Detecting underabundant neutralinos

The electroweak sector may play a crucial role in discovering supersymmetry. We systematically investigate the patterns of the MSSM-like electroweakinos, when the neutralino relic abundance $\Omega_\chi h^2\leq 0.12$, that is, also admitting for multi-component Dark Matter, in a broad range of the parameter space. We find that for a very large range of parameters the Direct Detection experiments are/will be sensitive to underabundant neutralinos, in spite of the strong rescaling of the flux factor. The second general conclusion is that the bound $\Omega_\chi h^2\leq 0.12$ together with the LUX (XENON1T) limits for the neutralino spin independent scattering cross sections constrain the electroweakino spectrum so that the mass differences between the NLSP and the LSP are smaller than 40 (10) GeV, respectively, with important implications for the collider searches. The future Direct Detection experiments and the high luminosity LHC run will probe almost the entire range of the LSP and NLSP mass spectrum that is consistent with the bound $\Omega_\chi h^2\leq 0.12$.


Introduction
Supersymmetry remains to be an attractive extensions of the SM even if merely for being one of the few UV complete frameworks, with no quadratic sensitivity to large mass scales. It may well be that the supersymmetric electroweak sector will play the leading role in discovering supersymmetry. Indeed, experimental searches for coloured superpartners, motivated by the issue of naturalness, have so far given null results. It is conceivable that supersymmetric models remain natural even with new coloured degrees of freedom heavier than few TeV (e.g. because the soft masses are correlated [1], because the Higgs mass is further protected [2] or it is protected by colourless degrees of freedom [3]) or it could be that supersymmetry plays no role in stabilizing the weak scale (like in split supersymmetry [4]).
However, in models with a stable neutralino and if one accepts the thermal history of the universe, the higgsino and gaugino masses are bounded from above by the thermal overabundance of the LSP. 1 So far, the interest in the supersymmetric electroweak sector has been often linked to the fact that a stable neutralino can account for the observed Dark Matter (DM) in the universe. It is, however, conceivable that DM has a multi-component structure. There is no reason why in the "dark" sector there would be only one stable particle. It is possible that the neutralino component in the observed DM is small or even very small and the bulk of DM has a different origin. The electroweak sector is then an interesting signature of supersymmetry in its own sake and there should be investigated the prospects for its discovery for any Ω χ ≤ Ω DM .
Partial results of such investigations do exist in the literature, particularly for collider signatures and for the pure higgsino and wino limits [8]- [31]. 2 In this paper we readdress this question, with the aim of an overall, systematic analysis in a large parameter space of the electroweak sector and with the focus on the interplay of the direct detection (DD) and collider experiments. Our global analysis leads to several new general conclusions. An additional theoretical motivation for such a global analysis is the variety of possible mechanisms for mediation of supersymmetry breaking, with different patterns of gaugino masses.
There are at least two different ways to discover those underabundant neutralinos, in DD experiments and in colliders. The latter are at present excluded by LUX [33] for where σ SI LUX is the upper bound on the cross section obtained with the local DM density ρ 0 = 0.3 GeV/cm 2 , corresponding to the observed dark matter abundance Ω DM [34]. For the future discovery potential in the direct detection, the σ SI LUX has to be replaced by the corresponding new • bino-wino with a heavy but not totally decoupled higgsino, to mediate some bino-wino mixing; this situation may happen in an anomaly mediated scenario with the higgs superfields acting as messengers of supersymmetry breaking [41,40].
Those limiting cases are a good reference point for subsequently investigating the general case in which higgsinos and both electroweak (EW) gauginos simultaneously contribute to the LSP composition (that might possibly occur in more sophisticated SUSY breaking schemes like e.g. mirage mediation [42] or mini-split supersymmetry [41] ).
The main conclusions of this paper are the following: first of all, in spite of the small relic abundance and the rescaling in the flux factor, the present and future DD experiments are/will be sensitive to neutralinos with Ω χ h 2 even two to three orders of magnitude below the observed value Ω DM h 2 = 0.12. 3 Thus, a discovery of a signal in DD experiments would not necessarily mean the discovery of the main DM component but might be a strong hint for supersymmetry. Similarly, the present and future limits on the spin independent scattering cross section put strong constraints on the electroweakino parameter space with underabundant neutralinos.
Secondly, the results of the DD experiments have strong impact on the search strategies in colliders for electroweakinos in the bulk of the supersymmetric parameter space, if sfermions are heavy. This is because then the smaller the σ SI χ and/or the Ω χ are/is, the smaller the mass splitting between the LSP and NLSP becomes, which is crucial for collider searches. Already the current LUX limit constrains this splitting to be less than 40 GeV. With the future direct detection experiments, such as XENON1T [43] and LZ [44], the bound on the LSP-NLSP mass splitting can be brought below 10 GeV, as a generic result for a MSSM-like spectrum with heavy sfermions. Qualitatively, that result can be understood as a consequence of a smaller bino contribution to the LSP, strongly constrained from above by the limits from the DD experiments, in addition to the constraint from the upper bound on Ω χ h 2 . Of course, if a signal was discovered in the DD experiments, similar remarks would apply to the searches for its direct confirmation in colliders.
Finally, focusing on the interplay of the DD and collider experiments, we identify the parameter regions where both may have comparable discovery potential and supplement each other and those where they are complementary to each other. There are regions of the parameter space in which the LSP escapes direct detection and we survey the prospects of the 13/14 TeV LHC to probe the SUSY EWkino states in these regions. In many cases existing search techniques for quasi-degenerate states at the 13/14 TeV LHC are able to close the gaps in the parameter space that are inaccessible to future direct detection experiments. However, for some regions of the parameters the spin independent scattering cross section is below the neutrino background [73] and parts of those regions are also inaccessible to the 13/14 TeV LHC experiments using present search techniques. We classify these regions to encourage search for new techniques to probe them at the LHC and future colliders.

Bino-Higgsino LSP
The electroweakino sector with decoupled wino component in the LSP and the prospects for its experimental discovery have already been studied in a number of papers [11,14,15,16,19,21,27,28,31,46]. In this paper we reanalyze this case for completeness of our presentation and also for stressing several general conclusions.
With heavy sfermions, pure bino has no annihilation channels and is excluded by the bound Ω χ h 2 ≤ 0.12 [34]. The annihilation cross section for pure higgsinoh is determined by the vertex h 0h± W ∓ . The dominant annihilation channel is into the gauge bosons and co-annihilation with almost mass degenerate remaining higgsino states is very important. The approximate formula for the relic abundance reads [8]: (2) Thermally produced pure higgsinos overclose the universe for |µ| 1 TeV. In the left column of Fig. 1 we exemplify the results of the scan over µ in the range |µ| = (100 GeV, 2 TeV) and M 1 in the range (100 GeV, 6 TeV), 4 with |M 2 | = mf = m A = 7 TeV, 5 for Ω χ h 2 versus the neutralino mass. Throughout this paper we calculate the SUSY spectrum using SOFTSUSY [48] and compute the Ω χ and the σ SI χ using micrOMEGAs [49]. We set the values of the soft SUSY breaking parameters and the µ parameter at 7 TeV. In the plots we divide the (mχ0 1 , Ω χ ) plane into (45 × 40) bins and keep the maximum and minimum of the scaled neutralino-nucleon cross section, σ SI χ · Ω χ /Ω DM , if there are more than one entries in the bin. For each bin we plot two points slightly displaced indicating these maximum and minimum values with the colourcoding that represents the value of σ SI χ · Ω χ /Ω DM . We use five different markers to classify the constraint/sensitivity on the cross section versus neutralino mass plane. The scaled cross section σ SI χ · Ω χ /Ω DM is: larger than the LUX limit and excluded for stars, allowed by LUX but within the reach of XENON1T for circles, beyond the reach of XENON1T but within the reach of LZ for diamonds, beyond the reach of LZ but above the neutrino background floor for triangles and below the neutrino floor for crosses. 6 We use the expected sensitivity of XENON1T corresponding to a three year run from 2015 and that of LZ also corresponding to a 3-year run with a projected start date of 2017. The projected sensitivities are taken from [73].
In the scanned parameter range, there is only a small admixture of the wino component (although it is not totally decoupled). As it can be seen in those plots, the minimal value of Ω χ h 2 ≈ 10 −3 corresponds to |µ| = 100 GeV. For a given value of the neutralino mass, approximately equal |µ| in the whole range of Ω χ h 2 ≤ 0.12, the approximately pure higgsino case, M 1 |µ|, corresponds to the smallest values of Ω χ , that is to the boundary of the scan. The neutralino relic abundance increases with the increasing bino component, that is for a decreasing value of M 1 , eventually reaching the observed value Ω DM h 2 = 0.12. There, |µ| ≈ M 1 , which is called the well tempered bino/higgsino region [8].
It is instructive to present the results of the scan in the (|µ|, M 1 ) plane as in the right column      of Fig. 1. First of all, we indeed see that the bound Ω DM h 2 = 0.12 corresponds to M 1 ≈ |µ| with M 1 < |µ| and M 1 > |µ| for low and close to 1 TeV values of |µ| ≈ mχ0 1 , respectively. This is easily understandable as the effect of the µ dependence of the pure higgsino relic abundance, eq. (2). Secondly, it is interesting to compare the contours of constant Ω χ h 2 in the plots in the right column of Fig. 1 with the results in the plots in the left column, remembering that mχ0 1 ≈ |µ|. A given value of Ω χ h 2 can be obtained only for a certain range of mχ0 1 ≈ |µ| and this is clearly seen in both sets of plots. Furthermore, the bottom-up increase of Ω χ h 2 with the increasing bino component corresponds to the top down change of M 1 for fixed µ.
Also in Fig. 1 there is given information about the magnitude of the spin independent scattering cross section to the nucleons and the present exclusion regions and the regions accessible in the future, in the direct detection experiments. Since the hχχ vertex vanishes for pure states, the tree level σ SI χ vanishes for pure higgsino. The loop effects included in the micrOMEGAs code and the residual mixing effects give non-zero but very small cross sections along the boundary of the scan in the (mχ0 1 , Ω χ h 2 ) plane. For a given neutralino mass, the larger the value of Ω χ is, the larger the event rate in the spin independent scattering cross section becomes because of the flux factor Ωχ Ω DM but also because of the larger bino-higgsino mixing angle. One can see the difference in the magnitude of the spin independent scattering cross sections between small and large values of tan β and between the two signs of µ, especially for small tan β. They can be understood in terms of the formulae for the mass eigenstates and the bino-higgsino mixing angle, collected for the sake of easy reference in the Appendix. Approximately, the σ SI χ reads [9]: where the coupling c hχχ is defined as L ∼ 1 2 c hχχ (χχ + χ † χ † )h and in the limit M Z sin θ W ||M 1 | − |µ|| reads: for |µ| > |M 1 | (this is the region almost totally excluded by the bound Ω χ h 2 ≤ 0.12) and for |µ| < |M 1 | (see eqs. (20) and (54) as well as the corresponding comments in the Appendix). Moreover, in the limit (see eq. (62) and the following discussion in the Appendix).
Those formulae explain the behaviour of σ SI χ , its tan β dependence and the dependence on the sign of µ for small tan β. An important effect is the existence of the so-called blind spots for the hχχ coupling, 7 that is the parameter regions where it is very small, for small tan β and µM 1 < 0, as it is evident from the above equations [9].
The main conclusion following from Fig. 1

is that, in spite of the rescaling by the flux factor
Ωχ Ω DM , the whole range of Ω χ h 2 values between 10 −3 and 0.12 is reachable in the direct detection experiments. A large part of the (µ, M 1 ) plane is either already ruled out by the present DD experiments or will be tested by the XENON1T and LZ experiments or at least corresponds to the spin independent cross sections above the neutrino background. The only exception is the large blind spot region for small tan β and µ < 0, not accessible in the DD experiments. We also note that (6) gives a blind spot near the diagonal |M 1 | ≈ |µ| for small tan β and µ < 0.
The results shown in Fig. 1 also confirm the known results [8,9], that the bino-higgsino LSP can still account for the observed DM. For large tan β with positive (negative) µ that would be a well-tempered bino-higgsino in a mass range from 800 (700) up to 1000 GeV corresponding to a pure higgsino. For small tan β and negative µ the whole range of masses between 100 and 1000 GeV is still allowed. The latter follows from the fact that for small tan β the well-tempered neutralino is close to the blind spot for the hχχ coupling. For small tan β and positive µ the hχχ coupling is enhanced by the µ sin(2β) term in (5) so only masses very close to 1 TeV, corresponding essentially to pure higgsino LSP, are allowed.
The exclusion/accessibility regions depend on the experimental limits which are in addition a function of the LSP mass (weaker bounds for heavier LSP). The interplay of both factors explains the pattern observed in the right column of Fig. 1.
We also check the indirect DM detection experiments in our parameter scan. The indirect detection bound is usually not as strong as that for direct detections. However, it can effectively constrain the spin-dependent scattering cross section. Since the structures of spin-dependent and spin-independent cross sections are not correlated to each other, the spin-dependent bound may become superior in the blind spot region of the spin-independent cross section.
One of the most stringent bounds on the spin-dependent cross section comes from the ICECUBE experiment. ICECUBE looks for the neutrinos coming from the annihilation of the neutralinos captured by the sun. When the capture and annihilation reach the equilibrium, the total annihilation of the neutralinos is fixed by the capture rate, which is proportional mainly to the spin-dependent cross section and the local neutralino density on the sun's trajectory. Therefore, if the neutralino annihilation produces neutrinos (e.g.χ 0 1χ 0 1 → W + W − ), the limit on the high energy neutrino flux from the sun can be translated to the limit on the spin-dependent cross section times the local neutralino density [55]. 8 We have checked the spin-dependent cross section at each parameter point of our scan and confronted it with the ICECUBE spin-dependent bound shown in Fig.2 of ref. [51] (obtained 7 Another type of blind spots involving cancellation between the light and heavy Higgs exchanges has also been discussed e.g. in [52,53,54]. 8 We thank Marc Kamionkowski for discussion on this point.

assuming 9χ0
1χ 0 1 → W + W − ). In ref. [51] the limits on the capture rate are converted into the limits on the spin dependent cross section assuming the standard local dark matter density of 0.3 GeV/cm 3 . For smaller DM density the bounds for spin dependent cross section given in that Fig.2 of ref. [51] have to be rescaled by Ω χ /Ω DM and are, of course, weaker. Another important point for understanding our results is the dependence of the SD scattering cross section on the LSP composition. The SD cross section is dominated by the Z boson exchange and the Zχχ coupling is proportional to (N 2 13 − N 2 14 ). This coupling vanishes for any of the pure neutralino states (there is no direct Z-wino-wino or Z-bino-bino coupling while in the case of a pure higgsino this follows from the equality N 2 13 = N 2 14 = 1 2 ). For the higgsino-dominated LSP its coupling to Z, given by eq. (21), is non-zero and suppressed by M 1 and M 2 . Thus, the smaller M 1 and/or M 2 (i.e. the larger the wino and/or bino component), the larger the Zχχ coupling and the SD cross section, up to the point where the higgsino component becomes very small (in this limit the Zχχ coupling is given by eqs. (37) and (38)). Thus, the Zχχ coupling becomes sizable for bino-higgsino or wino-higgsino mixed LSP (see also eq. (63)) but in the second case the neutralino relic abundance is smaller and after the rescaling the bounds on the SD cross section are weaker. This is why in our plots the ICECUBE bounds are relevant only for the bino-higgsino mixed LSP. We found that the ICECUBE spin-dependent constraint is less stringent than the LUX spin-independent constraint in most of the parameter region. We only found small excluded regions by ICECUBE around the M 1 ∼ |µ| < 200 GeV in the (M 1 , µ) plane with tan β = 2, µ < 0. This can be understood from eq. (63). The leading term of the Zχχ coupling is suppressed by |M 1 | + |µ| and enhanced when M 1 µ < 0, especially for small values of tan β. Those regions happen to be the ones where the blind spot cancellation in the spin-independent cross section is operative. They can be seen as the green regions in the lower right plot of Fig. 1 and the upper left plot of Fig. 3. We have checked that they are the only regions where the ICECUBE constraint is more stringent than the LUX one throughout our analysis presented in this paper.
For collider searches, an important information is the mass difference between the NLSP (usually chargino) and the LSP as well as between χ 0 2 and the LSP, and also the life time of the NLSP. In Fig. 1 we show the contours of ∆m ± ≡ mχ± 1 − mχ0 1 in the scanned region. In Fig. 2 we plot the points with Ω χ h 2 < 0.12 from our scans in the (∆m ± , σ SI χ Ωχ Ω DM ) plane for tan β = 10 and µ > 0. The colour-coding indicates σ SI χ and we use the same markers as used in the left column of Fig. 1 to classify the DD constraint/sensitivity. One can see that after imposing the LUX bound the mass differences ∆m ± are in the range (1-30) GeV and the expected sensitivity of the XENON1T will bring them down to (1)(2)(3)(4)(5)(6)(7)(8)(9)(10) GeV. This is the general result for most of the parameter space, except for small tan β and µ < 0 region where the mass difference will remain to be up to 40 GeV even after the XENON1T and LZ results.
The results can be qualitatively understood from eq. (12) in the Appendix. We see that and the latter as 1 M 1 . We note, however, that the decoupling of the wino and bino components in the formulae for the gaugino masses and mass differences is slow, only linear in M 2 and/or M 1 . Even for M 1 = M 2 =7 TeV one is still far from the pure higgsino limit. For pure higgsino states, the tree level mass difference between the lighter chargino and the LSP neutralino is zero. The loop effects give the mass difference around 350 MeV [58] 10 whereas in Fig. 1 it is at least twice that large. In the parameter range of Fig. 1, the chargino life time cτ is shorter than 10 −1 cm, where the upper bound corresponds to the smallest mass difference. The mass difference betweenχ 0 2 and the LSP is about twice as large as betweenχ + 1 and the LSP (see eq. (11)). The implications of all those facts for collider searches are discussed in the next subsection.
With the discussed above patterns for large |M 2 | (small wino component) as a reference frame, it is interesting to consider how those patterns change when the value of |M 2 | decreases and approaches the values of |µ| and/or M 1 . In Fig. 3 we show some generic examples of the results of the scan over M 1 and µ, with M 2 = ±1.1 min(M 1 , |µ|). The plots for both signs of M 2 and µ flipped are similar to those shown in Fig. 3. The blue region in the plot for tan β = 2, µ < 0 is excluded because the lighter chargino is the LSP and after the change of signs of M 2 and µ similar region is excluded by the LUX bound. The main effect is that in the M 1 < |µ| region the 10% degeneracy M 2 = ±1.1M 1 introduces some wino component in the LSP. The large wino annihilation cross section ensures that even with a small admixture of winos, the previously excluded regions (see Fig. 1) are now partially allowed. This effect is weaker for opposite signs of M 2 and µ since the admixture of wino is then smaller.     Xenon1T  [56] with the help of SUSYHIT program [57]. In the dark blue region the lighter chargino is the LSP. The small green region at M 1 ∼ |µ| < 200 GeV in the upper left plot is the excluded region by the ICECUBE experiment [51].
Another very important effect of a larger wino component in the LSP are generically larger values of the spin independent scattering cross sections (the blind spots disappear), so that neutralinos with the relic abundance in the whole range of Ω χ h 2 between 10 −3 and 0.12 are mostly within the reach of XENON1T. Finally, the ∆m ± remains below O(10) GeV and ∆m 0 ≡ mχ0 2 − mχ0 1 ≈ 2∆m ± (for the higgsino-dominated LSP this can be easily seen from eqs. (11) and (12) in the Appendix).

Collider
We have shown that in the bino-higgsino scenario the region where |µ| M 1 is excluded by the overproduction of the thermal DM or the direct DM detection limit given by the LUX      The conventional technique for the collider search is to focus on the production of heavier states and look for the energetic particles and missing energy originated from the decays of the produced particles. This strategy however does not work very efficiently in the phenomenologically allowed region, M 1 > |µ| and |µ| > ∼ M 1 . In the former case the production cross section of the heavier state namely the bino-like state is too small if squarks are decoupled. In the latter case the mass difference between the higgsino-like states and the bino-like LSP is small and the sensitivity of the conventional searches is degraded because of the softness of the decay products of the higgsino-like states, although some alternative channels based on radiative photon decays may work [22]. The same is also true for the M 1 > |µ| case for the events with production of higgsino-like states, since higgsino-like states are almost mass degenerate and the decays among these states only produce very soft particles.
The production of such quasi mass degenerate particles can nevertheless be detected if the mass difference between the charged state and the LSP is small enough so that the charged particle has a collider scale lifetime ( > ∼ 0.1 ns). Such long-lived charginos may leave the distinctive disappearing track signature in the trackers. We however found that higgsino-like states are almost always short lived in our scan except for the vicinity of the chargino LSP region shown in the up-right plot of Fig. 3. Another way of detecting quasi degenerate particles is to look for events where these particles are produced associated with hard initial state radiation. These events are sensitive to the monojet search which requires large missing energy recoiling against one or two energetic jets (See Fig. 4.). In refs. [15,16,17,31] the sensitivity of the monojet search to the higgsino-like LSP scenario has been studied. The results found in these literature vary because their simulation set up and selection cuts are different. The authors of [31] found the most optimistic results, albeit with very aggressive cuts. We use their result because they presented the expected sensitivities at the 13 TeV LHC as functions of mχ0 1 and ∆m ± , which enables us to translate their limit on our parameter plane. We project their 2-σ regions into our (|µ|, M 1 ) parameter plane in Fig. 5, where the darker (lighter) green region corresponds to the 100 (3000) fb −1 integrated luminosity. The monojet search is sensitive only for the ∆m ± < 20 − 30 GeV. Therefore the sensitivity dies off in the |µ| M 1 region because ∆m ± becomes too large. The LHC sensitivity (green) regions are similar for other combinations of the relative signs of the parameters and all values of tan β. They depend very weakly on the value on M 2 . We can see some complementarity between the DM direct detection experiments and the collider experiments, especially for the M 2 decoupled case in Fig. 5. For negative values of µ, there remain, unfortunately, some regions of the parameters not accesible neither at the LHC nor in the DD experiments.

Wino-Higgsino
The above discussion can be easily extended to neutralinos that are mainly a mixture of higgsino and wino (we take M 1 = 7 TeV), which are less explored in the literature (see, however, [20,12,19,27]). The annihilation cross section for pure winoW is determined by the vertex W 0W ± W ∓ . One has approximately [8] ΩW h 2 = 0.13 This formula does not include the Sommerfeld enhancement for the wino component [59]. It is not included in the micrOMEGAs code used by us, but this does not affect the main conclusions of the paper. 11 The annihilation of winos is more efficient than that of higgsinos. The minimal value of Ω χ h 2 (for M 2 = 100 GeV) reaches 2 · 10 −4 and the value of 0.12 is reached for M 2 ≈ 2.3 GeV. This is seen in the left plots of Fig. 6, for tan β = 2, µ < 0 and tan β = 10 and µ > 0. An admixture of higgsinos increases the value of the neutralino relic abundance. The values of     Ω χ h 2 , when shown as a function of the LSP mass, fall in the region between the two boundaries given by the pure higgsino and wino states. The tree level spin independent scattering cross section vanishes for pure higgsino and wino states. The hχχ coupling is approximately given by the equations (4), (5) and (6), with the following replacements: M 1 → M 2 , g 1 → g 2 , sin θ W → cos θ W and with the change of the sign of the first term in eq. (6).
Those equations explain the qualitative patterns of the results of the scan plotted in the (|µ|, M 2 ) plane shown in the right column of Fig. 6. 12 In general, the σ SI χ decreases in the direction perpendicular to the diagonal. There is an interesting dependence on tan β and on the sign of µ. One effect is again the existence of blind spots for small tan β and negative µ and a strong enhancement of the spin independent scattering cross sections for positive µ.     respect to the diagonal |M 2 | ≈ |µ|. They can be understood by looking at the equations (4), (5) and (6), updated to the present case. For instance, for large tan β the σ SI χ is larger for |µ| < |M 2 | (dominantly higgsino) than for |M 2 | < |µ| (dominantly wino) because of the 1 M 2 versus 1 µ 2 suppression of the couplings in eqs. (5) and (4), respectively. There is also some residual dependence on the sign of µ coming from the numerator in eqs. (4) and (5). For small tan β and negative µ the asymmetry with respect to the diagonal is reversed, as can be seen from the interplay of the numerators and denominators in eqs. (4) and (5). The important conclusion is that the vast parameter range is accessible in the DD experiments. However, it is clear that the dominantly wino or higgsino LSP regions will not be reachable in the DD experiments and these regions still take up sizeable portion of the (µ, M 2 ) plane, particularly in the dominantly wino case.
The separation into the two regions, |µ| < |M 2 | and |M 2 | < |µ|, is important for understanding the pattern of mass differences and the NLSP lifetime. The higgsino-like LSP region (|µ| < |M 2 |) is qualitatively similar to the bino-higgsino mixed LSP region discussed in the previous section. We observe that ∆m ± is also O(1 − 10) GeV but slightly larger than in the bino-higgsino case, because of the cos θ 2 W /M 2 corrections versus sin θ 2 W /M 1 corrections in the previous case (see eq. (12)). Also, as before, ∆m 0 ≈ 2 × ∆m ± .
In the wino-like LSP region (|M 2 | < |µ|) the tree level ∆m ± vanishes up to very small corrections (see eq. (41) and (42) in the Appendix) and ∆m ± ≈ 160 − 170 MeV is given by the loop effects [62]. The lifetime becomes large, of the order of O(0.1) ns. On the other hand, there can be arbitrarily large mass difference ∆m 0 ≈ |µ| − |M 2 | .
The effects of non-decoupling of M 1 in the scan over M 2 and µ are illustrated in Fig. 7. One can see, comparing Fig. 7 with Fig. 6, that the main patterns are quite similar to the decoupled case. In particular, this is true for the mass differences ∆m 0 (not shown in the Figures) and ∆m ± but the σ SI χ is generically larger, especially for |M 2 | > |µ|, making easier the detection of the LSP in the future DD experiments. Adding the bino component makes the values of Ω χ h 2 for the same neutralino mass somewhat larger, going above the higgsino bound seen in Fig. 6.

Collider
For the wino-higgsino scenario the strategy of collider search has new elements as compared to the bino-higgsino case. Both wino-like and higgsino-like states can have sizable production cross section. For sufficiently large splitting in the values of M 2 and µ, the heavier of the winolike or the higgsino-like states can decay to the higgsino-like or wino-like states, respectively, accompanied by W , Z or W , h 0 boson pairs (see Fig. 8). An interesting signature for |M 2 | > |µ| is then the decayW ±W 0 → W ± Z(h) + E miss T , whereW ± andW 0 are the wino-likeχ ± 2 and χ 0 3 , respectively and E miss T includes higgsino-likeχ ± 1 ,χ 0 2 andχ 0 1 , neglecting soft particles arising from theχ ± 1 andχ 0 2 decays into an almost mass degenerateχ 0 1 . Similarly, for |µ| > |M 2 |, we have the decaysh ±h0 → W ± Z(h) + E miss T and in this case,h 0 andh ± are higgsino-likeχ 0 2 ,χ 0 3 andχ ± 2 , respectively, and E miss T includes wino-likeχ ± 1 andχ 0 1 assuming the decay products of theχ ± 1 decay does not contribute to the signal regions in the analysis. Such W + Z(h) + E miss T signatures depend on the production cross sections of the heavy gaugino/higgsino pairs and on their branching ratios into those final states. Using the Goldstone equivalence theorem   [63] one can estimate [63,64] that the branching ratio of each initial particle into W Z(h) is 50%, with 25% for Z and h each, so that we have 50% probability for the W + Z(h) + E miss T signature and the remaining 50% goes into W W , ZZ and hh final states. There is no dedicated analysis of the LHC discovery potential for such signatures (such an analysis for 100 TeV colliders is presented in [64]). CMS have studied the projected sensitivity in the 14 TeV LHC with 3000 fb −1 for theχ ± 1χ 0 2 → (W ±χ0 1 )(Zχ 0 1 ) and theχ ± 1χ 0 2 → (W ±χ0 1 )(h 0χ0 1 ) processes [65], assuming wino-like production cross sections for the initial states and 100% W + Z(h) + E miss T signature. In this study, 5-σ sensitivities for three different models, BR(χ 0 2 → [Zχ 0 1 , hχ 0 1 ]) = (100, 0), (0, 100), (50, 50) %, are presented and they are found to be similar to each other. We can use those results for the purpose of a qualitative illustration of a ballpark sensitivity to our (|µ|, M 2 ) plane, keeping in mind that the CMS assumptions about the production cross sections and the decay signature are not strictly valid in our case, but just up to a factor of 2-3. We map the CMS 5-σ sensitivity for the BR(χ 0 2 → [Zχ 0 1 , hχ 0 1 ]) = (50, 50) % case (in accordance with the Goldstone equivalence theorem) by identifying m CMS The result is shown by the grey regions in Fig. 9 surrounded by the dashed curves. One should stress again that this is only a qualitative illustration of "an order of magnitude" for the expected sensitivity, because of the mentioned above simplified CMS assumptions about the production and decay rates, inadequate for our case.
As we discussed in section 2, the production of the lighter multiplet (lighter of the wino-or higgsino-like states) can be probed by the monojet search and the disappearing track search. In Fig. 9 and 10 we show the 2-σ sensitivity region found in [31] using the same procedure as in Fig. 5. Since the study of [31] assumes the higgsino-like LSP scenario, the green region in the wino-like LSP region should be regarded as conservative since the wino cross section is larger   than the higgsinos at the same mass, although we believe it is not too conservative by the same reason mentioned above. It is known that the lifetime of charged wino can be as long as the collider scale in the almost pure wino region. In Fig. 6 the charged wino lifetime is longer than 0.1 ns to the right of the black dashed curves, where the search exploiting the disappearing tracks can be sensitive. ATLAS [66] and CMS [67] have looked for disappearing tracks in the 8 TeV proton-proton collision data and identified the 95% CL excluded regions in the (mχ± 1 , ∆m ± ) plane. Since we can compute mχ± 1 and ∆m ± at each point in the (|µ|, M 2 ) plane, we can map these 95% CL excluded regions onto our parameter plane. We translate the ATLAS excluded region (Fig. 6 of [66]) in our (|µ|, M 2 ) plane, which are shown by the darkest red regions. We also project the 8 TeV excluded regions into the 14 TeV LHC using Collider Reach program [68] assuming the projected limit is obtained with the same number of signal events after the event selection as observed at the 8 TeV exclusion boundary. 13 The projected sensitivity for the 14 TeV LHC with 300 (3000) fb −1 is shown by the darker (light) red region.   For |M 2 | < M 1 the LSP and the NLSP are neutral and charged winos, respectively. The LSP relic abundance is that of a pure wino, already discussed in the previous section. The mass difference ∆m ± is about 160−170 MeV, given by the loop effects and the NLSP decay has a collider scale lifetime, cτχ± 1 ∼ 5 − 10 cm. The mass difference ∆m 0 is fixed by the difference M 1 − |M 2 |. The spin-independent scattering cross sections are very small, given by loop effects and below the neutrino background. The region M 1 < |M 2 | is excluded by the bound Ω χ h 2 < 0.12. The above simple picture is a good reference frame for discussing what happens when the values of the |µ| parameter come closer to the values of M 1 and/or |M 2 | (see also [15]). In Fig. 12  In the scan exemplified by Fig. 12 the higgsino is heavy, it mediates the bino-wino mixing but its admixture remains small. In Fig. 11 the higgsino component in the LSP plays already important role and the observed patterns can be understood by comparing with the plots for 10% degeneracies discussed in the previous section.
We see in Fig. 12 that most of the bino-dominated region is still excluded by the bound Ω χ h 2 ≤ 0.12. However, for M 1 ≈ M 2 an acceptable region opens up, although for µ > 0 mostly excluded by the LUX limits. For µ < 0 (not shown in the paper), in that well-tempered bino-wino region the spin-independent cross sections are often within the reach of the Xenon1T experiment. The recent result of a general 10 parameter MSSM scan, including the g − 2, the collider constraints as well as the DM constraints with Ω χ = Ω DM , also prefers this parameter region [72].   With |µ| = 1.1M 1 (see Fig. 11) the LSP becomes a mixture of all three components, with large higgsino-bino mixing, and only a part of the previously excluded region is still excluded by the bound Ω χ h 2 ≤ 0.12. This region resembles the regions with M 1 = 1.1|µ| in Fig. 7, that is the regions above the diagonal. The regions excluded by the overproduction of the neutralinos are, however, larger because of the stronger bino component. The spin independent scattering cross sections are large and the mass differences are of order O(10) GeV. |M 2 | < M 1 For |µ| = 1.1M 1 , the LSP remains dominantly wino-like but some admixture of bino makes the spin-independent cross sections partly accessible in the DD experiments. The mass differences are very small and the NLSP is long-lived, with strong implications for collider searches.
With |µ| = 1.1|M 2 |, the LSP is dominantly wino-higgsino. The patterns seen in Fig. 11 resemble those for M 2 = 1.1|µ| in Fig. 3 (i.e. above the diagonal), although the mass differences are typically smaller, closer to the pure wino case. The scattering cross section is below the LUX bound but above the neutrino bound.
In the right plots of Fig. 12 and 11 we show the estimated LHC discovery limits. We plot again the 2-σ sensitivity of the monojet search [31] in the (M 1 , M 2 ) plane with the dark (light) green region corresponding to the 13 TeV LHC with 100 (3000) fb −1 of the luminosity. The projected sensitivity for the 14 TeV LHC with 300 (3000) fb −1 to the disappearing track search, estimated as described in the previous section, is shown by the darker (light) red region.
Both, for |µ| = 1.1 max(M 1 , |M 2 |) and |µ| = 1.1 min(M 1 , |M 2 |), the bino-like LSP region (|M 2 | > M 1 ) is mostly excluded because of the overproduction of the neutralinos. In the other half of the parameter space (M 1 > |M 2 |), for |µ| = 1.1 max(M 1 , |M 2 |) the LSP is composed dominantly of wino, with some bino components. As seen in Fig. 12 the DD and the collider searches are complementary to each other and cover a large part of that parameter space.
With |µ| = 1.1 min(M 1 , |M 2 |), the lighter chargino cannot have long enough lifetime to contribute to the disappearing track signature and the only channel which can probe the wino production events would be the monojet search. As seen in Fig. 11, for strong enough wino component the LHC can detect such production events, which will be an important cross check with the direct detection experiments such as XENON1T and LZ.

Final Comments and Conclusions
In the previous sections we have presented the results of several scans over certain ranges of parameters, which together cover essentially the whole relevant parameter space of the MSSMlike electroweak sector. Two conclusions have emerged from that study. One is that the two DD experiments, XENON1T and LZ, will be sensitive to neutralinos (LSPs) in almost the entire range of neutralino masses and compositions allowed by the bound Ω χ h 2 ≤ 0.12. There are some exceptions, though. One to be mentioned are some regions with negative values of µ, particularly for small tan β, with a dominant higgsino component in the LSP, where some "blind spot" regions remain. This is also true for the LSP with a dominant wino component, irrespectively of the sign of µ. The second conclusion is that in the electroweakino spectrum, ∆m ± (defined as the mass difference between the lighter chargino and the LSP) is smaller than 30 (10) GeV after imposing the LUX (expected from XENON1T) bounds on the neutralino spin independent scattering cross sections on nuclei. One should note however that, again, the small tan β and µ < 0 is the exception, as the mass differences can remain up to 40 GeV even after the XENON1T and LZ results. Some of the "blind spots" regions are accessible at the LHC but not all of them. To make the generic character of those conclusions even more manifest, we show in Fig. 13 the combined results of the scans for a given value of tan β and a given sign of µ. So far, we have shown the results obtained with both slepton and squark masses set to 7 TeV. It is interesting to check how much our conclusions change when the sfermions are lighter, particularly when the sleptons are lighter. It turns out that they remain valid still when the sleptons (and of course the squarks, too) are 20% heavier than the LSP (but not lighter than 1 TeV). This is illustrated in Fig. 14, which shows the results of a scan over |µ|, M 1 with m˜ = max(1 TeV, 1.2 min(M 1 , |µ|)). Indeed, Fig. 14 and Fig. 1 are very similar.
Finally, we comment on the collider searches. We have presented rough estimates of the LHC sensitivity, based on the previous results of ref. [31] for the monojet search, ref.
[65] for χ ± 1χ 0 2 → (W ±χ0 1 )(Z(h 0 )χ 0 1 ) search and ref. [66] for the disappearing track search. A more dedicated analysis focused on the parameter range of interest emerging from the present paper would certainly be worthwhile. It should include a search for new interesting channels and techniques. For instance, some studies at 13 TeV LHC [22] and a 100 TeV [26] pp collider have been done to attack the compressed spectra that appear in the higgsino-like LSP scenarios. The idea is to look for a soft dilepton plus a soft photon originated fromχ ± 1 → W * χ0 1 and χ 0 2 → γχ 0 1 decays, respectively. Here we simply show in Fig. 15 by purple an example of the  Fig. 1 region with ∆m 0 > 3 GeV and Br(χ 0 2 → γχ 0 1 ) > 0.1. 14 This region is potentially sensitive to more extensive analysis dedicated to this channel.
The overall conclusion of this paper is that the electroweakino sector, being subject to important physical constraints, is a very promising territory in search for supersymmetry. In some regions of the parameter space the DD and the LHC experiments have comparable discovery potential and supplement each other and in some other regions they are complementary to each other. The collider discovery potential would significantly improve if new techniques were developed to search for the weakly produced states with the mass differences between the NLSP and LSP of order of 1 GeV.
14 Br(χ ± 1 → W * χ0 1 ) ∼ 1 across our (|µ|, M 1 ) parameter plane.         the denominators of many terms becomes very small. The problem is caused by the fact that in such limit one of the off-diagonal terms in the neutralino mass matrix (after diagonalization of the higgsino sub-matrix) becomes very small and one of the assumptions discussed before eq. (55) is not fulfilled. However, the first subleading contributons to the c hχχ with 1 + ζ 1 s 2β in the denominator cancell out and do not contribute to (62). The LSP coupling to the Z boson is approximately given by