower natK contamination than that of AS-WSII. Several ICP-MS measurements on this powder show on average of 16 ppb natK contamination. AS is currently growing a crystal with this powder. Separately, we have acquired 10 ppb SA-AG powder which is also in the crystal growing process. Second, the simultaneous production of a 1460 keV -ray with a 3 keV X-ray makes it possible to tag these events with surrounding detection devices. In the current setup, a Geant4-based simulation compared with data shows that the surrounding CsI(Tl) crystals tag 40 % of 40K-induced events. Studies to increase the veto-tagging efciency by incorporating the crystals inside a liquid scintillator veto (LSV) system are being performed. A separate Geant4 simulation estimates that the tagging efciency with a 40 cm thick LSV system can be better than 80 %. Therefore, the implementation of such a system for the KIMS-NaI experiment is expected to reduce the 40K-induced background by more than a factor of two. Finally, R&D on procedures for additional potassium reduction in the NaI powder are in progress. Column chromatography with certain resin compounds is known to remove contaminants in solutions via an ion-exchange mechanism. In the near future, we expect that some combination of all of the above will reduce the potassium background to a level lower than the level that has been achieved by DAMA/LIBRA.

2.3.2 238U background

238U is one of the most common radioisotopes in nature primarily because of its long decay time. Assuming an equilibrium in the 238U decay chain, the contamination level in NaI(Tl) crystals can be evaluated by exploiting the 237 s mean lifetime of a 214Po -decay (E = 7.7 MeV), which

immediately follows its production via -decay of 214Bi as

described in Refs. [21,24]. Taking advantage of pulse shape differences between -induced and -induced events, we used this technique to determine 238U contamination levels in the six crystals. We found no signicant time-dependent exponential components that are a characteristic of 214Po.

Upper limits on the activities were determined; no limit could be set for NaI-004 because of its low light yield. The 238U

background levels in the crystals are all below the ppt level (see Table 2).

2.3.3 232Th background

Contamination from the 232Th decay chain was studied by using time interval measurements in the crystals. In

this case, we looked for a 216Po -decay (E = 6.8 MeV)

component with a mean decay time of 209 ms that follows its production via -decay of 220Rn (E = 6.3 MeV). Fig

ure 2 shows the distributions of the time differences with exponential ts between two adjacent -induced events for NaI-005 and NaI-006. Other than NaI-006, all crystals show a small exponential component below 1 s for the characteristic

216Po decay time that indicates a small amount of 232Th contamination, assuming a chain equilibrium. NaI-006 contains a 216Po decay component, corresponding to a 8.90.04 ppt

of the 232Th contamination. The 232Th contents in these crystals, inferred assuming equilibrium in the 232Th decay chain,

are listed in Table 2.

2.3.4 210Pb background

The levels of 238U and 232Th contamination measured in the six crystals are too low to account for the total observed rates. This suggests that the bulk of the rate is due to decays of 210Po (E = 5.4 MeV) nuclei originating from

222Rn exposure that occurred sometime during the powder and/or crystal processing stages. This was conrmed by the observation of a 46.5 keV peak, which is characteristic of 210Pb. The 210Po level in NaI-005 was estimated from

the total alpha yield to be about 1/3 of that in NaI-002 (see Table 2), consistent with 46.5 keV -ray peak measurements.

In the 222Rn decay chain, 210Po ( half life = 138 days) is

produced by the beta decay of 210Pb (half life = 22 years) and

210Bi (half life = 5 days), and subsequently decays via alpha

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216Po sequential decays. While the t for NaI-005 is consistent with a at line, the t for NaI-006 shows signicant decay components that are indicative of a 232Th contamination

emission to 206Pb. Thus, if the 210Po contamination is zero at the time when 222Rn exposure occurs, it will grow with a characteristic time of Po = 200 days until an equilibrium

is reached. This change in the total alpha rate over time can provide information about the date of the 222Rn exposure.

Figure 3 shows the total alpha rates in the four crystals as a function of data-taking time (days). The 210Po alpha activity

grows as

R(t) A(1 e(tt0)/Po), (1)

where t0 is the time when the initial 210Pb contamination occurred, assuming that the contamination occurred over a single short time period. The ts to the time dependence of the 210Po alpha signals shown in Fig. 3 indicate that t0 coincides with the time that the crystal was grown. However, since the preparation of the NaI powder happens about 2 months prior to the crystal growing, it is still possible that some contamination occurred during powder production.

We asked the crystal growers to apply more systematic controls on contamination during the crystal growth. NaI-005 was a result of reduced radon contact and additional purication of the NaI powder by AS. As listed in Table 2, the total rate of NaI-005 was reduced by more than a factor of three compared to NaI-002. For further reduction of the 210Pb

contamination, we are investigating purication methods for the NaI powder that utilize ion-exchange resins that were previously applied in the Kamland-PICO experiment [20].

2.3.5 Background summary and its possible reduction

Figure 4 shows a comparison of the background levels in the NaI-002 and NaI-005 crystals. The factor of three reduction of 210Pb in NaI-005 compared to that for NaI-002 results

in a 2 dru (differential rate unit = counts/day/keV/kg) background level at 6 keV. Below 6 keV, the main contributors to the remaining background are three types. The X-ray of the

40K decay populates energies around 3 keV. Cosmogenically activated 125I (T1/2 = 59.4 days) decays via electron capture

to an excited state of 125Te producing X-ray/Auger electrons with energies of 4 keV. Similarly, 22Na (T1/2 = 2.6 years)

conversion to 22Ne produces a 0.85 keV k-shell X-ray. The cosmogenically activated background is expected to be substantially reduced after a year underground [4] but, because our required background level is less than 1 dru over the 210 keV energy range, additional reductions of these backgrounds is still needed.

To quantify the background contributions from internal radioisotopes, we used Geant4-based Monte-Carlo simulations. The background contribution from a 40 ppb contamination of natK in NaI-005 produces a background count rate of approximately 0.7 dru in the 24 keV energy range; the possibility for a reduction of an additional factor of nearly two has been demonstrated with the SA-AG powder in NaI-003 (25 ppb). Another factor of two reduction in future crystals could be accomplished by using a different batch of an SA-AG powder (10 ppb) or by using an AS-WSIII powder (16 ppb). The implementation of the LSV can further reduce this background contribution.

As for the 210Pb contamination in the crystals, the contribution to the total background in NaI-005 is about 0.5 dru for energies below 10 keV. The development of techniques using ion-exchange resins to remove 210Pb from NaI powder could

lead to an additional reduction of the 210Pb background by a factor of two (to less than 0.3 dru).

The remaining background comes from external sources such as long-lived radioisotopes in the PMTs, lead shields and surrounding rocks, as well as from cosmogenic nuclei,

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Fig. 3 Increases in alpha activity are tted to a model that assumes a single, instantaneous 210Po contamination event occurred for each crystal: a NaI-002, b NaI-003, c NaI-005, and d NaI-006. The best t is indicated as the red line with its 68 % uncertainty as a green band. Since

the event sample in the NaI-006 crystal contains additional events from a substantial 232Th contamination, the best t date precedes the crystal growth date by roughly 3 months

including those from cosmic-ray muon-induced events. The planned LSV system and other veto techniques can tag and veto more than 80 % of the background contributions from these external sources. We expect to achieve 0.5 dru for the external background for energies below 10 keV. Crystal growing with the incorporation of all recent developments is proceeding. With a subset of the improvements that are nearing completion, we expect to reach a background level of less than 1 dru.

3 KIMS-NaI experiment with a 200 kg NaI(Tl) array

Following up on the success of the background reduction for the NaI(Tl) crystals, we plan to grow 200 kg of crystals for the KIMS-NaI experiment that will be arranged in a 4 4

array of 12.5 kg NaI(Tl) modules; this could be completed

by mid 2016. We have set background goals in the NaI(Tl)

crystals of approximately 1 dru in the 210 keV energy

range. The underground area at Y2L has been expanded, and space has been prepared for this experiment. We are constructing a passive shield consisting of copper, lead, and polyethylene, as well as a plastic-scintillator muon veto and an LSV system. At least 3 years of stable operation will provide enough data to study the annual modulation and test the DAMA/LIBRA observation. Here we report sensitivity estimates for the KIMS-NaI experiment and compare them with the DAMA/LIBRA observed signals.

We generate monthly-binned histograms for WIMP nuclei scattering signals assuming the standard halo model with the consideration for the Earths orbital motion around the Sun as discussed in Ref. [30]. In Ref. [31], the DAMA/ LIBRA modulation signal is interpreted in terms of a WIMP nucleon cross section. To make a direct comparison with this interpretation we used the same quenching factors of 0.3 and0.09 for Na and I, respectively, where the quenching factor is the ratio of the recoil energy deposited by a WIMP to the

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energy deposited by an electron (or a -ray). Figure 5 shows the expected annual modulation signal in the 26 keV energy range for a 10 GeV/c2 WIMP and a 70 GeV/c2 WIMP for WIMPNa and WIMPI interactions, respectively. Here, we choose WIMPnucleon interaction cross sections that match the modulation amplitude observed by the DAMA/LIBRA experiment. For background events, we assume a at background with no modulation or decay components. We consider a 3-year period of uninterrupted data taking with a 200 kg NaI(Tl) crystal array with a 1 dru background rate.

We use an ensemble of Monte Carlo experiments to estimate the sensitivity of the KIMS-NaI experiment, expressed as the expected cross section limits for the WIMPnucleon

spin-independent interactions in the case of no signal. For each experiment, we determine a simulated modulation distribution for a background-only hypothesis. The background rate includes Poisson uctuations. We then t the modulation distribution with a signal-plus-background hypothesis with at priors for the signal. Additionally, we include a 10 % Gaussian prior for the background. This represents any constraints we may have on the background rate at the time of tting. This additional constraint has no signicant impact on the modulation sensitivity. It is, however, used as a conservative assumption to derive potential sensitivity for WIMP masses outside of the DAMA signal region, where total rate constraints will be stronger than modulation constraints.

The global t is performed with a Bayesian approach using the Bayesian Analysis Toolkit [18]. We construct a Bayesian likelihood for each bin (1 keV). The overall likelihood is obtained by multiplying the likelihood for each bin between 2 and 10 keV, considering the energy-dependent rate of WIMPNaI interactions for WIMP masses between5 GeV/c2 and 10 TeV/c2. The 90 % condence limit (CL) for each simulated experiment is determined such that 90 % of the posterior density of the WIMPnucleon cross-section falls below the limit. The median expected 90 % CL limits and their 1 and 2 standard-deviation probability regions are calculated from 2000 simulated experiments. Figure 6 shows the expected median limit, and 1 and 2 standard deviation probability regions, for the KIMS-NaI experiment using the annual-modulation analysis. We also include a more conservative limit that assumes a 2 dru background level, which we already achieved in the R&D stage crystal. These limits are compared with the DAMA/LIBRA 3 allowed signal region as interpreted in Ref. [31]. Since DAMA/LIBRA reports high signicances of the annual modulation sig-

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70 GeV/c2, and a cross-section of 6 106 pb (b) in the energy range

between 2 and 6 keV. Scenarios a and b correspond, respectively, to WIMPNa and WIMPI interpretations of the DAMA/LIBRA annual modulation signals

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)

Fig. 7 The median expected (black dotted line) signicance to observe the same annual modulation signal of DAMA/LIBRA as a function of data size. The dark (green) and light (yellow) shaded bands indicate the 1 and 2 standard deviation probability regions in which the signicances are uctuated. The arrow indicates a 3-year data exposure of the KIMS-NaI experiment

narios, the median expected signicance levels with a 3-year data sample are greater than 5, which would be enough to conrm the DAMA/LIBRA observation. If the KIMS-NaI experiment sees a similar annual modulation signal, we will also identify whether or not the annual modulation events originated from WIMP-induced nuclear recoil signals by taking advantage of relatively good pulse shape discrimination between nuclear recoil and electron recoil events of our NaI(Tl) crystals discussed in Ref. [27].

4 Conclusion

We developed and tested six R&D stage NaI(Tl) crystals as a part of a program to develop ultra low-background NaI(Tl) crystals for WIMP searches. We have reduced the 210Pb and

40K backgrounds in different crystals and achieved a 2 dru background level for recoil energies around 6 keV. Additional powder purication procedures and the implementation of an LSV system should further reduce the background level to about 1 dru. We have investigated the expected sensitivity of the KIMS-NaI experiment with a total mass of 200 kg and a 3-year period of stable operation with the assumptions of a 1 dru background rate and a 2 keV energy threshold. The comparison with the DAMA/LIBRA modulation signal gives condence that the KIMS-NaI experiment can test the parameter space claimed by DAMA/LIBRA using the same target material and can achieve similar sensitivity to the reported modulation signatures. This experiment can unambiguously conrm or refute the DAMA/LIBRA observation.

Fig. 6 The median expected 90 % CL upper limit on the WIMP nucleon spin-independent cross-section assuming the background-only hypothesis (black dotted line), shown together with WIMP-induced DAMA/LIBRA 3-allowed region (solid contour). The dark (green) and light (yellow) shaded bands indicate the 1 and 2 standard deviation probability regions over which the limits have uctuated. The red dotted line indicates the median expected limit assuming a 2 dru background level

nal and its allowed region for the interpreted cross-sections are tightly bounded, KIMS-NaI can exclude or conrm the parameter space with the baseline exposure. As one can see in the gure, 3years of KIMS-NaI experimental data can fully cover the DAMA/LIBRA 3 region even for the conservative background assumption of 2 dru.

We also estimate the precision with which we can measure the annual modulation signal if the KIMS-NaI experiment detects a modulation amplitude that is the same as DAMA/LIBRAs. The annual modulation amplitude observed by the DAMA/LIBRA experiment for the 26 keV events (where their signal has the highest significance) is 0.0112 0.0012 dru [16]. If we inject 10 GeV/c2

WIMPs with a 2.96 104 pb cross section (see in Fig. 5a),

our detector can observe the same modulation signal as DAMA/LIBRAs. Based on the Bayesian likelihood t discussed above, we extract the signal rate by performing 2000 simulated experiments to obtain a mean of the modulation amplitude as well as 68 % (1) and 95 % (2) coverage from 100 to 1050 kg year. Figure 7 shows the expected signicance for the observation of an annual modulation signal as a function of data size. In case of 3-year data exposure, corresponding to 600 kg year, the expected signicance is 7.2 1.0 , where the uncertainty means 68 % coverage.

Since DAMA/LIBRA reported a signal signicance of 9.3 with a 1.04 ton years exposure [16], our simulated experiments indicate a similar level of signicance as one can see in Fig. 7.

We repeated the analysis using simulated experiments that assume a 2 dru background level and obtain a signicance of 5.1 0.9 for the same exposure. In both background sce-

Data (kg year)

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Acknowledgments This research was funded by the Institute for Basic Science (Korea) under project code IBS-R016-D1 and was supported by the Basic Science Research Program through the National Research Foundation of Korea funded by the Ministry of Education (NRF-2011-35B-C00007).

Open Access This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/

Web End =http://creativecomm http://creativecommons.org/licenses/by/4.0/

Web End =ons.org/licenses/by/4.0/ ), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.

Funded by SCOAP3.

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