Abstract

Sterile neutrinos are possible dark matter candidates. We examine here possible detection mechanisms, assuming that the neutrino has a mass of about 50 keV and couples to the ordinary neutrino. Even though this neutrino is quite heavy, it is nonrelativistic with a maximum kinetic energy of 0.1 eV. Thus new experimental techniques are required for its detection. We estimate the expected event rate in the following cases: (i) measuring electron recoil in the case of materials with very low electron binding; (ii) low temperature crystal bolometers; (iii) spin induced atomic excitations at very low temperatures, leading to a characteristic photon spectrum; (iv) observation of resonances in antineutrino absorption by a nucleus undergoing electron capture; (v) neutrino induced electron events beyond the end point energy of beta decaying systems, for example, in the tritium decay studied by KATRIN.

1. Introduction

There exists evidence for existence of dark matter in almost all scales, from the dwarf galaxies, galaxies, and cluster of galaxies, with the most important ones being the observed rotational curves in the galactic halos; see, for example, the review [1]. Furthermore cosmological observations have provided plenty of additional evidence, especially the recent WMAP [2] and Planck [3] data.

In spite of this plethora of evidence, it is clearly essential to directly detect such matter in the laboratory in order to unravel its nature. At present there exist many such candidates, called Weakly Interacting Massive Particles (WIMPs). Some examples are the LSP (Lightest Supersymmetric Particle) [4–11], technibaryon [12, 13], mirror matter [14, 15], and Kaluza-Klein models with universal extra dimensions [16, 17]. Among other things these models predict an interaction of dark matter with ordinary matter via the exchange of a scalar particle, which leads to a spin independent interaction (SI) or vector boson interaction and therefore to a spin dependent (SD) nucleon cross section.

Since the WIMPs are expected to be extremely nonrelativistic, with average kinetic energy , they are not likely to excite the nucleus, even if they are quite massive, . Therefore they can be directly detected mainly via the recoiling of a nucleus, first proposed more than 30 years ago [18]. There exists a plethora of direct dark matter experiments with the task of detecting WIMP event rates for a variety of targets such as those employed in XENON10 [19], XENON100 [20], XMASS [21], ZEPLIN [22], PANDA-X [23], LUX [24], CDMS [25], CoGENT [26], EDELWEISS [27], DAMA [28, 29], KIMS [30], and PICASSO [31, 32]. These consider dark matter candidates in the multi-GeV region.

Recently, however, an important dark matter particle candidate of the Fermion variety in the mass range of 10–100 keV, obtained from galactic observables, has arisen [33–35]. This scenario produces basically the same behavior in the power spectrum (down to Mpc scales) with that of standard CDM cosmologies, by providing the expected large-scale structure [36]. In addition, it is not too warm; that is, the masses involved are larger than = 1–3 keV to be in conflict with the current Ly forest constraints [37] and the number of Milky Way satellites [38], as in standard WDM cosmologies. In fact an interesting viable candidate has been suggested, namely, a sterile neutrino in the mass region of 48–300 keV [33–35, 39–43], but most likely around 50 keV. For a recent review, involving a wider range of masses, see the white paper [44].

The existence of light sterile neutrinos had already been introduced to explain some experimental anomalies like those claimed in the short baseline LSND and MiniBooNE experiments [45–47], the reactor neutrino deficit [48], and the Gallium anomaly [49, 50], with possible interpretations discussed, for example, in [51, 52] as well as in [53, 54] for sterile neutrinos in the keV region. The existence of light neutrinos can be expected in an extended see-saw mechanism involving a suitable neutrino mass matrix containing a number of neutrino singlets not all of which being very heavy. In such models it is not difficult to generate more than one sterile neutrino, which can couple to the standard neutrinos [55]. As it has already been mentioned, however, the explanation of cosmological observations requires sterile neutrinos in the 50 keV region, which can be achieved in various models [33, 56].

In the present paper we will examine possible direct detection possibilities for the direct detection of these sterile neutrinos. Even though these neutrinos are quite heavy, their detection is not easy. Since like all dark matters candidates move in our galaxies with no relativistic velocities, with average value about  c, and with energies about 0.05 eV, not all of them can be deposited in the detectors. Therefore the standard detection techniques employed in the standard dark matter experiments like those mentioned above are not applicable in this case. Furthermore, the size of the mixing parameter of sterile neutrinos with ordinary neutrinos is crucial for detecting sterile neutrinos. Thus our results concerning the expected event rates will be given in terms of this parameter.

The paper is organized as follows. In Section 2 we study the option on neutrino-electron scattering. In Section 3 we consider the case of low temperature bolometers. In Section 4 the possibility of neutrino induced atomic excitations is explored. In Section 5 we will consider the antineutrino absorption on nuclei, which normally undergo electron capture, and finally in Section 6 the modification of the end point electron energy in beta decay, for example, in the KATRIN experiment [57], is discussed. In Section 7, we summarize our conclusions.

2. The Neutrino-Electron Scattering

The sterile neutrino as dark matter candidate can be treated in the framework of the usual dark matter searches for light WIMPs except that its mass is very small. Its velocity follows a Maxwell-Boltzmann (MB) distribution with a characteristic velocity about  c. Since the sterile neutrino couples to the ordinary electron neutrino it can be detected in neutrino-electron scattering experiments with the advantage that the neutrino-electron cross section is very well known. Both the neutrino and the electron can be treated as nonrelativistic particles. Furthermore we will assume that the electrons are free, since the WIMP energy is not adequate to ionize an the atom. Thus the differential cross section is given by where is the square of the mixing of the sterile neutrino with the standard electron neutrino and , where denotes the Fermi weak coupling constant and is the Cabibbo angle [58]. The integration over the outgoing neutrino momentum is trivial due to the momentum function yielding where , is the WIMP velocity, and is the WIMP-electron reduced mass, . The electron energy is given by where is the maximum WIMP velocity (escape velocity). Integrating (2) over the angles, using the function for the integration we obtain

We are now in a position to fold the velocity distribution assuming it to be MB with respect to the galactic center: In the local frame, assuming that the sun moves around the center of the galaxy with velocity , , we obtain where is now the cosine of the angle between the WIMP velocity and the direction of the sun’s motion. Eventually we will need the flux so we multiply with the velocity before we integrate over the velocity. The limits of integration are between and . The velocity is given via (3); namely, We find it convenient to express the kinetic energy in units of . Then Thus These integrals can be done analytically to yieldwhere is the error function and is its complement. The function characterizes the spectrum of the emitted electrons and is exhibited in Figure 1 and it is without any particular structure, which is the case in most WIMP searches. For a 50 keV sterile neutrino we find that

Figure 1 

The shape of the spectrum of the emitted electrons in sterile neutrino-electron scattering.

Now . Thus where

It is clear that with this amount of energy transferred to the electron it is not possible to eject an electron out of the atom. One therefore must use special materials such that the electrons are loosely bound. It has recently been suggested that it is possible to detect even very light WIMPS, much lighter than the electron, utilizing Fermi-degenerate materials like superconductors [59]. In this case the energy required is essentially the gap energy of about , which is in the meV region; that is, the electrons are essentially free. In what follows, we assume the valueswhile is taken as a parameter and will be discussed in Section 7. Thus we obtainThe neutrino particle density is while the neutrino flux where , being the dark matter density. Assuming that the number of electron pairs in the target is we find that the number of events per year is

The authors of [59] are perhaps aware of the fact that the average energy for very light WIMPS is small and as we have seen above a small portion of it is transferred to their system. With their bolometer detector these authors probably have a way to circumvent the fact that a small amount of energy will be deposited, about 0.4 eV in a year for . Perhaps they may manage to accumulate a larger number of loosely bound electrons in their target.

3. Sterile Neutrino Detection via Low Temperature Bolometers

Another possibility is to use bolometers, like the CUORE detector exploiting Low Temperature Specific Heat of Crystalline at low temperatures. The energy of the WIMP will now be deposited in the crystal, after its interaction with the nuclei via Z-exchange. In this case the Fermi component of interaction with neutrons is coherent, while that of the protons is negligible. Thus the matrix element becomes

A detailed analysis of the frequencies of can be found [60]. The analysis involved crystalline phases of tellurium dioxide: paratellurite -, tellurite , and the new phase -TeO2, recently identified experimentally. Calculated Raman and IR spectra are in good agreement with available experimental data. The vibrational spectra of and - can be interpreted in terms of vibrations of molecular units. The - modes are associated with the symmetry or 422, which has 5 irreducible representations, two 1-dimensional representations of the antisymmetric type indicated by and , two 1-dimensional representations of the symmetric types and , and one 2-dimensional representation, usually indicated by . They all have been tabulated in [60]. Those that can be excited must be below the Debye frequency which has been determined [61] and found to be quite low: This frequency is smaller than the maximum sterile neutrino energy estimated to be  eV. Those frequency modes of interest to us are given in Table 1. The differential cross section is, therefore, given bywhere will be specified below and is the momentum transferred to the nucleus. The momentum transfer is small and the form factor can be neglected.

In deriving this formula we tacitly assumed a coherent interaction between the WIMP and several nuclei, thus creating a collective excitation of the crystal, that is, a phonon or few phonons. This of course is a good approximation provided that the energy transferred is small, of a few tens of meV. We see from Table 1 that the maximum allowed energy is small, around 100 meV. We find that, if we restrict the maximum allowed energy by a factor of 2, the obtained results are reduced only by a factor of about . We may thus assume that this approximation is good.

Integrating over the nuclear momentum we get performing the integration using the function we get where

Folding with the velocity distribution we obtain We see that we have the constraint imposed by the available energy; namely,where integer part of . We thus find listed in Table 1. The functions are exhibited in Figure 2. The relevant integrals are for , , for , , for , and for . Thus we obtain a total of 17.8. The event rate takes with a target of mass which takes the form If we restrict the maximum allowed energy to half of that shown in Table 1 by a factor of two, we obtain 15.7 instead of 17.8.

(a)

(b)

(a)
(b)

Figure 2 

(a) The function , exhibited as a function of , associated with the mode   for increasing downwards. (b) The functions associated with   for and for  , , and for  , , exhibited as a function of , for thick solid, solid, dashed, and dotted lines, respectively. For definitions see text.

For a target () of 1 kg of mass get This is much larger than that obtained in the previous section, mainly due to the neutron coherence arising from the Z-interaction with the target (the number of scattering centers is approximately the same, . In the present case, however, targets can be larger than 1 kg. Next we are going to examine other mechanisms, which promise a better signature.

4. Sterile Neutrino Detection via Atomic Excitations

We are going to examine the interesting possibility of excitation of an atom from a level to a nearby level at energy , which has the same orbital structure. The excitation energy has to be quite low; that is, The target is selected so that the two levels and are closer than 0.11 eV. This can result from the splitting of an atomic level by the magnetic field so that they can be connected by the spin operator. The lower one is occupied by electrons but the higher one is completely empty at sufficiently low temperature. It can be populated only by exciting an electron to it from the lower one by the oncoming sterile neutrino. The presence of such an excitation is monitored by a tuned laser which excites such an electron from to a higher state , which cannot be reached in any other way, by observing its subsequent decay by emitting photons.

Since this is a one-body transition the relevant matrix element takes the form (in the case of the axial current we have and we need evaluate the matrix element of and then square it and sum and average over the neutrino polarization). expressed in terms of the Clebsch-Gordan coefficient and the nine-j symbol. It is clear that in the energy transfer of interest only the axial current can contribute to excitation.

The cross section takes the form Integrating over the atom recoil momentum, which has negligible effect on the energy, and over the direction of the final neutrino momentum and energy via the function we obtain where we have set .

Folding the cross section with the velocity distribution from a minimum to we obtain Clearly the maximum excitation energy that can be reached is  eV. The function is exhibited in Figure 3.

Figure 3 

The function for sterile neutrino scattering by an atom as a function of the excitation energy in eV.

Proceeding as in Section 2 and noting that for small excitation energy we findThe expected rate will be smaller after the angular momentum factor is included (see Appendix A). Anyway, leaving aside this factor, which can only be determined after a specific set of levels is selected, we see that the obtained rate is comparable to that expected from electron recoil (see (18)). In fact for a target with we obtain This rate, however, decreases as the excitation energy increases (see Figure 3). In the present case, however, we have two advantages. (i)The characteristic signature of photons spectrum is following the deexcitation of the level mentioned above. The photon energy can be changed if the target is put in a magnetic field by a judicious choice of .(ii)The target now can be much larger, since one can employ a solid at very low temperatures. The ions of the crystal still exhibit atomic structure. The electronic states probably will not carry all the important quantum numbers as their corresponding neutral atoms. One may have to consider exotic atoms (see Appendix B) or targets which contain appropriate impurity atoms in a host crystal, for example, chromium in sapphire.

In spite of this it seems very hard to detect such a process, since the expected counting rate is very low.

5. Sterile Neutrino Capture by a Nucleus Undergoing Electron Capture

This is essentially the process: involving the absorption of a neutrino with the simultaneous capture of a bound electron. It has already been studied [62] in connection with the detection of the standard relic neutrinos. It involves modern technological innovations like the Penning Trap Mass Spectrometry (PT-MS) and the Microcalorimetry (MC). The former should provide an answer to the question of accurately measuring the nuclear binding energies and how strong the resonance enhancement is expected, whereas the latter should analyze the bolometric spectrum in the tail of the peak corresponding to L-capture to the excited state in order to observe the relic antineutrino events. They also examined the suitability of ¹⁵⁷Tb for relic antineutrino detection via the resonant enhancement to be considered by the PT-MS and MC teams. In the present case the experimental constraints are expected to be less stringent since the sterile neutrino is much heavier.

Let us measure all energies from the ground state of the final nucleus and assume that is the mass difference of the two neutral atoms. Let us consider a transition to the final state with energy . The cross section for a neutrino (here as well as in the following we may write neutrino, but it is understood that we mean antineutrino) of given velocity and kinetic energy is given by where is the recoiling nucleus momentum. Integrating over the recoil momentum using the function we obtain We note that since the oncoming neutrino has a mass, the excited state must be higher than the highest excited state at . With indicating by the above equation can be written as Folding it with the velocity distribution as above we obtain or using the delta functionAs expected the cross section exhibits resonance behavior though the normalized function as shown in Figure 4. It is, of course, more practical to exhibit the function as a function of the energy ϵ. This is exhibited in Figure 5. From this figure we see that the cross section resonance is quite narrow. We find that the maximum occurs at 50 keV + 0.014 eV and has a width 0.04 eV. So for all practical purposes it is a line centered at the neutrino mass. The width may be of some relevance in the special case whereby the excited state can be determined by atomic deexcitations at the sub-eV level, but it will not show up in the nuclear deexcitations.