Perturbative Unitarity Constraints on Gauge Portals

Perturbative Unitarity Constraints on Gauge Portals

Sonia El Hedri, William Shepherd and Devin G. E. Walker Institut für Physik (THEP) Johannes Gutenberg-Universität, D-55099, Mainz, Germany SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, U.S.A. Santa Cruz Institute for Particle Physics and Department of Physics, Santa Cruz, CA 95064, U.S.A.
Abstract

Dark matter that was once in thermal equilibrium with the Standard Model is generally prohibited from obtaining all of its mass from the electroweak phase transition. This implies a new scale of physics and mediator particles to facilitate dark matter annihilation. In this work, we focus on dark matter that annihilates through a generic gauge boson portal. We show how partial wave unitarity places upper bounds on the dark gauge boson, dark Higgs and dark matter masses. Outside of well-defined fine-tuned regions, we find an upper bound of 9 TeV for the dark matter mass when the dark Higgs and dark gauge bosons both facilitate the dark matter annihilations. In this scenario, the upper bound on the dark Higgs and dark gauge boson masses are 10 TeV and 16 TeV, respectively. When only the dark gauge boson facilitates dark matter annihilations, we find an upper bound of 3 TeV and 6 TeV for the dark matter and dark gauge boson, respectively. Overall, using the gauge portal as a template, we describe a method to not only place upper bounds on the dark matter mass but also on the new particles with Standard Model quantum numbers. We briefly discuss the reach of future accelerator, direct and indirect detection experiments for this class of models.

preprint: SLAC-PUB-16173preprint: MITP/14-103preprint: SCIPP 14/17

I Introduction

Understanding the nature of dark matter (DM) is one of the most pressing unresolved problems in particle physics. Dark matter is needed to understand structure formation, the observed galactic rotation curves Kowalski:2008ez (); Ahn:2013gms (); Beringer:1900zz () and the acoustic peaks in the cosmic microwave background Ade:2013lta (). Moreover, the dark matter relic abundance is measured to be Ade:2013lta ()

(1)

A compelling argument for the origin of this abundance is to assume dark matter was once in thermal contact with the baryon-photon plasma during the early universe. Since all known forms of matter in the universe were once in thermal equilibrium, this type of dark matter is theoretically persuasive. In this scenario, the measured relic abundance is controlled by dark matter annihilations into Standard Model (SM) particles. Because of constraints from the observed large scale structure in the universe, dark matter must be stable and non-relativistic (cold) when departing thermal equilibrium Ahn:2013gms ().

The Standard Model (SM) alone cannot account for the missing matter in the universe Bertone:2004pz (). Current experimental constraints, however, provide some guidance on the structure of the underlying theory. For example, the lack of large missing energy signatures at the Large Hadron Collider (LHC) Aad:2014tda (); ATLAS:2014wra (); Aad:2013oja (); Aad:2014vka (); Aad:2014kra (); Chatrchyan:2014lfa (); Khachatryan:2014tva (); Khachatryan:2014rwa (); Khachatryan:2014rra (); Chatrchyan:2013lya (); Chatrchyan:2013xna () and other colliders Aaltonen:2012jb (); Aaltonen:2013har (); CDF:2011ah (); Abachi:1996dc (); Abazov:2012qka (); Abdallah:2003np (); Acciarri:1997dq (); Abbiendi:2004gf () suggest that dark matter is either heavy or has very small couplings with the SM so that it is not produced in high-energy collisions. Additionally, direct detection experiments Aprile:2012nq (); Ahmed:2011gh (); Akerib:2013tjd (), updated precision electroweak constraints, and precision Z-pole experiments devinjoannetim (); Baak:2012kk (); ALEPH:2005ab () all severely constrain the direct coupling of dark matter to the SM Higgs and/or Z bosons. These constraints all imply dark matter cannot obtain all of its mass from the SM Higgs alone devinjoannetim (). Thus, if dark matter is a weakly interacting massive particle (WIMP), we are led to scenarios where new mediators facilitate dark matter interactions with the SM. Moreover, a new fundamental scale of physics is needed that is (at least partly) responsible for the dark matter mass. Mediator-facilitated interactions help to evade current experimental constraints by partially decoupling the dark matter from the SM. Should these scenarios be realized in nature, the discovery of the mediator particles would be an important step in understanding the nature of dark matter. It is therefore crucial to place bounds on the masses and couplings of these mediators. The most popular ways for dark matter to annihilate via a mediator particle are through the Higgs Patt:2006fw () boson, through scalars that are colored or charged, or via a new neutral gauge boson. Some of us considered the perturbative unitarity constraints on the Higgs portal in Walker:2013hka (); Betre:2014sra (); Betre:2014fva (). In this work, we focus on placing constraints on a scenario where fermionic dark matter is charged under a new, dark gauge group, . This gauge group is spontaneously broken by a dark Higgs, , generating a massive, dark boson. This boson is also known in the literature as a dark photon. The dark mixes kinetically as well as through mixed mass terms with the SM boson. Thus, the mixing between the hidden sector and the SM allows dark matter (DM) to annihilate via the Higgses, and bosons.

We apply unitarity constraints in a manner reminiscent of Griest and Kamiokowski Griest:1989wd (). However, there are important differences: Here we focus on perturbative unitarity constraints which determine, in particular, when the dark matter couplings become strong. WIMP dark matter and perturbativity have always had an important conceptual association. Dark matter masses that violate the perturbative unitarity bounds imply the dark matter is efficiently forming bound states as well as annihilating as the temperature decreases toward the thermal decoupling temperature. Because the dark matter annihilates into lighter states, the annihilation diagrams can be altered (and sometimes dressed with these lighter states) to produce diagrams in which the bound states decay. The dark matter decays have a lifetime well shorter than the age of the universe. Thus, dark matter with a mass beyond the perturbative unitarity bounds is not an asymptotic state; this leads to a scenario without a viable dark matter candidate. Note, it is well known that viable dark matter candidates exist that are the result of strongly coupled or confining hidden sectors. However, in these models the dark matter annihilation processes are still perturbative Shepherd:2009sa (). We show our perturbative unitarity constraints are improved in comparison to the updated Griest and Kamiokowski bounds Profumo:2013yn (). Of central importance is the fact that our methodology places constraints on any particle associated with the dark matter annihilation. For this paper, our bounds on the masses and couplings of the new Higgs and dark gauge boson are novel.

Our basic perturbative unitarity arguments are straightforward. The DM annihilation cross section depends on the masses of the dark matter, the dark Higgs, and the , as well as the dark matter couplings to the dark Higgs and dark . As the dark matter gets heavier, its annihilation cross section decreases. In order for heavy dark matter to satisfy the relic abundance constraints, it must annihilate more efficiently and therefore have sizable couplings to the SM and hidden sectors. Eventually, the couplings required to obtain the correct relic abundance are so large that perturbative unitarity is violated. Perturbative unitarity arguments therefore set an upper bound on the dark matter mass. If the dark Higgs and gauge boson masses are raised to be larger than the dark matter mass, fewer (and more suppressed) annihilation channels are available. The annihilation cross section in these regimes of parameter space is thus diminished. Therefore these arguments yield bounds on the dark matter mass as well as on the mass of any other particle involved with the dark matter annihilation.

In the next section, we introduce a generic model on which to place our unitary bounds and introduce the parameters that need to be constrained as well as the constraints from electroweak precision tests (EWPT). In Section III., we show how to apply unitarity constraints on the various sectors of the model. Section IV. details how relic abundance and direct detection constraints on the DM sector impact the masses and couplings of the theory. Section V. gives our results by detailing the bounds on the particle masses obtained by applying the EWPT, unitarity and relic abundance constraints. Conclusion and Appendices follow.

Ii A Representative Model

We extend the SM with an additional gauge group with coupling that is spontaneously broken at a high scale. This dark group is associated to a dark gauge boson that mixes kinetically and via mass terms with SM hypercharge. The gauge group is broken by a new, dark Higgs, that gets a vev . The model then includes two Higgs fields

(2)

where is the SM Higgs. We also introduce a DM candidate , which is a chiral fermion, neutral under the SM gauge groups but charged under . All SM particles are taken to be neutral under . The dark charge assignments for the DM and the dark Higgs are

(3)

Anomaly cancellation mandates the introduction of the second chiral fermion. In this work, we take this additional fermion to be much heavier than the other particles so that it does not have any influence on the final results.

We adopt the notations and conventions from Babu:1997st (). The relevant parts of the lagrangian associated to new physics is

(4)

where the dark matter and gauge sectors are

(5)
(6)

and

(7)
(8)

is the Higgs sector. The kinetic mixing is parameterized by the mixing angle . The kinetic terms can be diagonalized by defining new fields and such that Babu:1997st ()

(9)

where the hatted fields are the fields before diagonalizing kinetic mixing. Denoting and as the SM hypercharge and weak couplings respectively, the covariant derivatives for the Higgs and DM fields then become

(10)
(11)
(12)
(13)

Any SM particle with non-zero hypercharge will then acquire a dark charge. We now have the effective dark gauge coupling

(14)

After symmetry breaking, the gauge bosons acquire masses. Kinetic mixing between and induces a mass mixing between and . The mass mixing angle, , is such that

(15)

where the hatted Weinberg angle is such that

(16)

and the masses terms are

(17)

EWSB also induces a mass mixing between the scalars and . The mixing angle is given by

(18)

We denote the light and heavy mass eigenstates in the Higgs and gauge sector by , , and respectively. The lightest mass eigenstates, and can be identified with the GeV SM Higgs and the SM boson, respectively.

The DM acquires a mass through the Yukawa coupling to the dark Higgs

(19)

Due to the charge assignements, the coupling of the DM to the dark gauge boson interaction eigenstate is purely axial-vector. The DM-Higgs Yukawa coupling also induces a purely scalar coupling between DM and the dark Higgs interaction eigenstate . The DM interaction Lagrangian can then be written as

(20)

The model now has seven independent parameters

(21)

to be constrained.

Figure 1: Vertices involving the hidden sector particles in the model detailed in Sec. II

.

ii.1 The Heavy Limit

Since we want to derive upper bounds on the masses of the particles in the hidden sector, we are particularly interested in the limit where these particles are heavy. In this limit, the mass mixings become negligible and we can work in the gauge eigenstate basis. Since kinetic mixing does not vanish at large masses, we work in the kinetic mixing eigenbasis, using the fields , , and .

The masses of the hidden sector particles in the heavy limit are

(22)

The kinetic mixing induces a non-zero coupling of the to SM particles of the form

(23)

This coupling does not vanish when the becomes heavy, and will play an important role in the s-channel annihilation of dark matter, as highlighted in Sec. IV. The vertices involving hidden sector particles are shown in Fig. 1. In this heavy limit, DM annihilation will be driven by the and couplings, and, in some channels, by the kinetic mixing .

ii.2 Precision Electroweak Constraints

Models with a hidden boson are generally expected to be constrained by precision electroweak measurements. Since the pole mass, the electron charge and the physical Weinberg angle have been measured very precisely, we set them to be equal to their SM values. Keeping these parameters fixed allows other parameters to deviate from their SM values. In particular, becomes

(24)

which is then in general not equal to the physical Weinberg angle. As shown in Babu:1997st (); Wells:2008xg (); Peskin:1991sw (); Holdom:1990xp (), the parameters that leads to the tightest precision electroweak constraints on the model introduced here are

(25)
(26)
(27)

where

(28)

We follow Wells:2008xg () and require .

Iii Constraints from Unitarity

This section details how to apply unitarity constraints on different scattering processes in the model studied. Although the scattering matrix is always unitary when resummed over all orders, it is not unitary at tree-level. As demonstrated in Aydemir:2012nz (), unitarity is restored by loop corrections. Schuessler and Zeppenfeld in Schuessler:2007av (); Schuessler:thesis () have derived a simple geometric argument that uses the tree-level scattering amplitudes to conservatively estimate the minimal amount of loop corrections needed to make a theory unitary. In particular, if the scattering amplitudes for a given process are too large at tree-level, large loop corrections are needed to restore unitarity and the theory is no longer perturbative. As mentioned in the introduction, if the couplings of the particle to Higgs or gauge bosons are non-perturbative, the DM candidate we have to consider is the bound state. The processes corresponding to the annihilation of and will then correspond to decay modes for the true dark matter particle, which then cannot be a suitable DM candidate because it has fast decays. In order for our model to provide a viable explanation for DM, the couplings and thus must be perturbative.

In what follows, we apply the procedure outlined in Schuessler:2007av (); Schuessler:thesis () and explained in detail in the case of the NMSSM in Betre:2014sra (). In order to enforce perturbativity, we require that the loop corrections to the scattering amplitudes studied have to be less than of the corresponding tree-level amplitudes. As shown in Schuessler:2007av (); Schuessler:thesis (), this perturbativity requirement translates into an upper bound on the eigenvalues of the partial-wave components of the transition operator , defined as

(29)

with , the S-matrix. Denoting the jth partial wave component of this operator by , the perturbativity requirement becomes

(30)

Generally, lower provide stronger bounds. In what follows, we will consider either the s-wave () or the p-wave () components of the scattering amplitudes. In what follows, we will work in the limit where

(31)

iii.1 Dark Matter Scattering Amplitudes

Ideally, setting bounds on scattering amplitudes in the s-wave provides the best constraints. However, in the case of fermion scatterings in the large limit, diagrams with an intermediate gauge boson exhibit a Coulomb-like pole. In this case, the amplitudes are logarithmically divergent at tree-level. Once higher order corrections are applied, we find that this logarithmic divergence corresponds in fact to the first term of the expansion of a phase and does not lead to perturbativity/unitarity violations. Applying unitarity bounds on tree-level scattering amplitudes then does not work in the s-wave, as it is sensitive to the logarithmic divergence. The p-wave scattering is not sensitive to this divergence, and unitarity constraints in the p-wave provide generally weaker but still non-trivial bounds.

In the p-wave, we consider the following fermion and scalar pairs

(32)

The and are the fermion helicities (also right and left). Since we work in the large limit, we can work in the interaction eigenstate basis. The p-wave scattering matrix in this basis is

(33)

We enforce the perturbativity requirement by requiring that the eigenvalues of verify

(34)

Fig. 2 shows the resulting unitarity bounds on and for and . The bounds depend only weakly on and can be estimated as

(35)
Figure 2: Unitarity bounds on and for (blue) and (red). To enforce perturbativity, we require the loop corrections to the scattering amplitudes to be less than of the tree-level value, which corresponds to the bounds shown in Eq. 34.

iii.2 Scalar-Scalar scattering amplitudes

At large , only the scalar four-point interactions contribute to the scattering amplitudes. Here, we can work in the s-wave if we consider the following set of pairs

(36)

In the interaction eigenstate basis, does not scatter against the first two states so we can consider the scattering matrix of the states and . In the s-wave, this matrix is

(37)

Requiring as before leads to

(38)

The maximum allowed values for are shown in Fig. 3 in function of and . Here, we also require that the vacuum be stable. This requirement provides an upper bound on of the form

(39)

The highest upper bounds on and are

(40)
Figure 3: Contours of the maximum values of versus and . We apply the unitarity bounds shown in Eq. 34 as well as the vacuum stability requirement from Eq. 39.

Iv Constraints on the Dark Matter Sector

iv.1 Relic Density

In the model studied, DM has a large number of possible annihilation channels. We can distinguish two sectors:

The s-channel sector:

In this region of parameter space, DM is either lighter than both the dark Higgs and the or close to an s-channel resonance. t-channel annihilation to a dark Higgs or a is then kinematically forbidden in the first case and largely subdominant in the second case. If the boson is not too much heavier than DM and DM is outside the Higgs funnel regions, DM will annihilate dominantly to SM fermions through s-channel exchange. If DM is much heavier than the SM fermions, annihilation occurs dominantly through p-wave. Writing the annihilation cross section times velocity as

(41)

the p-wave term is approximately

(42)

The reason why this annihilation channel dominates for heavy DM is that the couplings associated to the diagram are kinetic mixing suppressed and not mass mixing suppressed. Therefore, they do not vanish when the becomes heavy. Away from the s-channel resonance, the relic density constraint will provide a lower bound on , which –for heavy DM– will be in tension with the unitarity bound derived in Sec. III. Close to the s-channel resonance, low values for will still be allowed and the bounds on the DM mass will become much looser. If the is much heavier than DM and the dark Higgs, it can be integrated out and the model reduces to a pure Higgs portal, which has been described in detail in Walker:2013hka ().

The t-channel sector:

As soon as t-channel annihilation to hidden sector particles is kinematically allowed, it becomes the dominant annihilation mode for DM if the latter is away from funnel regions. t-channel annihilation to the hidden sector opens up when the DM is heavier than either the dark Higgs or the dark gauge boson. The corresponding diagrams are shown in Fig. 4. These channels in fact correspond to processes where DM annihilates to four SM particles via on-shell hidden sector particles, as shown in Fig. 5. The corresponding cross section can be written as

(43)

Generically, the branching ratios for hidden sector decays to SM are very close to . In our study, we assume them to always be , which leads to conservative estimates for the final upper bounds. The annihilation cross section in the t-channel region is then

(44)

Fig. 4 shows the coupling products associated to each annihilation diagram. Depending on what diagram dominates, the relic density requirement will then set lower bounds on either , or .

Figure 4: t-channel annihilation diagrams for Dark Matter in the model with the corresponding coupling factors.
Figure 5: Example of a Dark Matter annihilation process, via two on-shell bosons. Similar processes with intermediate heavy Higgs bosons are also possible. Each of the intermediate particles decays to two SM particles.

iv.2 Direct Detection Bounds

Since both the dark Higgs and the mix with their SM counterpart, DM spin-independent scattering with nuclei is allowed at tree-level. The scattering occurs in the t-channel through the diagrams shown in Fig. 6. The diagrams associated to a Higgs exchange, however, are mass mixing suppressed and proportional to the small Higgs Yukawa couplings to the and quarks. Diagrams with an intermediate are suppressed only by the kinetic mixing. However, the associated spin-independent cross section is velocity suppressed. The spin-independent direct detection (DD) cross section for our model is then expected to be extremely small and the current and future DM DD experiments are not expected to set any significant bounds on the DM mass. Since the current spin-dependent DD bounds are very loose, we do not expect them to give any additional constraint in the heavy DM sector.

Figure 6: Processes contributing dominantly to the DM direct detection cross section.

V Results

We perform a uniform scan over the set of parameters shown in Eq. 21. We fix the coupling by requiring the lightest Higgs mass to be 125 at tree-level. which reduces the number of parameters to six. We eliminate points that do not satisfy the EWPT, unitarity and relic abundance constraints detailed in Sec. II, III, IV respectively. We generate the model described in Sec. II using FeynRules Alloul:2013bka () and compute the DM relic density using MicrOmegas Belanger:2013oya () interfaced with CalcHEP Belyaev:2012qa (). We allow the DM, , to be a subdominant component of the measured relic abundance,

(45)

and therefore require the relic density to be less than its Planck value Ade:2013lta () plus .

We scan over the following regions of parameter space,

(46)
(47)
(48)
(49)
(50)
(51)

We apply the EWPT, unitarity and relic density constraints described in Sec. II, III and IV. The bounds associated to these different constraints are expected to be significantly loosened near s-channel resonances. In order to best identify these “funnel regions”, we define a fine tuning factor , as

(52)

If a parameter point is close to an s-channel resonance, will be small. The bounds quoted in this paper hold for . Since the low- funnel regions are particularly narrow, the bounds derived in this work can be considered generic in the context of a model.

Figure 7: vs. for the points that survive the EWPT, unitarity and relic density cuts. The red line is at . The low funnel region as well as the large -channel region, both described in the main text, can be clearly distinguished.
Figure 8: vs. for the points that survive the EWPT, unitarity and relic density cuts in the “pure gauge” scenario described in Eq. 55 (in red). The black line at corresponds to the upper bound on the DM mass for these “pure gauge” points. The sharp feature around is due to the first condition in Eq. 55. The low funnel region as well as the large -channel region, both described in the main text, can be clearly distinguished. The points corresponding to the mixed Higgs-gauge portal scenario shown in Fig. 7 are shown in light blue.


Fig. 7 shows the points that survive all the EWPT, unitarity and relic density constraints in the vs. plane. In this plane, the surviving points can be grouped into two distinct regions. The first region, also shown isolatedly in Fig. 9 corresponds to the -channel region described in Sec. IV. In this region, DM annihilates dominantly through -channel processes. As can be seen in Fig. 9, beyond about , only points close to -channel resonances can satisfy the relic abundance requirement and the allowed values for become lower as DM gets heavier. For DM masses larger than about efficient annihilation can occur only for . The second region in Fig. 7 corresponds to the -channel region introduced in Sec. IV. Here, DM annihilation is dominated by -channel annihilations to dark Higgs and/or gauge bosons. For , only a few of these processes are kinematically allowed. As can be seen in Fig. 7, then needs to increase with the DM mass in order to open more annihilation channels. For , all the -channel annihilation modes are allowed and the only way to increase the DM annihilation cross section is to increase the DM couplings. When these couplings reach their unitarity bounds, the DM mass reaches its maximum, which corresponds to the vertical cutoff for on Fig. 7. This cutoff corresponds to a DM mass of .

Fig. 8 shows the points that survive all the cuts and for which Dark Matter annihilate dominantly through modes involving only dark gauge bosons. We identify this “pure gauge” sector using the following criteria

(53)
(54)
(55)

The first requirement cuts away the dark Higgs funnel region while the second and third requirements forbid t-channel DM annihilation to final states involving a dark Higgs boson. For , the bound on the DM mass in this “pure gauge” sector is of about .

Figs 10 and 11 show the non-resonant points that survive all the EWPT, unitarity and relic density constraints in the plane and the plane, respectively. The blue points correspond to the mixed Higgs-gauge portal scenario while the yellow points on Fig. 11 correspond to the “pure gauge scenario”. The bound on the dark Higgs mass is of about . The bound on the mass is of about for . However, except for a few points close to the funnel regions, most points of the parameter space correspond to masses below . If we consider only the “pure gauge” points, the bound on the dark gauge boson mass goes down to . For perturbative DM and Higgs sectors, unitarity and relic density constraints then allow to set a bound of about on the masses of the DM and the dark Higgs and gauge bosons.

Figure 9: vs. for the points that survive the EWPT, unitarity and relic density cuts and annihilate dominantly through s-channel diagrams. The red line is at .
Figure 10: vs. for the points that survive the EWPT, unitarity and relic density cuts for . The region around that is sharply cut corresponds to the removed funnel region ().
Figure 11: vs. for the points that survive the EWPT, unitarity and relic density cuts for . The region around that is sharply cut corresponds to the removed funnel region (). The mixed Higgs-gauge points are shown in blue while the “pure gauge” points described in Eq. 55 are shown in yellow.
Figure 12: vs. for the points that survive the EWPT, unitarity and relic density cuts. In addition, we require .


The increasing sensitivity of accelerator, direct and indirect searches for dark matter provides an opportunity to definitively probe the gauge portal. In Figure 12, we plot versus . As a reminder, because of equation 23, the cross section scales as

(56)

A few of the points in Figure 12 for may lead to a greater sensitivity for accelerator and indirect searches in comparison to sequential SM models. The points for may be problematic. Moreover as described above, our model enhances the effective operators

(57)

which correspond to a DM-nucleon scattering cross section that is either velocity suppressed or spin-dependent. Thus, the spin-independent dark matter-nucleon cross section, to which the current experiments are highly sensitive, is small. A different model with a non-trivial operator

(58)

could give a significant signal in direct detection experiments. We postpone a thorough examination of these issues for future work.

Vi Conclusion

In this paper, we showed that combining perturbative unitarity and relic abundance constraints on dark matter in a generic gauge portal model allows upper bounds to be set on the dark matter, dark and dark Higgs masses. The bounds derived here are significantly improved with respect to the Griest and Kamionkowski bound Griest:1989wd (). The bounds shown in this paper are valid for all the model parameter space except in the narrow dark Higgs and funnel regions.

Finding the next scale of new physics is a crucial question for current and future experiments. Although naturalness provides strong arguments in favor of new physics around the scale, the existence of dark matter is one of the most compelling reason for new physics. Using fundamental principles in concert with experimental measurements to better constrain the DM sector provides a new avenue for cornering new physics at future colliders and DM experiments. For the model of dark matter explored here the most sensitive probes are future collider searches for new bosons. We find that there is a finite mass window within which dark matter and its associated new particles can appear, requiring that the be lighter than if it is dominantly responsible for dark matter annihilations. This is a very promising region of parameter space for future high-energy colliders.

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