Results from the Final Exposure of the CDMS II Experiment

Results from the Final Exposure of the CDMS II Experiment

Abstract

We report results from a blind analysis of the final data taken with the Cryogenic Dark Matter Search experiment (CDMS II) at the Soudan Underground Laboratory, Minnesota, USA. A total raw exposure of 612 kg-days was analyzed for this work. We observed two events in the signal region; based on our background estimate, the probability of observing two or more background events is 23%. These data set an upper limit on the Weakly Interacting Massive Particle (WIMP)-nucleon elastic-scattering spin-independent cross-section of cm for a WIMP of mass 70 GeV/c at the 90% confidence level. Combining this result with all previous CDMS II data gives an upper limit on the WIMP-nucleon spin-independent cross-section of cm for a WIMP of mass 70 GeV/c. We also exclude new parameter space in recently proposed inelastic dark matter models.

pacs:
14.80.Ly, 95.35.+d, 95.30.Cq, 95.30.-k, 85.25.Oj, 29.40.Wk

CDMS Collaboration

Cosmological observations Komatsu et al. (2009) have led to a concordance model of the universe where 85% of matter is non-baryonic, non-luminous and non-relativistic at the time of structure formation. Weakly Interacting Massive Particles (WIMPs) Steigman and Turner (1985) are a class of candidates for this dark matter which are particularly well motivated by proposed extensions to the Standard Model of particle physics and by thermal production models for dark matter in the early universe Lee and Weinberg (1977); Weinberg (1982); Jungman et al. (1996); Bertone et al. (2005). WIMPs, distributed in a halo surrounding our galaxy, would coherently scatter off nuclei in terrestrial detectors Goodman and Witten (1985); Gaitskell (2004); Salucci and Borriello (2003) with a mean recoil energy of tens of keV, presently limited by observation to a rate of less than 0.1 event kgday Lewin and Smith (1996); Jungman et al. (1996); Bertone et al. (2005). Direct search experiments seek recoil signatures of these interactions and have achieved the sensitivity to begin testing the most interesting classes of WIMP models Ahmed et al. (2009); Armengaud et al. (2009); Aprile et al. (2009); Lebedenko et al. (2009).

The Cryogenic Dark Matter Search (CDMS II) experiment, located at the Soudan Underground Laboratory, uses 19 Ge (230 g) and 11 Si (100 g) particle detectors operated at cryogenic temperatures ( mK) Akerib et al. (2005); Ahmed et al. (2009). Each detector is a disk 10 mm thick and 76 mm in diameter. Particle interactions in the detectors deposit energy in the form of phonons and ionization. Phonon sensors on the top of each detector are connected to four phonon readout channels to allow measurement of the recoil energy and position of an event. These phonon sensors are also the ground reference for the ionization measurement. The electric field for the ionization measurement is formed by applying a voltage bias to the bottom detector surface, which is segmented into two concentric electrodes. Events having an ionization signal in the outer ionization channel of the detector are excluded, defining an ionization fiducial volume. The detectors are grouped into five towers, each tower containing six detectors. Detectors are identified by their tower number (T1-T5) and their position within that tower (Z1-Z6). A direct line of sight between adjacent detectors in a tower allows identification of events scattering between detectors.

The ratio of the ionization to recoil energy (“ionization yield”) provides event-by-event rejection of electron-recoil events to better than 10 misidentification. Essentially all of the misidentified electron recoils are “surface events” occurring within the first few m of the detector surface, which can suffer from sufficiently reduced ionization collection to be misclassified as nuclear recoils. Due to interactions of phonons in the surface metal layers, these surface events have faster-rising phonon pulses than events occurring within the bulk of the detectors (“bulk events”). Hence, we use phonon pulse timing parameters to improve rejection of surface events to obtain an overall (yield and timing) misidentification probability of less than 10 for electron recoils. To attenuate external environmental radioactivity and to reject events caused by cosmogenic muons, the detectors are surrounded by layers of lead and polyethylene shielding and an active muon veto Akerib et al. (2005).

Data taken during four periods of stable operation between July 2007 and September 2008 were analyzed for this work. Between each data period the cryostat was warmed up for maintenance of the cryogenic system. All 30 detectors were used to identify particle interactions, but only Ge detectors were used to search for WIMP scatters. Five Ge detectors were not used for WIMP detection because of poor performance or insufficient calibration data; four more detectors were similarly excluded during subsets of the four periods. We excluded Si detectors in this analysis due to their lower sensitivity to coherent nuclear elastic scattering.

A subset of events were analyzed to monitor detector stability and identify periods of poor detector performance. Data quality criteria were developed on a detector-by-detector basis using Kolmogorov-Smirnov tests performed on parameter distributions. Our detectors require regular neutralization Akerib et al. (2005) to maintain full ionization collection. We monitor the yield distribution and remove periods with poor ionization collection. After these data quality selections, the total exposure to WIMPs considered for this work was 612 kg-days.

The data selection criteria (“cuts”) that define the WIMP acceptance region were calculated from calibration sets of electron and nuclear recoils obtained during regular exposures of the detectors to -ray (Ba) and neutron (Cf) sources. A 356 keV -line from the Ba source was used to calibrate the ionization and phonon energy scales of each detector. Nuclear recoils from the elastic scattering of neutrons emitted by the Cf source were used to define the WIMP signal region, taken to be the 2 band about the mean neutron ionization yield in the yield vs recoil energy plane (Fig. 1). Neutron activation of Ge results in the emission of 10.36 keV x-rays. The width of this x-ray line determined the ionization energy resolution at the 10 keV analysis threshold to be  keV on all detectors considered.

Phonon pulse shapes vary with event position and energy in our detectors. To enhance surface-event rejection, we characterized the variation of the resulting timing and energy estimators using our electron-recoil calibrations and corrected for it in both WIMP-search and calibration data. To ensure this correction works well at large radius, where position reconstruction degeneracies can lead to miscorrection, we included calibration electron-recoil events outside the ionization fiducial volume in the correction calculation. This technique obviated the additional fiducial volume cut in phonon position reconstruction parameters used in past analyses Ahmed et al. (2009).

Figure 1 demonstrates our surface-event rejection cut. We optimized this cut using calibration sets of nuclear and surface electron recoils from the Cf and Ba exposures. We verified that the sum of the rise time of the largest phonon pulse plus its delay relative to the ionization signal provided the best discrimination between surface events and nuclear recoils. Surface-event rejection criteria based on this discriminator were tuned on the calibration data by maximizing the expected sensitivity for a 60 GeV/c WIMP.

Figure 1: The power of the primary background discrimination parameters, ionization yield and phonon timing, is illustrated for a typical detector using in situ calibration sources. Shown are bulk electron recoils (red points), surface electron events (black crosses) and nuclear recoils (blue circles) with recoil energy between 10 and 100 keV. Top: Ionization yield versus recoil energy. The solid black lines define bands that are from the mean electron- and nuclear-recoil yields. The sloping magenta line indicates the ionization energy threshold while the vertical dashed line is the recoil energy analysis threshold. The region enclosed by the black dotted lines defines the sample of events that are used to develop surface-event cuts. Bottom: Normalized ionization yield (number of standard deviations from mean of nuclear recoil band) versus normalized timing parameter (timing relative to acceptance region) is shown for the same data. Events to the right of the vertical red dashed line pass the surface-event rejection cut for this detector. The solid red box is the WIMP signal region. (Color online.)

A blind analysis was performed, in which cuts were developed without looking at events that might appear in or near the signal region. Candidate WIMP-scatters were required to be within 2 of the mean ionization yield of nuclear recoils and at least away from the mean ionization yield of electron recoils, have recoil energy between 10 and 100 keV, and have ionization energy at least above the noise. They are required to occur within the detector fiducial volume, satisfy data quality criteria and pass the surface-event rejection cut. Since WIMPs are expected to interact only once (“single-scatter event”) in the experimental apparatus, a candidate event was further required to have energy deposition consistent with noise in 29 detectors. Additionally, we required the absence of significant activity in the surrounding scintillator veto shield during a 200- window around the trigger.

The efficiency of our analysis cuts for nuclear recoils was measured as a function of energy using both neutron-calibration and WIMP-search data. The fiducial volume estimate is corrected for neutron multiple-scattering based on simulations. Our efficiency for signal events has a maximum of 32% at 20 keV. It falls to 25% both at 10 keV, due to ionization threshold and flaring of the electron-recoil band; and at 100 keV, due to a drop in fiducial volume. The spectrum-averaged equivalent exposure for a WIMP of mass 60 GeV/c is 194.1 kg-days.

Neutrons with energies of several MeV can generate single-scatter nuclear recoils that are indistinguishable from possible dark matter interactions. Sources of neutron background include cosmic-ray muons interacting near the experimental apparatus (outside the veto), radioactive contamination of materials, and environmental radioactivity. We performed Monte Carlo simulations of the muon-induced particle showers and subsequent neutron production with Geant4 Agostinelli et al. (2003); Allison et al. (2006) and FLUKA Fasso et al. (2003); Ferrari et al. (2005). The cosmogenic background is estimated by multiplying the observed number of vetoed single nuclear recoils in the data by the ratio of unvetoed to vetoed events as determined by cosmogenic simulation. This technique predicts (stat) events in this WIMP-search exposure.

Samples of our shielding and detector materials were screened for U and Th daughters using high purity germanium counters. In addition, a global -ray Monte Carlo was performed and compared to the electromagnetic spectrum measured by our detectors. The contamination levels thus determined were used as input to a Geant4 simulation to calculate the number of neutrons produced from spontaneous fission and (, n) processes, assuming secular equilibrium. The estimated background is between 0.03 and 0.06 events and is dominated by U spontaneous fission in the copper cans of the cryostat. The radiogenic neutron background originating from the surrounding rock is estimated to be negligibly small compared to other sources.

The number of misidentified surface events was estimated by multiplying the observed number of single-scatter events failing the timing cut inside the nuclear-recoil band with the ratio of events expected to pass the timing cut to those failing it (“pass-fail ratio”). The former was estimated using observed counts from a previous analysis Ahmed et al. (2009), and the latter was estimated using three different methods. The first method computed the pass-fail ratio from events that reside within the nuclear-recoil band and multiply scatter in vertically adjacent detectors (“multiple scatter events”). The second method estimated the pass-fail ratio from multiple-scatter events surrounding the nuclear-recoil band (“wide-band events”). Wide-band events have different distributions in energy and in detector face (ionization- or phonon- side) from nuclear-recoil band events, affecting the pass-fail ratio. To account for these differences, the pass-fail ratio of these events was corrected using the face and energy distributions of events observed in the nuclear-recoil band that failed the timing cut. A third, independent estimate of the pass-fail ratio was made using low-yield, multiple-scatter events in Ba calibration data, again adjusted for differences in energy and detector-face distributions. All three estimates were consistent with each other and were thus combined to obtain an estimate prior to unblinding of (stat) surface events misidentified as nuclear recoils.

Upon unblinding, we observed two events in the WIMP acceptance region at recoil energies of 12.3 keV and 15.5 keV. These events are shown in Figs. 2 and 3.

Figure 2: Ionization yield versus recoil energy for events passing all cuts, excluding yield and timing. The top (bottom) plot shows events for detector T1Z5(T3Z4). The solid red lines indicate the electron and nuclear recoil bands. The vertical dashed line represents the recoil energy threshold and the sloping magenta dashed line is the ionization threshold. Events that pass the timing cut are shown with round markers. The candidate events are the round markers inside the nuclear-recoil bands. (Color online.)
Figure 3: Normalized ionization yield (number of standard deviations from mean of nuclear recoil band) versus normalized timing parameter (timing relative to acceptance region) for events passing all cuts, excluding yield and timing.Ê The top (bottom) plot shows events for detector T1Z5(T3Z4). Events that pass the phonon timing cut are shown with round markers. The solid red box indicates the signal region for that detector. The candidate events are the round markers inside the signal regions. (Color online.)

The candidate events occurred during periods of nearly ideal experimental performance, are separated in time by several months, and occur in different towers. However, a detailed study revealed that an approximation made during the ionization pulse reconstruction degrades the timing-cut rejection of a small fraction of surface events with ionization energy below 6 keV. The candidate event in T3Z4 shows this effect. Such events are more prevalent in WIMP-search data than in the data sets used to generate the pre-blinding estimate of misidentified surface events. A refined calculation, which accounts for this reconstruction degradation, produced a revised surface-event estimate of (stat)(syst) events. The systematic uncertainty is dominated by our assumption that the pass-fail ratio for multiple scatter events is the same as that for single scatter events. Based on this revised estimate, the probability to have observed two or more surface events in this exposure is 20%; inclusion of the neutron background estimate increases this probability to 23%. These expectations indicate that the results of this analysis cannot be interpreted as significant evidence for WIMP interactions, but we cannot reject either event as signal.

To quantify the proximity of these events to the surface-event rejection threshold, we varied the timing cut threshold of the analysis. Reducing the revised expected surface-event background to 0.4 events would remove both candidates while reducing the WIMP exposure by 28%. No additional events would be added to the signal region until we increased the revised estimate of the expected surface-event background to 1.7 events.

Figure 4: 90% C.L. upper limits on the WIMP-nucleon spin-independent cross section as a function of WIMP mass. The red (upper) solid line shows the limit obtained from the exposure analyzed in this work. The solid black line shows the combined limit for the full data set recorded at Soudan. The dotted line indicates the expected sensitivity for this exposure based on our estimated background combined with the observed sensitivity of past Soudan data. Prior results from CDMS Ahmed et al. (2009), EDELWEISS II Armengaud et al. (2009), XENON10 Aprile et al. (2009), and ZEPLIN III Lebedenko et al. (2009) are shown for comparison. The shaded regions indicate allowed parameter space calculated from certain Minimal Supersymmetric Models Ellis et al. (2005); Roszkowski et al. (2007) (Color online.)

We calculate an upper limit on the WIMP-nucleon elastic scattering cross-section based on standard galactic halo assumptions Lewin and Smith (1996) and in the presence of two events at the observed energies. We use the Optimum Interval Method Yellin (2002) with no background subtraction. The resulting limit shown in Fig. 4 has a minimum cross section of cm ( cm when combined with our previous results) for a WIMP of mass 70 GeV/c . The abrupt feature near the minimum of the new limit curve is a consequence of a threshold-crossing at which intervals containing one event enter into the optimum interval computation Yellin (2002). An improved estimate of our detector masses was used for the exposure calculation of the present work; a similar correction (resulting in a 9% decrease in exposure) was applied to our previous CDMS result Ahmed et al. (2009) shown in Fig. 4. While this work represents a doubling of previously analyzed exposure, the observation of two events leaves the combined limit, shown in Fig.  4, nearly unchanged below 60 GeV/c and allows for a modest strengthening in the limit above this mass.

We have also analyzed our data under the hypothesis of WIMP inelastic scattering Tucker-Smith and Weiner (2001), which has been proposed to explain the DAMA/LIBRA data Bernabei et al. (2008a) . We computed DAMA/LIBRA regions allowed at the 90% C. L. following the goodness-of-fit technique described in Savage et al. (2009), without including channeling effects Bernabei et al. (2008b). Limits from our data and that of XENON10 Angle et al. (2009) were computed using the Optimum Interval Method Yellin (2002). Regions excluded by CDMS and XENON10 were defined by demanding the 90% C. L. upper limit to completely rule out the DAMA/LIBRA allowed cross section intervals for allowed WIMP masses and mass splittings. The results are shown in Fig. 5. The CDMS data disfavor all but a narrow region of the parameter space allowed by DAMA/LIBRA that resides at a WIMP mass of 100 GeV/c and mass splittings of 80–140 keV.

Figure 5: The shaded green region represents WIMP masses and mass splittings for which there exists a cross section compatible with the DAMA/LIBRA Bernabei et al. (2008a) modulation spectrum at 90% C. L. under the inelastic dark matter interpretation Tucker-Smith and Weiner (2001). Excluded regions for CDMS II (solid-black hatched) and XENON10 Angle et al. (2009) (red-dashed hatched) were calculated in this work using the Optimum Interval Method. (Color online.)

The data presented in this work constitute the final data runs of the CDMS II experiment and double the analyzed exposure of CDMS II. We observed two candidate events. These data, combined with our previous results, produce the strongest limit on spin-independent WIMP-induced nuclear scattering for WIMP masses above 42 GeV/c  ruling out new parameter space.

The CDMS collaboration gratefully acknowledges the contributions of numerous engineers and technicians; we would like to especially thank Jim Beaty, Bruce Hines, Larry Novak, Richard Schmitt and Astrid Tomada. This work is supported in part by the National Science Foundation (Grant Nos. AST-9978911, PHY-0542066, PHY-0503729, PHY-0503629, PHY-0503641, PHY-0504224, PHY-0705052, PHY-0801708, PHY-0801712, PHY-0802575 and PHY-0855525), by the Department of Energy (Contracts DE-AC03-76SF00098, DE-FG02-91ER40688, DE-FG02-92ER40701, DE-FG03-90ER40569, and DE-FG03-91ER40618), by the Swiss National Foundation (SNF Grant No. 20-118119), and by NSERC Canada (Grant SAPIN 341314-07).

References

  1. E. Komatsu et al. (WMAP), Astrophys. J. Suppl. 180, 330 (2009).
  2. G. Steigman and M. S. Turner, Nucl. Phys. B253, 375 (1985).
  3. B. W. Lee and S. Weinberg, Phys. Rev. Lett. 39, 165 (1977).
  4. S. Weinberg, Phys. Rev. Lett. 48, 1776 (1982).
  5. G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rept. 267, 195 (1996).
  6. G. Bertone, D. Hooper, and J. Silk, Phys. Rept. 405, 279 (2005).
  7. M. W. Goodman and E. Witten, Phys. Rev. D31, 3059 (1985).
  8. R. J. Gaitskell, Ann. Rev. Nucl. Part. Sci. 54, 315 (2004).
  9. P. Salucci and A. Borriello, Lect. Notes Phys. 616, 66 (2003).
  10. J. D. Lewin and P. F. Smith, Astropart. Phys. 6, 87 (1996).
  11. Z. Ahmed et al. (CDMS), Phys. Rev. Lett. 102, 011301 (2009).
  12. E. Armengaud et al., arXiv:0912.0805 (2009).
  13. E. Aprile et al., Phys. Rev. C79, 045807 (2009).
  14. V. N. Lebedenko et al., Phys. Rev. D80, 052010 (2009).
  15. D. S. Akerib et al. (CDMS), Phys. Rev. D72, 052009 (2005).
  16. S. Agostinelli et al. (GEANT4), Nucl. Instrum. Meth. A506, 250 (2003).
  17. J. Allison et al., IEEE Trans. Nucl. Sci. 53, 270 (2006).
  18. A. Fasso et al. (2003), eprint hep-ph/0306267.
  19. A. Ferrari, P. R. Sala, A. Fasso, and J. Ranft (2005), cERN-2005-010.
  20. J. R. Ellis, K. A. Olive, Y. Santoso, and V. C. Spanos, Phys. Rev. D71, 095007 (2005).
  21. L. Roszkowski, R. Ruiz de Austri, and R. Trotta, JHEP 07, 075 (2007).
  22. S. Yellin, Phys. Rev. D66, 032005 (2002).
  23. D. Tucker-Smith and N. Weiner, Phys. Rev. D64, 043502 (2001).
  24. R. Bernabei et al. (DAMA), Eur. Phys. J. C56, 333 (2008a).
  25. C. Savage, G. Gelmini, P. Gondolo, and K. Freese, JCAP 0904, 010 (2009).
  26. R. Bernabei et al., Eur. Phys. J. C53, 205 (2008b).
  27. J. Angle et al. (XENON10), Phys. Rev. D80, 115005 (2009).
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