1 Introduction

{centering} SIMP dark matter with gauged symmetry

Soo-Min Choi and Hyun Min Lee

Department of Physics, Chung-Ang University, Seoul 156-756, Korea.

We consider a complex scalar field as SIMP dark matter in models with gauged discrete symmetry appearing as a remnant of dark local . Dark matter (DM) annihilates dominantly by the 3-to-2 scattering, due to the DM cubic coupling in combination with the DM quartic coupling or the gauge and dark Higgs couplings. We show that a light gauge boson makes DM in kinetic equilibrium with thermal plasma at freeze-out and it affects the DM relic density and perturbativity/unitarity constraints for DM self-interactions. We show that the large DM self-interactions are consistent with solving small-scale structure problems and explaining the DM halo separation recently observed in Abell 3827 cluster. Various bounds on the model from the SIMP conditions, DM self-interactions, searches, DM direct/indirect detection experiments, and Higgs signals, are also discussed.

Email: sm90515@cau.ac.kr

Email: hminlee@cau.ac.kr

## 1 Introduction

It is known that dark matter (DM) makes up about 85% of the matter density in the Universe [1] but the identity of dark matter has been regarded as one of the big mysteries in particle physics and cosmology communities. The Weakly Interacting Massive Particles (WIMP) paradigm has driven most of DM searches in terrestrial and satellite experiments, and typically, the abundance of WIMP is determined from the thermal number density at the time of freeze-out in terms of weak-scale DM mass and weak interactions with the SM particles. However, there has been no direct evidence for dark matter other than gravitational or cosmological effects and there are strong limits on the spin-independent DM-nucleon cross section [2, 3]. Therefore, it is also important to look for alternative testable scenarios for dark matter other than WIMP.

Strong Interacting Massive Particles (SIMP) [4, 5] have recently drawn attention due to the interesting property that a sub-GeV dark matter can be thermally produced due to (effective) 5-point self-interactions. SIMP dark matter might provide a new arena for the model building for dark matter that can be testable in the future dark matter searches. Large self-interactions of SIMP dark matter can play a role at the galaxy scales, for instance, for solving the cusp-core and too-big-to-fail problems [6, 7] and explaining the recently observed evidence for self-interacting dark matter in Abell 3827 cluster, namely, the separation between the dark matter halo and the galaxy’s stars [8, 9, 10]. Furthermore, the interactions of a light mediator between SIMP and the SM particles can be probed by various indirect and direct experiments [5].

In this article, as a SIMP dark matter candidate, we consider a complex scalar charged under a dark local , that is spontaneously broken down to a discrete group, after another complex scalar gets a nonzero VEV. The remaining symmetry ensures the stability of dark matter and generates the cubic self-interaction of dark matter dynamically due to the breaking. As a consequence, dark matter can self-annihilate through the 3-to-2 scattering processes, thanks to the help of DM quartic coupling or gauge and dark Higgs coupling. The dark Higgs could be a potential mediator to keep dark matter in thermal equilibrium via a mixing with the SM Higgs but it turns out to be insufficient due to the smallness of Higgs Yukawa couplings to the SM fermions at the time of SIMP freeze-out. Instead, the gauge boson or dark photon can mediate for DM to scatter off the SM fermions sufficiently in the presence of a gauge kinetic mixing [5].

We show that the gauge boson also gives sizable contributions to the DM annihilation and scattering processes for most of natural parameters of the model, while helping to realize SIMP as a thermal dark matter. We constrain the parameter space of our SIMP dark matter by considering the bounds coming from Bullet cluster [11] and halo shapes [12] and find that our model can accommodate a potential hint for self-interacting dark matter from Abell 3827 cluster as estimated in Ref. [10]. Various limits from direct and indirect searches for a light gauge boson are considered and compared to the SIMP conditions on the model. The direct detection of SIMP dark matter with electron recoil [13, 14] and the bound from indirect detection and the bound from Higgs signals are also briefly discussed.

The paper is organized as follows. We begin to describe the model of a complex scalar dark matter with gauge symmetry. Then, we present the results of the 3-to-2 annihilation and self-scattering processes of dark matter and consider the bounds on DM self-interactions. Next we show the complementarity of the SIMP conditions for the searches at colliders and comment on the direct/indirect detection of dark matter and the impact on Higgs signals. Finally, conclusions are drawn. There are two appendices summarizing the Higgs-portal and -portal interactions and the general formulas for annihilation and scattering cross sections.

## 2 The model

We consider dark matter as a complex scalar having a charge under the local symmetry, which is spontaneously broken by the VEV of another complex scalar with charge . Thus, the remaining discrete symmetry is of the gauge symmetry origin [15, 16] and ensures the stability of scalar dark matter . The SM particles are assumed to be neutral under . The charges are summarized in Table 1.

The Lagrangian for those scalars and the SM Higgs doublet is given 111The same local model has been considered for WIMP dark matter in Ref. [17] and the global case has been also studied in the context of WIMP [18] or SIMP [19] dark matter. by

 L=−14VμνVμν−12sinξVμνBμν+|Dμϕ|2+|Dμχ|2+|DμH|2−V(ϕ,χ,H) (1)

where the field strength tensor for dark photon is , and covariant derivatives are , , and , and the gauge kinetic mixing between dark photon and hypercharge gauge boson is introduced by . Then, the dark photon communicates between dark matter and the SM particles through the gauge kinetic mixing.

The scalar potential is with

 VDM = −m2ϕ|ϕ|2+m2χ|χ|2+λϕ|ϕ|4+λχ|χ|4+λϕχ|ϕ|2|χ|2 (2) +(√23!κϕ†χ3+h.c.)+λϕH|ϕ|2|H|2+λχH|χ|2|H|2, VSM = −m2H|H|2+λH|H|4. (3)

Here, we note that are dimensionless self-couplings of dark matter, is the coupling between dark matter and dark Higgs, and are Higgs-portal couplings. As will be shown in a later discussion on SIMP dark matter, the dark photon couplings to the SM fermions become important for keeping dark matter in kinetic equilibrium with the SM. Thus, although the Higgs-portal couplings could be interesting for direct/indirect detection, we focus on the -portal in the later discussion.

For a nonzero VEV of with , the symmetry is broken to a discrete subgroup and dark photon gets massive and can mix with the SM Z-boson. After expanding the dark Higgs as , the dark Higgs can mix with the SM Higgs by Higgs-portal interaction, . The interaction terms for dark/SM Higgses and dark photon are given in the appendix A .

## 3 Dynamics of SIMP dark matter

When dark Higgs and dark photon are heavier than dark matter, a pair of dark matter annihilate into neither a single dark matter a single dark Higgs (semi-annihilation) nor a pair of dark Higgses/dark photons (pair-annihilation). Nonetheless, dark Higgs and contribute to DM annihilation and scattering processes as intermediate states. Dark Higgs and can decay into a DM pair dominantly if kinematically allowed. For a sizable dark Higgs-DM coupling and gauge coupling, dark Higgs and would decay before the SIMP freeze-out, so they would not contribute to the observed DM relic density from their decays.

Due to the remnant discrete symmetry, dark matter self-annihilates dominantly through the following 3-to-2 self-annihilation processes, , , and their complex conjugates, as shown in Figs. 1 and 2. The scattering processes can be mediated by dark/SM Higgses or dark photon/SM -boson. In the presence of Higgs and/or portal interactions, the 2-to-2 annihilation such as with being the SM fermion is possible. The effect of the latter process will be discussed in the next section. We have adapted the CalcHEP package [20] to our model in order to compute the scattering matrix elements of DM annihilation processes.

As will be discussed in a later section, the portal interaction is important for keeping dark matter in kinetic equilibrium with the SM. We consider both and dark Higgs interactions to DM in computing the 3-to-2 annihilation cross sections, but we ignore the and Higgs portal interactions to the SM particles in this section. First, the squared amplitude for scattering is, in the non-relativistic limit, given by

 |Mχχχ∗→χ∗χ∗|2 = R216m2χ(74λχ−117R2−200g2Dm2χm2χ+m2Z′ (4)

where . Likewise, the squared amplitude for scattering is, in the non-relativistic limit, given by

 |Mχχχ→χχ∗|2 = 3R2m2χ(2λχ+9R2+25g2Dm2χm2χ+m2Z′ (5) +2λϕχm2χ(13m2χ−2m2h1)−λ2ϕχ(19m2χ−m2h1)m2Z′/(9g2D)(9m2χ−m2h1)(m2χ+m2h1))2

A nonzero cubic DM self-coupling only can make both 3-to-2 annihilation channels possible. Nonzero DM quartic coupling, dark gauge and dark Higgs couplings, can reduce or enhance the squared amplitudes, but the parameter space of DM self-couplings becomes strongly constrained due to unitarity bounds as will be discussed later.

Assuming CP conservation in the dark sector, the Boltzmann equation for dark matter number density, , with , is

 dnDMdt+3HnDM = −14(⟨σv2rel⟩χχχ∗→χ∗χ∗+⟨σv2rel⟩χχχ→χχ∗)(n3DM−n2DMneqDM) (6) −12⟨σvrel⟩χχ∗→¯ff(n2DM−(neqDM)2).

As a consequence, using the general formulas for the cross sections in Appendix B, the effective 3-to-2 annihilation cross section appearing in the above Boltzmann equation is obtained as

 ⟨σv2rel⟩3→2 = 14(⟨σv2rel⟩χχχ∗→χ∗χ∗+⟨σv2rel⟩χχχ→χχ∗) (7) = √51536πm3χ(|Mχχχ∗→χ∗χ∗|2+|Mχχχ→χχ∗|2)≡α3effm5χ.

Here, we note that the 2-to-2 annihilation channels in the dark sector are kinematically forbidden while mediators are assumed to couple to the SM particles weakly enough so that we can ignore the annihilation of dark matter into the SM particles.

Therefore, when the 3-to-2 annihilation is the dominant process at freeze-out, the relic density is determined by , leading the relic density condition [4, 5] as follows,

 mχ=αeff(κ2x4F√90g∗π2T2eqMP)1/3 (8)

where is the effective coupling of dark matter in the 3-to-2 annihilation defined in eq. (7) and is the temperature at matter-radiation equality given by . Taking , and for the temperature , and for , the above condition becomes

 mχ=0.03αeff(T2eqMP)1/3. (9)

For , we get . In the next section, we search for the parameter space where is of right magnitude for the SIMP dark matter, being compatible with perturbativity and unitarity and the bounds on the DM self-interactions. From the relic density condition (9) and the DM effective 3-to-2 interaction given in eq. (7), we find one of the DM parameters dependent, i.e., the DM quartic coupling is now a dependent parameter by .

## 4 Bounds on SIMP dark matter

In this section, we consider various bounds on SIMP dark matter, starting with bounds on DM self-interactions and -portal couplings to the SM fermions. The SIMP conditions provide new constraints on the parameter space of dark photon, being complementary to the searches at colliders. Direct detection of SIMP dark matter with electron recoil, indirect detection bounds and the impact on Higgs signals, are also discussed.

### 4.1 Self-scattering cross section

Dark matter self-scatters through the following 2-to-2 scattering processes, , its complex conjugate, and , as in Fig. 3. Like in the 3-to-2 self-annihilation, we include both dark Higgs and contributions to the scattering processes.

First, the squared amplitude for the self-scattering is

 |Mχχ|2=2(2λχ+3R2+4g2Dm2χm2Z′−λ2ϕχm2Z′9g2Dm2h1)2. (10)

On the other hand, the squared amplitude for the self-scattering is

 |Mχχ∗|2=4⎛⎝2λχ−9R2−2g2Dm2χm2Z′+λ2ϕχ(2m2χ+m2h1)m2Z′9g2D(4m2χ−m2h1)m2h1⎞⎠2. (11)

Therefore, in the non-relativistic limit for dark matter, the effective scattering cross section, with , is

 σself=164πm2χ(|Mχχ|2+|Mχχ∗|2). (12)

The self-interaction of dark matter is bounded from from Bullet cluster [11] and halo shapes [12].

We also impose the perturbativity and unitarity bounds on the DM couplings, respectively, as follows,

 λχ<4π,|Mχχ|,|Mχχ∗|<8π. (13)

We note that or its complex conjugate determines the unitarity bound dominantly.

On the left panel of Fig. 4, we present the parameter space of DM cubic coupling and DM mass by considering the relic density, the bounds from Bullet cluster and halo shapes as well as perturbativity and unitarity bounds. Here, we remind that the SIMP relic density condition, eq. (9), was solved for , and the self-scattering cross section and perturbativity/unitarity bounds were written in terms of the remaining parameters. The bound on DM self-scattering leads to a lower bound on DM mass on the left of Fig. 4. On the other hand, the perturbativity and unitarity conditions cut off the parameter space with larger DM masses, because . We find that a relatively light dark Higgs with nonzero is necessary to satisfy the unitarity bound for , because it cancels the DM self-coupling and dark gauge coupling contributions to the DM self-scattering amplitude. It turns out that the DM masses compatible with bounds on self-interactions are in the range between and depending on the dark Higgs and couplings. On the other hand, the parameter space that explains the DM halo separation observed in Abell 3827 cluster with at [10] is also shown on the right panel of Fig. 4. In this case, the DM self-interaction required for Abell 3827 can be accommodated for , namely, without dark Higgs contribution, and the DM masses range between and .

Keeping the relic density, the bounds from Bullet cluster and halo shapes as well as perturbativity and unitarity bounds, we have searched for the parameter space in dark mass vs gauge coupling on left and dark Higgs mass vs on right, in Fig. 5. We find that mass is bounded from above for a given gauge coupling while a relatively light dark Higgs with sizable is preferred. Lastly, in Fig. 6, we also depict the correlation between and dark Higgs masses, depending on gauge coupling and DM mass. In all Figs. 4-6, we marked the important constraints determining the boundaries of the remaining parameter space in the plots.

### 4.2 Z′ portal couplings to the SM

We need a nonzero interaction between dark matter and the SM particles in order for dark matter to keep in kinetic equilibrium until freeze-out, while the consequent DM annihilation into a pair of the SM particles should be subdominant as compared to the 3-to-2 DM annihilation. These are the SIMP conditions. The DM interactions with the SM particles can be induced by Higgs or portals, leading to DM annihilation or scattering as in Fig. 7. In the SIMP scenario, for a sub-GeV DM mass, it was shown that the Higgs-portal coupling is not sufficient for keeping DM in thermal equilibrium [19, 5]. But, for clarification, we present a separate discussion on the Higgs portals in a later section. In this section, we focus the -portal couplings and discuss bounds from SIMP conditions and direct searches.

In the presence of gauge kinetic mixing, dark matter can self-annihilate into a pair of the SM fermions through dark photon exchange in the s-channel as shown in the third Feynman diagram in Fig. 7. The amplitude for process is

 iMann=−igD(p1−p2)μ⋅−igμνs−m2Z′+imZ′ΓZ′⋅(−i)eQfε¯u(k1)γνv(k2) (14)

where is the electromagnetic charge of the SM fermion and for . Then, the squared amplitude is given by

 |Mann|2=4ε2Q2fe2g2D(s−m2χ)2[2(k1⋅(p1−p2))(k2⋅(p1−p2))−(k1⋅k2)(p1−p2)2−m2f(p1−p2)2]. (15)

Therefore, in the non-relativistic limit for dark matter, the annihilation cross section for with for charged leptons is

 ⟨σvrel⟩ann = 164πp01p02∫dΩ⟨|→k2|√s|Mann|2⟩ (16) =

On the other hand, dark matter can scatter with the SM fermions that are in thermal equilibrium at dark matter freeze-out. The amplitude for process as shown in the last Feynman diagram in Fig. 7 is

 iMscatt=−igD(p1+k1)μ⋅−igμνt−m2Z′⋅(−i)eQfε¯u(k2)γνu(p2) (17)

with . Then, the spin-averaged amplitude squared is given by

 |Mscatt|2=2ε2Q2fe2g2D(t−m2Z′)2[2(k2⋅(p1+k1))(p2⋅(p1+k1))−(k2⋅p2)(p1+k1)2+m2f(p1+k1)2]. (18)

Around the freeze-out, the SM fermions in thermal equilibrium are relativistic so we can take the momenta relevant for the DM-SM fermion scattering to be and , in the center of mass frame where is the scattering angle of dark matter. Therefore, we obtain the kinetic scattering cross section for with as

 ⟨σvrel⟩scatt = 164πp01p02∫dΩ⟨|→k1|√s|Mscatt|2⟩ (19) = 3ε2e2g2Dm2χ2πm4Z′(Tmχ)≡δ22m2χ.

The cross section for process is given by the same formula in eq. (19).

The SIMP conditions are imposed at freeze-out temperature, as follows,

 nDM⟨σvrel⟩ann

The above conditions (20) constrain the 2-to-2 annihilation cross section and the dark matter kinetic scattering in terms of defined in eqs. (16) and (19) and , as follows,

 δ1≲2.4×10−6αeff,δ2≳10−9α1/2eff. (21)

Then, using eqs. (16) and (19) with , the SIMP conditions bound the dark gauge coupling and the gauge kinetic mixing as a function of dark photon mass as

 2.2×10−8α1/2effm2Z′m2χ≲|ε|gD≲4.4×10−5αeff ⎷(4−m2Z′m2χ)2+Γ2Z′m2Z′m2χ. (22)

The parameter space of dark photon can be constrained by direct searches at colliders [21, 22, 23, 24, 25, 26, 27] and lepton experiments [28], etc. There has been a recent study on the limits on light dark matter in the context of a vector messenger [27]. In Fig. 8, various limits are imposed in the parameter space of the gauge kinetic mixing vs , and some values of DM-electron scattering cross sections are presented. The direct limits from monophoton MET at BaBar in light blue[22, 23, 24, 25] and the future prospects at Belle2 in dashed lines [24] are given; the indirect limits from electron in orange and EWPT are presented; the muon favored region in green is shown too. The SIMP conditions, (SIMP I in red is the dominance of the 2-to-2 annihilation into the SM fermions while SIMP II in purple is the decoupling of SIMP from thermal plasma), rule out the parameter space that is not covered by direct and indirect limits on dark photon. The parameter space with in gray is ruled out due to the dominance of the 2-to-2 annihilation into dark photons.

The recent BaBar search for monophoton dilepton (not shown) [26] can limit at the level of for dark photon masses in the range GeV, but the limits depend on the decay branching fraction of dark photon. When the decay of dark photon into a pair of dark matter is open, it dominates easily, so the previously mentioned monophoton MET is more constraining. For instance, the monophoton MET at BaBar applies for dark photon mass being above in Fig. 8, while the monophoton dilepton at Babar applies and limits at the level of for . There are other bounds from beam dump experiments (not shown) [21, 25] that limit at the level of in our parameter space below . The planned SPS target experiment at CERN [29] could improve the limits from beam dump experiments further.

### 4.3 Direct detection

In the case of , which is true of our SIMP dark matter 222When the momentum transfer of order is greater than mass, then the DM scattering cross section becomes enhanced due to a Coulomb singularity [14]. , we can take the momenta, and , in the calculation of the matrix element squared in eq. (18). Then, the DM-electron scattering cross section with -portal interaction is, at present,

 σDD = 164π2s∫dΩ|→k1||→p1||Mscatt|2 (23) = ε2e2g2Dμ2πm4Z′

where is the reduced mass of the DM-electron system. For , the DM-electron scattering cross section depends little on the DM mass, but is sensitive to the gauge coupling and mass of dark photon. The electron recoil energy can be used to search for the signal of a sub-GeV light dark matter [13, 14].

In Fig. 9, we depict the DM-electron scattering cross section as a function of the mass by varying the dark photon gauge coupling between but with fixed gauge kinetic mixing . The result is insensitive to the SIMP mass, which ranges between and as shown from the left figure of Fig. 4. In Fig. 8, we also present the DM-electron scattering cross section on the parameter space of vs . The direct search for dark matter with electron recoil in XENON10 [13] can give stronger bounds than beam dump experiments, at the level of for with . XENON10 [13] constrains the DM-electron scattering cross section to be below at best at about so the SIMP parameter space in our model that is compatible with direct searches satisfies the current XENON10 limits. But, the case with a light gauge boson could be also probed by future superconducting detectors [14].

### 4.4 Higgs portal couplings and Higgs signals

We discuss the impact of Higgs portal couplings on the DM scattering and annihilation processes. As shown in the second Feynman diagrams in Fig. 7, the SM Higgs and the dark Higgs contribute to the DM scattering with the SM charged leptons. The corresponding annihilation cross section is given by

 ⟨σvrel⟩χf→χf=116πm2χ(mfv)2∣∣ ∣∣yh1χ∗χm2h1+yh2χ∗χm2h2∣∣ ∣∣2(3mχTF+m2f) (24)

where is the freeze-out temperature and and .

On the other hand, the annihilation cross section for is

 ⟨σvrel⟩χχ∗→f¯f=14π(mfv)2(1−m2fm2χ)3/2∣∣ ∣∣yh1χ∗χ4m2χ−m2h1+yh2χ∗χ4m2χ−m2h2∣∣ ∣∣2. (25)

We digress to the bounds from Higgs signals, which constrain the Higgs mixing angle and the DM coupling to the SM Higgs, . The bound on the branching fraction of the Higgs invisible decay is at CL from the VBF Higgs production at ATLAS [33]. The production at ATLAS [34] and the VBF production CMS [35] leads to less strong bounds, and , respectively. On the other hand, the Higgs signal strength is bounded to at CL from ATLAS/CMS data combined [36].

The partial decay rates for additional Higgs decay modes in our model are

 Γ(h2→χχ∗) = y2h2χ∗χ16πmh2 ⎷1−4m2χm2h2, (26) Γ(h2→h1h1) ≃ λ2ϕHv232πmh2 ⎷1−4m2h1m2h2. (27)

Then, from the bound on the Higgs invisible decay, we obtain . On the other hand, scaling the total and individual Higgs decay rates as well as the Higgs production cross section approximately by , the Higgs signals bounds the Higgs mixing angle as . In our case, the Higgs mixing angle is approximated to for , and . Thus, it is consistent with the Higgs visible decays. Given the bounds, and , we find that the dark Higgs contributes dominantly to the DM scattering and annihilation, as compared to the SM Higgs. As for portal, we can parametrize the 2-to-2 cross sections with dark Higgs exchanges by and , in eqs. (25) and (24), respectively. Therefore, taking the charged lepton to be electron or positron 333When DM is heavier than muon, it can annihilate into a muon pair too. But, the DM scattering rate with muon is suppressed by Boltzmann factor at freeze-out [5], because the typical freeze-out temperature is small, . and choosing , we get . Therefore, unless , the Higgs portal does not satisfy the SIMP condition.

### 4.5 Indirect detection

The SIMP dark matter can be searched for by indirect detection experiments with diffuse gamma-rays. Although the Fermi-LAT is sensitive to gamma-rays of energies from to , its current limits, for instance, from dwarf spheroidal galaxies (dSphs) of the Milky Way [30], do not extend down to . On the other hand, the AMS positron fraction in primary cosmic rays is within the energy range from 0.5 to 500 GeV [31]. The current best upper limits on annihilation cross section is at from Fermi-LAT dSphs [30] and at similar DM masses from AMS-02 positron fraction [32]. More importantly, there are diffuse X-ray and gamma-ray observations near the center of the galaxy such as INTEGRAL [37], COMPTEL [38] and EGRET [39] and Fermi-LAT [40]. In particular, COMPTEL leads to the bounds stronger than the thermal annihilation cross section around , for DM masses below [41].

SIMP can annihilate into or depending on its mass, through or Higgs portal with the annihilation cross section,

 ⟨σvrel⟩l+l−=(1.2×10−27cm3/s)(δ110−6)2(100MeVmχ)2. (28)

In the case of portal, the annihilation cross section is p-wave suppressed as where from the SIMP condition, we get at present. On the other hand, the annihilation cross section with Higgs-portal is given by , which could be as large as for . Therefore, in either or Higgs portal, there is no current bound from indirect detection.

## 5 Conclusions

We have shown that models with gauged symmetry provide a consistent SIMP scalar dark matter with sub-GeV masses that can be in kinetic equilibrium with the SM fermions via -portal interactions. The resulting large self-scattering cross section of the SIMP dark matter could explain the DM halo separation observed in Abell 3827 cluster, although there is a tension with the previous bounds coming from Bullet cluster and halo shapes. Inclusion of gauge boson and dark Higgs changes DM annihilation and scattering processes and opens up a new parameter space of the SIMP self-couplings and masses. We found that SIMP conditions are complementary to indirect and collider searches, DM direct/indirect detection and Higgs signals. The SIMP parameter space could be explored further by future collider and indirect/direct detection experiments.

## Acknowledgments

We would like to thank Jong-Chul Park, Seong Chan Park and Min-Seok Seo for discussion. The work of HML is supported in part by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (2013R1A1A2007919). The work of SMC is supported by the Chung-Ang University Graduate Research Scholarship in 2015.

Appendix A: Higgs and portal interactions to dark matter

After the breakdown of electroweak symmetry and dark , we can take the SM Higgs and dark Higgs in unitary gauge,

 H=1√2(0v+h),ϕ=1√2(v′+h′). (A.1)

On the other hand, the VEV of scalar dark matter is assumed to vanish. Then, the mass matrix for is given by

 M=(2λϕv′2λϕHv′vλϕHv′v2λHv2). (A.2)

where the VEVs are determined by the following conditions,

 v2=4λϕm2H−2λϕHm2ϕ4λHλϕ−λ2ϕH,v′2=4λHm2ϕ−2λϕHm2H4λHλϕ−λ2ϕH. (A.3)

Then, the conditions for a local minimum are

 4λϕλH>λ2ϕH,λϕ>0,λH>0, (A.4) 2λϕm2H−λϕHm2ϕ>0, (A.5) 2λHm2ϕ−λϕHm2H>0. (A.6)

The mass matrix can be diagonalized by the rotation by

 (h1h2)=(cosθ−sinθsinθcosθ)(h′h) (A.7)

where are mass eigenstates. The mass eigenvalues of Higgs-like states are

 m2h1,h2=λϕv′2+λHv2∓√(λϕv′2−λHv2)2+λ2ϕHv′2v2 (A.8)

and the mixing angle is

 tan2θ=λϕHv′vλHv2−λϕv′2. (A.9)

Consequently, the self-interactions and Higgs-portal interactions of dark matter are

 −Lscalar = (λϕχv′cosθ−λχHvsinθ)h1|χ|2+(λϕχv′sinθ+λχHvcosθ)h2|χ|2 (A.10) +12(λϕχcos2θ+λχHsin2θ)h21|χ|2+12(λϕχsin2θ+λχHcos2θ)h22|χ|2 +(λϕχ−λχH)sinθcosθh1