Signals of Leptophilic Dark Matter at the ILC

# Signals of Leptophilic Dark Matter at the ILC

Sukanta Dutta\thanksrefaddr1,e1 SGTB Khalsa College, University of Delhi. Delhi-110007. India.Department of Physics and Astrophysics, University of Delhi. Delhi-110007. India.    Bharti Rawat \thanksrefaddr2,e2 SGTB Khalsa College, University of Delhi. Delhi-110007. India.Department of Physics and Astrophysics, University of Delhi. Delhi-110007. India.    Divya Sachdeva \thanksrefaddr2,e3 SGTB Khalsa College, University of Delhi. Delhi-110007. India.Department of Physics and Astrophysics, University of Delhi. Delhi-110007. India.
###### Abstract

Adopting a model independent approach, we constrain the various effective interactions of leptophilic DM particle with the visible world from the WMAP and Planck data. The thermally averaged indirect DM annihilation cross-section and the DM-electron direct-detection cross-section for such a DM candidate are observed to be consistent with the respective experimental data.

We study the production of cosmologically allowed leptophilic DM in association with , at the ILC. We perform the analysis and compute the 99% C.L. acceptance contours in the and plane from the two dimensional differential distributions of various kinematic observables obtained after employing parton showering and hadronization to the simulated data. We observe that the dominant hadronic channel provides the best kinematic reach of 2.62 TeV ( = 25 GeV), which further improves to 3.13 TeV for polarized beams at TeV and an integrated luminosity of 1 ab.

###### Keywords:

dark matter, relic density, mono- with at ILC
###### pacs:
95.35.+d, 13.66.-a, 13.66.De

\thankstext

e1e-mail: Sukanta.Dutta@gmail.com \thankstexte2Corresponding Author,   e-mail: bhartirawat87@gmail.com \thankstexte3e-mail: divyasachdeva951@gmail.com

## 1 Introduction

Dark Matter provides the most compelling explanation for many cosmological and astrophysical observations which defy an understanding in terms of luminous matter alone. However, in the absence of any direct evidence, the existence of such matter has, rightly, been questioned and several alternatives proposed, including the modification of gravity at large distance scales. It should be appreciated, though, that starting with orbital velocities of stars in a galaxy or those of the galaxies themselves in a cluster galaxy:RubinFord (), gravitational lensing grav_lensing (); weaklensing (), the dynamics of galactic (cluster) collisions Clowe:2006eq () etc., the observations span a wide range of distance scales, and no single simple modification of gravitation can explain all, whereas dark matter (DM) can and does play an important role in understanding the data. Similarly, the fitting of the cosmological observables  Hinshaw:2012aka (); Abadi:2002tt (); Ade:2015xua (), requires that DM contributes about 23% to the energy budget of the universe, in contrast to only 4% contained in baryonic matter. Finally, post-inflation, perturbations in the DM distribution, along with the gravitational perturbations, are supposed to have provided the seed for large-scale structure formation in the universe Abadi:2002tt (). The constraints from the latter are rather strong. Indeed, while neutrinos would have been logical candidates for DM within the Standard Model (SM), a large energy component in neutrinos would have disrupted structure formation. For example, a recent study claims that if the equation of state for the DM be parametrized as , then the combined fitting of the cosmic microwave background, the baryon acoustic oscillation data and the Hubble telescope data restricts , thereby clearly preferring a cold and dusty DM Thomas:2016iav ().

With the DM particle, by definition, not being allowed to have either electromagnetic111While DM with ultra-suppressed electromagnetic couplings has been considered Overduin:2004sz (), such models are extremely ungainly and are unlikely to survive closer scrutiny. or strong interaction, the most popular222An alternative could be an ultralight boson, such as that in Ref.Hui:2016ltb (). However, such a solution would, essentially, be untestable in the laboratory in the foreseeable future. Similar is the case for an ultralight gravitino DM candidate Moultaka:2006su (); Dutta:2015ega () candidate is the weakly interacting massive particle (WIMP). Recently, the authors of reference Davoudiasl:2017jke () have proposed the cosmologically allowed super-light fuzzy dark matter of the order of 10 eV which can possibly be testable in terrestrial neutrino oscillation experiments. And while its exact nature is unknown, several theoretical scenarios such as multi-Higgs models, supersymmetry, extra-dimensional theories, little Higgs models, left-right symmetric models all naturally admit viable candidates. Consequently, one of the most challenging tasks today is to identify the nature of the DM particle Feng:2010gw (). This, in principle, could be done in three kind of experiments. Direct detection can be achieved by setting up apparatii (very often ultra-cold bolometric devices) that would register the scattering of a DM particle off the detector material. While the DAMA experiment Bernabei:2013xsa () did indeed claim the existence of a DM particle of mass from observed seasonal variation in the detector signal (originating, possibly, from a varying DM wind as the Earth traverses its path), subsequent experiments like CoGeNT  Aalseth:2012if (), CRESST-II  Angloher:2016rji (), XENON100  Aprile:2016wwo (), PandaX-II  Yang:2016odq (); Tan:2016zwf () and LUX  Akerib:2016vxi () have not validated this; rather, they have only served to impose bounds in the plane described by the DM particle mass and its coupling to nucleons. Indirect detection experiments, largely satellite-based, depend on the annihilation of a pair of DM particles in to SM particles which are, subsequently, detected. Although there, occasionally, have been claims of anomalies in the data, unfortunately the experiments have failed to validate each other’s positive sightings, resulting, once again, in further constraintsFermi-LAT:2016uux (); Adriani:2008zr (); Aguilar:2013qda (). Finally, we have the collider experiments, wherein excesses (over the SM expectations) in final states with large missing momentum are looked for. It should be realized, though, that even if such an excess is established, a DM explanation would still only be an hypothesis, for the only statement that can be made with certainty is that the produced neutral and colour-singlet particle is stable over the detector dimensions.

It is the last mentioned approach that we assume in this paper. While an investigation of the nature of the DM particles needs an understanding of the underlying physics, we adopt, instead, a model independent approach. Eschewing the details of the underlying dynamics, we begin by postulating a fermionic DM particle, and consider four-fermi operators involving these and the SM fermions. The relative strengths of these operators would, of course, be determined by the underlying dynamics. We assume that the operators involving quark currents are subdominant, as could happen, for example, if the dynamics, at a more fundamental level, involved a leptophilic boson. This immediately negates the constraints from the direct detection experiments Aprile:2016wwo (); Yang:2016odq (); Tan:2016zwf (); Akerib:2016vxi () (as the dominant interactions therein are with the nucleons) as also bounds from the LHC Bhattacherjee:2012ch (); Goodman:2010ku (); Carpenter:2012rg (); Petrov:2013nia (); Carpenter:2013xra (); Berlin:2014cfa (); Lin:2013sca (); Bai:2010hh (); Birkedal:2004xn (); Gershtein:2008bf (); Fox:2011fx (); Bai:2012xg (); Crivellin:2015wva (); Petriello:2008pu (); Feng:2005gj ().

Such an assumption also alters the conclusions (on the interrelationship between the DM-mass and the coupling strength) drawn from the deduced relic density. Starting with the Boltzmann equations describing the evolution of the particle densities, we derive the constraints on the same. As for the search strategies at a linear collider, the attention of the community, so far, has been largely commandeered by the final state comprising a single photon accompanied by missing energy Chae:2012bq (); Dreiner:2012xm (); Yu:2013aca (); Bartels:2007cv (). While this continues to be an important channel, we augment this by other channels that are nearly as sensitive. Furthermore, we consider some novel effects of beam polarization.

## 2 Fermionic Dark Matter : A mini review

As we have already mentioned, rather than considering the intricacies of particular models, we adopt the more conservative yet powerful concept of an effective field theory. Assuming that we have a single-component DM in the shape of a Dirac fermion , we consider the least-suppressed (namely, dimension-six) operators involving a -current and a SM fermion-current 333We do not consider operators involving the SM bosons as they play only a subservient role in both direct and indirect detection.. This simplifying assumption rules out the possibility of resonances and co-annihilations affecting, significantly, the relic abundance of dark matter particle Griest:1990kh (). Furthermore, to reduce the number of possible operators, as also not induce flavour changing neutral current processes, we restrict ourselves to only flavour-diagonal currents. A convenient parametrization of such operators, for a single SM fermion , is given by

 OVV=¯χγμχ¯ψγμψOAA=¯χγμγ5χ¯ψγμγ5ψOSS=¯χχ¯ψψOPP=¯χγ5χ¯ψγ5ψOVA=¯χγμχ¯ψγμγ5ψOAV=¯χγμγ5χ¯ψγμψOSP=¯χχ¯ψiγ5ψOPS=¯χiγ5χ¯ψψ, (1)

with the subscripts on the operators reflecting the Lore-ntz structure. The full interaction Lagrangian involving can, then, be parametrized as

 Lint=∑f∑MN∈OperatorsgfMNΛ2OfMN, (2)

where is a typical operator amongst those listed in eq.(1) and the corresponding strength. refers to the cut-off scale of the effective theory.

Before we analyze any further, it is useful to consider the DM pair-annihilation cross section engendered by these operators Zheng:2010js (). Restricting ourselves to a single species444For multiple fermions, the cross-sections, of course, add incoherently. , and denoting , we have

 σannVV = (gfVV)2Nc16πΛ4βfβχs(1+xχ)(1+xf) (3a) σannAA = (gfAA)2Nc12πΛ4βfβχs[1−2(xχ+xf)+7xχxf] (3b) σannVA = (gfVA)2Nc12πΛ4β3fβχs(1+xχ) (3c) σannAV = (gfAV)2Nc12πΛ4βfβχs(1+xf) (3d) σannSS = (gfSS)2Nc16πΛ4β3fβχs (3e) σannPP = (gfPP)2Nc16πΛ4βfβχs (3f) σannSP = (gfSP)2Nc16πΛ4βfβχs (3g) σannPS = (gfPS)2Nc16πΛ4β3fβχs , (3h)

where for leptons (quarks) and are the center-of-mass frame velocities of () with . Clearly, for non-relativistic DM particles, and are the smallest. Similarly, for (as is the case except when is the top-quark), we have

 σannVA≈σannVV ,σannAV≈σannAA ,σannPP≈σannPS .

These approximations would prove to be of considerable use in further analysis.

Dark matter interactions, as exemplified by equation (1), have been well studied in the context of the LHC Bhattacherjee:2012ch (); Goodman:2010ku (); Carpenter:2012rg (); Petrov:2013nia (); Carpenter:2013xra (); Berlin:2014cfa (); Lin:2013sca (); Bai:2010hh (); Birkedal:2004xn (); Gershtein:2008bf (); Fox:2011fx (); Bai:2012xg (); Crivellin:2015wva (); Petriello:2008pu (). Clearly, the LHC would be more sensitive to operators involving the quarks. In this paper, we would be primarily interested in the orthogonal scenario, namely one wherein the DM current couples primarily to the SM leptons. To this end, we will assume that for all of the operators. As we shall see in the next section, this would render insensitive even the dedicated direct search experiments.

## 3 Relic Density of Leptophilic Dark Matter

Before we proceed further with our analysis, it behooves us to consider the existing constraints on such a DM candidate. This is best understood if we consider a single operator at a time, and, henceforth, we shall assume this to be so. In other words, all operators bar the one under discussion shall be switched off. As to the couplings , we consider two cases555Note that such a normalization of couplings is quite standard in effective field theories., namely (a) Leptophilic: for all leptons , and (b) Electrophilic: with all others vanishing.

Concentrating first on the epoch where the DM has frozen out, let us consider their pair-annihilation to produce two light particles , which, we assume, is in complete equilibrium, viz. . The Boltzmann equation gives us:

 a−3ddt(nχa3)=⟨σv⟩[n2χeq−n2χ] (4)

where is the scale factor and represents the thermal average. Here, is the relative velocity of a pair of ’s, and is the annihilation cross section.

In the radiation era, which we are interested in, the temperature scales as . We can, therefore, rewrite the Boltzmann equation, in terms of new dimensionless variables

 Y≡nχT3andx≡mχT , (5)

as

 dYdx=−m3χ⟨σv⟩H(mχ)x2(Y2−Y2eq) , (6)

where is the Hubble rate when the temperature equals and is given by

 H(mχ)=√4π3GNg⋆45m2χ. (7)

Here is the effective number of the degrees of freedom at that epoch.

To find the present density of DM particles, we need to find the solution of eq. (6) in terms of the final freeze out abundance, (at ). While this, can be done only numerically, it is instructive to consider an approximate analytic solution. At early times () reactions proceeded rapidly, and was close to its equilibrium value, , or . As the temperature falls below , the equilibrium abundance is exponentially suppressed. Conseque-ntly, the DM particles become so rare that they do not find each other fast enough to maintain the equilibrium abundance. This is the onset of freeze-out. In other words, well after freeze out, and

 dYdx=−m3χ⟨σv⟩H(mχ)x2Y2 (8)

Integrating equation  (8) from the freeze out temperature until very late times , we get

 Y∞≃xfH(mχ)m3χ⟨σv⟩. (9)

The energy density, for the now non-relativistic DM, , falls as . The number density in this post freeze out epoch at any given temperature behaves as . The number of the degrees of freedom also changes with the temperature from at the freezing epoch to that of today 3.36 at the present day temperature . The present energy density of DM can, thus, be re-written as

 ρχ=mχY∞T30(g0(x0)gf(xf)). (10)

It is customary to parametrize , where cm is the critical density of the universe and the Hubble constant today being expressed as   km   s   Mpc. We have, then,

 Ωχh2=√4π3GNg⋆(xf)45xfT30g0ρc⟨σv⟩g⋆(xf) . (11)

Using = 2.72548 0.00057 K Fixsen:2009ug (), the contribution of the Dirac fermion , with its two degrees of freedom, is

 Ω(χ)DMh2≈2×xf1.04×109GeV−1mpl√g⋆(xf)⟨σv⟩ . (12)

While the WMAP 9-year data gives = 0.1138 0.0045, the Planck 2015 resultsAde:2015xua () suggest a marginally different value, namely, = 0.1199 0.0022. This translates to a strict relation in the mass-coupling plane for . However, a conservative assumption would be that the relic density of the does not saturate the observed DM energy density, or . This would impose a lower bound on the self-annihilation cross-section for the , or, in other words, an upper bound on .

### 3.1 The annihilation cross-sections

In the calculation of the probability of a DM particle being annihilated by another one, it is useful to consider the rest frame of the first and re-express the aforementioned annihilation cross sections in terms of the velocity of the second particle in his frame. Clearly, and, working with a small expansion (relevant for non-relativistic DM), we have and . The corresponding -expansions, to , are

 σannSSv ≃ (glSS)2Nc8πΛ4(1−ξf)3/2m2χv2 (13a) σannPPv ≃ (glPP)2Nc2πΛ4√1−ξfm2χ[1+ξfv28(1−ξf)] (13b) σannVVv ≃ (glVV)2Nc2πΛ4√1−ξf(2m2χ+m2f) (13c) ⎡⎣1+−4+2ξf+11ξ2f24(1−ξf)(2+ξf)v2⎤⎦ σannAAv ≃ (glAA)2Nc2πΛ4√1−ξfm2f (13d) ⎡⎣1+8ξ−1f−28+23ξf24(1−ξf)v2⎤⎦ ,

where . Clearly, the -independent terms emanate from -wave scattering alone, while the piece receives contributions from both -wave and -wave annihilation processes.

The quantity of interest is not just , but the thermal average since this provides a measure of the rate at which a DM particle will meet another with the appropriate velocity and get annihilated. Assuming to be the dominant channel into which the ’s annihilate, we can estimate the thermally-averaged value of .

The inferred value of when ascribed to WIMPs with a mass of a few hundred GeVs, requires . Taking cue from this, we analyze upper bounds on in section  5 from the sensitivity study of the DM signatures from ILC for the kinematically accessible DM mass range.

In Figure 1 we present the relic density plots for the interactions parametrized by the operators mentioned in section 2 corresponding to the Leptophilic and Electrophilic scenarios. We implement the model containing effective interactions of DM particle with the SM sector using FeynRules  Christensen:2008py () and generate the model files for CalcHEP which is required for the relic density calculation in micrOmegas Belanger:2001fz (). These results have been verified with MadDM Backovic:2013dpa (); Backovic:2015tpt ().

The curves in Figure 1 imply that the correct amount of energy density requires the mass of dark matter particles to increase with . We can infer this behaviour from (12) as mainly depends on . From equations (13a)-(13d) we see that the thermal average in equation  (12) i.e. is proportional to for values greater than 10   GeV. This implies that for a fixed value of , is a constant. This, in turn, translates to .

## 4 Direct and Indirect Detection

### 4.1 DM-electron scattering:

We now turn to direct detection search, where both electrophilic and leptophilic DM are scattered by

1. the bound electron of an atom and hence the recoiled electron is ejected out of the atom,

2. the bound electron and the recoil is taken by the atom as a whole and

3. the quarks, where the DM is attached to the loop of charged virtual leptons which in turn interacts with the quarks via photon exchange and hence the nucleus recoil is measured in the detector.

In this article we restrict our study for the DM-electron scattering only. We analyze the free electron scattering cross-sections with the DM for the scalar, pseudoscalar, vector and axial couplings respectively and are given as

 σSSχe = (glSS)2m2eπΛ4 (14a) σPPχe = (glPP)2m2e3πΛ4m2em2χv4 (14b) σVVχe = (glVV)2m2eπΛ4 (14c) σAAχe = 3(glAA)2m2eπΛ4 (14d)

where , is the DM velocity in our halo. We observe that the cross section with the axial-vector couplings of DM dominates over all others. The pesudoscalar type coupling is highly suppressed due to its dependence on the fourth power of the electron mass and velocity. Respective cross sections for the case of bound electrons are likely to be enhanced than that of free electrons nearly by a factor of Kopp:2009et (). Using the constraints from the relic density on the lower bound of the couplings for a given DM mass , in Figure  2, we present the scattering cross section of the DM with free electrons via the most dominant channel with axial-vector couplings. We compare our result with the recent limits from the DAMA/ LIBRA experiment Kopp:2009et () and 90% C.L. data from XENON100 Aprile:2015ade (). However, even with the inclusion of the correction factor arising from the the bounded electrons, the contribution of the axial-vector couplings of DM to the scattering cross-section are much below these experimental upper bounds.

Indeed, the Xenon100 collaboration has constrained the pb at 90% C.L. for666The exclusion limits do have a dependence on with the maximum sensitivity occurring at and relaxing by an order of magnitude for the highest values.  Aprile:2015ade () for the case of axial-vector coupling. Expectedly, these constraints are much stronger (by nearly an order of magnitude) than the cross sections required to explain the DAMA/Libra results Bernabei:2013xsa (). Interestingly, the strongest bounds emanate from solar physics. In general, the neutrino flux coming from DM annihilations inside the sun is proportional to the DM scattering cross section. But, working in the region where DM capture and its annihilations inside the star are in equilibrium, makes the neutrino flux independent of the DM annihilation. As the DM particles can be trapped in the solar gravitational field, their annihilation into neutrinos would modify the solar neutrino spectrum and, consequently, the SuperKamiokande measurements  Kopp:2009et (). This translates to pb and pb which are relevant for the general leptophilic case with axial-vector coupling. Understandably, no such bound exists for the purely electrophilic case.

### 4.2 DM Annihilation:

Next we discuss the bounds from the indirect detection experiments, wherein we can directly use the cross sections given in equations (3a)- (3h) and fold them with the local velocity of the DM particle. The latter, of course, would depend crucially on the particular profile of the DM distribution that one adopts. In Fermi-LAT:2016uux (), the expected sensitivity is given as a limit on the thermally averaged DM annihilation cross section for the channel.

From equation (13a)-(13d), the thermally averaged annihilation cross- section of a leptophilic DM of mass can be estimated using the relic-density allowed lower bound on the scalar, pesudoscalar, vector and axial-vector couplings of DM. The annihilation cross-section for the leptophilic DM is marginally higher than electrophilic DM and roughly are of the same order of magnitude for GeV. We compute the annihilation cross-section for the leptophilic DM with these lower bounds on DM couplings and depict in Figure  3. We compare our thermally averaged cross-section of leptophilic DM with the bounds from the current indirect detection searches Fermi-LAT:2016uux ().

## 5 Interesting Signatures at ILC

While DM particles can be produced in many different processes at a given collider, only a few of them are, potentially, of interest. Remembering that the DM particle has to be produced only in pairs, and that there must be at least one visible particle in the final state so as to register the event in a detector, the simplest process at a linear collider is, of course, , and it has, rightly, been well studied in many different contexts Chae:2012bq (); Dreiner:2012xm (); Yu:2013aca (). Although the signature, namely monophoton with missing energy-momentum, can be masqueraded by both detector effects as well as a large and irreducible background emanating from , the kinematic profiles are sufficiently different enough to merit the possibility of a discovery.

Given the exceeding simplicity of the aforementioned channel, attention has focussed on it almost exclusively. However, it is worthwhile to explore complementary channels, like, DM pair-production in association with on-shell or off-shell ,

 e+e−→χ¯χ+Z(Z→jj,μ+μ−,e+e−) (15)

where refers to a jet arising from any of . In this paper, we shall not attempt to impose any -tagging (or -veto) requirements, and, hence, the -jet is equivalent to any other light quark jet777While similar analyses have been attempted in Refs. Neng:2014mga (); Yu:2014ula (), we differ substantially from their conclusions even when we adopt an approach identical to theirs. Furthermore, we present, here, a much more refined analysis.. To effect a realistic analysis, we have to include, though, off-shell contributions as well and, thus, need to consider , where . The corresponding irreducible SM backgrounds emanate from888In all our analysis, the dijet (plus missing energy) signal is actually an inclusive one, in that we demand a minimum of two jets.

 e+e− → 2jets+∑iνi¯νi, (16a) e+e− → μ+μ−+∑iνi¯νi, (16b) e+e− → e+e−+∑iνi¯νi. (16c)

respectively. The largest contribution to the first mode in eqn. (16a) accrues from with and splitting to two jets followed by the fusion channel and t-channel W exchange diagrams. Feynman diagrams analogous to both these sets also contribute to the two other processes given in (16b) and (16c) respectively. The relative strengths of these channels depend on a multitude of factors, such as the center-of mass energy, beam polarization (if any) and the kinematical cuts imposed.

We use MadGraph5  Alwall:2014hca () to perform the simulations for both SM background and the signal. We employ PYTHIA6  Sjostrand:2006za () to carry out the parton shower and hadronization. PGS  pgs () is used for Fast detector simulation with anti- algorithm for jet reconstruction. In accordance with technical design report for ILC detectors  Behnke:2013lya (), we set the energy smearing parameters of the electromagnetic calorimeter and the hadronic calorimeter in the PGS card as

 ΔEE = 17%√E/GeV⊕1% (17a) ΔEE = 30%√E/GeV (17b)

The other accelerator parameters used in our analysis are also set according to the technical design report for ILC  Behnke:2013xla () and we tabulate them in Table 1 for convenience.

Before we commence an analysis of the cross sections and the kinematic distributions we must impose basic (acceptance) cuts on transverse momenta (), rapidities () and separation () of the visible entities (jets and , ) along with the the missing transverse energy (), which commensurate with the typical detector capabilities on the one hand, and theoretical considerations (such as jet definitions) on the other.

• 10 GeV where ,

• 2.5 and 5,

• where  ,

• where ; for the hadronic channel, this invariant mass actually refers to that for all the jets together,

• 25 GeV.

The corresponding cross-sections with these basic cuts for the polarized and unpolarized beams of electron and positron are summarized in Table  2. Feynman diagrams consisting of different topologies and contributing to the background (16a) can be further suppressed by imposing the most-dominant invariant-mass cut of the visible particles 999For , the deviation from such a dominance is quite significant. Precisely for this reason, this turns out to be to be the least sensitive of the three channels., and thus allowing final state with the on-shell decaying into the two visible entities, and the off-shell going to a neutrino-pair. Within this approximation, the diagrams contributing to the SM background processes (16a)-(16c) have identical topologies and differ only in the coupling of the to the final state fermions. Consequently, this difference would manifest itself essentially only in the total rates with differences in the normalized distributions being of a subleading nature. This is true even for the signal events corresponding to these final states. Hence we have displayed the one-dimensional normalized differential cross-section for process with only jets as final state in Figures  4 and 5.

### 5.1 Analysis with one and two dimensional distributions:-

In order to augment the signal-to-noise ratio by imposing additional selection cuts on the kinematic observables, we recourse ourselves to the detailed study of the normalized one dimensional differential cross-section distributions w.r.t. for all the sensitive kinematic observables e.g. , , and sum of energies from a jet or lepton pair for the signal with varying DM mass as well as varying effective DM pair - SM fermion pair couplings at = 500 GeV and 1 TeV.

The very structure of the DM interaction Lagrangian implies that, for a given final state, the normalized differential distributions for the , , and cases are very similar to each other, with the differences being proportional to the difference in mass of the SM fermions in the final state (i.e., , or the light quarks). Similarly, the normalized distributions for the , , and the cases are, again, very similar to each other. Therefore, we have chosen to display the normalized histograms for the observables , , and from signal processes at the three representative values of the DM masses namely 75, 225 and 325 GeV in Figures 4 and 5 corresponding to the scalar and vector interactions of the DM bilinears with SM fermion pair at = 1 TeV and = 1 TeV. We list our observations as follows:-

• In Figure 4, we observe that, as we increase the DM mass, the respective shape profile of the all kinematic observables become more and more distinct w.r.t. the SM contribution. This difference in shape profile for the scalar coupling with that of SM can be attributed to the chirality-flip interactions of the DM which becomes much more pronounced for higher values of .

On contrary, the shape profiles of all the kinematic distributions with vector coupling of DM in Figure 5, behave the same as those of SM coupling.

• We find that in the lower region, the jet pair remains highly boosted as in the case of SM and hence, the peak of the differential cross-section distribution w.r.t. coincides with that of SM background around . The peak however shifts towards higher values of as we increase .

• We find that the energy profile of the visible pair are sensitive to the choice of the DM mass and thus advocating that the upper limit on this kinematic observable can be used as a dynamic mass dependent selection cut to reduce the continuum background. This is realized by invoking a cut on the invariant mass of visible particles to be around , where GeV. This restriction translates to an upper limit on the variable as a function of :

 Ej1+Ej2≤s+m2Z−4m2χ2√s. (18)

Since we are primarily interested in production associated with on-shell , we shall use the condition on the total visible energy  (18) as the Selection cut for the rest of our analysis. The signatures where a pair of leptons appear in the final state due to the alternative decay modes of boson, the differential cross-section distributions w.r.t. the observables and are similar to the observables and which are obtained from the respective . Therefore, we adopt the similar selection cut criteria on the and .

Based on the study of 1-D differential cross-section distributions at the given luminosity we select the two most sensitive kinematic observables say and either or for the further analysis of two dimensional differential cross-section distributions. We analyse the efficiency of the Selection cut  (18) through the double distributions of the simulated associated DM pair production events (for values at 75, 225 and 325 GeV), which are then compared with the double differential cross-section distributions of the SM at the given integrated luminosity.

In Figure  6, we exhibit the normalized two dimensional differential cross-section with the Selection cuts in the and plane for the background and the DM with = 325 GeV. These 3D lego plots are generated from MadAnalysis 5 Conte:2012fm () at = 1 TeV, =1 TeV and = 1. The bin width is 15 GeV for the while it is 0.1 for the distribution.

We observe that the suppression of background processes due to the implementation of selection cuts enhances the sensitivity of the signal. We study the signal efficiency () at = 1 TeV with the integrated luminosity 1 ab and in the Table  3 we compare the 3 reach of the cut-off at a given mass for the dominant signature corresponding to the three representative masses of DM.

### 5.2 χ2 Analysis

In this subsection we study the sensitivity of the cut-off scale with the DM mass keeping the couplings of the DM bilinears with the SM fermionic pair to be unity. The analysis is performed with the sum of the variance of the differential bin events at a given integrated luminosity due to the presence of the new physics (NP) contribution over the SM events.

We define the for double distribution as

 χ2=n1∑j=1n2∑i=1⎛⎜ ⎜⎝NNPij√NSM+NPij+δ2sys(NSM+NPij)2⎞⎟ ⎟⎠2 (19)

where are number of differential events given by New Physics and are total number of differential events for grid in double distribution. is the total systematic error in the measurement. Although the systematic uncertainty inclusive of the luminosity uncertainty is considered to be of the order of 0.3% in the literature Behnke:2013xla (), We have considered a conservative total systematic error to be of order of 1%. Further, we find that the sensitivity of the cut-off can be increased with the increase in the luminosity as the cut-off scales for a given . Thus, for = 1 TeV and Luminosity = 1 ab the sensitivity of the signal will improve by 10 %.

From the analysis, we obtained the contours in the plane corresponding to all the three processes in Figures  7 and  8. We present the estimation of the 3 sensitivity reach of the maximum value of the cut-off that can be probed in ILC at = 500 GeV and 1 TeV with an integrated luminosity = 500 fb and 1 ab respectively in Table 3.

We compare our results for the unpolarized beams at = 500 GeV and = 500 fb which are displayed in Figure  7 with Figures 4d and 4e of reference Yu:2014ula () corresponding to pseudo-scalar and axial-vector couplings respectively. We find that our analysis can provide a better kinematic reach ( GeV ) for the pseudo-scalar coupling. We can probe upto 0.98 TeV, which is further improved to 1.07 TeV with the enhanced integrated luminosity of = 1 ab. However, for the case of axial-vector couplings we can only probe upto 0.88 TeV as compared to 0.92 TeV given in Figure 4e of Yu:2014ula ().

On the same note, we would like to compare our results for = 1 TeV and = 1 ab which are displayed in Figure  8 with Figures 4d and 4e of reference Yu:2014ula () corresponding to the pseudo-scalar and axial vector respectively. We find that the sensitivity for the pseudo-scalar can be improved = 2.62 TeV in comparison to 2.3 TeV given in Figure 4d of Yu:2014ula (). Similarly, for axial-vector couplings, we agree with given in Figure 4e of Yu:2014ula ().

### 5.3 Effect of Polarized Beam

We further study the sensitivity of dependence on with the polarized initial beams. The rate of pair production of the fermionic DM through Scalar () and PseudoScalar () interactions can be enhanced by increasing the flux of right (left) handed electrons and right (left) handed positrons. Similarly and interaction of the fermionic DM can be enhanced by choosing the right(left) handed electron beam and left(right) handed positron beam. The background contribution from -channel exchange diagram can be suppressed significantly by choosing right handed polarized electron beam which then leaves us with the following choices of polarization combination w.r.t. helicity conserving(,) and helicity flipping (,) interactions respectively

1. and

2. and

We exhibit the 99% C.L. contours corresponding to the polarized initial and beams in Figures 7 and 8 in the - plane for all possible visible signatures associated with DM pair production at = 500 GeV and 1 TeV with an integrated luminosity of 250 fb and 500 fb respectively. We find that, for scalar and pseudoscalar (vector and axial vector) DM couplings, we can probe values upto 1.1 TeV (0.89 TeV) with polarized initial beams at an integrated Luminosity of 250 fb. Similarly, we observe that the analysis with = 1 TeV and an integrated luminosity of 1 ab the sensitivity of can be improved to 3.13 TeV (2.05 TeV) for scalar and pseudoscalar (vector and axial-vector) DM couplings.

We perform the combined analyses from all the three processes involving the DM pair production for both unpolarized and polarized initial beams. We compute the 99% confidence limit contours and plot them in Figures 9 and 10 for = 500 GeV and 1 TeV respectively.

### 5.4 Comparison with the existing analysis

We present a comparison of our results with those that exist in the recent literature.

#### 5.4.1 Sensitivity from mono-photon channel

First, we make an overall comparison with the other complementary dominant DM production mono-photon channel studied in the reference Chae:2012bq (). We have calculated and verified the cross sections and significance of various interactions in the mono-photon channel with the cuts mentioned in Chae:2012bq (). Our analysis shows that the sensitivity of is higher than that of the mono-photon channel, when mediated by the scalar coupling of the DM, specially in the lower region and behave as competitive DM production channel upto DM mass 300 GeV. It is important to mention that the enhancement in the sensitivity are obtained inspite of our conservative input for the systematic uncertainty 1% in contrast to that of 0.3% in the reference Chae:2012bq ().

#### 5.4.2 Results from mono-Z channels

Next, we compare our results with the existing analysis on the DM production channels in association with boson which decays to pair of light quarks, electrons and muons.

DM interactions mediated through the vector and axial vector couplings are compared with the results of the reference Neng:2014mga () in Table 4. We marginally improve the upper limit ( at = 10 GeV) corresponding to the unpolarized initial beams. However, it should be noted that the authors of reference  Neng:2014mga () have assumed to be 137 at = 500 GeV or 1 TeV instead of 127.9, thus leading to the gross under-estimation of the background events. Rectifying the error will further bring down the efficiency of the sensitivity of their analysis.

We also compare the significance of the mono- channel processes in the hadronic decay mode with those given in reference  Yu:2014ula () at = 500 GeV. We summarize this in Table 5 for some representative values of and . We find that the our cuts strategy and analysis shows enhancement in the signal significance w.r.t. the pseudo-scalar and axial-vector interactions of DM with charged leptons for both unpoalrized and polarized initial beams.

## 6 Summary and Outlook

The fact that a massive stable particle with near–weak scale interactions can constitute an attractive candidate for the Dark Matter in the universe (while satisfying all of competing constraints from the relic density, large-scale structure formation as well as myriad other cosmological and astrophysical observations) is well-known. While the correct relic abundance can be reproduced by ensuring the right annihilation cross-sections into any of the SM particles, direct detection of the DM candidate largely hinges on its having unsuppressed interactions with the first-generation quarks.

It, then, is of interest to consider the possibility that has very suppressed (if any) interactions with quarks and gluons. Not only would the direct-detection experiments have very little sensitivity to such particles, their pair-production cross-section at the LHC would be suppressed too. In such circumstances though, the DM must have significant couplings to at least some of the leptons and/or the electroweak gauge bosons.

In this article, we have investigated the first of the two possibilities. We obtained the upper bound on the cut-off for the given range of electrophilic and/ or leptophilic DM mass from the relic density constraints which is displayed in the Figure 1. Using these upper bounds on for a given , we estimated the thermally averaged annihilation indirect detection cross-section and leptophilic DM direct detection scattering cross-section and are displayed in Figures  3 and  2 respectively. We find that the present experimental limits in the respective searches not only favours the allowed parameter space from the relic density, but also constraints the DM model by providing the lower bound on the for a given DM mass .

If the couplings to the charged leptons be unsuppressed, the linear collider could play an interesting role in establishing the existence of such a . Using the allowed coupling to the electron, this has, traditionally, been undertaken using the mono-photon (accompanied by missing energy-momentum) channel. We have investigated, here, the complementary channel, namely , where is any of the light charged fermions (jets, electrons and muons) and exhibited the significance of these processes with basic kinematic cuts in Table 2.

We analysed the sensitivity of DM scalar and vector couplings through the one and two dimensional normalised differential kinematic distributions corresponding to the most dominant signature in Figures 4, 5 and 6 respectively. 99 % C.L. contours for various sets of run parameters based on the analysis of these differential distributions are shown in Figures  7,  8. Combining the