# Dark Matter and Global Symmetries

###### Abstract

General considerations in general relativity and quantum mechanics are known to potentially rule out continuous global symmetries in the context of any consistent theory of quantum gravity. Assuming the validity of such considerations, we derive stringent bounds from gamma-ray, X-ray, cosmic-ray, neutrino, and CMB data on models that invoke global symmetries to stabilize the dark matter particle. We compute up-to-date, robust model-independent limits on the dark matter lifetime for a variety of Planck-scale suppressed dimension-five effective operators. We then specialize our analysis and apply our bounds to specific models including the Two-Higgs-Doublet, Left-Right, Singlet Fermionic, Zee-Babu, 3-3-1 and Radiative See-Saw models. Assuming that (i) global symmetries are broken at the Planck scale, that (ii) the non-renormalizable operators mediating dark matter decay have couplings, that (iii) the dark matter is a singlet field, and that (iv) the dark matter density distribution is well described by a NFW profile, we are able to rule out fermionic, vector, and scalar dark matter candidates across a broad mass range (keV-TeV), including the WIMP regime.

###### pacs:

95.35.+d, 14.60.Pq, 98.80.Cq, 12.60.Fr## I Introduction

Particle physics models achieve stability for dark matter (DM) particle candidates by advocating the presence of either discrete or continuous global symmetries. Discrete symmetries arise, for example, from broken gauge (local) symmetries, which are respected at the Planck scale Martin (1992); Krauss and Wilczek (1989). Continuous global symmetries, instead, are generically violated at the Planck scale, leading to important implications on the dark matter phenomenology of the associated models.

There are several reasons why continuous global symmetries are not expected to be present in a consistent theory of quantum gravity, which rely on general facts in gravity and quantum mechanics:

(i) No-Hair Theorem: Since local symmetries are effectively identical to Gauss’s law, any observer outside a Black Hole (BH) horizon can determine the BH charge. However, if there existed continuous global symmetries, when a charged particle gets trapped inside the BH there would be no way to assess this from outside the horizon. Thus the charge would appear to be “deleted”, in contradiction to its conservation Kallosh et al. (1995).

(ii) Hawking Radiation: The main problem with continuous global symmetries has to do with Hawking radiation Hawking (1975). Since there are no gauge interactions associated with continuous global symmetries, one could throw a large amount of charged particles into a BH and increase its charge () indefinitely Hawking (1975); Banks et al. (2006). However, the theory of Hawking radiation indicates that until , where is the mass of the lightest charged particle pair, the BH does not radiate charge. Combining this with the bound on the BH mass, namely , where is the Planck mass, we find . This limit can however be violated by making sufficiently large. Hence, if were conserved we could have identical BHs with an infinite number of states labelled by .

(iii) Entropy: Since an external observer cannot infer a global charge, in order to assign an entropy to a given BH one would have to count all micro-states of all charges, finding an entropy of order . Now, taking indefinitely large, one would violate the Bekenstein-Hawking formula, which says that entropy counts the number of states of a BH. Therefore, such objects are ruled out, as are continuous global symmetries Banks et al. (2006).

While there are general arguments for the breaking of continuous global symmetries at the scales of quantum gravity, those are not well-established. For example, Ref. Dvali (2016) disputes such asguments based on non-thermal deviations from Hawking radiation. This notwithstanding , hereafter, we assume that continuous global symmetries are indeed broken at the Planck scale and show that the notion of such symmetries being broken at the Planck scale has profound implications on DM phenomenology.

In this study, we assess the possibility of using continuous global symmetries to stabilize DM particles. In order to derive results applicable to a variety of particle physics models, we consider Planck-scale suppressed, dimension-five effective operators that mediate the decay of generic DM particles of spin 0, 1/2 and 1; the operators under consideration violate continuous global symmetries, and thus induce the decay of DM particles whose stability relies on such continuous global symmetries. The decay of long-lived but metastable DM particles can inform us on the DM particle nature (see e.g. Hambye (2011); Boucenna et al. (2013)); for example, stringent bounds on the lifetime of electroweak-scale DM stem from the observed diffuse gamma-ray flux Cirelli et al. (2012), which implies lifetime s, thus a billion times longer than
the age of the Universe. We emphasize the fact that even though continuous global symmetries might break down to discrete symmetries at low energies, one can always generically construct Planck-suppressed effective operators that would induce the decay of the DM particle: our results can thus be applied to any continuous global symmetry.

Naively, one might expect that Planck-scale suppression might have a negligible impact on the phenomenology of models which advocate the existence of continuous global symmetries to stabilize the DM particle. Using current cosmic-ray, X-ray, gamma-ray, neutrino and CMB data, spanning the entire keV-TeV energy range, we show that, somewhat surprisingly, continuous global symmetries are strongly disfavored as a mechanism to stabilize DM particles. In particular, we rule out, under the aforementioned assumptions, a rather large DM mass range, including the classic WIMP mass range around the electroweak scale.

## Ii Observational Constraints

In this section we summarize how we derive our model-independent limits on the DM lifetime. We employ throughout our analysis an NFW profile Navarro et al. (1997),

(1) |

with a scale radius, kpc, and , such that to reproduce a local density of Catena and Ullio (2010). We point out that our results would all scale linearly with other choices for the local dark matter density, unlike for the dark matter pair-annihilation case.

I suspect the limits will essentially stay the same, since DM decay signals at high latitudes are not very sensitive to this.

### ii.1 CMB data

Precise measurements of the Cosmic microwave background (CMB) provide robust limits on DM decays, since the latter alter the ionization and heating history of the CMB as well as its power spectrum. Using combined data from Planck Ade et al. (2014), WMAP9 Hinshaw et al. (2013), Atacama Telescope Sievers et al. (2013), South Pole Telescope Hou et al. (2014), Hubble Space Telescope Riess et al. (2011) and Baryonic Acoustic Oscillations Anderson et al. (2013), we derive limits on the DM lifetime for several final states. Typically, those limits come from constraints on new sources of ionization and heating stemming from the products of DM interactions. Here we pay special attention to DM particle decays. Our findings rely on several standard assumptions namely: (i) the DM lifetime is large than the age of the universe; (ii) the DM particle accounts for the DM cosmological abundance; (iii) the DM particle decays fully to SM particles; (iv) the energy fraction which the DM particle deposit into the intergalactic Medium is determined by the transfer functions provided in Ref. Slatyer (2013). The rate at which a given DM particle decay induces heating and ionization of the baryonic component of the IGM is proportional to

(2) |

where is the Hubble rate and is the number density of hydrogen in the Universe at a given redshift with being the present-day value, and

(3) |

where is in general a function of the DM mass and redshift. We closely follow Ref. Lopez-Honorez et al. (2013) and average over the redshift dependence to get as a function of the DM mass only, according to Table II of Ref. Diamanti et al. (2014). We then modify the energy deposited into the intergalactic medium by inputting the equation above into the CosmoRec Chluba and Thomas (2011) package to compute deviations on the ionization history, which now depend on the DM mass and lifetime for a given decay final state. We obtained values for for the ,, final states in agreement with Ref. Diamanti et al. (2014). In addition, we calculated the efficiencies for decays into quarks and gauge bosons using the recipe of Slatyer (2013). In detail, in order to compute the bounds for and final states, we rescale the limits from Ref. Lopez-Honorez et al. (2013) by using the appropriate energy deposition efficiency, which in those cases is slightly larger than for the final state, resulting into a slightly more restrictive limit as what shown in Fig.1, and in agreement with Slatyer (2013).

### ii.2 Antiproton Data

Since DM decays produce, in principle, matter and antimatter in equal amount, antiprotons are an interesting target for indirect DM searches, due to the relative rarity of antimatter produced in astrophysical processes. In this section we revisit the procedure to place bounds on the DM lifetime using antiprotons data from AMS-02 collaboration (2015). Antiproton data can be used to set stringent limits on the DM lifetime, since DM decays should at some level produce a sizable amount of antiprotons, even for leptonic final states through the inclusion of electroweak corrections (radiation of a gauge boson which decays hadronically)Cirelli et al. (2011).

With recent AMS-02 precise measurements of the antiproton/proton () fraction for energies up to 450 GeV one can derive new restrictive limits on the DM lifetime for several decay modes such as and , since no evidence of new sources of antiprotons were found in the data ^{1}^{1}1See Ref. Hooper et al. (2015) where a claim was put forth about excess antiprotons in the PAMELA data.. We follow Ref. Boudaud et al. (2015), where constraints on the DM annihilation cross section were derived using an older data set for the Einasto DM profile based on the total antiproton flux. Here we will instead obtain limits on the DM lifetime with an NFW profile using the latest AMS data on the ratio, and compare our finding with existing limits.

The derivation of limits based on antiproton data is subject to large astrophysical uncertainties associated with production, propagation and solar modulation. Here, we employ the standard set of Min-Med-Max propagation models. Min-Med-Max represent values of diffusion parameters which produce a mininum-to-maximum antiproton flux from a DM decay as shown in Table I (See Ref. Ibarra et al. (2013) for a recent review). Current data seem to disfavor the Min propagation model Lavalle et al. (2014) and the Max-model induces arguably overestimated bounds, so we base our limits on the Med propagation model and an NFW DM distribution. To obtain limits on the DM lifetime we first solve the cosmic-ray transport equation in the Galaxy, in a steady state condition for the number density of antiprotons () per unit of kinetic energy ,

(4) |

where we have neglected energy losses and re-acceleration processes. We describe below the physical meaning of each of those components:

(i) The first term refers to the primary production of antiproton from DM decays expressed as,

(5) |

where is the DM halo profile assumed to be NFW, and is the energy spectrum generated using PPPC4DM Cirelli et al. (2011).

(ii) The second term accounts for the diffusion of cosmic-rays through their propagation in the interstellar medium. It is typically assumed to be constant in the diffusion zone and often parametrized in terms of the particle rigidity (momentum/atomic number) as follows,

(6) |

with , where the normalization () and the spectral index () are associated with the properties of the interstellar medium and derived from measurements of the primary-to-secondary flux ratios of cosmic-rays such as Boron to Carbon Boudaud et al. (2015), and obviously for antiprotons.

(iii) The third term refers to the convection mechanism which accounts for the drift of charged particles away from the disk, assumed to be infinitely thin with a half-height of 100pc Ibarra et al. (2013), induced by the Galactic Wind with a characteristic velocity and spatially constant in the diffusion zone, i.e., . Departures from the thin disk assumption lead to one order of magnitude changes in the final limits as one can see in Fig.6 of Ref. Cirelli et al. (2014).

(iv) The fourth term represents the annihilations of antiprotons with the interstellar gas which is proportional to

(7) |

where, , for GeV and for GeV Tan and Ng (1982); Protheroe (1981). In Eq.7 we assumed that the helium-antiproton annihilation cross section is simply a rescaling of the proton-antiproton Cirelli et al. (2014).

We now have all ingredients to solve the transport equation and to compute the astrophysical and DM decay predictions for the antiproton flux. A final physical effect, solar modulation, affects the prediction of the antiproton flux at the Earth’s atmosphere at energies below GeV, as result of the solar cosmic-ray wind and magnetic field.

We take into account this effect using the force-field approximation, which determines the antiproton flux as a function of the kinetic energy of the antiproton at the atmosphere () by re-scaling the interstellar flux which depends on the antiproton kinetic energy () as follows Gleeson and Axford (1968):

(8) |

with - , where is the Fisk potential as given in Table I.

Using a data-driven model to account for the proton flux for the energy range of interest as presented by the PAMELA collaboration Adriani et al. (2011), which is well fitted by a Fisk potential (see fifth column of Table 1 of Cirelli et al. (2014)), one can finally compute the total ratio from primary and secondary production processes, as discussed above, and enforce the condition that the predicted ratio does not exceed the ratio measured by AMS-02 data collaboration (2015) at 95% C.L, for the specific choices of DM lifetime and mass; That results in constraints on the DM lifetime versus mass plane shown in the second panel of Fig.1. Our results were obtained with PPPC4DMID code Cirelli et al. (2011).

Notice that our limits are competitive with existing ones derived using PAMELA Ibarra et al. (2013) and AMS-02 Giesen et al. (2015). In particular, our limits are mildly similar to Ref. Giesen et al. (2015) which performed a through analysis by including several energy loss processes we ignored.

Antriproton Propagation Model

MED | ||
---|---|---|

Kpc |

### ii.3 Line Searches

If bright enough to be distinguishable from background continuum emission, and if morphologically diffuse Carlson et al. (2013), gamma-ray spectral lines are known as a veritable smoking gun for DM annihilation or decay signals. Several experiments have searched for line emission at energies between GeV up to 400 GeV: (i) Chandra and X-ray Multi-Mirror Mission (XMM) X-ray telescopes cover the 0.007 keV-12 keV range Boyarsky et al. (2008a); Bazzocchi et al. (2008); (ii) High Energy Astronomy Observatory (HEAO) accounts for the 3-48 keV Boyarsky et al. (2006); (iii) INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) the 20k eV-7 MeV Boyarsky et al. (2008b); (iv) The Imaging Compton Telescope (COMPTEL) along with The Energetic Gamma Ray Experiment Telescope (EGRET) screens the MeV-100GeV Yuksel and Kistler (2008); (v) Fermi-LAT covering energies up to 462 GeV Ackermann et al. (2015, 2012). Here, we simply combine all of those constraints. We point out that we make use here of the latest Fermi-LAT limits on the flux at 95% C.L for the region centered at the Galactic Center (R180), as described in Ref. Ackermann et al. (2015, 2013). Limits on the DM lifetime are obtained after solving for the DM lifetime using the differential flux equation,

(9) |

The combination of the bounds listed above are shown in Fig.1, third panel. Note that some operators discussed in our work give rise to and lines: for those we correct the energy of the gamma-ray line using the relation , where is either the Z or Higgs mass, and divide the lifetime by a factor of two since we have one photon in the final state instead.

### ii.4 Neutrino Data

Neutrino detectors are sensitive to DM decays and have been used to place limits on the DM lifetime. For a NFW profile for , the full sky differential neutrino flux from DM decays reads Bertone et al. (2005),

(10) |

Another source of neutrinos from DM decays stems from cosmological decays of DM particle producing a diffuse neutrino flux from decays at all redshifts which reads:

(11) |

where is the cosmological DM density, is the expansion rate of the universe, and is the universe opacity to neutrinos obtained in Ref. Alvarez-Muniz and Halzen (2001). The neutrino oscillation probabilities in vacuum is assumed to remain unchanged at the detector. Thus the primary neutrino flux from a specific flavor is redistributed equally into all neutrino flavors, so that the number of expected events is given by,

(12) |

By comparing with the 95% C.L limits on the number of events observed, constraints on the DM lifetime for two body decays were derived: (i) Ref. Covi et al. (2010); Palomares-Ruiz (2008); El Aisati et al. (2015) used AMANDA and Super-K data; (ii) Ref. Sjostrand et al. (2006) analyzed recent ICECUBE data; However, operator O14 in Table II induces three body decays (). Hence, we take the limits from those references and use PYTHIA 6.4 Sjostrand et al. (2006) to derive the corresponding bounds on three body decay as shown in Fig.2, rightmost panel. We emphasize that the 95% C.L. limits were obtained by requiring the theoretical predictions not to overshoot the data in any point.

### ii.5 Gamma-ray data

Observations of the continuous emission of gamma rays give rise to stringent limits on the DM lifetime. Here we employ limits derived from: (i) the extragalactic gamma-ray background, as derived in Ref. Ando and Ishiwata (2015), which postulates that the sum of the isotropic component from blazars (making up nearly of the total intensity), star-forming galaxies (SFGs), misaligned active galactic nuclei and DM decays not exceed the measured flux at C.L (Fig.4 of Ref. Ando and Ishiwata (2015)); (ii) limits from Fermi-LAT observations of eight galaxy clusters at gamma-ray frequencies, in squared regions centered on the clusters Huang et al. (2012). We do not duplicate those results here, but we use them in what follows to derive our bounds. For several discussions related to gamma-ray constraints and other topics which provide complementary limits we point to RefsBrun et al. (2007); Boehm et al. (2010); De Lope Amigo et al. (2009); Cholis (2011); Garny et al. (2011); Evoli et al. (2012); Hooper et al. (2013); Cirelli et al. (2012); Ibarra et al. (2014); Jin et al. (2013); Gonzalez-Morales et al. (2014); Lovell et al. (2015); Cembranos et al. (2015); Rott et al. (2015); Kappl et al. (2015); Chen et al. (2016); Jin et al. (2015); Chen et al. (2015); Hamaguchi et al. (2015); Baring et al. (2015); Harding and Dingus (2015); Cheng et al. (2015).

## Iii Bounds on the Dark Matter Lifetime

As discussed in the previous section, we assume that continuous global symmetries are broken due to gravitational effects (see Ref. Dvali (2016) otherwise); in the presence of a continuous global symmetry, one should thus consider Planck-suppressed effective operators which break continuous global symmetries, leading to metastable DM particles. Limits on the lifetime of DM particles from observations in a broad range of frequencies thus allow us to derive general constraints on these operators in settings that advocate continuous global symmetries to stabilize DM candidates.

We list in Table II a set of dimension-five gauge and non-gauge invariant operators that violate continuous global symmetries and induce DM decay. We point out that our list is not exhaustive or complete; rather, it should serve as a proof of principle, since it includes operators mediating several decay modes that produce significant continuum gamma-ray emission, spectral lines, antiproton, charged leptons and neutrino fluxes; in addition, the set we consider encompasses a variety of DM particle quantum numbers. Here we show results for the gauge-invariant operators only, while in the appendix we present results for the non-gauge invariant ones. Notice that other functional forms are possible for Planck-scale operators violating continuous global symmetries, for example because of the effects of D-brane instantons, see e.g.Ref. Blumenhagen et al. (2009).

Name | Interaction Term |
---|---|

O1 | |

O2 | |

O3 | |

O4 | |

O5 | |

O6 | |

O7 | |

O8 | |

O9 | |

O10 | |

O11 | |

O12 | |

O13 | |

O14 | |

O15 | |

O16 |

In the Table, we have introduced the dimensionless couplings , whose value depends on the unknown mechanism for the quantization of gravity. As we argue below, the precise values of are irrelevant to our conclusions, but we keep the ’s as free parameters and obtain our limits in the vs DM mass plane. For each of the Planck-suppressed operator, we apply the most stringent limit on the DM lifetime for a given particle mass. Our results are collected in Figures 3-4. In Figure 3 we show the result for gauge invariant operators, whereas in figure 4 for non-gauge invariant one. Notice that several bounds are truncated at some DM mass due to the lack of data at lower energies. Moreover, the sudden change in the behavior of the limits in the figures has to do with the shift in the data set used to constrain a given effect operator. For instance, for operator O1, for masses below GeV we had to shift from gamma-ray to CMB data that yields much weaker constraints, accounting for the abrupt change in the limit at GeV.

Figures 3 shows that models that advocate the presence of continuous global symmetries to stabilize scalar DM candidates might produce a line emission with a very short lifetime (through operator O2/O3), well below the age of the universe, thus ruling out DM masses larger than keV. It is clear that for any scalar DM operator the whole electroweak WIMP range as well as the large mass range of warm DM is ruled out, since only for keV are couplings of order one achieved.

As for fermionic DM candidates stabilized by continuous global symmetries, operator O14 arises naturally at the Planck scale, yielding an appreciable neutrino and cosmic-ray flux as displayed in the right panel of Fig.3. The result clearly shows that we are able to exclude DM masses above MeV. Lastly, in models where vector DM particles are stabilized via the existence of continuous global symmetries, operator O15 would automatically be present at the Planck scale, leading to DM decay into fermion pairs. After employing a combination of the bounds shown in Fig.1, we find that masses larger than MeV induce cosmic-ray and gamma-ray fluxes that exceed the measured values. Conclusions regarding the remaining operators in Table II can be straightforwardly drawn.

In summary, we find that dimension-five effective operators at the Planck scale make continuous global symmetries problematic to stabilize DM particles outside very special, restricted mass ranges. In the next section we show how our bounds highly constrain several well-known models in the literature.

## Iv Concrete Models

In what follows, we work under four assumptions: (i) global symmetries are in fact broken at the Planck scale;(ii) O(1) non-renormalizable couplings are a good approximation; (iii) dark matter field is a singlet field; (iv) the dark matter density distribution is well described by a NFW profile.

It is important to keep in mind as caveats that despite the existence of plausible arguments ruling out global symmetries at the Planck Scale, the validity of such arguments is still under debate. Moreover, in general continuous global symmetries can be replaced by other symmetries such as discrete symmetries, circumventing our constraints. We assume non-renormalizable couplings for the non-renormalizable operators mediating decay. Any departure from this assumption is easily factoring in by rescaling using the expressions for the width rate given in Table 3.

We apply here the results from the previous sections to concrete models, widely discussed in the literature where the dark matter field is a singlet field, for which our bounds are directly applicable.

Left-Right Model

We consider the left-right mirror symmetric model with the continuous global symmetry of Ref. Yang (2013, 2014). There, the continuous global symmetry prohibits the term , where is a fermionic DM candidate. However, such symmetry is generically violated at the Planck scale and therefore the O14 operator ought to exist, thus ruling out DM masses above 100 MeV. Ref. Yang (2013, 2014) also invokes the case of WIMP scalar DM protected by the continuous global symmetry, but once again, as we see in the left panel of Fig.2, the entire corresponding WIMP mass range is excluded. As a result, the model described in Ref. Yang (2013, 2014) does not appear to have a plausible DM candidate. Unless the invoked continuous global symmetry can be replaced by a discrete symmetry of some sort, the model is strongly disfavored by data.

Two Higgs Doublet Model

In the original two Higgs doublet model no DM candidate is present. Nevertheless, if the second Higgs doublet is odd under a symmetry the CP-even scalar of that doublet can be a DM candidate. This is the case in the so-called Inert Two Higgs Doublet Model (I2HDM) Lopez Honorez et al. (2007). Recently, a continuous global symmetry has been proposed to replace the symmetry Bhattacharyya et al. (2013). The authors focus on the spontaneous symmetry breaking of the continuous global symmetry through the vev of the second Higgs doublet and comment on the possibility of having an unbroken continuous global symmetry. Despite the interesting Higgs physics implications produced by the use of the continuous global symmetry Bhattacharyya et al. (2013), operator O2 should be present at the Planck scale; thus, from Fig. 2 we conclude that DM masses larger than keV are problematic along with the possibility of having viable WIMP DM candidates in the model.

Singlet Fermion Model

The minimal fermionic DM model studied in Ref. Baek and Okada (2014) advocates a continuous global symmetry responsible for stabilizing a singlet fermion which yields the desired thermal relic abundance and is consistent with direct searches. The Planck suppressed effective operator O14, however, rules out the entire WIMP mass range. As we mentioned before, in principle one could replace the continuous global symmetry by a discrete symmetry, since is a subgroup of . However, the necessary discrete symmetry might turn out to imply a rather large and unnatural tuning of the model.

Radiative See-Saw Model

A radiative lepton model in which the charged lepton masses are generated at one-loop level whereas and the neutrino masses at two-loop level has been proposed in Ref. Baek et al. (2014). In this model the continuous global and symmetry have been invoked and two DM candidates postulated. A singlet fermion, referred to as in Table I of Ref. Baek et al. (2014), is not odd under the symmetry, and claimed to be a WIMP due to the presence of a continuous global symmetry. Similarly to the previous model, Planck-suppressed dimension-five operators discard such possibility.

Zee-Babu Model

The Zee-Babu model adds to the SM a singly-charged and a doubly-charged scalar Lindner et al. (2011). Recently, an extension of the Zee-Babu model has been put forth by adding a singlet fermion which is stabilized by a continuous global symmetry. This continuous global symmetry also forbids terms like . There, the neutral fermion does not carry a lepton number so it is purely a neutral fermion. Nevertheless, as we discussed, this continuous global symmetry does not hold up to the Planck scale and consequently the operator O14 arises, inducing an excess production of neutrinos, gamma-ray and comic-rays, which results into the exclusion of DM masses below MeV, in tension with what presented in Figs.1-2 of Ref. (Lindner et al., 2011).

3-3-1 Models

3-3-1 models refer to gauge extensions of the Standard Model Foot et al. (1993). In Ref. Mizukoshi et al. (2011) a continuous global symmetry with the purpose of avoiding undesirable mixing among the gauge bosons and of guaranteeing that the lightest particle charged under the continuous global symmetry be stable. Both a complex scalar and a heavy Dirac fermion were studied as potential WIMP DM candidates. In a similar vein to what discussed above, the WIMP mass regime in this model is in jeopardy due to the aforementioned gravity effects. In the urge of preventing the use of continuous global symmetries in the model, Ref. Dong et al. (2014) proposed adding an extra gauge symmetry, which would completely change the associated DM phenomenology.

## V Conclusions

Based on general lessons from quantum mechanics and general relativity, it reasonable to assume that no global symmetries are allowed in a consistent theory of quantum gravity. We have presnted, in a model-independent approach, robust gamma-, X-ray, CMB, and cosmic-ray constraints on decaying DM particles, using a large set of data, including data from Fermi-LAT, AMS-02, Super-Kamiokande, Planck, WMAP9, AMANDA, and Icecube among others. We have then applied those bounds to scalar, vector and fermion DM particles decaying through dimension-five Planck-suppressed effective operators. We stress that our findings are based on the following assumptions:

(i) global symmetries are broken at the Planck scale;

(ii) the operators mediating dark matter decay have non-renormalizable couplings;

(iii) the dark matter particle is represented by a singlet field;

(iv) the dark matter density distribution in the Galaxy is well described by a NFW profile.

Under these assumptions, we have derived the following constraints on the possible mass range:

(i) scalar DM: keV ;

(ii) fermionic DM: MeV ;

(iii) Vector DM: MeV .

Lastly, we have applied our limits to instances of parameter space of Left-Right, Two-Higgs Doublet, Singlet Fermionic, Zee-Babu, 3-3-1 and Radiative See-Saw models to conclude that the occurrence of DM particles in such models is generically problematic outside the DM particle mass ranges listed above. Our results basically rule out the entire WIMP mass range for models invoking continuous global symmetries to stabilize the DM particles.

We emphasize that our results rely on the critical assumptions listed above, especially on the hypothesis that continuous global symmetries are violated at the Planck scale. Notice that if one uses non-renormalizable couplings smaller than unit, our limits can be simply rescaled using Table 3 containing the decay rates. Moreover, if one adopted a different density profile that would quantitatively change the acceptable DM mass ranges, but leave the overall conclusions unchanged. However, if the DM particle belongs to a multiplet, and thus only higher dimension operators induce the dark matter decay, our limits would not be relevant. In summary, our bounds and conclusions can be subject to significant changes.

## Acknowledgement

The authors thank Michel Dine, Dan Hooper, Herbi Dreiner, Pavel Fileviez Perez, Alejandro Ibarra, Paul Langacker, Will Shepherd, Christoph Weniger, and, especially, Marco Cirelli for useful discussions. We are indebted to Tom Banks for important comments and reading the manuscript in early stages. Y.M was partially supported by the Spanish MICINN’s Consolider-Ingenio 2010 Programme under grant Multi-Dark CSD2009-00064, the contract FPA2010-17747; European Union FP7 ITN INVISIBLES (Marie Curie Actions, PITN-GA-2011- 289442); ERC advanced grants HiggsLHC and MassTeV; Research Executive Agency (REA) of the European Union under the Grant Agreement PITN-GA2012-316704 (”HiggsTools”); and LIA-TCAP of CNRS. SP is partly supported by US Department of Energy Award SC0010107. FSQ thanks UCSC for its hospitality and funding from US Department of Energy Award SC0010107 during early stages of this work.

## Vi Appendix:Decay widths and non-gauge invariant operators

In Table III we list the decay width associated with each operator discussed in the manuscript; in addition we discuss some non-gauge invariant operators (O6-O9-O12-O13) that might appear in more complex setups such as non-Abelian theories Gross et al. (2015). We also show the limits stemming from such operators in Fig.4.

Name | Interaction term | Decay Rate |
---|---|---|

O1 | = | |

O2 | = | |

O3 | = | |

O4 | = | |

O5 | = | |

O6 | = | |

O7 | = | |

O8 | = | |

O9 | = | |

O10 | = | |

O11 | = | |

O12 | = | |

O13 | = | |

O14 | = | |

O15 | = | |

O16 | = |

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