Direct Detection Signals from Absorption of Fermionic Dark Matter

TL;DR

This paper introduces a new class of direct detection signals involving the absorption of fermionic dark matter, exploring their theoretical operators, detection prospects, and experimental constraints.

Contribution

It identifies the operators responsible for fermionic dark matter absorption and demonstrates the potential for detection in current and future experiments despite the dark matter's inherent instability.

Findings

Fermionic dark matter absorption signals can be detected in existing experiments.

Operators up to dimension six enable fermionic absorption detection.

Current experiments can probe unexplored parameter space for sub-GeV dark matter.

Abstract

We present a new class of direct detection signals; absorption of fermionic dark matter. We enumerate the operators through dimension six which lead to fermionic absorption, study their direct detection prospects, and summarize additional constraints on their suppression scale. Such dark matter is inherently unstable as there is no symmetry which prevents dark matter decays. Nevertheless, we show that fermionic dark matter absorption can be observed in direct detection and neutrino experiments while ensuring consistency with the observed dark matter abundance and required lifetime. For dark matter masses well below the GeV scale, dedicated searches for these signals at current and future experiments can probe orders of magnitude of unexplored parameter space.

Figures

Equations

$${\mathcal{O}}_{\text{NC}}=\frac{1}{{\Lambda }^2}\bar{\chi }{\gamma }_{\mu }{P}_R\nu \left(\bar{n}{\gamma }^{\mu }n+\bar{p}{\gamma }^{\mu }p\right)+\text{h.c.}.$$

$$q\simeq m_{\chi },E_R\simeq \frac{m_{\chi }^2}{2M},$$

$$\frac{dR}{d{E}_R}$$

$$R=\frac{{\rho }_{\chi }}{m_{\chi }}{\sigma }_{\text{NC}}\sum _j{N}_{T,j}{A}_j^2{F}_j^2\Theta (E_{R,j}^0-E_{\mathrm{th}}),$$

$${\Gamma }_{\chi \to \nu \gamma \gamma \gamma }$$

$${\mathcal{O}}_{\text{CC}}=\frac{1}{{\Lambda }^2}\left[\bar{\chi }{\gamma }^{\mu }e\right]\left[\bar{n}{\gamma }_{\mu }p\right]+\text{h.c.}.$$

$$m_{\chi }>m_{\text{th}}^{\beta }\equiv M_{A,Z+1}^{(\ast )}+m_e-M_{A,Z}.$$

$$\displaystyle E_{R}\simeq\left\{\begin{array}[]{lr}m_{\chi}-m_{\text{th}}^{\beta}&{\rm(electron)}\\ \big{(}m_{\chi}-m_{\text{th}}^{\beta}\big{)}^{2}/2M_{A,Z+1}^{(*)}&{\rm(nucleus)}\end{array}\right.\,.$$

$$R$$

$$⟨\sigma v{⟩}_j=\frac{|{\vec{p}}_e{|}_j}{16\pi m_{\chi }{M}_{A_j,Z_j}^2}\overline{|{\mathcal{M}}_{N_j}{|}^2},$$

$${\mathcal{M}}_N=\sqrt{\mathcal{F}(Z+1,E_e)}{F}_V(q^2)\mathcal{M}.$$

$$R$$

Full text

The search for dark matter (DM) is rapidly expanding both theoretically and experimentally. Weakly interacting massive particle (WIMP) DM searches have pushed the limit on the WIMP-nucleon cross-section near the neutrino floor for masses around the weak scale Tan et al. (2016); Akerib et al. (2017); Aprile et al. (2017). These null results have sparked a renaissance in DM model building, in search of alternative thermal histories which predict lighter DM Griest and Seckel (1991); Pospelov et al. (2008); Hochberg et al. (2014, 2015); Kuflik et al. (2016); Carlson et al. (1992); Pappadopulo et al. (2016); Farina et al. (2016); Dror et al. (2016, 2018). For masses below the GeV scale, DM which scatters off a target will typically deposit energy below the threshold of the largest direct detection experiments (${\cal O}({\rm keV})$), significantly relaxing the direct constraints.

To discover these lighter DM candidates, the direct detection program is moving toward detecting smaller energy deposits with novel scattering targets and lower-threshold detectors Essig et al. (2012a); Graham et al. (2012); Essig et al. (2012b, 2016); Hochberg et al. (2017); Derenzo et al. (2017); Essig et al. (2017); Budnik et al. (2018); Cavoto et al. (2018); Kurinsky et al. (2019). Current technology is already sensitive to energy deposits of $\mathcal{O}\left(\rm eV\right)$ Abramoff et al. (2019) and new proposals could detect energy deposits of $\mathcal{O}\left(\rm meV\right)$ Hochberg et al. (2016a, b, c); Schutz and Zurek (2016); Knapen et al. (2017); Hochberg et al. (2018); Knapen et al. (2018); Griffin et al. (2018). As the direct detection program pushes the low-mass frontier, it can also broaden its searches for different signals to increase its impact with little additional cost.

Particle DM detection strategies can be grouped into two classes: scattering and absorption. Searches for scattering look for a DM particle depositing its kinetic energy onto a target within the detector, typically a nucleus or an electron. In contrast, searches for absorption look for signals in which a DM particle deposits its mass energy. Absorption signals have primarily been considered for bosonic DM candidates with studies of fermionic absorption signals limited to induced proton-to-neutron conversion in Super-Kamiokande Kile and Soni (2009) and sterile neutrino DM Bezrukov and Shaposhnikov (2007); Ando and Kusenko (2010); Liao (2010); Li and Xing (2011); de Vega et al. (2013); Long et al. (2014); Campos and Rodejohann (2016); Lasserre et al. (2016) (see also exothermic DM Graham et al. (2010) and self-destructing DM Grossman et al. (2017) for related signals).

In this Letter, we systematically study direct detection signals from the absorption of fermionic DM. We describe novel signals and their corresponding lowest-dimension operators; project the sensitivities of ongoing and proposed DM direct detection and neutrino experiments to these signals; and demonstrate the consistency of these signals with the issues of DM stability and abundance.

Signals and operators.

For simplicity, we take DM ($\chi$) to be a Dirac fermion charged under lepton number, and impose only Lorentz, ${\rm SU(3)}_{C}\times{\rm U(1)}_{{\rm EM}}$, CP, lepton and baryon number symmetries. Baryon number conservation is necessary to avoid proton decays while lepton number allows the (Dirac) neutrino to remain light. We enumerate operators in the effective theory with the fields $\left\{\chi,n,p,e,\nu,F_{\mu\nu}\right\}$, where $F_{\mu\nu}$ is the EM field strength tensor. We do not include other QCD resonances as they have no bearing on direct detection.

Consider first dimension-6 operators of the form, $\left[\bar{\chi}\Gamma_{i}\nu\right]\left[\bar{\psi}\Gamma_{j}\psi\right]$, where $\psi\supset\{n,p,e,\nu\}$ and $\Gamma_{i}=\left\{{\mathbf{1}},\gamma_{5},\gamma_{\mu},\gamma_{\mu}\gamma_{5},\sigma_{\mu\nu}\right\}$ denotes the different possible Lorentz structures of the bilinear. These “neutral current” operators generate the first class of new signals we consider; $\overset{\textbf{(---)}}{\chi}+{T}\rightarrow\overset{\textbf{(---)}}{\nu}+{T}$, where $T$ is a target nucleus or electron which absorbs a fraction of the DM mass energy. We will focus on nuclear absorption, where the rates may be coherently enhanced, and postpone the study of electron absorption Dror et al. (2019).

Next, consider dimension-6 operators of the form, $\left[\bar{\chi}\Gamma_{i}e\right]\left[\bar{n}\Gamma_{j}p\right]$. These generate a class of “charged current” signals; $\overset{\textbf{(---)}}{\chi}+\isotope[A][Z]{X}\rightarrow e^{\pm}+\isotope[A][Z\mp 1]{X}_{*}^{\mp}$, in which DM can induce $\beta^{\pm}$ decay in nuclei which are stable in vacuum. This process potentially has multiple correlated signals: a detectable $e^{\pm}$, a nuclear recoil, a prompt $\gamma$ decay from the excited final nucleus, and further nuclear decays if the final nucleus is unstable. Induced $\beta^{+}$ decays have significantly smaller rates relative to $\beta^{-}$ due to the Coulomb repulsion between the emitted $e^{+}$ and the nucleus, so we focus on DM-induced $\beta^{-}$ decays and leave the $\beta^{+}$ decays for future work Dror et al. (2020) 111$\beta^{+}$ decays induced by DM with $m_{\chi}\gg~{}{\rm MeV}$ were proposed for Hydrogen targets in Super-Kamiokande Kile and Soni (2009).. The same charged current operators can also shift the endpoint of the $\beta^{\pm}$ distribution for nuclei which already undergo $\beta^{\pm}$ decays in vacuum. While this might be detectable at PTOLEMY Betts et al. (2013); Baracchini et al. (2018), these kind of experiments have small exposures and large backgrounds, so we defer their study Dror et al. (2020).

Finally, DM candidates which have fermionic absorption signals decay. At dimension-5, the operator $\bar{\chi}\sigma^{\mu\nu}\nu F_{\mu\nu}$ induces decays of $\chi$ as do the dimension-6 operators, $\bar{\chi}\gamma^{\nu}\Gamma_{(5)}\partial^{\mu}\nu F_{\mu\nu}$, where $\Gamma_{(5)}\equiv\left\{{\mathbf{1}},\gamma_{5}\right\}$. At higher dimensions, there exist operators allowing multiphoton decays. The single photon channel can be detected with the usual line search, while the multiphoton channels are constrained by diffuse photon emission. Detectable fermionic absorption signals, consistent with indirect detection bounds, typically require lighter dark matter as the decay rates scale with a large power of $m_{\chi}$. We include a discussion of decays below for each signal and operator we consider.

Neutral current signals: nuclear recoils

We first study the process $\rm\chi+N\to\nu+N$, where N is a target nucleus. We will focus on two operators:

[TABLE]

We choose this Lorentz structure for concreteness. However, the neutral current signal is not highly dependent on it as long as there is some amount of vector coupling to the nucleons. These can arise from a theory of a heavy $Z^{\prime}$ coupled to quarks and $\chi$ with some mixing between the right handed components of $\chi$ and $\nu$. The incoming $\chi$ is non-relativistic, so its mass dominates its energy resulting in a momentum transfer ($q$) and nuclear recoil energy ($E_{R}$):

[TABLE]

where $M$ is the mass of the nucleus. For contrast, elastic scattering off a nucleus yields at most $E_{R}=2v^{2}\mu^{2}/M,$ where $\mu$ is the reduced mass and $v$ is the DM velocity (see Lin (2019) for a recent review). This $1/v^{2}$ increase in $E_{R}$ relative to WIMP scattering allows searches for lighter DM with both direct detection experiments and higher-threshold, neutrino experiments.

The differential rate of neutral current nuclear recoils from absorbing fermionic DM is;

[TABLE]

where $N_{T}$ is the number of target nuclei, $\rm\rho_{\chi}\simeq 0.4\,GeV/cm^{3}$ is the local DM energy density, $E_{R}^{0}\equiv m_{\chi}^{2}/2M$, $E_{{\rm th}}$ is the experiment’s threshold, and $\overline{\left|{\cal M}_{N}\right|^{2}}$ is the matrix element squared (at $q$) averaged over initial spins and summed over final spins. In elastic scattering, the spread in incoming DM velocities causes a spread in recoil energies, but in fermionic absorption, the rate is sharply peaked at $E_{R}=E_{R}^{0}$. Every isotope in an experiment has a distinct peak with width ($\Delta E_{R}$) determined by higher order corrections to Eq. (2), corresponding to $\Delta E_{R}/E_{R}\sim 10^{-3}$. There are no modulation signals or rate uncertainties arising from the DM velocity distribution.

The total rate for absorption by multiple nuclei is

[TABLE]

where $N_{T,j}$, $A_{j}$, $E_{R,j}^{0}$, and $F_{j}$, are the number, mass number, recoil energy, and Helm form factor Lewin and Smith (1996) (evaluated at $q=m_{\chi}$ and normalized to 1) of target isotope $j$. The cross section per-nucleon is $\sigma_{\text{NC}}=m_{\chi}^{2}/\left(4\pi\Lambda^{4}\right)$. Absorption has the unique signature of correlated, peaked counts in $dR/dE_{R}$ bins containing $E_{R,j}^{0}=m_{\chi}^{2}/\left(2M_{j}\right)$ for the different target isotopes with masses $M_{j}$. This can be a powerful discriminator from backgrounds since the relative heights and spacing of the peaks is completely determined. Whether an experiment can resolve these distinct peaks depends on its energy resolution and the mass splitting between the target isotopes.

For $m_{\chi}\lesssim~{}{\rm MeV}$, future experiments are necessary to probe the small nuclear recoil energy. Detailed projections are challenging due to the breadth of proposals and possible absorption by collective modes of nuclei. So, we roughly estimate the sensitivity of such future detectors in Fig. 1 (Left) where, for simplicity, we require at least 10 events to set our projections, independent of mass or experiment. The cross sections are smaller than those in typical WIMP searches due to the larger number densities of lighter DM. We consider Hydrogen and Lithium targets with energy thresholds of ${\rm eV}-100\,{\rm eV}$ for 1 kg-year and 100 kg-year exposures (see Budnik et al. (2018) for one possible realization). In the Lithium target, the detection of two correlated signals from both isotopes is possible. For $m_{\chi}\gtrsim~{}{\rm MeV}$, we project the sensitivity of current experiments in Fig. 1 (Right). Interestingly, which experiments best probe the neutral current absorption signal are not always the same as those which best probe WIMPs (e.g., Borexino). Each experiment can only detect the absorption signal off a target isotope when its distinct nuclear recoil energy is larger than the threshold energy, hence the edges in Fig. 1.

We now address the stability of $\chi$. For concreteness, we consider a model where a heavy $Z^{\prime}$ couples in an isospin-invariant way to quarks, with gauge coupling $g_{Z^{\prime}}$, and to $\chi$ and $P_{R}\nu$ in an off-diagonal way 222This suppresses the $\chi\to\nu\nu\nu$ decay; this off-diagonal coupling appears in inelastic dark matter models TuckerSmith:2001hy.. Quark loops induce a kinetic mixing, $\epsilon$, between the $Z^{\prime}$ and the photon of order $\epsilon\sim g_{Z^{\prime}}e/16\pi^{2}$ allowing the decay $\chi\rightarrow\nu e^{+}e^{-}$. Without additional $Z$ or $Z^{\prime}$ mass suppressions, the decay $\chi\rightarrow\nu\gamma$ is forbidden by gauge invariance while $\chi\rightarrow\nu\gamma\gamma$ is forbidden as a consequence of charge conjugation (also known as Furry’s theorem). For $m_{\chi}\lesssim~{}{\rm MeV}$, the electron channel is kinematically forbidden and the dominant decay is $\chi\rightarrow\nu\gamma\gamma\gamma$, whose primary contribution proceeds through a kinetic mixing and the Euler-Heisenberg Lagrangian, yielding the approximate rate

[TABLE]

Estimating the DM decay rates in this simple UV completion, we find future experiments can quickly probe new parameter space while cross-sections accessible to current experiment are ruled out by indirect detection bounds Essig et al. (2013).

However, it is possible to suppress DM decays by fine-tuning the UV contribution to the kinetic mixing against the IR piece estimated here. Concretely, we define this fine-tuning as $\text{F.T.}\equiv\left|\epsilon_{\text{UV}}-\epsilon\right|/\epsilon$ and we show the fine-tuning necessary to evade indirect detection constraints with dashed gray lines labeled “F.T.” in Fig. 1. We note that the projected direct detection sensitivities in Fig. 1 are insensitive to the details of the UV completion. We study ways to reduce fine-tuning by incorporating flavor-dependent couplings to suppress $\epsilon$ in future work Dror et al. (2020).

Also shown in Fig. 1 are direct constraints from LHC mono-jet searches on the $Z^{\prime}$ model, which bound new neutral currents below the TeV scale Belyaev et al. (2019). Dijet constraints are model dependent: in the $Z^{\prime}$ model, dijet bounds are suppressed in the limit where the quark coupling to the $Z^{\prime}$ is much smaller than the $\chi$ coupling to $Z^{\prime}$. The excess neutrino flux emanating from the Sun and Earth due to Eq. (1) is not quite large enough to be seen in neutrino observatories in the near future. Cosmological bounds depend on initial conditions (e.g., the reheat temperature) and the UV completion. While we postpone a detailed study of the dark matter relic abundance, we comment that a simple way to populate such light dark matter is through its thermal production and relativistic decoupling followed by its dilution from the decay of another heavy particle—a mechanism considered for sterile neutrinos Asaka et al. (2006). If the dark matter $\chi$ decouples while it is relativistic, which with only the quark coupling, will occur at the latest around the QCD phase transition, it will be overproduced. After relativistic decoupling of $\chi$ another state becomes non-relativistic leading it to quickly dominate the energy density of the universe. This mechanism can produce and sufficiently dilute DM to achieve its observed relic abundance over the entire DM mass range shown in Fig. 1. While other production mechanisms are possible, one must carefully avoid spoiling Big Bang Nucleosynthesis (BBN) for DM lighter than $\mathcal{O}(1\text{ MeV})$ Sabti et al. (2020), e.g. via freeze-in. Neutron absorption of $\chi$ through $n+\chi\rightarrow p+e$ could also spoil BBN, but the number density of $\chi$ is substantially less than that of SM neutrinos and the rate of scattering is suppressed relative to that of neutrinos by $\left(m_{W}/\Lambda\right)^{4}$ making this negligible.

Charged current signals: DM-induced $\beta^{-}$ decays

Next, consider signals from $\chi+\isotope[A][Z]{X}\rightarrow e^{-}+\isotope[A][Z+1]{X}_{*}^{+}$ (or at the nucleon level, $\chi+n\rightarrow p+e^{-}$), which we refer to as an induced $\beta^{-}$ decay. This process can cause stable elements to become unstable in the presence of DM if $m_{\chi}$ is large enough to overcome the kinematic barrier. Such a signal may proceed through the dimension-6 charged current vector operator,

[TABLE]

This can be generated by a $W^{\prime}$ which can appear if the electroweak gauge group is embedded in a larger gauge group which subsequently breaks into the SM.

We consider the vector operator in Eq. (6) to leverage known results from the neutrino and nuclear physics literature. The vector-vector interaction primarily induces Fermi transitions which are characterized by their conservation of spin ($J$) and parity ($P$) of the nucleus Pirinen et al. (2019), also known as $J^{P}\rightarrow J^{P}$ transitions. However, we emphasize that the DM induced $\beta^{-}$ decay signal is more general, with different vertex structures allowing different transitions. We leave a study of additional interactions to Dror et al. (2020).

Denoting the mass of a nucleus of mass number $A$ and atomic number, $Z$, by $M_{A,Z}$, we focus on isotopes which satisfy $M_{A,Z}<M_{A,Z+1}^{(*)}+m_{e}$, such that the nucleus is stable against $\beta^{-}$ decay in a vacuum (the (∗) is included to emphasize the daughter nucleus may be in an excited state, typically $200\,\text{keV}-1\,\text{MeV}$ heavier in mass). Then DM induced $\beta^{-}$ decay is kinematically allowed if

[TABLE]

In these induced decays, $\chi$ is absorbed by the target nuclei and transfers the majority of its rest mass to the outgoing electron. In the limit where $m_{\chi}-m_{\text{th}}^{\beta}\gg m_{e}$, the electron and nuclear recoil energies are analogues to the neutral current case with $m_{\chi}\rightarrow m_{\chi}-m_{\text{th}}^{\beta}$, and are given by;

[TABLE]

Therefore, the energetic outgoing electron will shower in the detector, and can be searched for. The nuclear recoil energy, as with the neutral current case, is independent of DM velocity, and can be searched for as well. Additional correlated signals result from the possible de-excitation of the daughter nucleus and its subsequent decay (typically many days later). These multiple signals make possible correlated searches to reduce backgrounds. The specific signals depend on the experiment, the particular isotope, and the DM mass.

The rate for DM-induced $\beta^{-}$ decays is;

[TABLE]

where we sum over all isotopes in a given target material, $N_{T,\,j}$ is the number of target isotope $j$, and $\left\langle\sigma v\right\rangle_{j}$ is an isotope’s velocity averaged cross-section

[TABLE]

where $|\vec{p}_{e}|^{2}_{j}=(m_{\text{th},\,j}^{\beta}-m_{\chi})(m_{\text{th},\,j}^{\beta}-m_{\chi}-2m_{e})$ is the electron’s outgoing 3-momentum in the center of mass frame (which is approximately the lab frame), in the limit that $m_{e},\,m_{\chi},m_{\text{th},\,j}^{\beta}\ll M_{A_{j},Z_{j}}$. The amplitude $\mathcal{M}_{N}$ is for absorption by the whole nuclei (the momentum transfer is not enough to resolve individual nucleons), which can be related to the nucleon level amplitude $\mathcal{M}$ (with the spinors normalized to $p_{\mu}p^{\mu}=M_{A_{j},Z_{j}}^{2}$) through the Fermi function, ${\cal F}(Z,E_{e})$ and a form factor, $F_{V}(q^{2})$:

[TABLE]

The Fermi function accounts for the Coulomb attraction of the ejected electron and can enhance the cross-section by several orders of magnitude for heavier elements. The form factor is equal to $1$ for small momentum transfer relative to the nucleon mass, $q^{2}\ll m_{n}^{2}$, while for larger $q^{2}$ the dependence can be extracted from the neutrino literature Formaggio and Zeller (2012). In principle, (12) must contain a sum over all possible nuclear spin states. The assumption made here is that this sum will be dominated by $\Delta J^{P}=0$ transitions as is the case of a vector coupling Pirinen et al. (2019). Excitation of additional final states is possible if $q\gtrsim r_{N}^{-1}$, where $r_{N}\simeq 1.2A^{1/3}{\rm fm}$ is the nuclear radius Engel et al. (1992), however for simplicity we focus on lighter masses such that these do not contribute significantly to the rate for any isotope considered here.

The total rate is found by summing over the contributions from each isotope. Evaluating (12) in the limit where $m_{e}\,,m_{\chi}\,,m_{\text{th}}^{\beta}\ll M_{A,Z}$, the total rate is;

[TABLE]

where we have integrated over all energies with the assumption that such a signal could be detected by most experiments under consideration here given the multitude of correlated high energy signals.

We project the sensitivity of current experiments to the charged current signal in Fig. 2 where we again require at least 10 events to set our projections, independent of isotope mass or experiment. Sensitivities are displayed in terms of the theoretically interesting quantity $m_{\chi}^{2}/2\pi\Lambda^{4}$ (to which Eq. (12) reduces in the limit of large $M_{A_{j},Z_{j}}$ and $m_{\chi}\gg m_{\text{th},\,j}^{\beta}$, modulo the Fermi function). As with the neutral current case, limits depend on the different isotopes in a given experiment. In particular, the kinks in Fig. 2 occur at $m_{\chi}\sim m_{\text{th},\,j}^{\beta}$ for every relevant isotope in a given experiment.

To estimate the DM decay constraints from a typical UV completion, we consider a model with a $W^{\prime}$ coupled vectorially to up and down quarks without any direct couplings to leptons. When kinematically allowed, the dominant decay is $\chi\rightarrow e^{+}e^{-}\nu$ which arises from a kinetic mixing between $W^{\prime}$ and the SM $W$ boson of order $\sim g_{W^{\prime}}e/16\pi^{2}$. The decay $\chi\to\nu\gamma$ is subdominant since it is at two-loop order, making it roughly $\left(4\pi\right)^{2}$ smaller. We estimate the decay rate and show the resulting indirect constraints Essig et al. (2013) in gray in Fig. 2. The decay bounds are much weaker than in the neutral current case as they are suppressed by both the weak scale and the $W^{\prime}$ mass.

In addition to decays, there are direct bounds from LHC searches for $pp\rightarrow\ell\nu$. A search was done by CMS at 8 TeV looking for helicity-non-conserving contact interaction models which have contact operators with vertex structure different than that of the SM Khachatryan et al. (2015) which sets a powerful constraint on the charged current operators. For the $W^{\prime}$ model, this constraint corresponds to a scale in Eq. (6) of $\Lambda\gtrsim 3.2~{}{\rm TeV}$. In the $W^{\prime}$ model, there is also a $Z^{\prime}$ which could lead to direct bounds. However, direct searches for $Z^{\prime}$ are not as stringent as those for the $W^{\prime}$ as the $Z^{\prime}$ can be somewhat heavier than the $W^{\prime}$ and elastic scattering constraints are negligible for the masses and $\Lambda$ of interest here. We also consider low energy searches for modifications to the $V-A$ gauge structure of the SM Hardy and Towner (2015); Gonzalez-Alonso et al. (2019) and for light fermions in charged pion decays: $\pi^{\pm}\rightarrow e^{\pm}\chi$ Aoki et al. (2011), but find they are subdominant to the CMS constraint. Cosmological constraints require detailed assumptions about the initial conditions and the full set of interactions. As for $\mathcal{O}_{\text{NC}}$, a simple production mechanism with $\mathcal{O}_{\text{CC}}$ has the DM decouple from the SM bath while relativistic, followed by late decays of a dominating particle Bezrukov et al. (2010); Patwardhan et al. (2015); Evans et al. (2019).

Discussion

In this Letter, we have introduced a novel class of signals from fermionic DM absorption in direct detection and neutrino experiments. We have studied the sensitivities of future and current experiments to neutral current signals from the process $\rm\chi+N\to\nu+N$, as shown in Fig. 1. This neutral current causes target isotopes to recoil with distinct energies and correlated rates, enabling significant background reduction in searches. We have also studied the sensitivities of current experiments to induced $\beta^{-}$ decays from the process $\chi+\isotope[A][Z]{X}\rightarrow e^{-}+\isotope[A][Z+1]{X}_{*}^{+}$, as shown in Fig. 2. This charged current enjoys multiple signatures from a sequence of events starting with a nuclear recoil and ejected $e^{-}$, followed by a likely $\gamma$ decay and often a final $\beta$ decay or electron capture event several days later. For both signals, ongoing experiments can probe orders of magnitude of unexplored parameter space by performing dedicated searches.

Without yet knowing the true nature of DM, it is impossible to know how it will appear in an experiment. Perhaps, it has been a fermion, depositing its mass energy into unsuspecting targets all along.

Acknowledgements.

We thank Artur Ankowski, Carlos Blanco, Tim Cohen, Lawrence Hall, Simon Knapen, Tongyan Lin, Ian Moult, Maxim Pospelov, Harikrishnan Ramani, Tien-Tien Yu, and Zhengkang Zhang for useful discussions, and Vetri Velan, Jason Detwiler, and Lindley Winslow for input on the capabilities of DM direct detection and neutrino experiments. We also thank Yonit Hochberg, Tongyan Lin, Lorenzo Ubaldi, Lindley Winslow, and Tien-Tien Yu for helpful comments on the manuscript. JD is supported in part by the DOE under contract DE-AC02-05CH11231. GE is supported by U.S. Department of Energy, under grant number de-sc0011637. RM was supported by the National Science Foundation Graduate Research Fellowship Program for a portion of this work.