How light a higgsino or a wino dark matter can become in a compressed scenario of MSSM

Higgsinos and Wino have strong motivations for being Dark Matter (DM) candidates in supersymmetry, but their annihilation cross sections are quite large. For thermal generation and a single component DM setup the higgsinos or wino may have masses of around 1 or 2-3 TeV respectively. For such DM candidates, a small amount of slepton coannihilation may decrease the effective DM annihilation cross section. This, in turn reduces the lower limit of the relic density satisfied DM mass by more than 50%. Almost a similar degree of reduction of the same limit is also seen for squark coannihilations. However, on the contrary, for near degeneracy of squarks and higgsino DM, near its generic upper limit, the associated coannihilations may decrease the relic density, thus extending the upper limit towards higher DM masses. We also compute the direct and indirect detection signals. Here, because of the quasi-mass degeneracy of the squarks and the LSP, we come across a situation where squark exchange diagrams may contribute significantly or more strongly than the Higgs exchange contributions in the spin-independent direct detection cross section of DM. For the higgsino-DM scenario, we observe that a DM mass of 600 GeV to be consistent with WMAP/PLANCK and LUX data for sfermion coannihilations. The LUX data itself excludes the region of 450 to 600 GeV, by a half order of magnitude of the cross-section, well below the associated uncertainty. The similar combined lower limit for a wino DM is about 1.1 TeV. There is hardly any collider bound from the LHC for squarks and sleptons in such a compressed scenario where sfermion masses are close to the mass of a higgsino/wino LSP.


Introduction
One of the most interesting features of low energy supersymmetry (SUSY) [1][2][3] is that it can provide with a viable candidate for dark matter (DM) [4,5]. The lightest supersymmetric particle (LSP), typically the lightest neutralino, in R-parity conserving scenarios of the Minimal Supersymmetric Standard Model (MSSM) [1][2][3] is a strong candidate for DM. In MSSM, the neutralinos are composed of gauginos (bino and wino) and higgsinos. Whether the LSP in a particular MSSM scenario is able to satisfy the right relic abundance, depends crucially on its gaugino-higgsino compositions.
For example, in the minimal supergravity model (mSUGRA) [3,6] that assumes SUSY breaking at a high scale, the LSP is bino-like for most of the parameter space. Bino being a gauge singlet, its annihilation occurs mainly through t-channel exchange of sfermions, giving rise to the bulk annihilation region [2]. With the discovery of a 125 GeV Higgs boson at the Large Hadron Collider (LHC) of CERN [7], the sfermion masses are pushed towards higher values, particularly for the universal models like mSUGRA. This makes bulk annihilation rather an inefficient mechanism for obtaining the right relic density [8]. It is however possible to have a bino-LSP giving the correct abundance of DM in some specific regions of parameter space of mSUGRA, like the stau coannihilation, funnel (resonant Higgs annihilation) or hyperbolic branch (HB) [9,10]/ focus point (FP) [11] regions. While most of the former two regions of parameter space are ruled out by the Higgs data [7], a large part of the HB/FP region, which corresponds to a significant degree of bino-higgsino mixing, is disfavored by DM direct detection experiments [12]. There is also a higgsino LSP region in mSUGRA but this comes with a baggage of a very large gluino mass and a heavy SUSY spectra in general. A SUSY scenario where the spectra may not necessarily be so heavy while the LSP is still highly higgsino dominated in nature may be realized in a few nonuniversal gaugino mass models [13][14][15][16][17][18][19][20][21][22], nonuniversal Higgs scalar models [23] or models with non-holomorphic soft terms [24].
Apart from bino, one may have the right relic abundance in MSSM if the LSP is a higgsino, wino or a well-managed admixture of bino, wino and higgsinos [25]. For the higgsino-like LSP scenario, the lightest neutralino ( χ 0 1 ) mass is close to the value of the higgsino mixing parameter µ. In this case the lightest chargino χ ± 1 and the second lightest neutralino χ 0 2 are almost mass degenerate with χ 0 1 with their masses are close to µ. For a thermally generated single component dark matter, it has been typically accepted that the LSP mass for obtaining the right DM abundance is around 1 TeV for a higgsino-like LSP [10,12]. Below this limit the annihilation and coannihilations among χ 0 1 , χ 0 2 and χ ± 1 are too strong causing the DM relic density to become underabundant. On the other hand, a wino-like LSP may be possible to realize if M 2 < (M 1 , µ) where M 2 and M 1 are the SU (2) L and U (1) Y gaugino mass parameters respectively. A wino may be the candidate for LSP in many theoretically well-motivated models like the Anomaly Mediated Supersymmetry Breaking (AMSB) [26]. For a wino LSP, m χ 0 1 and m χ ± 1 lie very close to M 2 allowing strong coannihilations. A thermally generated wino dark matter is underabundant up to ∼ 2 TeV. It satisfies the relic density data for a wino mass of 2-3 TeV 1 [27][28][29][30][31].
Focusing on the collider information as received from the LHC we note that the SUSY searches at the LHC in generic MSSM spectra i.e. in an uncompressed sparticle mass scenario, have imposed stringent bounds on the masses of strong sector sparticles [32,33]. The strong sector scalar masses are increasingly pushed above a TeV regime that is even superseded by the gluino mass limits. On the other hand, the direct mass bounds on the electroweak (EW) sector sparticles from the LHC searches are rather mild [34,35]. In the context of mass limits of sparticles, we must however remember that the LHC searches are restricted to the so-called "simplified models" that are characterized by certain assumptions on sparticle masses and compositions of the EW sector gauginos (electroweakinos). The searches in the 3l + E / T channel[36] for example consider χ 0 1 to be purely a bino and χ ± 1 / χ 0 2 to be completely wino dominated. Imposing basic constraints like the Higgs mass, dark matter relic density and muon g − 2 there have been studies that effectively probed the SUSY parameter space for the above types of electroweakinos [37][38][39]. However, it turns out that the collider limits get significantly degraded once we start varying the composition of the electroweakinos. This may be seen in Ref. [40] where the authors considered χ ± 1 to be higgsino dominated or a mixture of a wino and higgsinos in a bino dominated LSP ( χ 0 1 ) situation. Similar to the above, changed composition of the LSP itself may significantly alter the collider limits. For example, the trilepton search limits are hardly of any importance in a higgsino dominated LSP scenario where χ 0 1 , χ 0 2 and χ ± 1 are almost mass degenerate. This is simply because the resulting leptons come out to be very soft. For collider studies of benchmark points that satisfy the observed relic density range, one may however use monojet + E / T analysis [41]. However, the bounds are seen to be very weak [42]. Apart from all the above, collider bounds of sfermions including also squarks get severely diluted if one considers a compressed scenario of sparticle masses where the LSP is higgsino/wino dominated in its composition with its mass close to that of sleptons and/or squarks as appropriate in a LSP-sfermion coannihilation study.
In this analysis we use a compressed SUSY scenario in a phenomenological MSSM (pMSSM) [43] framework so as to explore how light the higgsinos and wino can become while having relic density values within the phenomenologically accepted range. We will consider appropriate coannihilations of the LSP separately with sleptons and squarks or both of them together.
We will now briefly outline the commonly explored coannihilation scenarios. To determine the relic density including coannihilations one computes a thermally averaged effective annihilation cross-section < σ ef f v > for the LSP [44]. < σ ef f v > is obtained from self-annihilation and various coannihilation cross-sections that are weighted by factors exponentially suppressed by relative mass differences between the DM and the coannihilating partners. The DM relic density is inversely proportional to < σ ef f v >. In the context of mSUGRA, excluding a few specific regions of parameter space, the LSP is generally bino (B)-dominated in its composition [3]. Except the t-channel slepton exchange that requires very light sleptons or the s-channel Higgs modes, a bino typically undergoes a tiny amount of self-annihilation that leads to overabundance in most of the mSUGRA parameter space. The situation changes when bino-slepton or in particular bino-stau coannihilation comes into the picture. Here the non-relativistic threshold S-wave coannihilation cross-sections such as σB −l R and σ l R −l * R , l R being the right handed stau, are not suppressed by fermionic mass factors. The above coannihilation cross-sections are much larger than the self-annihilation cross-section of a highly bino-dominated LSP [45]. Thus, in mSUGRA, the coannihilation of χ 0 1 withτ 1 is able to reduce the relic density to fall within the WMAP/PLANCK [46,47] specified range. A detailed analysis was made in Ref. [48] where all possible kinds of coannihilations were considered in a bino-dominated LSP scenario in an mSUGRA setup. However, we must remember that masses of sparticles in mSUGRA are correlated that causes mostly LSP-stau coannihilations to be relevant. Thus, a significant amount of change in the DM relic density via coannihilations, leads to an acceptable value, but this is possible only in a limited zone of parameter space.
Models with essentially unconstrained sparticle masses such as pMSSM when considered in a compressed scenario are able to probe the true potential of coannihilations. Here, the LSP may find several coannihilating partners almost mass-degenerate with itself that would overcome the associated exponential suppression encountered in computing the effective annihilation cross section.
In this analysis, we will focus on higgsino and wino dominated LSPs that undergo coannihilations with sfermions, both sleptons and squarks, separately or together. We will see that there may be rather uncommon occurrences when coannihilations may potentially cause a decrease in the effective annihilation cross-sections, thereby causing an increase in the DM relic density. This was discussed in Refs. [49,50] where the latter reference named the coannihilating species as parasite degree of freedom in which the authors investigated the role of sleptons coannihilating with the LSP.
In this work, we will systematically analyze the effects of coannihilations with all the sfermions in a compressed scenario and probe the mass reach of the LSP as a higgsino/wino in relation to the latest phenomenological constraints involving dark matter, Higgs mass and the relevant bounds from collider data.
We emphasize that the effect of considering a coannihilating particle, in particular whether it would cause a decrease or increase of the relic density depends on several factors [44,49], namely, i) the annihilation cross section σ χ i −χ 0 of the coannihilating particle χ i with the LSP (χ 0 ), ii) the cross section σ χ i −χ i for the coannihilating particle annihilating with itself, iii) σ χ i −χ j , where i and j refer to different species of coannihilating particles, iv) the relative mass gap between the sparticles namely, , thereby on the extent of exponential suppression, v) appropriate weight factors arising out of the degrees of freedom of the associated particles undergoing coannihilations.
We must remember that while a bino does not have any gauge charge, a higgsino (wino) is associated with isospin 1 2 (1) . This translates into a larger internal degrees of freedom, namely 8 for a higgsino and 6 for a wino type of LSP considering its Majorana nature. Expectedly, a large number of internal degrees of freedom contributes more toward the self-annihilation cross section of the LSP. In addition to the above, one must also consider large coannihilations involving candidates like χ ± 1 , χ 0 2 for a higgsino type of LSP and χ ± 1 for a wino type of the same. All the above lead to a substantially large effective annihilation cross-section for the above two types of LSP. Among the coannihilating sfermions, the left handed ones have larger internal degrees of freedom. This further gets multiplied by the color degrees of freedom for squarks. In computing the effective annihilation rates out of individual cross-sections, one notes that the associated weight factors for different coannihilating species play very important roles in either decreasing or increasing the total rate itself. As mentioned before, unlike a bino LSP, a higgsino or a wino LSP is intrinsically associated with a larger amount of self-annihilation as well as LSP-electroweakino coannihilations. We will refer this as a generic higgsino or wino DM scenario. It turns out that in a compressed sfermion scenario all the appropriate degrees of freedom of the coannihilating sfermions may contribute to the averaging process toward < σ ef f v > in such a way that the latter becomes smaller than the case of having no sfermion coannihilations over most of the parameter space satisfying the DM relic density limits. Thus, for a given LSP mass the relic density increases. This on the other hand is synonymous with a decreased lower limit of the mass of LSP satisfying the WMAP/PLANCK data. However, apart from the typical trend mentioned above, we will come across a parameter region corresponding to a higgsino as LSP where the outcome due to squark-squark coannihilations may become dominant over the electroweakino part of the LSP depletion cross section.
We will also study the direct and indirect detection prospects for the types of DM considered in this analysis. The LUX [51] experiment puts strong bounds on spin-independent (SI) DM direct detection cross-sections. The χ 0 1 −nucleon scattering cross-section that LUX relies on is enhanced for sufficient gaugino-higgsino mixing [52]. However, in our scenario the cross section is supposed to be small for LSP being so pure, either a higgsino or a wino. On the other hand, the DM indirect detection experiments [53,54] look for signals coming from stable final state particles of DM annihilation processes in the solar or galactic cores. Since the sfermion-coannihilations make the smaller DM mass zones to become valid in relation to the relic density data, it is important to find whether the indirect detection rates can also be large for much smaller values of higgsino or wino masses satisfying the DM relic density limits.
The paper is organized as follows. In Section 2 we briefly discuss the effect of sfermion coannihilations in the calculation of the effective cross-section. In Section 3 we present the relic density computation results for higgsinos and wino types of LSP by considering slepton and squark coannihilations separately or together. We will start the section by discussing the roles of the relevant electroweakino mass differences that potentially affect the higgsino and wino relic density results.
Constraints coming from the direct and indirect DM detection experiments on our results are discussed in Section 4. Finally, we conclude in Section 5.

Sfermion Coannihilations with Higgsino and Wino Types of LSP
Let us consider the evolution of a class of particles χ i , i = 1, ...N , in the Early Universe. We assume the particles are different from SM candidates by assuming an R-parity conserved scenario of SUSY. The Boltzmann equation governing the number density n i of the i-th kind of particle at any instant of time t is given by [49], where the first term is due to the expansion of the universe and H is the Hubble parameter [5].
The second term arises because of coannihilations between i-th and j-th sparticles leading to SM particles in the final state i.e. for processes like χ i χ j → X. The total cross-section for scattering off the cosmic thermal background, χ i X → χ j Y is given by σ Xij , where X and Y are SM type of particles. The last term describes the decay of χ i and Γ ij refers to the total decay width for the processes χ i → χ j X. Since in an R-parity conserving scenario all the existing sparticles will eventually decay into the LSP, its number density is given as n = N i=1 n i . Now, an assumption for the distribution of χ 0 1 maintaining its thermal equilibrium value i.e. n i n n eq i n eq , Eq. 2.1 leads to, where, In the non-relativistic approximation, one has, 4) where g i is the number of internal degrees of freedom of the i-th particle, δ i = m i −m 1 m 1 (for i > 1), x = m 1 T , m 1 being the mass of the LSP and g ef f = N i=1 g i exp(−xδ i )(1 + δ i ) 3/2 . In this analysis with slepton and squark coannihilations each δ i corresponding to a sfermion type i is allowed to vary up to a chosen limit δ max . Thus, each sfermion mass mf i will have an upper limit of m χ 0 1 (1 + δ max ). δ max is chosen as 20% keeping in mind the exponential suppression within Eq.2.4. Considering a slepton coannihilation scenario in pMSSM, as an example, we note that the first two generations of sleptons do not differ much in their mass values among themselves and these will be close to Ml (= Ml R ), the pMSSM common slepton mass parameter 2 . First, let us consider only the sleptons of the first two generations to undergo coannihilations. For a given m χ 0 1 2 Only small differences come from the D-term contributions of the left and the right sleptons as well as sneutrinos. and δ max , the sleptons will have a maximum mass value of m χ 0 1 (1 + δ max ) and this will be close to the maximum value of Ml. For a given LSP mass, calling the average of all the associated δ i values as δ, one finds that the highest possible δ becomes close to δ max , the chosen degree of maximum relative mass deviation, irrespective of tan β. Next, we allow the third generation of sleptons to have mass values in the coannihilation zone. Consequent of the L-R mixing effect (which is more prominent for a larger tan β), mτ 1 and mτ 2 are largely separated among themselves. Only the heavier stau will have its maximum mass value near m χ 0 1 (1 + δ max ) and all other sleptons will have much smaller masses. Thus, the reach of Ml becomes smaller and so is the average value of all the three generations of slepton masses. Hence, the average relative deviation δ will have its maximum value significantly smaller than δ max , an effect that would increase with tan β. Additionally, when LSP mass is in the smaller zone meaning a stronger degree of electroweakino coannihilations, the requirement of slepton coannihilations increases so as the satisfy the relic density limits. Thus, the slepton masses are needed to stay within the close vicinity of m χ 0 1 . Consequently, δ as well as its range of variation both become smaller for a given mass of the LSP. Here, the aforesaid range becomes smaller because of the stau L-R mixing since coannihilation effects of both the staus are quite required in the process. In other words, the stau masses cannot be too far away from m χ 0 1 , or the associated δ i values can not be large, thus avoiding an exponential suppression. It follows that the minimum mass of the LSP satisfying Eq.3.1 becomes larger for a larger tan β. Similarly, squark coannihilations, in principle, will also show qualitatively identical behaviour 3 based on the availability of the all the generation of squarks for coannihilations. However, we will consider only the first two generations of squarks in this study keeping the top-squarks in a decoupled zone because of a very large L-R mixing, particularly arising from the requirement of satisfying the Higgs mass data.
In regard to a book-keeping of the internal degrees of freedom (d.o.f.) we note that for a given generation of the right and left handed sleptons likeτ R,L there are 2 internal d.o.f. available for each R and L while the sneutrinoν τ along with its anti-particle would have one internal d.o.f.

Results for Relic Density
In spite of the fact that the PLANCK [47] data for the DM relic density has a very small uncertainty (Ω CDM h 2 = 0.1199 ± 0.0022), we note that there is about a 10% level of theoretical uncertainty in computing the SUSY DM relic density [55]. This is approximately six times the observational uncertainty, as concluded in Ref. [55]. It was shown that higher order SUSY-QCD corrections may cause a significant degree of shift of the relic density in some scenarios and the uncertainty arising out of renormalization scheme and scale variations can be quite significant. Several recent analyses used such a degree of theoretical error or even more (see for example Refs. [56,57]). Thus, we will use Ω χ 0 1 h 2 = 0.12 ± 0.012 that leads to the following bounds.
We use the code SuSpect (version 2.43) [58] for spectrum generation. For the calculation of DM relic density and direct and indirect detection observables we use the code micrOMEGAs version 3.2 [59]. We have also verified agreement with the code DarkSUSY [60] by choosing various representative points over the parameter space.
Throughout the analysis we impose the Higgs mass range of 122 to 128 GeV considering the uncertainty in computing SUSY Higgs mass m h with radiative corrections [61].

Quasi degeneracy of electroweakino masses
Since the electroweakino coannihilations play a dominant role in computing the DM relic density both for higgsino and wino types of LSPs, it is important to discuss briefly the role of the appropriate electroweakino mass differences [62][63][64][65][66][67]. In regard to a higgsino type of LSP, both the mass Typically the latter is about double the former at the tree level [63]. For a higgsino type of LSP, with M 2 > µ, M W , an expansion in 1/M 2 leads to the following tree level mass difference [65].
In the wino limit of the LSP, one has M 2 < |µ|, |M 1 | causing the difference m χ ± 1 − m χ 0 1 to become small. An expansion in 1/µ leads to the following tree level relationship [65].
Additional suppression comes for large tan β since sin 2 (2β) ∼ 4/tan 2 β. Thus, the terms up to the order 1/µ 3 are suppressed indicating the lowest contributing order to be 1/µ 4 which is given as follows [66].
One finds that the above mass splitting is small even for moderate values of µ. Thus, the radiative corrections for the two electroweakino masses or rather that of their difference become important [68,69]. The dominant corrections to the masses come from top-stop and γ(Z)-higgsino loops [68]. On the other hand, the renormalization of the mass difference is controlled by the gauge boson loops as pointed out in Refs. [64,67]. However, in our analysis we find a non-negligible reduction in the mass gap when µ and/or squark masses are taken to be very large (∼ 10 TeV) and we agree with the conclusion of Ref. [63] in this regard. In this analysis, since we are looking for slepton and squark coannihilations with the LSP while trying to probe the lower mass limit of the latter, we undertake a minimalistic approach of considering not too much different mass values for the scalars among themselves. We also limit µ so as to have only an adequate degree of wino purity of the LSP while trying to respect naturalness [9][10][11]70] as far as possible. Hence, we will prefer not to take very large values for the scalar masses or µ.

Higgsino dominated LSP
A higgsino dominated LSP with mass close to µ can be made out of the choice M 2 > M 1 > µ. We will quantify the degree of higgsino content of the LSP via Z h defined as Z h = (N 2 13 + N 2 14 ), where N ij , i, j = 1, 2, 3, 4 are the elements of the neutralino-mass diagonalizing matrix [3]. In particular, we have used the following choice: M 1 = 2µ and M 2 = 2.4µ. We then vary µ in the range of 100 GeV < µ < 2 TeV that covers the typical relic density satisfied higgsino mass zone of 1 TeV. In a correlated scanning setup, for each value of µ we vary the common slepton mass parameter for all the three generations of sleptons within the range 50% below and above the value of µ. The common squark mass parameters are chosen to be large (3 TeV). For squarks, we allow coannihilations only with the first two generations for reasons described in Sec.2 while taking sleptons as well as the third generation of squarks to be heavy (3 TeV). As before, we vary µ in the range of 100 GeV < µ < 2 TeV. Then, for each value of µ we vary the common squark mass parameters for the first two generations within the range 50% below and above the value of µ.
Furthermore, while µ being varied, we scan the trilinear soft breaking parameter A t from −2 TeV to −7 TeV, so as to satisfy the higgs mass data. However, we must emphasize that the choice of A t has a very small impact in our study of sfermion coannihilations. The squark mass parameters of the third generation as well as the electroweak symmetry breaking (EWSB) scale are taken as 3 TeV throughout the slepton and squark coannihilation studies. The SU (3) C gaugino mass parameter M 3 is also chosen to be 3 TeV whereas the mass of the CP-odd Higgs (M A ) is set at 5 TeV. The latter avoids a Higgs resonance annihilation region. In order to study the effect of slepton coannihilations on the relic density of DM, we make sure that the physical slepton masses stay within 20% of the LSP mass irrespective of the generation. The same is true for the case of first two generations of squarks while we analyze the effects of squark coannihilations. We like to emphasize that with the above nearly degenerate squark masses close to that of the LSP, the commonly discussed LHC limits[71] for squarks would not apply to our scenario. The color codes are same as those of (a). Reduction of the lower limit and enhancement of the upper limit of the LSP mass are notable. Fig.1(a) shows the scatter plot of the higgsino fraction Z h vs LSP mass when the LSP efficiently coannihilates with sleptons and sneutrinos of all the three generations. We note that the LSP-sfermion coannihilations take place in the background of strong electroweakino coannihilations. The significance of higgsino purity level in turn is directly related to the level of coannihilations between the electroweakino states χ 0 1 , χ 0 2 and χ ± 1 . The squarks are taken to be very heavy (3 TeV). The reference results for the generic higgsino LSP or the case of no sfermion coannihilations are shown in green and blue points for tan β = 10 and 30 respectively. The black and red points refer to tan β = 10 and 30 respectively for the cases with slepton coannihilations. All the points in the scatter plot satisfy the lower and upper limits of DM relic density. Clearly as seen in Sec.2. We extend the results to LSP-squark coannihilations in Fig.1(b). All the internal degrees of freedom are taken into account including the colors. The sleptons, on the other hand, are chosen to be very heavy (3 TeV) as mentioned before. The color codes are same as those of Fig.1(a).
Here, squarks refer only to the first two generations for reasons mentioned in Sec.2. For the lower limit of the LSP mass, one finds m χ 0 1 840 GeV irrespective of tan β. In any case, the above is rather a modest reduction from about 1 TeV corresponding to the case of a generic higgsino DM.
We must also note that for squark coannihilations the upper limit of m χ 0 1 is stretched by about 200 GeV corresponding to the no sfermion coannihilation case. In this zone of large LSP mass, the relic density decreases compared to the generic higgsino DM case due to the dominance of squark-squark coannihilations. We will come back to it for further discussion while describing Fig.2  As seen in the figure, this leads to a higgsino dominated LSP with mass as low as 450 GeV satisfying Eq.3.1. The associated coannihilating sleptons correspond to δ less than 2%. We also note that as explained in Sec.2 as well as in the description of Fig.1(a), an analysis with only the first two generations of sleptons would hardly show any dependence on tan β concerning the lower limit of the LSP mass satisfying the relic density constraint of Eq.3.1. Fig.2(b) shows the result for the LSP-squark coannihilations where we have considered only the first two generations of squarks for which the outcome is essentially independent of tan β. On the lower side, the LSP mass satisfying Eq.3.1 is reduced to around 840 GeV from 1 TeV corresponding to the generic higgsino DM case.
On the other end, the higgsino LSP mass may extend to about 1300 GeV, about a 20% increase than the generic higgsino DM upper limit. There is a "notch" region corresponding to δ ∼ 0.05 spreading across the values of the LSP mass. In this quasi degenerate LSP-squark setup, the above arises due to a relatively rapid change of the DM relic density coming out of the enhancement of qqχ 0 1,2 effective couplings. We will discuss this at the end of Sec.4.1.
In the zone of relatively large LSP mass and for nearly degenerate squarks and the LSP i.e.
small values of δ, a detail check of the outgoing products of annihilation and coannihilations confirms that the squark-squark coannihilations dominate over the generic higgsino DM effective annihilation cross-section. We note that the latter, which is inversely proportional to the DM relic density, decreases with increase in higgsino mass 4 . Additionally, for larger values of δ and larger LSP mass, in spite of a smaller degree of generic electroweakino annihilation/coannihilations due to heavier LSP, the squark-squark coannihilations are more and more exponentially suppressed. Thus, even for slightly larger values of δ we get overabundance of DM. of the higgsino LSP mass satisfying the DM relic density constraint is around 500 GeV. 4 For the generic higgsino LSP case one has Ω χ 0 1 h 2 = 0.10( µ 1 TeV ) 2 [25], where µ is given in TeV. A similar relation for a wino LSP with mass mW reads ΩW h 2 = 0.13( mW 2.5 TeV ) 2 = 0.021m 2W [25], denoting a factor of 5 stronger effective annihilation cross section compared to the higgsino case. As we will see the squark-squark coannihilation contributions are not large enough to supersede the generic wino DM depletion cross section. Hence, the wino dominated LSP scenario with squark coannihilations will not encounter any stretching of the LSP mass region satisfying the relic density data on the higher side.
The result of a combined analysis of the above slepton (three generations) and squark coannihilations (two generations) is given in Fig.3. The colors refer to the same convention as that of

Wino dominated LSP
A wino-like LSP in MSSM implies nearly degenerate χ 0 1 and χ ± 1 , both of whose masses being essentially determined by the SU (2)  The presence of sleptons with masses close to m χ 0 1 leads to many new coannihilation channels and affects the averaging procedure 5 We must note that a wino mass of 1.8 TeV satisfying the relic density data is low compared to what is seen in the literature, typically above 2 TeV. Obtaining a heavier wino that satisfies the DM relic density limits is possible i) via considering larger sfermion mass and µ as explained in the text in Sec.3.1 and ii) most importantly, via including non-perturbative effects like Sommerfeld correction. Sommerfeld correction is known to increase the wino mass that satisfies the relic density limits. We have not included such an effect particularly for the fact that a low wino mass like 1.1 TeV would hardly have an appreciable degree of Sommerfeld effect. We would like to mention Ref. [29] (their toward the effective cross section and as we will see this increases the DM relic density so that Eq.3.1 is satisfied for much smaller masses of the LSP.  The amount of the wino component in the LSP is expressed in terms of the wino fraction defined as, Z W = N 2 12 . The wino fractions for different LSP masses with/without sfermion coannihilations are shown in Fig.4. We only show the parameter points that satisfy Eq.3.1 for the limits of DM relic density. Fig.4(a) shows the scatter plot of the wino fraction Z W vs LSP mass when the LSP efficiently coannihilates with sleptons and sneutrinos of all the three generations. We note that the Fig.2) and Ref. [30] (their Fig.2) in support of the smallness of the correction for our relevant zone of wino mass.
Considering the fact that the relic density ∝ M 2 2 , using Ref. [30] we estimate a 10-12 % level of enhancement of M2 for its lower bound that would satisfy the observational relic density limits. Thus, the lower limit of the wino mass is estimated to change from 1.1 TeV to around 1.2 TeV (as we will come across in Fig.4) if we include the Sommerfeld effect.
(a) (b) Figure 5. a) Scatter plot for the mass of LSP m χ 0 1 vs δ, the relative deviation of slepton masses with respect to the mass of the LSP for LSP-slepton coannihilation scenarios including also sneutrinos, where the LSP is highly wino dominated in its composition. For a given slepton mass labeled as ml i the relative deviation is given as δ i = LSP-sfermion coannihilations take place in the background of strong electroweakino coannihilations. The significance of wino purity level in turn is directly related to the level of coannihilations between the electroweakino states χ 0 1 and χ ± 1 . As before, we have considered a maximum of 20% deviation in masses for the coannihilating particles with respect to the mass of the LSP. The squark masses of the first two generations are kept at 4 TeV . The reference results with no slepton coannihilations are shown in green and blue points for tan β = 10 and 30 respectively. The black and red points refer to tan β = 10 and 30 respectively for the cases with slepton coannihilations. Clearly, as seen in Fig.4(a), the slepton coannihilations reduce the lower limit of the LSP mass satisfying Eq.3.1 to m χ 0 1 1.1 TeV and 1.3 TeV respectively for tan β = 10 and 30. There is a dissimilarity in the lower limits in the results for the two different values of tan β for similar reasons as in the case of higggsino LSP mentioned in Sec.3.2. We extend the results to LSP-squark coannihilations in Fig.4(b). Here the sleptons are chosen to be very heavy (4 TeV). The color codes are same as those of Fig.4(a). The squarks again refer only to the first two generations for reasons mentioned earlier.
One finds the lower limit as m χ 0 1 1.1 TeV for both values of tan β. points belong to parameter space that satisfy Eq.3.1. Fig.5(a) shows the scatter plot in the (m χ 0 1δ) plane. Apart from the sleptons we also include the three generations of sneutrinos in this analysis.
δ is similarly defined as in the higgsino case of Sec.3.2. The color codes are same as those of Fig.2.
The left and right hand side white regions indicate LSP to be underabundant and overabundant respectively. The regions with large δ refer to smaller degrees of coannihilation because of larger exponential suppression. The brown region corresponding to tan β = 30 is associated with a larger degree of stau L-R mixing. Demanding bothτ 1 andτ 2 along with the first two generations of sleptons to have masses within 20% of the LSP mass restricts the reach of δ for reasons mentioned in Sec.2. The effect of slepton coannihilations is more prominent for tan β = 10 and this leads to a wino dominated LSP having the right abundance with mass as low as 1.1 TeV when the coannihilating sleptons have δ less than 2%. Similar to the higgsino analysis, the tan β dependence of the lower limit of m χ 0 1 satisfying Eq.3.1 would cease to exist if we had excluded the third generation of sleptons to take part in coannihilations. Fig.5(b) shows a similar result for the LSP-squark coannihilations where we consider only the first two generations of squarks as before. Clearly, being devoid of any top-squark coannihilations the result is essentially independent of tan β. The lowest LSP mass that satisfies the DM relic density constraint is around 1.1 TeV. Unlike the higgsino case, there is no dominance of squark-squark coannihilations over the parameter space that satisfies the DM relic density constraint. This is indeed related to the large annihilation cross section that a wino has compared to that of a higgsino for a given mass of the LSP (see footnote#4). Similar to the higgsino case, there is a "notch" region corresponding to δ ∼ 0.05 spreading across the values of the LSP mass. In this quasi degenerate LSP-squark setup, the above arises due to a relatively rapid change of the DM relic density coming out of the enhancement of qqχ 0 1 effective coupling. We will discuss this at the end of Sec.4.1.
The results of a combined analysis of the above slepton (three generations) and squark coannihilations (two generations) is given in Fig.6. The two different colors namely cyan (circle) and brown (square) refer to the cases of tan β = 10 and 30 respectively. The left and right hand side white regions indicate LSP to be underabundant and overabundant respectively. The regions with large δ refer to smaller degrees of coannihilation. The lower limit of the wino LSP mass satisfying the DM relic density constraint is around 900 GeV.
We would like to mention here that the ATLAS and CMS collaborations presented their results for chargino searches in the high transverse momentum (p T ) disappearing tracks [72] and long lived particle search channels for nearly degenerate χ ± 1 and χ 0 1 [73]. The mass range of χ ± 1 considered in this analysis is well within these bounds.

Direct and Indirect Detection of DM
In this section we will probe the prospect of direct and indirect detection of the lightest neutralino.
We will particularly come across the importance of squark exchange diagrams in computing the SI direct detection cross section. The squark exchange diagrams are usually less important since the Higgs exchange diagrams typically dominate. As we will see, in this analysis we are in a different situation because of considering quasi-degenerate squarks and LSP for the requirement of coannihilations.

Direct Detection
Direct detection of DM involves finding the recoil energy deposited when a DM particle scatters off a detector nucleus [4,5]. Spin-independent LSP-proton scattering may take place through s-channel squark exchange and t-channel Higgs exchange diagrams. When the squarks are considerably heavy, the Higgs exchange diagrams typically dominate [74,75] The Higgs-χ 0 1 -χ 0 1 coupling for the higgsino-LSP case can be written down in the form [52]: where t W = tan θ W etc. with θ W being the Weinberg angle. Similarly, for the wino-LSP case, the couplings are as follows [52]: From the above expressions it is clear that the couplings and hence the scattering cross-section would be large if there is a large degree of mixing between the gaugino and the higgsino components of the LSP. We also note that couplings become weaker for increased gaugino masses and µ. On the other hand, a pure higgsino or a wino LSP with very little mixing can hardly be able to produce large values of spin-independent cross-section. Fig.7 shows our results for DM direct SI detection cross-section where only the points satisfying Eq.3.1 are shown for a higgsino type of LSP undergoing LSP-slepton coannihilations ( Fig.7(a)) and LSP-squark coannihilations ( Fig.7(b)).
The cyan and brown points correspond to tanβ = 10 and 30 respectively. The red line (solid) is the LUX 2016 exclusion contour [51] and the maroon dashed line shows the expected limit from the future XENON1T experiment [76]. Clearly, the recent LUX data rules out low higgsino mass region below 600 GeV ( Fig.7(a)). We must also remember the existence of uncertainty, around one order in magnitude, in the computation of the SI direct detection cross-section. Factors like strangeness content of nucleon, local DM density, velocity distribution profiles, all contribute toward such uncertainty amount (See Ref. [37] and references therein). As seen in Fig.7(a) the higgsino LSP scenario may be effectively probed via XENON1T. Fig.7(b) shows similar results for the LSP-squark coannihilations. Here, the lowest LSP mass that survives after the LUX 2016 data is about 840 GeV. Additionally, a large region of parameter space 7 is discarded via the same 7 By parameter space one really means here a smeared region of squark masses around a given LSP mass. experiment without however affecting the lowest possible value of the LSP mass. Compared to the case of Fig.7(a) here the SI direct detection cross-sections are generally large. This is a signature of having a quasi-degenerate squark and LSP scenario that comes into our study of the LSPsquark coannihilations. Here the effective coupling constant for quark-LSP scattering drastically increases [77] causing the cross-section to be larger, often much more than the LUX limit for a significant zone of the LSP mass. Thus, the squark exchange diagrams are potentially able to compete with or even dominate over the Higgs exchange diagrams while contributing to the total direct detection cross-section 8 . This is of course true for some region of parameter space where the degree of the LSP-squark mass degeneracy is higher. We remind that the above is unlike the usually encountered MSSM parameter regions where Higgs exchange diagrams dominate over the squark exchange diagrams in the SI direct detection cross-section. Coming back to Fig.7(b) we see that a lot of parameter space is eliminated via LUX 2016 data. The remaining parameter space can fully be probed in the XENON1T experiment. The effect of including both slepton and squark coannihilations is shown in Fig.7(c). The lowest LSP mass limit satisfying the LUX data is around 680 GeV. Eq.3.1 are shown for a wino type of LSP undergoing slepton coannihilations ( Fig.8(a)) and squark coannihilations ( Fig.8(b)). The cyan and brown points correspond to tanβ = 10 and 30 respectively.
The red line (solid) is the LUX 2016 exclusion contour [51] and the maroon dashed line shows the expected limit from the future XENON1T experiment [76]. Clearly, as seen in Fig.8(a) the crosssection is too low so that even XENON1T would not be able to probe this scenario except around the 1.1 TeV region for LSP mass. We must additionally clarify that a comparison of Fig.7(a) and Fig.8(a) shows that contrary to what we would naively expect, the SI cross-section in the latter case is in general smaller. The reason lies in the fact that the values of m χ 0 1 that satisfy the relic density limits for a wino like LSP are much higher than that of a higgsino dominated LSP. Fig.8(b) shows similar results for the LSP-squark coannihilations. Here, the lowest LSP mass that survives after the LUX 2016 data is about 1.27 TeV. Additionally, a large region of parameter space is discarded via the same experiment while eliminating a window of 1.1 TeV to 1.27 TeV of LSP mass. XENON1T would not be able to probe this scenario except the region close to 1.2 TeV of the LSP mass. Similar to the case of higgsino-squark coannihilations, the SI direct detection cross-section is much larger for wino-squark coannihilation scenario compared to the wino-slepton results. The squark exchange contributions can be significantly large for the parameter points associated with near degeneracy of the squark and LSP masses as explained before. Here, we observe that the cross-section can be quite large even for squark masses > ∼ 1.2 TeV. The Higgs-exchange contributions are sub-dominant in this case of wino-dominated LSP that has a very small higgsino content. We must also note 8 The extent of any cancellation effect on the contrary is small, unlike the wino scenario that we will see soon.
that for a fixed value of m χ 0 1 we get a wide degree of variation in cross-section with some points exceeding the LUX limit whereas some points having values below the limit. In the latter case there is a cancellation among the contributions from the squark and Higgs exchange diagrams that pushes the cross-section to very low values. Similar to what happens for the higgsino LSP case as in Fig.7(b), this is a signature of quasi-degenerate squarks and LSP that leads to a large increase in the effective coupling constant for quark-LSP scattering [77].
Finally, the effect of including both slepton and squark coannihilations is shown in Fig.8(c).
The lowest LSP mass limit satisfying the LUX data is about 1 TeV.
We will come to the discussion of the notch regions of Fig.2(b) and Fig.5(b). Apart from direct detection, enhancement of qqχ effective coupling near the degenerate zone of squarks and LSP masses has its important signature also on the DM relic density. For a wino dominated LSP that does not have a quasi degenerate neutralino state, the notch region is found to coincide with the mentioned cancellation region of σ SI χp (i.e. cancellation between the higgs exchange and the squark exchange diagrams). Corresponding to a given mass of the LSP, this is the region of δ where the above effective coupling becomes large. The situation for a higgsino-LSP case is more involved. This is principally because on the top of the coannihilations a wino LSP would undergo, there are additional coannihilation processes like χ 0 2 χ 0 1 , χ 0 2q contributing toward the higgsino relic density. As a result, in spite of a cancellation zone of σ SI χp for certain values of δ, coannhilation effects potentially smear the abrupt change in the higgsino relic density coming out of the effect of enhanced χ 0 1q q and χ 0 2q q coupling strengths. Consequently, for a higgsino DM the values of δ that correspond to a cancellation or an enhancement zone in σ SI χp are not the same where the anomalous "notch" zone of the relic density occurs. However, the enhancement of coupling remains a valid fact. It is seen that for a given m χ 0 1 there is an abrupt decrease of the DM relic density corresponding to some range of δ. Once a lower and a upper limit of the relic density are imposed, the above decrease in relic density irrespective of the LSP mass, leads to the formation of the notch regions for some effective range of values of δ. Details may be explained by examining the relevant coupling enhancements as given in Ref. [77] 9 .

Indirect Detection
DM particles may get trapped due to gravity inside astrophysically dense objects like the Sun or the Earth by losing energy through repeated scattering with the nucleons. Inside the core of these objects DM particles may undergo pair annihilations leading to SM particles like fermionantifermion pairs, gauge bosons etc. in the final state. The resulting antiparticles, neutrinos and gamma rays can offer interesting indirect signals of DM in the galaxy.
The high energy neutrinos produced as end products of DM pair annihilation in the solar core can produce muons through charged current interactions. The IceCube experiment [53] provides bounds on the muon flux for the pair annihilation channel DM DM → W + W − . Fig.9(a) shows a scatter plot of the values of muon flux as a function of m χ 0 1 for higgsino dominated LSPs undergoing slepton coannihilations for parameter points satisfying Eq.3.1. The cyan and brown points correspond to tan β = 10 and 30 respectively. The green and blue lines are the current and projected limits from the IceCube experiment [53,54] in the χ 0 1 χ 0 1 → W + W − channel. Similarly, Fig.9(b) shows the results for LSP-squark coannihilations. Clearly, the fluxes in both the above figures are in general too small to be probed. The results of muon flux for the case of a wino dominated LSP is shown in Fig.10. Fig.10(a) shows the results for LSP-slepton coannihilations for parameter points that satisfy Eq.3.1 for wino dominated LSPs undergoing slepton coannihilations. The color convention and the details of the limits from IceCube data are similar to Fig.9(a). Clearly, the flux is too small to be probed for the LSP-slepton coannihilation scenario. Similarly, Fig.10(b) shows the results for LSP-squark coannihilations. The result does not show any more exclusion of low mass LSP region compared to what is seen in Fig.8(b) for the SI direct detection cross section.
Let us now discuss the constraints on spin-dependent DM-nucleon interaction cross-section as derived from the IceCube data. Inside the solar core, the number density N of DM particles at any instant of time t is obtained from the following [4], where, C c is the capture rate of DM by interaction with the nucleons present at the surface of the Sun whereas C A is related to the annihilation rate Γ A as : . Hence, the capture rate is determined by the annihilation rate and when the age of the universe is much greater than τ (which occurs for large C c and C A ), an equilibrium is reached so that Γ A = 1 2 C c . Thus, it is possible to put bounds on the annihilation and capture cross-sections by looking at the indirect DM signals from the Sun. Since, capture of the DM particles occurs through spin-independent/dependent (SI/SD) DM interactions with the nucleons, these bounds get translated into the bounds on DM SI/SD interaction cross-sections. χ 0 1 can have spin-dependent interaction with the quarks via s-channel squark exchange and t-channel Z-boson exchange processes. Similar to the SI case, while considering LSP-slepton coannihilations, we can safely ignore the contributions from the squark exchange processes since the squarks are taken to be heavy. The tree level Z χ 0 1 χ 0 1 coupling is given by c Z χ 0 For the higgsino LSP case the coupling is given as [52], (4.4) with µ > 0(µ < 0). The same coupling for the wino case takes the form [52], Thus, in general the couplings get suppressed as the LSP, irrespective of a higgsino or a wino becomes heavy. Fig.11(a) shows the results for the SD cross section for the higgsino dominated LSP scenario for LSP-slepton coannihilation. Fig.11(b) shows the LSP-squark coannihilation case for which the degeneracy between squark and the LSP masses (similar to what was described in the SI case) may push up the SD cross section. In general the IceCube limits would be inadequate to probe such higgsino models.   12 shows the results for the SD cross section for the wino dominated LSP scenario for LSP-slepton coannihilation ( Fig.12(a)) and LSP-squark coannihilation ( Fig.12(b)) cases. Although the IceCube limits may eliminate some region of parameter space where the LSP undergoes squark coannihilations, the result does not show any more exclusion of low mass LSP region compared to what is seen in Fig.8(b) for the SI direct detection cross section.
In Table 1 we show two benchmark points (BP) satisfying WMAP/PLANCK relic density limits of Eq.(3.1) as well as the direct and indirect detection limits from the LUX and IceCube experiments respectively. BP1 and BP2 correspond to the case of a higgsino-LSP undergoing slepton and squark coannihilations for masses 617 GeV and 760 GeV respectively for tan β = 10.
Monojet searches at the 14 TeV LHC can probe pure higgsino scenario only upto the mass of m χ 0 1 ∼ 410 GeV [78]. However, the situation looks more promising for a 100 TeV collider where higgsinos may be probed upto 1.2 TeV. Existing disappearing track searches at the LHC do not have much sensitivity to a higgsino LSP. However, with modifications in search strategy, as suggested in Refs. [79], higgsinos upto ∼ 600 GeV and ∼ 1.1 TeV could be probed by the 14 TeV high luminosity (HL)-LHC and a 100 TeV collider respectively. BP3 and BP4 refer to wino-like LSP participating in slepton and squark coannihilations with masses 1011 GeV and 1188 GeV respectively for the same value of tan β. Although a HL-LHC at 14 TeV seems to be unable to probe these benchmark points, a 100 TeV collider, with an exclusion reach of ∼ 1.8 TeV in the monojet search channel can decisively explore such scenarios [78]. These benchmark scenarios for wino-like DM is likely to evade the HL-LHC even with disappearing track searches. However, the same searches at a 100 TeV collider can conclusively probe these cases. Apart from collider searches, all the four BPs will be probed in near future with the XENON1T experiment. However, they are unlikely to produce any signal in future indirect detection experiments. turns out to be a higgsino, these processes include pair-annihilation and coannihilations among χ 0 1 , χ ± 1 and χ 0 2 . The same for a wino-LSP situation include coannihilations between χ 0 1 and χ ± 1 . It is known that these processes are too strong to cause the LSP to become an underabundant component of DM unless its mass is around 1 TeV for a higgsino or a little above 2 TeV for a wino type of LSP. We consider a compressed scenario of pMSSM where sfermions may take a very significant role as coannihilating sparticles. Our purpose is to examine how light the LSP as a higgsino or a wino can be while it satisfies both the lower and the upper limit of the DM relic density as given by the WMAP/PLANCK data. We choose two representative values of tan β, namely 10 and 30 and consider both sleptons and squarks as coannihilating partners. In regard to the LSP-slepton coannihilations we consider all the three generations of sleptons including also the sneutrinos while keeping the squark masses heavy. We perform the analysis by requiring a maximum of 20% mass difference between that of the LSP and each of its coannihilating partners.
Consideration of the slepton coannihilations reduces the effective cross section leading to an increase in the relic density. This is how the relic density gets modified or in other words this is how the lower limit of the LSP mass satisfying the relic density limits decreases. We find that for a higgsino dominated LSP the lowest LSP mass that satisfies the relic density limits is about 450 GeV, about a 60% reduction corresponding to the case of no sfermion coannihilations and this occurs for tan β = 10. The dependence on tan β comes via the L-R mixing of tau-sleptons and the exponential suppression generically associated with coannihilation toward the effective annihilation cross-section. The same reduction in the lower limit for a wino type of LSP occurs for tan β = 10 and it is about 1.1 TeV, more than a 100 percent reduction in the value corresponding to the case of no sfermion coannihilations. For squarks, we allowed coannihilations with only the first two generations of squarks while imposing a similar 20% limit as before for the deviation of masses of the coannihilating particles from the LSP mass keeping the third generation of squarks as well as sleptons of all the generations very heavy. The reason of omitting the third generation lies in the fact that a large splitting between the two top-squark masses as required by a 125 GeV Higgs boson would take away a lot of parameter space if we need a uniform 20% limit for the difference of each of the squarks and the LSP masses. In the absence of coannihilating third generation of squarks, our results become essentially independent of tan β. The lowest LSP mass satisfying the relic density limits is about 840 GeV for the higgsino case, only a modest reduction by 10-15% from the generic higgsino LSP scenario. For the higgsino-squark coannihilation scenario we additionally obtain a region of parameter space where the relic density is decreased when squark coannihilations come to the picture, thus increasing the upper limit of the LSP mass satisfying the relic density data. This happens only in a very limited zone of parameter space with nearly degenerate squark and LSP masses and toward the end of the upper limit of the LSP mass satisfying the DM relic density data.
Coming to wino, the lower limit of the LSP mass with the above squark coannihilations is around 1.1 TeV. Additionally, computation for a scenario of combined slepton and squark coannihilations shows that the lower limit of higgsino-LSP is about 500 GeV whereas for a wino-LSP the same is about 900 GeV. We also note that throughout our study we consider the CP-odd Higgs boson (A) to be sufficiently heavy so as to avoid an s-channel A-pole.
We further analyze the direct and indirect detection prospects of DM for the above types of LSPs for the two kinds of sfermion coannihilations considered in this work. In the part of the analysis that involves squark-LSP coannihilations, because of the near degeneracy of squarks with the LSP, the squark exchange diagrams in the direct detection cross section can be very important. These may even exceed the contributions from the Higgs exchange diagrams which typically dominate the generic MSSM parameter space.
The SI direct detection cross section may exceed the recent LUX data for a higgsino type of LSP undergoing slepton coannihilations for a mass below 600 GeV. For squark coannihilations, the above number is about 840 GeV. The corresponding number for the case of slepton plus squark coannihilations is around 680 GeV. The same occurs at around 1.27 TeV for a wino-LSP undergoing squark coannihilations whereas there is no direct detection constraint for the part of the study involving slepton coannihilations. The case of combined slepton and squark coannihilations gives a lower mass limit of a wino DM as 1 TeV. However, in spite of the appearance of the above limits we must keep in mind that there can be an order of magnitude of uncertainty in the computation of the SI direct detection cross-section. This may potentially lower the above mass limits by 10 to 15%. The indirect detection data such as that from the IceCube for the muon flux do not put any additional constraint than whatever is given by the relic density and the SI direct detection cross section data in combination. Regarding future experiments, XENON1T would be able to probe only the higgsino LSP scenario with both kinds of sfermion coannihilations. Finally, with relevant bounds from ATLAS and CMS being satisfied, we pointed out that for LSP and χ ± 1 either being a higgsino or a wino dominated in nature there is hardly any collider bound to worry about while considering the compressed pMSSM scenario where the sfermion masses would be suitable for DM coannihilations.
Acknowledgments UC is thankful to receive the hospitality from CERN Theory division where a major part of this work was completed. MC would like to thank TRR33 "The Dark Universe" project for financial support.