LHC SUSY and WIMP dark matter searches confront the string theory landscape

The string theory landscape of vacua solutions provides physicists with some understanding as to the magnitude of the cosmological constant. Similar reasoning can be applied to the magnitude of the soft SUSY breaking terms in supersymmetric models of particle physics: there appears to be a statistical draw towards large soft terms which is tempered by the anthropic requirement of the weak scale lying not too far from ∼ 100 GeV. For a mild statistical draw of msoftn with n = 1 (as expected from SUSY breaking due to a single F term) then the light Higgs mass is preferred at ∼ 125 GeV while sparticles are all pulled beyond LHC bounds. We confront a variety of LHC and WIMP dark matter search limits with the statistical expectations from a fertile patch of string theory landscape. The end result is that LHC and WIMP dark matter detectors see exactly that which is expected from the landscape: a Standard Model-like Higgs boson of mass 125 GeV but as yet no sign of sparticles or WIMP dark matter. SUSY from the n = 1 landscape is most likely to emerge at LHC in the soft opposite-sign dilepton plus jet plus MET channel. Multi-ton noble liquid WIMP detectors should be able to completely explore the n = 1 landscape parameter space.


Introduction
It is sometimes lamented that the emergence of the landscape of string vacua [1][2][3] has rendered string theory non-predictive since how are we to pick out the (meta-stable) vacuum corresponding to our universe from (perhaps) of order 10 500 possibilities? Such sentiment ignores one of the great predictions of the latter 20th century [4,5]: namely that given a multiverse which includes a vast assortment of pocket-universes with varying cosmological constants, then it may not be surprising to find Λ ∼ 10 −120 m 4 P since if it was much bigger, then galaxy condensation would not occur and we would not even be here to discuss the issue. The situation is portrayed in figure 1 which depicts the fact that the cosmological constant ought to be at its most natural value subject to the constraint that we can exist to observe it. Such anthropic reasoning relies on the existence of a vast landscape of possibilities that is provided for by the discretuum of flux vacua from string theory [1-3, 6, 7].
Can such reasoning be applied to the origin of other mass scales that appear in fundamental physics? 1 An obvious target would be the magnitude of the weak scale (m weak m W,Z,h 100 GeV) and why it is suppressed by 16 orders of magnitude compared to the (reduced) Planck scale m P 2.4 × 10 18 GeV. Anthropically, one expects a universe with electroweak symmetry properly broken such that weak bosons gain mass m W,Z ∼ 100 GeV while solutions with charge or color breaking minima would be excluded. In addition, nuclear physics calculations by Agrawal et al. [9,10] require that the magnitude of the weak scale shouldn't exceed its measured value by a factor of 2-3 in order to gain a livable universe. Given that quantum corrections to the Higgs mass diverge quadratically with the theory cutoff Λ SM , it seems the Standard Model (SM) with Λ SM m weak would be a rare occurrance within the landscape since one would be required to select only those vacuum solutions with highly fine-tuned scan parameters. In a landscape containing both SM and supersymmetric SM solutions (SSM), one would expect vastly more SSM solutions with m weak 100 GeV since then quantum corrections to m h diverge only logarithmically.

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In fact, this discussion brings up the issue of how naturalness is connected to vacua selection in the multiverse. Here we adopt the notion of practical naturalness: An observable O ≡ o 1 + · · · + o n is natural if all independent contributions o i to O are comparable to or less than O. This is because if any o i O, then some other contribution o j (j = i) would have to be fine-tuned to a large opposite-sign value to keep O at its measured value. The notion of practical naturalness may be compared with what Douglas calls stringy naturalness [11]: An effective field theory (or specific coupling or observable) T 1 is more natural in string theory than T 2 if the number of phenomenologically acceptable vacua leading to T 1 is larger than the number leading to T 2 .
In a landscape of vacua where independent contributions o i to observable O are uniformly distributed, then it follows that many more vacua are likely to exist where the o i are comparable to O than where some o i O so that some other value o j =i −o i . Thus, we expect these two definitions to be equivalent descriptions of naturalness. The landscape, if it is to be predictive, is predictive in the statistical sense: the more prevalent solutions are statistically more likely. This gives the connection between landscape statistics and JHEP04(2019)043 naturalness: vacua with natural observables are expected to be far more common than vacua with unnatural observables. 2 Thus, in this paper we will focus on vacua solutions which include the Minimal Supersymmetric Standard Model (MSSM) as their weak scale effective theory. This restricts our attention to a fertile patch of landscape solutions which include the SM as the weak scale effective theory (in accord with experiment) but where the weak scale is stable against quantum corrections (as in the MSSM). We will further assume that the MSSM arises from a 4-d supergravity theory (SUGRA) where SUSY breaking occurs via spontaneous SUGRA breaking in a hidden sector of the theory with a, perhaps, complicated SUSY breaking sector including possibly numerous SUSY breaking F -and D-term fields which gain vevs. The question that can be addressed is then: what does a statistical sampling of this fertile patch of the landscape say about the scale of SUSY breaking, and hence the likelihood of observable signals at the CERN Large Hadron Collider (LHC) or at WIMP dark matter direct and indirect detection experiments? Indeed, this question has already been investigated early on by Douglas et al. [13][14][15], Susskind [12] and by Dine et al. [16,17]. (For some reviews, see e.g. refs. [18,19].)

Statistics of the SUSY breaking scale
In this section, we assume a vast ensemble of string vacua states which give rise to a D = 4, N = 1 supergravity effective field theory at high energies. Furthermore, the theory consists of a visible sector containing the MSSM along with a perhaps large assortment of fields that comprise the hidden sector. The scalar potential is given by the usual supergravity form [20] where W is the holomorphic superpotential, K is the real Kähler potential and F i = D i W = DW/Dφ i ≡ ∂W/∂φ i + (1/m 2 P )(∂K/∂φ i )W are the F -terms and D α ∼ φ † gt α φ are the D-terms and the φ i are chiral superfields. Supergravity is assumed to be broken spontaneously via the super-Higgs mechanism either via F -type breaking or D-type breaking or in general a combination of both leading to a gravitino mass m 3/2 = e K/2m 2 P |W |/m 2 P . The (metastable) minima of the scalar potential can be found by requiring ∂V /∂φ i = 0 with ∂ 2 V /∂φ i ∂φ j > 0 to ensure a local minimum. The cosmological constant is given by Since the landscape allows for an apparently unnatural value of Λcc m 4 P , it is sometimes interpreted that vacua with other highly unnatural observables should also be entertained. In the case of Λcc, we should find ourselves in a universe where the cosmological constant is as natural as possible such that we gain a livable universe. Then we would expect Λcc ∼ 10 −120 m 4 P rather than say 10 −200 m 4 P .

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where m 4 hidden = i |F i | 2 + 1 2 α D 2 α is a mass scale associated with the hidden sector (and usually in SUGRA-mediated models it is assumed m hidden ∼ 10 12 GeV such that the gravitino gets a mass m 3/2 ∼ m 2 hidden /m P ). According to Douglas et al. [14] from investigations of flux compactifications in IIB string theory, the distribution of vacua ought to have the form where we define the weak scale m weak m W,Z,h 100 GeV and where m hidden sets the scale for SUSY breaking with m 2 hidden = i |F i | 2 + 1 2 α D 2 α for a (in general) more complicated SUSY breaking sector containing multiple sources of SUSY breaking, as may be expected to occur in string theory.
The function f SUSY contains the expected statistical distribution of SUSY breaking scales. This is related to the mass scale of MSSM soft terms as m soft m 2 hidden /m P . If the sources of SUSY breaking have uniformly distributed vacuum expectation values (vevs), then it is surmised that where n F is the number of F -breaking fields and n D is the number of D-term breaking fields in the hidden sector [11][12][13][14]. We will denote the collective exponent in f SUSY as n ≡ 2n F + n D − 1. Since the F terms are complex-valued but the modulus |F | sets the scale of SUSY breaking, then they contribute as (m 2 hidden ) 2n F whereas the real valued D terms contribute as (m 2 hidden ) n D . In terms of MSSM soft SUSY breaking parameters, one would expect a statistically uniform distribution of soft terms m 0 soft only for a single Dterm breaking field so that n D = 1. A single F -term breaking field leads to f SUSY ∼ m 1 soft so that there is a linearly increasing preference for large soft terms. For more complex configurations with larger number of n F and n D , then there is an even greater statistical preference for large soft terms which could lead to a preference for models with high scale SUSY breaking.
Regarding the role of the cosmological constant in determining the SUSY breaking scale, a key observation of Denef and Douglas [13,14] and Susskind [12] was that W at the minima is distributed uniformly as a complex variable, and the distribution of e K/m 2 P |W | 2 /m 2 P is not correlated with the distributions of F i and D α . Setting the cosmological constant to nearly zero, then, has no effect on the distribution of supersymmetry breaking scales. Physically, this can be understood by the fact that the superpotential receives contributions from many sectors of the theory, supersymmetric as well as nonsupersymmetric. The cosmological fine-tuning penalty is f cc ∼ Λ/m 4 where the above discussion leads to m 4 ∼ m 4 string rather than m 4 ∼ m 4 hidden , rendering this term inconsequential for determining the number of vacua with a given SUSY breaking scale.
The final term f EWFT merits some discussion. Following ref. [21], an initial guess [12,14,16,17] for f EWFT was that f EWFT ∼ m 2 weak /m 2 soft which may be interpretted as conventional naturalness in that the larger the Little Hierarchy between m weak and m soft , then the greater is the fine-tuning penalty. As pointed out in ref. [22], there are several problems with this ansatz.
1. As soft terms such as the trilinear A t terms increase, one is ultimately forced into charge-or-color-breaking vacua of the MSSM [23,24]. These sorts of vacua must be entirely vetoed on anthropic grounds.
2. As high-scale soft terms such as m 2 Hu increase too much, then they are no longer driven to negative values and electroweak symmetry isn't even broken. These non-EWSB solutions also should be vetoed on anthropic grounds.

As the high scale soft term m 2
Hu increases, its weak scale value actually becomes smaller and smaller until EWSB is barely broken [25,26]. This means the weak scale value of m 2 Hu becomes more natural -a phenomena known as radiatively driven naturalness (RNS) [27,28]. 4. As the soft term A t increases, then cancellations can occur in the Σ u u (t 1,2 ) contributions to the weak scale scalar potential, rendering their contributions closer to, not further from, the weak scale whilst at the same time lifting up the Higgs mass m h to the 125 GeV range. 5. Even in the event of appropriate EWSB, the factor f EWFT ∼ m 2 weak /m 2 soft penalizes but does not forbid vacua with a weak scale far larger than its measured value. In contrast, Agrawal et al. [9,10] have shown that a weak scale larger than ∼ 3 times its measured value would lead to much weaker weak interactions and a disruption in nuclear synthesis reactions, and likely an unlivable universe as we know it. In addition, Susskind posits that an increased weak scale would lead to larger SM particle masses and consequent disruptions in both atomic and nuclear physics. From these calculations, it seems reasonable to veto SM-like vacua which lead to a weak scale more than (conservatively) four times its measured value.
To account for these issues, in ref. [22] the alternative of was suggested where ∆ EW is the electroweak fine-tuning measure which just requires that weak scale contributions to m 2 Z should be comparable to or less than m 2 Z . From the minimization conditions for the MSSM Higgs potential [29] one finds The naturalness measure ∆ EW compares the largest contribution on the right-hand-side of eq. (2.7) to the value of m 2 Z /2. The radiative corrections Σ u u and Σ d d include contributions from various particles and sparticles with sizeable Yukawa and/or gauge couplings to the Higgs sector. Usually the most important of these are Q 2 − 1 and the optimized scale choice for evaluation of these corrections is Q 2 = mt 1 mt 2 . In the denominator of eq. (2.8), the tree level expressions of m 2 t 1,2 should be used. Expressions for the remaining Σ u u and Σ d d terms are given in the appendix of ref. [28].
In the remainder of this paper, we will assume a solution to the SUSY µ problem such as the gravity-safe, electroweak natural axionic hybrid CCK model based on a Z R 24 symmetry in ref. [30]. As such, we invert the usual usage of ∆ EW with fluid soft terms and µ term: instead, the weak scale (as typified by the value of m Z ) is no longer fixed at its measured value but is instead determined by eq. (2.7). In this case, values of ∆ EW 30 correspond to a value of m weak four times its measured value (in our sub-universe). The Θ function in eq. (2.6) guarantees that we veto vacua with CCB minima or no EWSB. It also vetoes properly broken Higgs potentials but where the weak scale is generated at more than four times its measured value.

Brief review of some previous work and goals of the present work
In ref. [26], an approach similar to Weinberg's anthropic solution to the cosmological constant was applied to determination of the SUSY breaking scale. It was assumed that there was a mild draw of the landscape towards large soft terms which was tempered by the anthropic requirement of a value for the weak scale which was not too far from its measured value by a factor ∼ four. The draw of m 2 Hu towards large values, tempered by an appropriate breakdown of EW symmetry, led to barely-broken EW symmetry. This is the same as the naturalness condition that m 2 Hu is driven to small negative values at the weak scale, and so gave a mechanism for why m 2 Hu should be driven to natural values. It was also emphasized that the statistical draw to large soft terms must avoid CCB and no EWSB vacua while at the same time drawing towards a weak scale not too far from its measured value. The combined statistical/anthropic draw would pull soft terms towards a region where A t is large (but not too large) and where m h ∼ 125 GeV.
In ref. [22], previous work by DD was adopted wherein soft SUSY breaking terms were actually selected according to f SUSY ∼ m n soft with n = 2n F + n D − 1 while f EWFT was adopted as in eq. (2.6). This allowed for landscape probability distributions to be calculated for a host of superparticle and Higgs masses. Calculations were performed using the threeextra parameter non-universal Higgs model (NUHM3) with parameter space given by where separate first/second and third generation soft scalar masses and a negative A 0 term were used. For n = 1 or 2, then the differential probability distribution for the Higgs mass dP/dm h acquired a firm peak around m h ∼ 125 GeV. Results from a scan over soft terms with µ : 100-360 GeV with A 0 < 0 and n = 1 (corresponding to a single SUSY breaking field F ) are shown in figure 2 for the case where the generated weak scale is less than a factor four from its measured value. The green histogram shows results when LHC search constraints (except Higgs mass) are also imposed (see below). Furthermore, the probability distributions for other sparticle masses gave

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From these results, one may conclude that the present LHC Run 2 results of finding a SMlike Higgs boson with m h = 125 GeV and no sign of sparticles is seeing exactly that which the landscape with n = 1 or 2 predicts will be seen. Furthermore, the higgsino-like WIMPs would form only a portion of dark matter (along with a SUSY DFSZ-like axion). Since the higgsino-like WIMPs typically constitute only ∼ 10% of dark matter, their detection rates lie below present WIMP search limits.
We also have checked the case with positive A term. Sparticles are pulled to higher masses due to the statistical draw but the Higgs mass peaks at 120 GeV and less than 1% of the scan points give correct Higgs mass. Since our main motivation for the landscape picture is the prediction of m h at its measured value, we do not consider experimental implications of A 0 > 0 for the remainder of the paper.
Our goal for the present paper is to confront the panoply of recent LHC and WIMP search experiment results with the predictions from the string theory landscape.

JHEP04(2019)043 3 Landscape predictions vs. LHC search limits
In this section, we confront the string theory landscape predictions for n = 1 with LHC sparticle search constraints and projected reach limits.

Landscape predictions for NUHM2 model
In years past, it was common to portray collider search limits in the m 1/2 vs. m 0 plane of the mSUGRA/CMSSM model [31,32]. In this model, the matter and Higgs soft mass terms are unified to a common GUT scale value m 0 , where the GUT scale is defined as that scale m GU T 2×10 16 GeV where the gauge couplings g 1 and g 2 unify. In the mSUGRA/CMSSM model, since m 2 Hu = m 2 H d ≡ m 2 0 as an input parameter, then µ is constrained by eq. (2.7) so as to ensure the measured value of m Z = 91.2 GeV. The natural portion of parameter space using Barbieri-Giudice fine-tuning [33] was found to be the lowest allowed values of m 0 and m 1/2 200 GeV [34]. This region is long-since excluded by LHC sparticle search constraints which with 80 fb −1 of integrated luminosity now require mg 2.25 TeV and mt 1 1.1 TeV. The value of µ in the LHC-allowed region is only natural ∼ 100-300 GeV in the focus point (FP) region [35][36][37]. But the FP region appears only for the smaller range of A 0 where m h is too low [38]. Thus, the region of mSUGRA/CMSSM parameter space with m h ∼ 123-127 GeV is always highly fine-tuned [39]. For this reason, we work instead first in the two-extra-parameter non-universal Higgs model NUHM2 [40][41][42][43][44][45] which allows independent input values of m 2 Hu and m 2 H d (since the Higgs live in independent GUT multiplets anyway). The values of m 2 Hu and m 2 H d may be traded for weak scale inputs µ and m A . This allows us to adopt a natural value of µ 200 GeV over all parameter space. We use Isajet 7.88 for our SUSY spectra generation and calculation of ∆ EW [46].
In figure 3 we display the m 1/2 vs. m 0 plane of the NUHM2 model for µ = 200 GeV, tan β = 10, A 0 = −1.6m 0 and m A = 2 TeV. The soft terms m 0 and m 1/2 are generated randomly for m 0 : 0 → 10 TeV and m 1/2 : 0.3-3 TeV but with the n = 1 increasing distribution and ∆ EW < 30 so that the weak scale is within ∼ 4 of its measured value. We see that the low m 0 and m 1/2 region is now sparsely populated due to the (mild) draw of the landscape towards large soft terms. In this plot, the density of points actually reflects the assumed vacuum statistics of the landscape with n = 1. The density increases with increasing m 0 and m 1/2 until the points cut off where soft term contributions to the weak scale exceed the measured weak scale by a factor four (∆ EW > 30). The red line denotes the latest LHC Run 2 bound of mg 2.25 TeV. The green points are LHC-allowed while black points above the red contour at lower m 0 have m h < 123 GeV (we assume an approximate ±2 GeV theory error in the Isajet m h calculation). The green LHC-allowed points range up to mg ∼ 3.5 TeV although for other parameter choices and moving to the NUHM3 model then gluinos can range as high as 6 TeV [47]. The most densely populated region of parameter space remains beyond current LHC reach and it may require an upgrade to high energy LHC (HE-LHC with √ s = 27 TeV and 15 ab −1 of integrated luminosity) to completely cover the remaining parameter space in the gluino pair production search channel [48].

Landscape predictions for NUHM3 model
In this subsection, we investigate landscape predictions within the more general NUHM3 model where first/second generation matter scalars have different soft terms from third generation matter scalars. This sort of setup is motivated in part by investigations of the minilandscape of heterotic string models compactified on an orbifold [49]. In these models, the first/second generation multiplets live near orbifold fixed points and obey localized grand unification [50]: they live in the 16-dimensional spinor reps of SO (10). In contrast, the third generation matter scalars, Higgs multiplets and gauginos live more in the bulk of the compactified orbifold and hence live in the usual SM split multiplets.
In this section, we will scan over soft parameters as m n=1 soft with the following ranges: while we scan over tan β : 3-60 and µ : 100-360 GeV uniformly since tan β is not dimensional and µ arises from our assumed solution to the SUSY µ problem. The lower limit of the µ term comes from the LEP2 limit on the lightest chargino mass, χ ± 1 > 103.5 GeV.

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(a) We show regions of ∆ EW > 30 (blank) and CCB minima (lower left) in the scalar potential. The blue points are LHC Run 2 and DMallowed.
(b) LHC Run 2 limit for mg > 2.25 TeV is shown by the red contour. • m h = 125 ± 2 GeV (to account for theory error of the calculation) The blue shaded points have acceptable vacua and obey both LHC and WIMP search constraints. The red points are LHC-allowed but excluded by recent XENON1T spinindependent (SI) direct WIMP detection (DD) searches [55] (see later figure 10). The main lesson from figure 4a is that the acceptable points lie in a very restricted regions where m 0 (3) and −A 0 are correlated: if A 0 gets too large (negative), then the model is forced into CCB minima so the gray region is disallowed. Likewise, if for fixed A 0 then m 0 (3) gets too large, then third generation contributions to the weak scale Σ u u (t 1,2 ) exceed the measured weak scale by over a factor four (blank region).
In figure 4b we show the m 1/2 vs. m 0 (3) soft term plane. The LHC Run 2 requirement that mg 2. correspond to values of mg over 6 TeV. Few scan points exist for m 0 (3) 2 TeV since the n = 1 scan prefers linearly increasing soft terms. Few points also exist for m 0 (3) 12 TeV since these points would give too large Σ u u (t 1,2 ) contributions to the weak scale. In figure 5a, we show our n = 1 landscape scan points in the m χ 0 1 vs. mg plane which is the usual simplified model plane in which LHC gluino searches are usually presented. The current LHC Run 2 exclusion contour based on 80 fb −1 of integrated luminosity is shown as the black contour. It is also interesting that the XENON1T dark matter search excludes significant regions of the lighter LSP masses for gluino masses of order 2-3.5 TeV. HL-LHC will be able to cover points with gluinos only up to 2.8 TeV via the gluino pair production channel [56]. We also show the recently computed 95% CL HE-LHC projected search limit for √ s = 27 TeV and 15 ab −1 which reaches to mg ∼ 6 TeV. Evidently a complete examination of n = 1 landscape points in thegg search channels will require HE-LHC.
In figure 5b, we show n = 1 landscape points in the m χ 0 1 vs. mt 1 simplified model plane. The current LHC Run 2 search limits are shown as the black contour. There is a high density of LHC-allowed (blue) points extending from mt 1 ∼ 1.1 to 2.7 TeV. The projected reach of HL-LHC with √ s = 14 TeV and 3 ab −1 extends to mt 1 ∼ 1.7 TeV and covers perhaps the greatest density of blue points. Nonetheless, it will require an upgrade to HE-LHC to cover the complete set of n = 1 landscape points [48].
In figure 6, we show the n = 1 landscape points in the mg vs. mt 1 plane. Of note here is that the points with the largest values of mg have the smaller range of mt 1 and vice-versa. Thus, if somehow for instance gluinos were able to escape LHC detection on account of them being too heavy, the top squarks would surely be seen (and vice-versa). A complete coverage of the n = 1 landscape parameter space will require HE-LHC with 15 ab −1 of integrated luminosity.
In figure 7, we show the m 0 (1, 2) vs. m 0 (3) plane of the NUHM3 model for the n = 1 landscape. The important lesson from this plot is that first/second generation matter scalar soft terms tend to inhabit the 10-30 TeV range whilst third generation matter scalar soft terms lie typically below 10 TeV. RG and mixing effects then cause the third generation JHEP04(2019)043  squarks/sleptons to lie in the few TeV range (so their loop-suppressed contributions Σ u u to the weak scale are small) while first/second generation squarks and slepton (with mass mq ,˜ ∼ m 0 (1, 2)) lie well beyond even HE-LHC reach and offer at least a partial decoupling solution to the SUSY flavor and CP problems. The reason they can be so heavy is that the first/second generation sfermion contributions to the weak scale are D-term contributions which largely cancel [57].
Another important LHC search plane is the µ vs. m χ ± 2 plane This plane is important for presenting search limits from same-sign diboson (SSdB) production arising from wino pair production in SUSY models with light higgsinos. The reaction is pp → χ ± 2 χ 0 4 where χ ± 2 → W ± χ 0 1,2 while χ 0 4 → W ∓ χ ± 1 so that half the time one arrives at a final state with two same-sign W bosons plus large E T . For leptonically-decaying W bosons, then the final state consists of a same-sign dilepton + E T signature which is relatively jet free-in contrast to same-sign dileptons originating from gluino and squark pair production. The same-sign channel has rather tiny SM backgrounds [58][59][60]. So far, no search results have been presented by ATLAS or CMS. From figure 8a, we see that LHC-allowed points only begin at wino masses m χ ± 2 ∼ 800 GeV and then extend out to m χ ± 2 ∼ 2300 GeV. This is to be compared with the projected HL-LHC 95% CL search limit which is the brown contour reaching to m χ ± 2 ∼ 1100 GeV [60]. Projected search limits for HE-LHC in the SSdB channel have yet to be computed.
In figure 8b, we show the n = 1 landscape points in the ∆m ≡ m χ 0 2 −m χ 0 1 vs. m χ 0 2 plane. This plane is important for the light higgsino pair production searches pp → χ 0 2 χ 0 1 (and χ 0 2 χ ± 1 ) where χ 0 2 → + − χ 0 1 giving rise to a soft opposite-sign dilepton pair whose invariant mass is bounded by m χ 0 2 − m χ 0 1 [61][62][63]. To trigger on such events, it seems necessary to require a hard jet radiation from the initial state against which the soft dileptons can recoil. Recent search limits have been presented by both ATLAS [54] and CMS [64]. We show as a black contour the recent ATLAS limit. An important point of the n = 1 landscape is that it favors heavier gauginos while µ must not be too far from the weak scale. The combination squeezes down the inter-higgsino mass gap m χ 0 2 − m χ 0 1 so that in this case all the LHC-allowed points have ∆m 10 GeV. We also show recently computed projected HL-LHC 95% CL reach contours [65]. The ATLAS contour has focussed on the small mass gap region and appears to cover nearly all parameter space. This has important implications for how SUSY is likely to be revealed at LHC. Gluinos and top squarks are expected to be drawn to large values, possibly beyond HL-LHC reach. The soft dilepton plus jet+ E T channel (SDLJMET) is the only channel that seems to be (nearly) completely covered by HL-LHC. Thus, we would expect a SUSY signal in this channel to emerge slowly but conclusively during the next 15 years as LHC acquires its full complement of 3 ab −1 of integrated luminosity! A final natural SUSY search channel occurs in the Higgs sector by looking for pp → A, H → τ + τ − events. These searches are typically presented in the tan β vs. m A plane which we show in figure 9. We also show the recent LHC excluded region as the black contour [53]. This latter contour assumes only SM decay modes for the A and H but for the landscape then the decay modes H, A → higgsinos should almost always be open as well (and might lead to 4 + E T signatures [66]). The added H, A → higgsinos decay modes hardly affect the search limits since a diminution of Higgs to SM branching fractions can be offset by increasing the Higgs production cross sections by moving to somewhat larger tan β [67]. From the plot, we see that the LHC-allowed points are typically well beyond the current LHC reach limits and the greatest density populates the region of m A ∼ 2-5 TeV and at lower tan β values where bb fusion contributions to the production cross section are not so big. Thus, we see only a small likelihood of a signal emerging in this channel at LHC.

Landscape predictions vs. WIMP DM search limits
In n = 1 landscape SUSY, we expect soft terms to be drawn to large values whilst the µ term is not too far from the weak scale. This results in a Little Hierarchy (LH) with µ m soft which turns out to be non-problematic. In such a scenario, then the lightest JHEP04(2019)043 SUSY particle is the lightest higgsino-like neutralino with mass m χ 0 1 ∼ 90-360 GeV. These natural higgsino-like WIMPs are thermally underproduced as dark matter, which may be a reason why they had not been considered much previous to 2011 [68][69][70]. However, one must recall that the QCD sector of the SM also suffers a naturalness issue in the form of the strong CP problem. Including an axion sector into the MSSM is thus well-motivated both for solving the strong CP problem but also to solve the SUSY µ problem (for a recent review, see e.g. ref. [71]) via a DFSZ-type SUSY axion. Thus, in natural SUSY it is expected that the DM is a WIMP-axion admixture (i.e. two dark matter particles). If the natural SUSY WIMPs (with m χ 0 1 350 GeV) were all of DM, then they would actually be excluded by current WIMP search constraints [72]. But if the DM is mainly axions, then there are far fewer relic WIMPs present in the cosmos and they can escape present limits from WIMP search experiments. A full evaluation of mixed WIMP-axion dark matter requires an eight-coupled Boltzmann equation evaluation which accounts also for axino, saxion and gravitino production and decay in the early universe [73].
We first examine WIMP search limits via ton-scale noble liquid experiments using targets such as Xenon or Argon. To compare WIMP search limits to landscape projections, one must calculate ξσ SI ( χ 0 1 , p) where ξ ≡ Ω χ 0 1 h 2 /0.12, i.e. it is the fractional abundance of WIMPs in making up the totality of dark matter. Usually this is just the WIMP thermal abundance divided by the measured abundance although it is possible the WIMP abundance is supplemented by non-thermal processes such as axino or saxion decay in the early universe.
In figure 10, we plot the locus of n = 1 landscape points in the ξσ SI ( χ 0 1 , p) vs. m χ 0 1 plane. We also show current search limits from the XENON-100 experiment [74] (black contour) and the XENON1T experiment [55] (red contour). A subset of LHC-allowed points are already excluded, and denoted as red points. However, the bulk of n = 1 JHEP04(2019)043 landscape points are still allowed, and extend down to an order of magnitude below present limits. These points do not extend all the way to the neutrino floor since in SUSY the WIMPs couple to nucleons mainly via light Higgs exchange and this coupling involves a production of gaugino times higgsino components [70]. In natural SUSY, the WIMP is mainly higgsino, but with non-negligible gaugino component (lest heavy gauginos give too large a contribution to the weak scale). Thus, it appears that projected seach limits from XENONnT (multi-ton Xenon detector), LUX-ZEPLIN (LZ) [75] and other multi-ton-scale detectors [76,77] should cover the entire n = 1 landscape parameter space, even if WIMPs comprise only a portion of the dark matter.
In figure 11a, we show the spin-dependent (SD) direct detection scattering rate ξσ SD ( χ 0 1 , p) vs. m χ 0 1 plane along with projected n = 1 landscape rates. We also show JHEP04(2019)043 recent limits from the PICO-60 experiment [78] and IceCube in the W + W − annihilation mode [79]. In this case, the LHC-allowed landscape points tend to lie about an order of magnitude below the current limits. We also show the projected future reach of LZ [75]. Even this contour does not quite reach the expected theory region.
In figure 11b, we show the indirect WIMP detection rates (IDD) in the ξ 2 σ ·v vs. m χ 0 1 plane, where ξ 2 is required since these signals arise from WIMP-WIMP annihilation in the cosmos and is thus suppressed by the fractional WIMP abundance squared. We show also the recent Fermi-LAT+Magic limits from observation of dwarf spheroidal galaxy Segue-1 [80]. The current limit is over an order of magnitude above the expected LHC-allowed points from the n = 1 landscape. A signal from the IDD search channel would point to non-thermal production of WIMPs (i.e. from decays of axinos/saxions) in addition to the thermally-produced neutralinos.

Conclusions
Rather general arguments regarding the statistics of the landscape of flux vacua in string theory point to a statistical draw towards large soft SUSY breaking terms governed by a power law m n soft where n = 2n F + n D − 1 involves the number of F and D term SUSY breaking fields in a (possibly) complicated hidden sector. With only the draw towards large soft terms, one would expect a huge value for the weak scale since m weak is determined by the visible sector soft terms and the SUSY µ parameter. A huge weak scale would mean highly suppressed weak interactions and huge particle masses which would likely lead to a non life-supporting universe. Agrawal et al. calculated that an increase in m weak by a factor of ∼ 3 would lead to a non-livable universe. Therefore, we have tempered the statistical draw of the landscape to large soft terms with the anthropic requirement of a weak scale no more than (conservatively) four times its measured value. For a fixed natural value of µ (arising from some solution to the SUSY µ problem such as hybrid CCK which also solves the strong CP problem and introduces axionic along with higgsino-like WIMP dark matter [30]), then one may implement random scans over power-law increasing soft terms tempered by an anthropic requirement of the weak scale not too far from m weak ∼ 100 GeV. The cases for n = 1 and 2 lead to a landscape probability distribution for the light Higgs mass which peaks around ∼ 125 GeV. Also, most superparticle masses are pulled to large values beyond LHC reach. In this case, LHC sparticle and WIMP dark matter search experiments are seeing exactly that which is expected from the n = 1, 2 landscape: a Higgs mass of 125 GeV and no sign yet of sparticles.
Our goal in this paper was a practical one: place the n = 1 landscape statistical predictions on the same plots that LHC sparticle and WIMP dark matter search experiments use in order to assess where sparticle and WIMP masses might be located relative to present and future search limits. In these sorts of plots, the density of points actually has meaning since it would reflect the assumed statistics of string theory vacua in a fertile patch which includes the MSSM as the weak scale effective theory.
Our findings are that strongly interacting sparticlesg andt 1 are likely to lie beyond present LHC search bounds and possibly beyond HL-LHC projected search limits. It may JHEP04(2019)043 require an upgrade to HE-LHC to cover the entire n = 1 landscape parameter space in thẽ gg andt 1t * 1 modes as manifested in the context of the natural NUHM3 SUSY model. Also, the SSdB signal may or may not be detected by HL-LHC and the A, H → τ + τ − signals are likely to lie well beyond the reach of LHC upgrades. However, the SDLJMET signal arising from higgsino pair production offers a search channel wherein HL-LHC may cover the entire projected parameter space. In this case, we would expect a SUSY signal to emerge slowly but conclusively by ATLAS and CMS as more and more integrated luminosity accrues.
Regarding WIMP searches, it appears that a full complement of data from multiton noble liquid SI direct detection experiments should cover the entire n = 1, NUHM3 landscape parameter space. This can occur even though in natural SUSY the higgsino-like WIMPs make up only a portion of dark matter with SUSY DFSZ axions making up the remainder. Meanwhile, even upgraded SD detectors may well fall short of covering the portion of parameter space occupied by the n = 1 landscape model. It appears that IDD WIMP search experiments will also have a hard time accessing the full parameter space since now the expected signal rates are diminished by the square of the fractional WIMP abundance. The search for SUSY DFSZ axions, addressed in ref. [81], is also difficult due to the presence of higgsinos circulating in the aγγ coupling diagram: they tend to suppress the DFSZ axion coupling to much lower values than are typically displayed in axion search result plots.
To summarize: • The n = 1 landscape statistics predict m h ∼ 125 GeV with superparticles beyond the reach of present LHC and WIMP DD experiments.
• LHC signals in SDLJMET channel should emerge slowly as LHC attains higher and higher integrated luminosity. A signal should likely be seen with 3 ab −1 at HL-LHC if not sooner. Signals in other channels such asgg,t 1t * 1 and SSdB may emerge at HL-LHC if we are lucky but otherwise may require an upgrade to HE-LHC.
• WIMP detection signals should emerge in SI DD experiments using multi-ton noble liquids. Signals in SD DD or IDD are much less likely to emerge in the near future.
[51] ATLAS collaboration, Search for supersymmetry in final states with missing transverse momentum and multiple b-jets in proton-proton collisions at √ s = 13 TeV with the ATLAS detector, ATLAS-CONF-2018-041.