A CaMoO{}_{4} Crystal Low Temperature Detector for the AMoRE Neutrinoless Double Beta Decay Search

A CaMoO Crystal Low Temperature Detector for the AMoRE Neutrinoless Double Beta Decay Search

G.B. Kim Institute for Basic Science, Daejeon 305-811, Republic of Korea Department of Physics and Astronomy, Seoul National University, Seoul 151-747, Republic of Korea Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea    S. Choi Department of Physics and Astronomy, Seoul National University, Seoul 151-747, Republic of Korea    F.A. Danevich Institute for Nuclear Research, Kyiv 03680, Ukraine    A. Fleischmann Kirchhoff-Institut für Physik, Universität Heidelberg, D-69120, Heidelberg, Germany    C.S. Kang Institute for Basic Science, Daejeon 305-811, Republic of Korea Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea    H.J. Kim Physics Department, Kyungpook National University, Daegu 702-701, Republic of Korea    S.R. Kim Institute for Basic Science, Daejeon 305-811, Republic of Korea Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea    Y.D. Kim Institute for Basic Science, Daejeon 305-811, Republic of Korea Department of Physics, Sejong University, Seoul 143-747, Republic of Korea    Y.H. Kim yhkim@kriss.re.kr Institute for Basic Science, Daejeon 305-811, Republic of Korea Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea Korea University of Science and Technology, Daejeon 305-350, Republic of Korea    V.A. Kornoukhov Institute for Theoretical and Experimental Physics, Moscow 117218, Russia    H.J. Lee Institute for Basic Science, Daejeon 305-811, Republic of Korea Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea    J.H. Lee Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea    M.K. Lee Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea    S.J. Lee Now at NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea    J.H. So Institute for Basic Science, Daejeon 305-811, Republic of Korea Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea    W.S. Yoon Institute for Basic Science, Daejeon 305-811, Republic of Korea Korea Research Institute of Standards and Science, Daejeon 305-340, Republic of Korea Korea University of Science and Technology, Daejeon 305-350, Republic of Korea
Abstract

We report the development of a CaMoO crystal low temperature detector for the AMoRE neutrinoless double beta decay () search experiment. The prototype detector cell was composed of a 216 g CaMoO crystal and a metallic magnetic calorimeter. An over-ground measurement demonstrated FWHM resolution of 6-11 keV for full absorption gamma peaks. Pulse shape discrimination was clearly demonstrated in the phonon signals, and 7.6  of discrimination power was found for the and separation. The phonon signals showed rise-times of about 1 ms. It is expected that the relatively fast rise-time will increase the rejection efficiency of two-neutrino double beta decay pile-up events which can be one of the major background sources in searches.

Keyword

Double beta decay, low temperature detector, CaMoO crystal scintillator, particle discrimination

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I Introduction

Recent neutrino oscillation experiments have been unveiling the properties of neutrinos Beringer et al. (2012); Mohapatra et al. (2007). Their experimental evidences strongly suggest that neutrinos are massive and encounter flavor mixing of mass eigenvalues. The mixing angles and the differences between the square masses have been estimated. However, those observations do not provide a direct measurement of the absolute mass, and do not answer the question of whether neutrino is its own anti-particle (Majorana-type) or not (Dirac-type).

Search for neutrinoless double beta decay () is a key experiment to reveal un-answered nature of neutrinos Elliott and Vogel (2002); Avignone et al. (2008); Rodejohann (2011); Giuliani and Poves (2012); Gómez-Cadenas et al. (2012). The double beta decay () that accompanies the simultaneous emission of two electrons and two anti-neutrinos is a rare process that is an allowed transition in the standard model. Another type of double beta decay that does not emit any neutrinos, , can occur if neutrino is massive Majorana particles (i.e., it is its own anti-particle). In the process, the full available energy of the decay is carried by the two electrons and the recoiled daughter which has a very small amount of energy compared with that of the electrons. Therefore, while the electron sum energy spectrum in the is continuous up to the available energy release (), in the , the spectrum should have a sharp peak at  Mohapatra et al. (2007).

The observation of would clearly demonstrate that neutrino is not Dirac-type but rather is Majorana-type particle. In that case, physical processes that do not conserve lepton number would be allowed. Moreover, the absolute mass scale, so-called “effective Majorana neutrino mass”, can be estimated using the half life ,

(1)

where is the electron mass, is the kinematic phase-space factor calculable with reasonable precision, and is the model dependent nuclear matrix element. Here, the Majorana mass is defined as

(2)

where the ’s are the mass eigenstates of the neutrino, ’s are the elements of the mixing matrix between the flavor states and mass eigenstates.

Experimentally, the measurement limit of half life is often used as the sensitivity to probe the rare event Gómez-Cadenas et al. (2012). In a measurement with non-negligible backgrounds, the sensitivity becomes

(3)

where is the concentration of isotope in the detector, is the detection efficiency, is the detector mass, is the measurement time, is the background rate per unit mass and energy, and is the energy resolution of the detector, in other words, the region of interest (ROI) of the energy window at the value. However, in a case of a zero-background experiment that observes no event in ROI during the measurement time, the sensitivity becomes proportional to the detector mass and the measurement time,

(4)
Figure 1: (Color online) Low temperature detector setup with a 216 g CaMoO crystal and an MMC sensor.

To increase the detection sensitivity, it is essential to have a detector with high concentration of the isotope of interest, detection efficiency, energy resolution and efficient background rejection capability as well as to minimize backgrounds from internal and external sources in the region of interest. High energy resolution and detection efficiency experiment can be realized with crystal detectors containing the isotope of interest. The detector performance of recently developed low temperature detectors (LTDs) that operate at sub-Kelvin temperatures can perfectly meet the requirements by utilizing state-of-the-art detector technologies with extreme energy sensitivity, such as neutron transmutation doped (NTD) Ge thermistors, superconducting transition edge sensors (TESs), or metallic magnetic calorimeters (MMCs) Enss (2005).

The AMoRE (Advanced Mo-based Rare process Experiment) project is an experiment to search for of Mo Bhang et al. (2012). AMoRE uses CaMoO crystals as the absorber and MMCs as the sensor Lee et al. (2011); Kim et al. (2014). CaMoO is a scintillating crystal that has the highest light output at room and low temperatures among Mo-containing crystals (molybdates) Kim et al. (2010); Pirro et al. (2006).

Choosing of Mo as the source of is advantageous. The nucleus has a high Q value of 3034.40(17) keV Rahaman et al. (2008) that is above the intensive 2615 keV gamma quanta from Tl decay (Th family). The natural abundance of Mo is 9.8% Wieser and Laeter (2007), which is comparatively high. Furthermore, enriched Mo can be produced by centrifugation method in amount of tens of kilograms per year with a reasonable price. Also, the theoretically estimated half life of Mo is relatively shorter than that of other candidates Barea et al. (2012); Vergados et al. (2012). However, of Ca with keV (despite rather low concentration of the isotope ) can be an irremovable background source in the ROI of Mo. The AMoRE collaboration has successfully grown CaMoO crystals using Mo enriched and Ca depleted materials. Three of the doubly-enriched crystals with masses in the range of 0.2-0.4 kg were tested in a low background 4 veto system to determine their internal backgrounds So et al. (2012).

The present experimental work aims to test the low temperature detection concept with a CaMoO crystal and an MMC that is suitable for a high resolution experiment to search for of Mo. A 216 g natural CaMoO crystal with an MMC phonon sensor was employed in this experiment, which was performed in an over-ground measurement facility. The energy resolution and linearity of the detector setup, particle and randomly coinciding events discrimination by pulse shape analysis for background rejection in a experiment are discussed in this report.

Ii Experimental Details

Figure 2: (Color online) A typical signal of 2.6 MeV gamma-ray full absorption events at 40 mK in DC (blue, bigger) and AC (red, smaller) coupling.

The detector setup was structured in a cylindrical shape with copper support details as shown in Fig. 1. A CaMoO crystal with 4 cm in diameter and 4 cm height was mounted inside the copper structure using metal springs. The mass of the crystal was 216 g. It was grown with natural Ca and Mo elements at the Bogoroditsk plant in Russia. A patterned gold film was evaporated on one side of the crystal to serve as a phonon collector. An MMC device, the primary sensor for detecting the phonon signals absorbed in the gold film, was placed on a semi-circular copper plate over the crystal. The thermal connection between the gold film and the MMC was made using annealed gold wires. Details regarding the measurement principle and the detector structure of the MMC device were presented in previous reports Yoon et al. (2012, 2014).

When a particle hits a dielectric material, most of the energy deposited into the absorber is converted into the form of phonons. High energy phonons with frequencies that are close to the Debye frequency are generated initially. However, they quickly decay to lower frequency phonons via anharmonic processes. When their energy becomes 20-50 K, they can travel ballistically in the crystal Wolfe (2005). The major down-conversion processes of these athermal phonons are isotope scattering, inelastic scatterings by impurities and lattice dislocations, and inelastic scatterings at crystal surfaces Leman (2012). These excess phonons eventually change the equilibrium thermal phonon distribution, thereby causing temperature increase.

In the detector setup with the CaMoO crystal and the gold phonon collector film, the ballistic athermal phonons can hit the crystal and gold interface, transmit into the gold film, and transfer their energy to the electrons in the film Kim et al. (2004). The electron temperature of the gold film increases quickly via electron-electron scatterings. This temperature change is measured by the MMC sensor that is thermally connected with the gold wires. The size of the gold film and number of gold wires were chosen based on a thermal model study that considered the efficient athermal heat flow process Kim et al. (2014). Consequently the gold film had a diameter of 2 cm, a thickness of 200 nm, and an additional gold pattern of 200 nm thickness on top of the gold film. to increase the lateral thermal conductivity of the gold film.

The detector assembly was installed in a dilution refrigerator in an over-ground laboratory at KRISS (Korea Research Institute of Standards and Science). The refrigerator was surrounded by a 10 cm thick lead shield (except the top surface) to reduce environmental gamma ray background.

Figure 3: A scatter plot of the mean-time and pulse height obtained from the background measurement of 95 h in an over-ground laboratory. and (including cosmic muons) events are clearly separated in terms of their mean-time values.

The detector with an MMC operates well in the temperature range of 10-50 mK. The signal size increases at lower temperatures since the MMC sensitivity enhanced and the heat capacities decreased. However, the signals have slower rise and decay times at lower temperatures as thermal conductances become poorer. Larger signal size improves the energy threshold and baseline energy resolution of the detector. The energy resolution of the detector measured for particle absorption events can be worse than the baseline resolution because of any uncorrelated mechanism that affects the signal size and shape. Examples of such mechanisms include temperature fluctuations due to instrumental instability or frequent event rates, position dependence of signal shapes, or scintillation processes that are associates with phonon generations in an inhomogeneous way. Therefore, larger signal size does not guarantee a better energy resolution at certain temperatures. At the present experimental condition including the background rate from cosmic muons and external gamma-rays, 40 mK was selected as the main measurement temperature. At this temperature, about 1 ms rise-time was obtained for the 2.6 MeV gamma line without degrading the energy resolution. A typical signal of 2.6 MeV gamma-ray full absorption events is shown in Fig. 2. The rise-time of the DC coupled signal is 1.1 ms, which is somewhat slower than that of earlier measurements for which shorter gold wires were used Kim et al. (2014).

Iii Pulse Shape Analysis

Figure 4: Distribution of mean-time parameter in 4 MeV 5 MeV region of alpha-equivalent energy. Discrimination power was found to be 7.6 from fiting each group of distribution with a normal Gaussian function. Right-hand side tail is noticeable for the two groups toward higher mean-time value.

A two dimensional scatter plot of the pulse heights and mean-times of signals obtained in a 95 h background measurement is shown in Fig. 3. The pulse height is the difference between the maximum value and baseline level of a signal. The maximum value is found using a quadratic polynomial fit to the region of the signal near the pulse maximum. The baseline level is the average voltage value in the time region before the signal rises. The mean-time parameter is defined as

(5)

where is the measured voltage value at time subtracting the baseline level, is the time when it reaches 10% of the pulse height, and and indicate the time length of the signal toward left and right directions from , respectively, to calculate the mean-time. is set to reach the time at the baseline level, while is a free parameter that was selected to achieve the most efficient particle discrimination. Here, the value was set to not include the negative part of an AC coupled signal (see Fig. 2), which was used for the energy spectrum because it was recorded with finer digitizer resolution (i.e., bigger gain is used) than the DC coupled signal.

Figure 5: (Color online) Averaged pulse shapes of induced signals from Th decays (blue) and the corresponding (i.e., with the same pulse height) muon-induced signals (red). The signals are normalized for their pulse height, and shifted in time to align the maximum point of signals.

The pulse-shape discrimination (PSD) between and particles can be realized with the mean-time as a pulse shape parameter due to the difference in the rise and decay times of the two types of events. A similar tendency of PSD was reported for other low temperature scintillating detectors Arnaboldi et al. (2011). The separation into two groups of the events in the energy region between 4 and 5 MeV of alpha-equivalent energy can be readily observed from the distribution of mean-time values shown in Fig. 4. The energy of induced events was determined as described in the following section. Although the two peaks have noticeable right-hand tails toward higher mean-time values, normal Gaussian functions were used to fit the distributions. We interpret the right-hand tails as a result of signal pile-up. A parameter of discrimination power () is defined as

(6)

where are the mean values, are the standard deviations of the Gaussian distributions for and events. DP was found to be 7.6.

The averaged pulse shapes for the two groups of events are compared in Fig. 5. Templates of events were obtained by averaging out the Th -decay events pulse profiles with energy release in the crystal 4082 keV (due to the contamination of the crystal by thorium), whereas the events caused by cosmic muons with the same pulse height were selected for the template of induced events. The normalized pulses of alpha and beta templates are aligned at the time of their maximum values, as shown in Fig. 5. Both the rise and decay times of the and signals are clearly different. The signals induced by events have faster rise and faster decay than those of the events.

Figure 6: Energy spectrum measured with an external source over 65 h.

According to scintillation measurements of a CaMoO crystal at 7-300 K Mikhailik et al. (2007); Mikhailik and Kraus (2010), the scintillation decay-time of the CaMoO crystal reaches hundreds of s at 7 K. The crystal also shows different light output for and events Annenkov et al. (2008). A slowly decaying scintillation mechanism would cause slow generation of phonon in the CaMoO crystal. and particle events may have different fractions of slow component for phonon generation. This difference in slow phonon generation at mK temperatures may induce different pulse shapes for and particle events.

Iv Energy spectrum

Because athermal phonon absorption in the phonon collector significantly contributes to the signal size Kim et al. (2014), the signals have some degrees of position dependence for their pulse height and shape. In this detector, the signals with faster rise-times show bigger pulse heights for the same energy events. This effect can be observed in Fig. 3. The distribution of mean-time values and pulse heights for alpha and gamma-ray full absorption lines has anti-correlated slopes. This negative slope more dominantly appears in the alpha signals, which is likely because the full-energy peaks originate from multiple Compton scatterings in the crystal that smear the position dependence on the event location. The pulse height is not an optimal parameter to obtain a high resolution. In the optimal filtering method Yuryev et al. (2011) that is often adopted in high resolution micro-calorimeters, the signals are assumed to have one shape but with different amplitudes. Thus, the optimal filtering method is not applicable to provide a high resolution spectrum for the present signals.

Figure 7: (Color online) Ratio of signal amplitude () and energy in linear calibration for (circle, blue) and (triangle, red) peaks (upper). Quadratic calibration lines (dotted and dashed lines) are shown for and peaks, respectively. Deviations of the ratios from each quadratic functions are shown in the lower figure.

In the present analysis, a new parameter, (left area) was used as an amplitude parameter to reduce the position dependence effect of the large crystal detector. It is defined as

(7)

where the variables are as defined in Eq. 5. is a partial integration for the leading part of a signal. Because the integration range of the parameter is set by a shape-dependent parameter, the mean-time, this parameter is less influenced by the pulse shape. For instance, the correlation coefficient between the pulse height and mean-time was 0.62 for 4082 keV signals, but it was 0.08 between the and mean-time.

In a calibration run, a thoriated tungsten rod was used as an external gamma-ray source. The source was placed in the gap between the cryostat and the lead shield.

When a linear energy calibration was applied to gamma-ray peaks, deviations from the linear calibration of less than 0.4% were found for low-energy peaks. A quadratic function with no constant term was used for the calibration of electron-equivalent energy for 511, 583, 911 and 2615 keV peaks for the spectrum shown in Fig. 6. The corresponding energy resolutions of the peaks are listed in Table 1.

Fig. 7 shows the linearities of the electron and alpha signals. The values of the electron and alpha peaks divided by the linear calibration of the gamma-ray peaks are plotted in the upper figure. The /energy ratios for the alpha peaks are about 6% larger than those for the gamma-ray peaks. The quadratic fit functions are shown as dotted and dashed lines for gamma and alpha peaks, respectively. The residuals in the lower figure indicate deviations from the quadratic functions for the two groups. With the quadratic calibration, a very small deviation is expected near 3 MeV for electron measurements. It implies that this method can supply an accurate energy calibration at the value of the of Mo.

Figure 8: Energy spectrum of bulk alpha events in a background measurement.
Energy (keV) FWHM (keV)
511 7.2 0.6
583 6.5 0.5
911 6.8 0.3
2615 10.9 0.4
Table 1: Energy resolutions of gamma-ray full absorption peaks in the calibration measurement.

Alpha events can be separated from events using the mean-time parameter. The energy spectrum of alpha events is shown in Fig. 8. An energy calibration for this spectrum was performed with a quadratic function for the alpha peaks as discussed above. These background were bulk events of alpha decays in the crystal, mainly from radionuclides of U and Th decay chains, most of them are identified as shown in Fig. 8. Because this crystal was developed to investigate the scintillation properties of CaMoO, its internal background was not exceptionally low. The AMoRE collaboration has developed CaMoO growing technology with low radio-impurities. Internal alpha activities of about 80 Bq/kg of Ra and 70 Bq/kg of Th were found in a 196 g CaMoO So et al. (2012).

Not only alpha signals can be rejected efficiently, but also decays of Bi, Bi and Tl can be tagged and eliminated from the data by using information about associated alpha-emitting nuclides. Random pile-ups of events (first of all from the ) could be a substantial source of background of LTD to search for due to the poor time resolution Chernyak et al. (2012). Relatively fast response of the MMC among the LTDs is a certain advantage to discriminate the background.

V Conclusion

LTDs made of crystal scintillators containing isotopes of interest have distinct advantages in searches. Such LTDs make it possible to provide a high detection efficiency to the . Taking the advantage of high resolution sensor technologies, these dielectric detectors in the heat (phonon) measurement can have comparable energy resolution to those of HPGe detectors. The comparison in heat/light measurement channels makes unambiguous separation of alpha events from electron events. As discussed in this report, pulse shape discrimination is also possible using only the phonon measurement. This PSD capability of the phonon sensor increases discrimination power for alpha background signals, or can simplify the detector cell design by using only one phonon sensor without a photon sensor that is commonly used for particle discrimination Artusa et al. (2014), and will reduce the number of measurement channels.

In comparison with signals from PMTs or conventional semiconductor detectors, phonon signals from a crystal detector in the LTD concept are typically slow. Even though the energy resolution of these detectors does not suffer from the slow signal in the low activity environment of an underground experiment, random coincidence of events lead to an unavoidable background because of the slow rise-time Chernyak et al. (2012). Two consecutive electron events that occur in a time interval that is much shorter than the signal rise-time can be regarded as a single event. Such randomly coincident events, particularly of , are an unavoidable source of backgrounds in the taking into account that the event rate of Mo is expected to be about 10 mBq in 1 kg CaMoO.

In the present experiment, the phonon signals had rise-times of 1.1 ms, which is much faster than the rise-times of LTDs with NTD Ge thermistors. The fast rise-time provides efficient rejection possibility for randomly coincident events Chernyak et al. (2014). Moreover, a photon detector composed of a 2 inch Ge wafer and an MMC sensor showed a temperature independent rise-time of about 0.2 ms with reasonable energy resolution Lee et al. (2015). Simultaneous measurements with the photon detector will increase the discrimination power not just for alpha events but also for randomly coincident events.

For the AMoRE project, CaMoO crystals will be used as the detector material together with MMCs in phonon and photon measurement setups. We aim to reach a zero background with improved energy resolution of a few keV. The first stage experiment is expected to be constructed with a 10 kg prototype detector by 2016. We plan to perform a large scale experiment with 200 kg CaMoO crystals in the next 5-6 years. The sensitivity of the experiment to the effective Majorana neutrino mass is estimated to be in the range of 20-50 meV, which corresponds to the inverted scheme of the neutrino mass.

Conflict of Interests

The authors declare that there is no conflict of interests regarding the publication of this paper.

Acknowledgment

This research was funded by Grant No. IBS-R016-G1, and partly supported by the National Research Foundation of Korea Grant funded by the Korean Government (NRF-2011-220-C00006, and NRF-2013K2A5A3000039). F.A. Danevich was supported in part by the Space Research Program of the National Academy of Sciences of Ukraine.

References

  • Beringer et al. (2012) J. Beringer, J. F. Arguin, R. M. Barnett, K. Copic, O. Dahl, D. E. Groom, C. J. Lin, J. Lys, H. Murayama, C. G. Wohl, et al. (Particle Data Group), Phys. Rev. D 86, 010001 (2012).
  • Mohapatra et al. (2007) R. N. Mohapatra, S. Antusch, K. S. Babu, G. Barenboim, M.-C. Chen, A. de Gouvêa, P. de Holanda, B. Dutta, Y. Grossman, A. Joshipura, et al., Rep. Prog. Phys. 70, 1757 (2007).
  • Elliott and Vogel (2002) S. R. Elliott and P. Vogel, Annu. Rev. Nucl. Part. Sci. 52, 115 (2002).
  • Avignone et al. (2008) F. T. Avignone, S. R. Elliott, and J. Engel, Rev. Mod. Phys. 80, 481 (2008).
  • Rodejohann (2011) W. Rodejohann, Int. J. Mod. Phys. A 20, 1833 (2011).
  • Giuliani and Poves (2012) A. Giuliani and A. Poves, Adv. High Energy Phys. 2012 (2012).
  • Gómez-Cadenas et al. (2012) J. Gómez-Cadenas, J. Martín-Albo, M. Mezzetto, F. Monrabal, and M. Sorel, RIVISTA DEL NUOVO CIMENTO 35, 29 (2012).
  • Enss (2005) C. Enss, Cryogenic particle detection, vol. 99 (Springer, 2005).
  • Bhang et al. (2012) H. Bhang, R. S. Boiko, D. M. Chernyak, J. H. Choi, S. Choi, F. A. Danevich, K. V. Efendiev, C. Enss, A. Fleischmann, A. M. Gangapshev, et al., J. Phys. Conf. Ser. 375, 042023 (2012).
  • Lee et al. (2011) S. J. Lee, J. H. Choi, F. A. Danevich, Y. S. Jang, W. G. Kang, N. Khanbekov, H. J. Kim, I. H. Kim, S. C. Kim, S. K. Kim, et al., Astropart. Phys. 34, 732 (2011).
  • Kim et al. (2014) G. B. Kim, S. Choi, Y. S. Jang, H. J. Kim, Y. H. Kim, V. V. Kobychev, H. J. Lee, J. H. Lee, J. Y. Lee, M. K. Lee, et al., J. Low Temp. Phys. 176, 637 (2014).
  • Kim et al. (2010) H. J. Kim, A. N. Annenkov, R. S. Boiko, O. A. Buzanov, D. M. Chernyak, J. H. Cho, F. A. Danevich, A. E. Dossovitsky, G. Rooh, U. K. Kang, et al., IEEE trans. Nucl. Sci. 57, 1475 (2010).
  • Pirro et al. (2006) S. Pirro, J. Beeman, S. Capelli, M. Pavan, E. Previtali, and P. Gorla, Phys. At. Nucl. 69, 2109 (2006).
  • Rahaman et al. (2008) S. Rahaman, V.-V. Elomaa, T. Eronen, J. Hakala, A. Jokinen, J. Julin, A. Kankainen, A. Saastamoinen, J. Suhonen, C. Weber, et al., Phys. Lett. B 662, 111 (2008).
  • Wieser and Laeter (2007) M. E. Wieser and J. R. D. Laeter, Phys. Rev. C 75, 055802 (2007).
  • Barea et al. (2012) J. Barea, J. Kotila, and F. Iachello, Phys. Rev. Lett. 109, 042501 (2012).
  • Vergados et al. (2012) J. D. Vergados, H. Ejiri, and Fšimkovic, Rep. Prog. Phys. 75, 106301 (2012).
  • So et al. (2012) J. H. So, H. J. Kim, V. V. Alenkov, A. N. Annenkov, H. Bhang, R. S. Boiko, O. A. Buzanov, D. M. Chernyak, J. H. Choi, S. Choi, et al., IEEE trans. Nucl. Sci. 59, 2214 (2012).
  • Yoon et al. (2012) W. S. Yoon, Y. S. Jang, G. B. Kim, K. J. Kim, M. S. Kim, J. S. Lee, K. B. Lee, M. K. Lee, S. J. Lee, H. J. Lee, et al., J. Low Temp. Phys. 167, 280 (2012).
  • Yoon et al. (2014) W. S. Yoon, G. B. Kim, H. J. Lee, J. Y. Lee, J. H. Lee, Y. S. Jang, S. J. Lee, M. K. Lee, and Y. H. Kim, J. Low Temp. Phys. 176, 644 (2014).
  • Wolfe (2005) J. P. Wolfe, Imaging phonons: acoustic wave propagation in solids (Cambridge University Press, 2005).
  • Leman (2012) S. W. Leman, Rev. Sci. Instr. 83, 091101 (2012).
  • Kim et al. (2004) Y. H. Kim, H. Eguchi, C. Enss, Y. H. Huang, R. E. Lanou, H. J. Maris, A. N. Mocharnuk-Macchia, G. M. Seidel, B. Sethumadhavan, and W. Yao, Nucl. Instr. and Mech. A 520, 208 (2004).
  • Arnaboldi et al. (2011) C. Arnaboldi, C. Brofferio, O. Cremonesi, L. Gironi, M. Pavan, G. Pessina, S. Pirro, and E. Previtali, Astropart. Phys. 34, 797 (2011).
  • Mikhailik et al. (2007) V. B. Mikhailik, S. Henry, H. Kraus, and I. Solskii, Nucl. Instr. and Mech. A 583, 350 (2007).
  • Mikhailik and Kraus (2010) V. B. Mikhailik and H. Kraus, Phys. Status Solidi B 247, 1583 (2010).
  • Annenkov et al. (2008) A. N. Annenkov, O. A. Buzanov, F. A. Danevich, A. S. Georgadze, S. K. Kim, H. J. Kim, Y. D. Kim, V. V. Kobychev, V. N. Kornoukhov, M. Korzhik, et al., Nucl. Instr. and Mech. A 584, 334 (2008).
  • Yuryev et al. (2011) Y. N. Yuryev, Y. S. Jang, S. K. Kim, K. B. Lee, M. K. Lee, S. J. Lee, W. S. Yoon, and Y. H. Kim, Nucl. Instr. and Mech. A 635, 82 (2011).
  • Chernyak et al. (2012) D. M. Chernyak, F. A. Danevich, A. Giuliani, E. Olivieri, M. Tenconi, and V. I. Tretyak, Eur. Phys. J. C 72 (2012).
  • Artusa et al. (2014) D. Artusa, F. Avignone III, O. Azzolini, M. Balata, T. Banks, G. Bari, J. Beeman, F. Bellini, A. Bersani, M. Biassoni, et al., arXiv preprint arXiv:1404.4469 (2014).
  • Chernyak et al. (2014) D. M. Chernyak, F. A. Danevich, A. Giuliani, M. Mancuso, C. Nones, E. Olivieri, M. Tenconi, and V. I. Tretyak, Eur. Phys. J. C 74, 2913 (2014).
  • Lee et al. (2015) H. J. Lee, J. H. So, C. S. Kang, G. B. Kim, S. R. Kim, J. H. Lee, M. K. Lee, W. S. Yoon, and Y. H. Kim, Nucl. Instr. and Meth. A 784, 508 (2015).
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