1 Introduction
Abstract

The requirement that SUSY should solve the hierarchy problem without undue fine-tuning imposes severe constraints on the new supersymmetric states. With the MSSM spectrum and soft SUSY breaking originating from universal scalar and gaugino masses at the Grand Unification scale, we show that the low-fine-tuned regions fall into two classes that will require complementary collider and dark matter searches to explore in the near future. The first class has relatively light gluinos or squarks which should be found by the LHC in its first run. We identify the multijet plus signal as the optimal channel and determine the discovery potential in the first run. The second class has heavier gluinos and squarks but the LSP has a significant Higgsino component and should be seen by the next generation of direct dark matter detection experiments. The combined information from the 7 TeV LHC run and the next generation of direct detection experiments can test almost all of the CMSSM parameter space consistent with dark matter and EW constraints, corresponding to a fine-tuning not worse than 1:100. To cover the complete low-fine-tuned region by SUSY searches at the LHC will require running at the full 14 TeV CM energy; in addition it may be tested indirectly by Higgs searches covering the mass range below 120 GeV.

CERN-PH-TH/2010-005

CPHT-RR001.0111

LPSC-11026

OUTP-11-32P

Fine-tuning implications for complementary dark matter and

[2mm] LHC SUSY searches


S. Cassel, D. M. Ghilencea 444on leave from Theoretical Physics Department, IFIN-HH Bucharest MG-6, Romania, S. Kraml, A. Lessa, G. G. Ross 222e-mail addresses: s.cassel1@physics.ox.ac.uk, dumitru.ghilencea@cern.ch, sabine.kraml@lpsc.in2p3.fr,
lessa@nhn.ou.edu, g.ross1@physics.ox.ac.uk

[0pt]

Rudolf  Peierls  Centre for Theoretical Physics,  University  of  Oxford,

[0pt]1 Keble Road, Oxford OX1 3NP, United Kingdom.

[3pt]

Department of Physics, CERN - Theory Division, CH-1211 Geneva 23, Switzerland.

[3pt]

Centre de Physique Theorique, Ecole Polytechnique, CNRS, 91128 Palaiseau, France.

[1pt]

Laboratoire de Physique Subatomique et de Cosmologie, UJF Grenoble 1, CNRS/IN2P3, INPG, 53 Avenue des Martyrs, F-38026 Grenoble, France.

[3pt]

Dept. of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA.



1 Introduction

Weak scale supersymmetry (SUSY) has been proposed as a solution to the hierarchy problem, i.e. it ensures that the electroweak breaking scale is consistent with radiative corrections without undue fine-tuning. However, to achieve this, the new SUSY states must be relatively light. To quantify how light the SUSY states should be and and how much stress experimental limits already put on SUSY, one can apply a measure of fine-tuning. In [1] an analysis using SOFTSUSY [2] was made of the status of SUSY searches in the constrained minimal supersymmetric standard model (CMSSM) using the electroweak (EW) fine-tuning measure, , introduced in [3] computed to two-loop order. A scan of the CMSSM parameter space was performed, requiring acceptable radiative electroweak breaking, non-tachyonic SUSY particle masses (avoiding colour and charge breaking vacua), consistency with the experimental bounds on superpartner masses and with constraints from BR, BR and the muon as detailed in [1].

In Figure 1 the envelope of the shaded region shows the EW fine-tuning . One may see that, imposing all the constraints listed above except for the LEPII bound on the Higgs mass, there is a minimum of the EW fine-tuning, , for a Higgs mass of  GeV.111Note that the calculation of is subject to a theoretical uncertainty of about 2–3 GeV [4], see also [1]. Although the analysis presented here is concerned with the CMSSM, this class of model permits the presence of a scalar focus point, which favours small fine tuning of the electroweak scale [5] relative to more generic MSSM models. Thus if one excludes the low-fine-tuned regions of the CMSSM one can say that much larger ranges of the MSSM parameter space are also disfavoured. To date the only class of non-CMSSM models with MSSM spectrum that have lower fine-tuning are those with non-universal gaugino masses with a ‘natural’ relation between them that reduces the gluino mass relative to the CMSSM case [6, 7] .

In addition to EW fine-tuning, another important constraint is that the thermal relic abundance of the lightest supersymmetric particle (LSP), which contributes to dark matter, should be consistent with cosmological observations, under the assumption of R-parity conservation. Here we use MicrOMEGAs [8] as computational tool. Imposing the constraints of [9] limits the allowed region to be in the coloured regions of Figure 1. In regions 1 (red) and 5 (black points superposed on the green region) and resonant annihilation respectively are responsible for reducing the dark matter abundance within current bounds. Region 2 (purple) has significant bino-higgsino mixing in the LSP, and annihilation proceeds via higgsino t-channel exchange to EW gauge bosons. Finally, for regions 3 (green) and 4 (blue), the dominant processes are stau and stop co-annihilation, respectively. Overall, requiring that the SUSY dark matter relic density should be within present bounds raises the minimal fine-tuning to , still quite reasonable, corresponding to  GeV.

Figure 1: Two-loop fine-tuning versus Higgs mass for the scan over CMSSM parameters with no constraint on the Higgs mass. The solid line is the minimum fine-tuning with (0.1176, 173.1 GeV). The dark green, purple, crimson and black coloured regions have a dark matter density within  [9] (i.e. 3 saturation) while the lighter coloured versions of these regions lie below this bound. The colours and their associated numbers refer to different LSP structures as described in the text. Regions 1, 3, 4 and 5 have an LSP which is mostly bino-like. In region 2, the LSP has a significant higgsino component. Representative phase space points for regions 1,2…5, denoted SUG1, SUG2,…,SUG5, respectively, will be analysed in detail later on, together with the point of minimal EW denoted SUG0.

An immediate question is what is the best way to test the low-fine-tuned region of SUSY parameter space and will it be tested soon? In this the search for the Higgs boson plays a very important role because, c.f. Figure 1, for large Higgs masses, quantum corrections make the fine-tuning exponentially sensitive to the Higgs mass. Thus, if the Higgs is not found below 120 GeV, it will imply that the fine-tuning is uncomfortably large, . However, a LHC Higgs discovery at such low mass will be difficult and is likely to take several years. Given this, it is of interest to consider to what extent direct SUSY searches will probe the regions of low fine-tuning.

In this paper we consider both collider searches and dark matter searches. For this it is important to analyse the nature of the SUSY spectrum in the region of low fine-tuning () in light of the Higgs mass and dark matter constraints. Of course, if the LHC is to detect new SUSY states in its first run with of fb luminosity at a CM energy of 7 TeV, some states with coupling to the gluon, i.e. squarks or gluinos, must be light enough to have a sizeable cross section. In [10], the discovery reach of the LHC with 1 (2) fb luminosity at a CM energy of 7 TeV was determined as  GeV for , and  GeV for . The first results from CMS [11] for 35 pb of data exclude gluino masses below 500 GeV for  GeV, but no limit is obtained for  GeV.

(a) (b)
Figure 2: (a) Fine-tuning versus scalar mass parameter, (b) fine-tuning versus gluino mass; in both cases the constraint on the Higgs mass,  GeV is applied.

How does this compare to the expectation for the regions of low fine-tuning? From Figure 2(a) one sees that these regions (which we take as ) can either have light squarks (region 3, green points) or be close to the scalar “focus point” corresponding to heavy squarks.222The few points of region 4 that satisfiy the Higgs mass limit have very large fine-tuning, , and are not shown in Figures 24. Relaxing the Higgs mass constraint by 2-3 GeV has a negligible effect on the plots, except for region 3 where reduced fine tuning () becomes possible Figure 2(b) shows that the low fine-tuned points with heavy squarks (regions 1, 2 and 5) have two components. The first, region 1, has a small gaugino mass parameter and corresponds to gluinos with mass of about 400–500 GeV, potentially accessible to LHC discovery in the first run. The remaining regions (2 and 5) have gluino masses beyond the LHC reach in the 7 TeV run. However these regions may be accessible to dark matter searches. Such searches put limits on, e.g., the spin-independent scattering cross section for neutralino dark matter and this in turn is dominated by Higgs-boson exchange coupling to the higgsino and bino components in the neutralino. Typically the LSP has a large bino component but in restricted regions of parameter space it may also have a sizeable higgsino component. In Figure 3 we plot the higgsino component versus the fine-tuning measure. One can see that only the purple points, region 2, have a significant higgsino component.

(a) LSP component (b) LSP component
Figure 3: The higgsino components in the LSP, again requiring  GeV.

Once one knows the composition of the LSP it is straightforward to compute the spin independent cross section relevant to the direct dark matter searches. This is shown in Figure 4, plotted against the LSP mass. Here, the cross-section has been rescaled by , to take into account of the dark matter abundance at each of the points. Also shown is the current best bound coming from the CDMS experiment [13]. For more details see [14]. One sees that this already provides a significant test of region 2. A factor of 10 improvement in the dark matter sensitivity, which should be achieved by SuperCDMS in 2013, will probe almost the full range of region 2, the exception being points that do not saturate the dark matter density. For these latter points a two orders of magnitude improvement will be needed. The points in region 1, 3 and 5 have very small higgsino component and dark matter searches do not test this region. However, as may be seen from Figure 1, the bulk of this data is very fine-tuned with . The situation for is depicted in Figure 5. We see that the parameter space still needing to be explored has shrunk considerably: only a small part of regions 1 and 3 and an even smaller part of region 5 remains to be tested.

These results are also illustrated in Figure 6 in the plane, which shows the same points of low fine-tuning that pass the constraints mentioned. Notice that all these points are also consistent with the latest CMS observed exclusion area [11] (situated below the black curve), and all but a fraction of the region 3 points are consistent with the latest ATLAS exclusion limit [12] . We will discuss below the LHC configuration needed to scan the SUSY spectrum for these residual regions.

We conclude this Introduction with a side-remark: one often states that the very small area of points left in the moduli space , that respect all experimental constraints, renders supersymmetry an unlikely solution to the hierarchy problem. However, even if this area is reduced to few points due to further experimental constraints, recall that many of them have acceptable fine-tuning (in our case ). That is, the density and size of the area of points allowed in Figure 6 does not necessarily have a physical relevance, and cannot be used to conclude that only few points left would immediately invalidate supersymmetry as a solution to the hierarchy problem. It would rather indicate the most likely values of these moduli , that a fundamental theory beyond MSSM should fix dynamically, to avoid degenerate vacua.

(a) (b)
Figure 4: Scaled spin independent cross section for LSP-proton scattering, with  GeV. The scaling factor has been applied. The solid line is the CDMS-II limit. All points satisfy , with those with darker shading lying within of the WMAP bound, . The mSUGRA phase space scan was discrete only in the dimension with 30 slices in the range , and two further slices at .
(a) (b)
Figure 5: Same as Figure 4 but imposing in addition .
(a)  GeV (b)  GeV
Figure 6: Regions of low fine-tuning () in the versus plane, summed over and . All points satisfy the SUSY and Higgs mass limits, (dark points having ), the B-physics and constraints, and the CDMS-II bound on the dark matter detection cross section. The area below the black line shows the CMSSM exclusion (for and ) from the CMS dijet analysis [11], and that below the red line the ATLAS exclusion area [12]. The different lower bounds on of these plots are applied to show the impact of the 2-3 GeV theoretical uncertainty in the calculation of [1, 4].

2 Testing the low fine-tuned regions at the LHC

We turn now to a discussion of the LHC sensitivity to the low-fine-tuned SUSY regions of parameter space. The LHC searches are complementary to the dark matter searches, being sensitive to the points with a light gluino or squark, which correspond to a LSP with a spin independent cross section that is too small to be seen by the dark matter searches. Therefore it is of interest to consider the prospects for the LHC to probe the remaining regions of parameter space that will not be probed by the dark matter searches even though they may have heavy coloured states beyond the reach of the 7 TeV run. Accordingly, we consider five representative points, listed in Table 1, see also Figure 1, which we will study in detail: SUG0 (point of minimal fine-tuning ), SUG1 (of region 1, red), SUG2 (of region 2, purple), SUG3 (of region 3, green), SUG5 (of region 5, black). Unlike the SUG0 point, the points SUG1, SUG2,…, SUG5 have neutralino dark matter within of the observed dark matter abundance.

SUG0 SUG1 SUG2 SUG3 SUG5
1455 1508 2270 113 725
160 135 329 383 535
238 1492 30 -220 1138
22.5 22.5 35 15 50
191 433 187 529 581
482 414 900 898 1252
1469 1509 2331 826 1315
876 831 1423 602 1000
106 104 168 293 416
108 104 181 293 416
60 53 123 155 222
9 50 45 68 84
0.41 0.13 0.10 0.13 0.10
BR 3.4 3.7 3.4 3.2 3.2
BR 3.0 2.9 2.9 3.4 1.7
4.5 3.2 3.2 22.5 16.6
(pb) 108 5 432 24 101
TeV) (pb) 8 12 0.9 0.4 0.02
TeV) (pb) 40 75 3 5 0.4

Table 1: CMSSM parameters and sparticle masses in GeV for the points used in our LHC analysis. We also show for each of the points the amount of fine-tuning, the neutralino relic density, the branching ratios of and , the SUSY contribution to the muon anomalous magnetic moment , the spin-independent LSP scattering cross section off protons , and the total leading-order sparticle production cross-sections for the LHC at and 14 TeV.

The first point, SUG0, has a gluino mass of 482 GeV and a total cross-section of 8 (40) pb at (14) TeV. Although this point has a too large neutralino relic abundance, it possesses the smallest fine tuning found when imposing the non-dark-matter experimental constraints. We include it here for the purpose of comparison with the other representative points. The SUG0 point could also respect the dark matter constraint without changing the EW fine-tuning significantly, for example by adding a small amount of R-parity violation causing the LSP to decay [15], or if the true dark matter consists of axions/axinos [16, 17]. Indeed, as shown in [17] for an axino LSP the usual dark matter constraint can be relaxed. In this case the SUG0 point could also satisfy the relic abundance constraint, without changing its LHC phenomenology, due to the smallness of the axino coupling.

The second representative point (SUG1) corresponds to a dark red point in Figure 1 with moderate fine-tuning, . As may be seen from Figure 2(b), the dark red points all have low gluino mass; for the point chosen GeV and the total cross-section is 12 (75) pb at (14) TeV. The LSP is predominantly bino with a scattering cross section off nuclei that is too small to be probed by the next generation of direct dark matter searches.

The third representative point (SUG2) is chosen to lie in region 2, close to the CDMS bound. It has a heavy gluino,  GeV, and TeV-scale squarks, resulting in a total cross-section of 0.9 (3) pb at (14) TeV, mostly dominated by chargino-pair production. The LSP has significant bino and higgsino components and therefore a sizable .

The fourth representative point (SUG3) lies in region 3 and has the lowest fine-tuning, , in that region. It saturates the dark matter density and might be probed by direct dark matter searches if the sensitivities can be improved by more than an order of magnitude. It has a gluino mass of 898 GeV and an LSP with a mass of 155 GeV that is almost a pure bino. The total sparticle production cross-section at (14) TeV is 0.4 (5) pb.

The fifth and final representative point (SUG5) is in region 5 and also has the lowest fine-tuning, , in that region. It saturates the dark matter density and may be probed by direct dark matter searches in the near future. It has both gluinos and squarks at the TeV scale, with a sparticle production cross-section of only 0.02 (0.4) pb at (14) TeV. The LSP has a mass of 222 GeV and is almost a pure bino.

2.1 LHC at 7 TeV and 1 fb

In order to probe the discovery potential of the LHC at 7 TeV and with 1 fb of integrated luminosity we first consider the following set of cuts:

  • GeV, , GeV, GeV and

where is the transverse sphericity. Figures 7(a) and (b) show the and opposite sign/same flavor dilepton invariant mass () distributions for the five CMSSM points from Table 1 along with the SM background (BG). The BG was generated using AlpGen [18] and Pythia [19] and includes all the processes listed in [10]. The SUSY decay branching ratios were computed using the SUSYHIT [20] package and the signal events were generated using Pythia’s SLHA interface. For more details on the Monte Carlo simulation, see Ref. [10].

The signals from points SUG0 and SUG1 are dominated by gluino pair production with subsequent 3-body decays to quarks plus a neutralino or chargino, resulting in an distribution slightly harder than that of the BG, as seen in Figure 7(a). On the other hand, point SUG3 has a heavier gluino, but lighter squarks and its cross-section is dominated by squark-pair and gluino-squark production. In this case the lighter states decay mainly to , since is mostly a bino state. Therefore the SUG3 point presents a much harder distribution, peaking around 350 GeV. This is different for SUG2: despite having a larger total cross-section than point SUG3, the events from SUG2 are largely dominated by chargino/neutralino pair production, resulting in a much softer spectrum. Finally, the funnel region, represented by point SUG5, has too small cross-sections to be seen during the first run of the LHC.

(a) (b)
(c)

Figure 7: , and distributions calculated for the LHC at 7 TeV CM energy. In frames (a) and (b) the cuts imposed are . In frame (c) the cuts imposed are . The blue, red, purple, green and black curves correspond to the SUG points listed in Table 1. The SM background is shaded in grey.

We also show the () distributions for the same set of cuts. The ones from points SUG0 and SUG1 exhibit the characteristic edge at , while the BG is mainly featureless, since the cut vetoes most of the events. Although the distribution can in principle be used to extract the mass gap, the curves shown in Figure 7(b) are at the few fb level, what makes a measurement during the first LHC run improbable. We also point out that despite having a sizeable cross-section after cuts, the co-annihiliation point (SUG3) is poor in dilepton events, since it has a light stau ( GeV), which enhances decays (40% branching ratio) and suppress decays to ’s and ’s (7%).

Finally, Figure 7(c) shows the jet multiplicity distributions for the points SUG0–SUG5 and the BG. Here, a harder cut of  GeV is used, while the requirements for jets and leptons and the cut are the same as above. As one can see, at SUG0 and SUG1 the signal exceeds the BG for and , respectively, while at SUG2 and SUG3 this is the case only for .

To determine the best search strategy for our reference points, we next optimize over a grid of cuts including number of jets, , number of leptons, number of b-jets and s of first and second jets, following the same procedure as outlined in Ref. [10]. The discovery channel is defined as the set of cuts which satisfies and maximizes , where () is the number of signal (background) events. The ATLAS collaboration estimates [21] that the systematic uncertainty on the data-driven background determination can range from 20% to 50% for 1 fb. In order to incorporate these uncertainties in our discovery analysis, we take the conservative value of 50% for the total background systematical uncertainty and add it in quadrature to the statistical error (). The total uncertainty on the BG is then given by and it is used to compute the signal significance  [21].

(a) (b)
(c)

Figure 8: distributions for the points SUG0, SUG1 and SUG3 after the respective optimized cuts have been applied, with exception of the cut. The discovery channel (optimized set of cuts) for each point is shown on top of each plot. The SM background is shaded grey and the error bars correspond to the combined systematical (50%) and statistical errors, as described in the text.

In Figure 8 we show the distribution for the points SUG0, SUG1 and SUG3 in their respective discovery channels, without cutting on . As mentioned above, the lowest fine-tuning point (SUG0) and point SUG1 have heavy squarks and a light gluino. The latter decays to two quarks and a neutralino/chargino through 3-body decays, resulting in a signal rich in jets. As a consequence, the optimized cuts for both points corresponds to a soft cut ( GeV), with a high jet multiplicity (). However, for the SUG0 point the optimal channel is for , while the SUG1 point has a better ratio in the channel. Assuming 1 fb, this optimized set of cuts gives 130 and 138 events for the SUG0 signal and background, respectively. For the SUG1 point the number of signal and background events are 182 and 103. As seen from Figures 8(a) and (b), both points are above the BG for  GeV. However, both points are below the level if we assume 50% systematical uncertainties for the BG. If the BG uncertainties can be reduced below 30% (10%), the point SUG1 (SUG0) would be above the discovery threshold during the first LHC run. We also point out that we have only considered simple counting signals and once evidence for a signal has been seen, the distribution shapes can be used to improve the reach potential. Moreover, the analysis may be further optimized by means of reference priors [22]. We therefore conclude that points SUG0 and SUG1 will likely be visible during the first LHC run.

As seen from Figure 7(a), the point SUG3 has a much harder spectrum and a smaller production cross-section. The discovery channel in this case corresponds to a very hard cut in the channel. The signal is expected to have 32 events in this channel, while the SM expectation is 5 events. Furthermore, the SUG3 signal distribution has a very distinct shape, what can help to distinguish it from the background. We therefore conclude that the SUG3 point, which is representative for the co-annihilation region, should also be visible during the first LHC run.

However, even after applying our optimization procedure, the signals of points SUG2 and SUG5 are not visible with 7 TeV CM energy and 1 fb of data. We estimate that (20) fb would be necessary for a discovery of point SUG2 (SUG5) at 7 TeV.

As shown in Figures 7 and 8, the first LHC run at 7 TeV with 1 fb luminosity will clearly be able to find unambiguous evidence for non Standard Model physics scenarios with a light gluino or sub-TeV squarks, in agreement with the results of Refs. [10] and [23]. However, once a signal is seen, it will be important to distinguish between the different regions of SUSY parameter space and indeed to check whether it is a gluino and/or squarks that are initially produced. The accessible scenarios for the first LHC run, represented by the points SUG0, SUG1 and SUG3, have distinct properties that can provide an indication of which class of events is realized. Here we focus on three main distinguishing characteristics: the , and distributions.

From Figure 7(a) we see that the amplitude of the signal of each point is directly related to its respective gluino mass. Therefore the observed number of signal events could point to the gluino mass scale. Region 1 (red) has a light LSP in the 50–60 GeV mass range, see Fig. 5, in order to have a resonant annihilation. Consequently the gluino is also light, with a mass between 400 and 500 GeV (assuming ). On the other hand, the co-annihilation region (region 3) features heavier LSPs of 120–250 GeV mass and a small mass difference; this results in  GeV, as seen in Figure 2(b). Therefore, these two scenarios, represented by points SUG1 and SUG3, belong to disconnected regions in the CMSSM parameter space. Finally, the remaining low-fine-tuned region that does not satisfy the WMAP bound, represented by the SUG0 point, lies in the intermediate gluino mass range, with  GeV. If a signal is observed during the first LHC run, the number of observed events can indicate the gluino mass scale. Unless lies in the overlap region, which is disfavoured by dark matter considerations, it could point to the relevant scenario.

Another important discriminant between the co-annihilation and resonant annihilation regions is the jet multiplicity. Since the former has , in most cases the jets from gluino decays will be soft and escape detection. Therefore the signal will mostly consist of 2–4 jet events coming from squark cascade decays. For the red points (region 1), on the other hand, the light gluinos will go through 3-body decays and generate events rich in jets. As a consequence, region 1 will most likely be primarily observed in the multijet channel, while region 3 (green points) will be visible at lower jet multiplicities, as already indicated by the discovery channels discussed above. Figure 7(c) shows the jet multiplicities for GeV and GeV. Although the SUG3 point is not visible in this channel, it illustrates the behavior just described: the SUG3 signal peaks at low jet multiplicities () and points SUG1 and SUG0 show a peak at .

So far the and distributions seem to provide useful tools to distinguish between regions 1 and 3. However, both these distributions are similar for the SUG0 and SUG1 points and give little hope of distinction between these two scenarios. On the other hand, the dilepton invariant-mass distribution in Figure 7(b) shows an interesting distinction between points SUG0 and SUG1. While both points display the mass edge, only the events from SUG0 have a visible peak at the mass. Such a peak is characteristic of the low-fine-tuned region in Figure 1 that does not satisfy the WMAP bound, in which there are significant gluino decays to the heavier neutralinos . This is not the case for region 2 (red points), as here is systematically larger333For the decays of the gluino to , the fraction of points where the channel is kinematically accessible is: for the low fine-tuned region that does not satisfy the WMAP bound, for the light red points in Figure 1 that sub-saturate the relic density and for the dark red points that saturate the relic density., as seen in Table 1. However, as the total number of Z di-lepton events expected in the 7 TeV run is only about 3, one will have to wait for the second stage of LHC running to use this measure to distinguish between these scenarios. Nevertheless the distribution can still provide another important information about the underlying model. As discussed above, the excess of dilepton events at low invariant mass is characteristic of decays with . For the resonance annihilation (red region), the mass difference of the two lightest neutralinos has a rough Gaussian distribution of GeV ( of all points are within the range 49–61 GeV). Therefore, if the neutralino mass difference is greater than this, but the observed signal still is consistent with a light gluino ( GeV), then CMSSM neutralino dark matter is not likely. Finally, the observation of a signal rich in dijets (and taus) plus but poor in dilepton events would point to the SUG3 scenario.

2.2 LHC at 14 TeV

As shown in the previous section, the first LHC run will be able to test a considerable portion of the low fine-tuned CMSSM, the exceptions being the resonant annihilation (SUG5) and the low , high (SUG2) regions. While the latter will be accessible to the next generation of dark matter direct detection experiments, it is still desirable to have a corroboratory signal at the LHC. Therefore we now address whether the LHC operating at its design CM energy of  TeV would be able to probe low-fine-tuned models in regions 2 and 5.

(a) (b)
(c)

Figure 9: , and distributions calculated for the LHC at  TeV. The cuts imposed are . The black and purple curves correspond to the SUG5 and SUG2 points, respectively. The SM BG is shaded in grey.

To this aim, Figure 9 shows the distributions of , number of jets and number of -jets for points SUG2 and SUG5 along with the respective SM BG distributions. The following set of cuts has been applied:

  • GeV, , GeV, GeV and

The SUG2 events that pass the cuts come mostly from gluino-pair production. Since the is much lighter than the first and second generation squarks, the gluino decays of the time to third generation quarks. As a result, there is a large -jet multiplicity in the SUG2 signal, as shown in Figure 9(c). This point would hence be easily visible above BG in the channels. The SUG5 point has a heavier gluino ( TeV) and lighter 1st/2nd generation squarks, so the signal after cuts is dominated by gluino-squark production and the distribution is softer than in the SUG2 scenario. However, due to the large branching ratio for decays, the SUG5 point has a hard spectrum, similar (in shape) to the SUG3 point. Thus the SUG5 signal could be observed in the multijets channel with a hard cut, as seen in Figure 9(b). We estimate that, for TeV, a discovery for both points would require an integrated luminosity of .

3 Conclusions

In summary, using the fine-tuning measure, we have made a detailed study of the possibility of testing in the near future the CMSSM as a solution to the hierarchy problem. Broadly, the regions of low fine-tuning split into two characteristic classes. The first class has light gluinos or light squarks and will likely be tested in the 7 TeV run at the LHC. The second class has a heavy gluino but the LSP has a significant higgsino component; this class is testable by direct dark matter searches in the near future. Together, these complementary experiments will be able to cover almost all of the parameter space with fine-tuning . To cover all of this parameter space by SUSY searches at the LHC will require running at the full 14 TeV CM energy. In addition, the low-fine-tuned regions can be tested indirectly by Higgs searches covering the mass range  GeV.

4 Acknowledgements

The research presented here was partially supported by the EU ITN grant UNILHC 237920 (“Unification in the LHC era”) and by the French ANR project ToolsDMColl, BLAN07-2-194882. SC is supported by the UK Science and Technology Facilities Council under contract PPA/S/S/2006/04503. The work of DG is supported in part by CNRS research contract 225933 at Ecole Polytechnique and by the ERC advanced grant 226371 (“Mass TeV”). AL is partially supported by the Fulbright Program and CAPES.

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