1 Introduction

CERN-PH-TH/2008-159

UMN–TH–2708/08

FTPI–MINN–08/28

IPPP/08/53

DCPT/08/106

Sneutrino NLSP Scenarios in the NUHM with Gravitino Dark Matter

John Ellis, Keith A. Olive and Yudi Santoso

TH Division, CERN, Geneva, Switzerland

William I. Fine Theoretical Physics Institute,

University of Minnesota, Minneapolis, MN 55455, USA

Institute for Particle Physics Phenomenology,

Durham University, Durham DH1 3LE, UK

Abstract

We analyze scenarios in which some flavour of sneutrino is the next-to-lightest supersymmetric particle (NLSP), assuming that the gravitino is the lightest supersymmetric particle (LSP) and provides the cold dark matter. Such scenarios do not arise in the constrained supersymmetric extension of the Standard Model (CMSSM) with universal gaugino and scalar masses input at the GUT scale. However, models with non-universal Higgs masses (NUHM) do allow scenarios with a sneutrino NLSP, which are quite generic. We illustrate how such scenarios may arise, analyze the possible metastable sneutrino lifetime, and explore the theoretical, phenomenological, experimental and cosmological constraints on such scenarios. We also discuss the collider signatures of such scenarios, how they may be distinguished from neutralino LSP scenarios, and how different flavours of sneutrino NLSP may be distinguished.

CERN-PH-TH/2008-159

July 2008

1 Introduction

In the framework of supersymmetry with conserved parity, the lightest supersymmetric particle (LSP) can have neither electromagnetic nor strong interactions: otherwise it would have bound to conventional matter and been detected in searches for anomalous heavy nuclei [1]. Within the minimal supersymmetric extension of the Standard Model (MSSM), weakly-interacting candidates for the LSP are the lightest sneutrino , the lightest neutralino , and the gravitino . The (left-‘handed’) sneutrino LSP hypothesis is excluded by a combination of neutrino counting at LEP and direct dark matter searches [2]. Accordingly, general attention is focused on the neutralino (NDM) [3] and gravitino dark matter (GDM) [4, 5] possibilities, and in this paper we assume the latter.

The next question is the possible nature of the next-to-lightest supersymmetric particle (NLSP) in a GDM model. Two natural possibilities are the other candidates for the LSP, namely the sneutrino and the neutralino, but the NLSP could equally well be charged and even coloured. Indeed, the lighter stau slepton is a natural candidate for the NLSP [6] within the constrained MSSM (CMSSM) with gravity-mediated supersymmetry breaking, in which the soft supersymmetry-breaking scalar masses , trilinear parameters and gaugino masses are each assumed to be universal at a GUT input scale [7, 8]. The lighter stau is also a natural possibility within minimal supergravity (mSUGRA), in which the gravitino mass is fixed: , and there is an additional relation between trilinear and bilinear soft supersymmetry-breaking parameters [9]. Another possibility for the NLSP within a scenario with non-universal Higgs masses (NUHM) [10, 11, 12, 13, 14] is the lighter stop [15].

In this paper we study the other possibility for the NLSP within the NUHM with gravity-mediated supersymmetry breaking, namely the lightest sneutrino, assuming that the gravitino provides the cold dark matter 111The possibility of a sneutrino NLSP has also been studied within gaugino-mediated models of supersymmetry breaking [16].. Like other NLSP candidates in gravity-mediated scenarios, the sneutrino NLSP within the NUHM is expected to be very long-lived. The dominant decays of the other NUHM NLSP candidates produce particles with copious interactions such as charged particles and photons, which are subject to strong cosmological limits [17]. These limits are strong enough to exclude effectively all of the parameter space where the lightest neutralino is the NLSP [18] 222If the gravitino mass is much lighter than the neutralino mass, these limits might still be satisfied.. However, the dominant decay mode of the sneutrino is , and the cosmological limits on neutrino injection are much weaker than those on the injection of photons and charged particles [19, 20]. Therefore the cosmological limits on NUHM NLSP scenarios are relatively weak, leaving considerable scope for a sneutrino NLSP. On the other hand, the sneutrino must appear at the end of the decay chain of every MSSM sparticle produced at a collider, and the particles produced in supersymmetric decay cascades provide distinctive experimental signatures for a sneutrino NLSP [21]. In particular, the charged leptons produced in association with a NLSP provide tools for diagnosing its flavour.

The structure of this paper is as follows. In Section 2 we discuss sneutrino properties within the NUHM, including its mass and lifetime. In Section 3 we discuss the relic abundance of sneutrinos after freeze-out from a primordial plasma in thermal equilibrium. In Section 4 we analyze the NUHM parameter space and identify regions where the NLSP may be either the or the . In Section 5 we discuss the cosmological constraints on NLSP scenarios, and show that they are not severe. In Section 6 we discuss some signatures of metastable sneutrinos in different NUHM scenarios, in particular those with different lepton flavours accompanying the NLSP. Our conclusions are summarized in Section 7. Calculations of the three-body decay are described in an Appendix.

2 Sneutrino NLSP Properties

We assume that the GUT scale is the effective input scale at which the soft masses are specified, presumably via some gravity-mediated mechanism, and make the NUHM assumptions that the gaugino masses are universal, as are the squark and slepton masses, whereas the soft supersymmetry-breaking contributions to the Higgs scalar masses are non-universal. We then calculate the physical supersymmetric mass parameters at a low energy scale from the running given by the renormalization-group equations (RGEs). We assume that the right-handed neutrino supermultiplets, being singlets, get very large Majorana masses, and therefore decouple from the low-energy effective theory 333However, if the decoupling energy scale is significantly below the GUT scale, the low-energy spectrum may be affected [22] through the RGEs. This effect is neglected here.. The sneutrino NLSP discussed in this paper is essentially the scalar partner of some left-handed neutrino. The flavour of the NLSP is, however, model-dependent, as we discuss below.

2.1 Sneutrino Mass

In order to calculate the sneutrino mass, we first look at the RGEs of the slepton sector 444Although we write the one-loop RGEs for simplicity, our calculations include two-loop contributions. [23, 24, 25]:

 dm2˜LLdt = dm2˜eRdt = dm2˜L3Ldt = dm2˜τRdt = 18π2(−4g21M21+2h2τ(m2˜L3L+m2˜τR+m21+A2τ)+4S), (1)

where

 S ≡ g214(m22−m21+2(m2˜QL−m2˜LL−2m2˜uR+m2˜dR+m2˜eR) (2) +(m2˜Q3L−m2˜L3L−2m2˜tR+m2˜bR+m2˜τR)).

The term vanishes and does not contribute in models with universal soft masses such as the CMSSM. However, for non-universal models, can be far from zero and its contribution to the RGEs can be significant. When , and assuming universal soft breaking masses for the and sleptons at the GUT scale, the slepton is lighter than the slepton at the weak scale. However, since contributes in opposite ways for and sleptons, if is large and negative, could be lighter than . Furthermore, there are additional -terms,

 m2~eL = m2~νL = m2˜LL+cos(2β)12m2Z, (3)

that split the sneutrino and charged-slepton masses. Since for , the sneutrino is lighter than its charged-slepton partner.

Comparing the first two generations and the third generation, we see that the tau sneutrino could be lighter than the electron and muon sneutrinos because of the Yukawa terms in the RGEs. However, this is not always the case, due to the fact that could be negative and large, and we display examples later where the NLSP has electron or muon flavour. The lighter stau mass is also suppressed by off-diagonal terms in the mass matrix. Thus, depending on the model parameters, either the tau sneutrino or the lighter stau might be lighter.

Therefore, a sneutrino could be the NLSP if is large and negative 555One could also obtain a light sneutrino within a supersymmetric SU(5) GUT with different soft masses for the and multiplets [20]. Another alternative is within a gaugino-mediated supersymmetry breaking model, in which the Higgs masses are again different from the other sfermion masses [16].. We see from (2) that is negative when  666Assuming that these are the dominant terms in , which is the case for the NUHM that we consider here., which is not possible in the CMSSM, for which by assumption. We now study how this may occur in the NUHM model, using the freedom that the Higgs soft supersymmetry-breaking masses at the GUT scale are not necessarily equal to , the universal scalar mass for sleptons and squarks.

The electroweak symmetry breaking conditions may be written in the form:

 m2A(Q)=m21(Q)+m22(Q)+2μ2(Q)+ΔA(Q) (4)

and

 μ2=m21−m22tan2β+12m2Z(1−tan2β)+Δ(1)μtan2β−1+Δ(2)μ , (5)

where and are loop corrections [23, 24, 26] and  777Our convention is such that , and .. The values of the NUHM parameters at are related to their values at through the known radiative corrections [23, 27, 25] and :

 m21(Q) = m22(Q) = μ2(Q) = μ2+cμ. (6)

Solving for and , one has

 m21(1+tan2β) = (7) −ΔA(Q)tan2β−12m2Z(1−tan2β)−Δ(1)μ

and

 m22(1+tan2β) = (8) −ΔA(Q)+12m2Z(1−tan2β)+Δ(1)μ .

The correction is positive and generally of . From here we can see that there are two possible ways to get negative via negative : the first is by using very large , and the second is by using very large . If is relatively small while is very large, the Higgs masses-squared may be negative at the GUT scale, which could lead to a vacuum stability problem [28].

A weak-scale scalar mass-squared with generally produces a vev of order the weak scale that disappears as the RGEs are run down to the weak scale. Such negative masses-squared are not dangerous. It may happen, however, that an instability occurs along some and flat direction. In this case, a negative mass-squared may be large and still present at a renormalization scale, [29]. Models in which the Universe becomes trapped in such non-Standard Model vacua are clearly excluded 888Whether this occurs or not depends on the specific cosmological history during inflation [30, 31].. This possibility has been studied in the NUHM along the and flat directions of the MSSM [31]. We delineate below regions in the parameter plane where these vacua may be problematic.

In the GDM scenario used here, the sneutrino NLSP would eventually decay into the gravitino, and the dominant decay channel is the two-body decay

 ˜ν→˜G+ν , (9)

with the decay rate

 Γ2b=148πm5~νM2Plm2˜G⎛⎝1−m2˜Gm2~ν⎞⎠4, (10)

where is the gravitino mass and is the Planck mass:  GeV.

We plot in Fig. 1 the sneutrino lifetime, , as a function of the gravitino mass for , and 1000 GeV respectively. Note that we plot the lifetime only for  GeV. Clearly, a smaller mass gap would yield an even longer lifetime. We see that the sneutrino lifetime could be less than 1 second only when is large, or the gravitino mass is (much) less than 1 GeV. On the other hand, if the mass gap is small, the sneutrino lifetime can be very long, potentially even longer than the age of the Universe, which is  s. However, there are cosmological and astrophysical constraints on the possibility of a sneutrino with lifetime longer than the age of the Universe at recombination that we discuss in more detail later.

3 Cosmological Sneutrino Density

Assuming thermal equilibrium in the early Universe, one can calculate the sneutrino relic density after decoupling but before its decay into the gravitino. This is done by the usual use of the Boltzmann equation and calculation of the sneutrino annihilation and coannihilation cross sections. The calculations are identical to those required to calculate the relic sneutrino density if it is the LSP.

The possible sneutrino-pair annihilation two-body final states are the following [12]:

Initial State Final States

If the soft masses for the sfermions are universal as assumed here, the electron sneutrino is always degenerate with the muon sneutrino, and the tau-sneutrino mass might be nearby. In the NUHM case that we consider here, there could also be other sparticles that are almost degenerate with the sneutrinos, such as the lightest neutralino and chargino, and charged sleptons. We list below the corresponding coannihilation processes and their possible final states:

• Coannihilation with other sneutrino flavours:

Initial State Final States
• Coannihilation with charged sleptons:

Initial State Final States

In the first line above, the coannihilation is between a sneutrino and a charged slepton of the same generation, whereas in the second and third lines they are not necessarily from the same generation.

• Coannihilation with the lightest neutralino:

 Initial State Final States χ~ν νZ,νh,νH,νA,ℓ−W+,ℓ−H+

and similarly for .

• Coannihilation with the lighter chargino:

Initial State Final States

and similarly for .

In our scenario, the sneutrino NLSP eventually decays into the gravitino before the current epoch. Consequently, the gravitino relic density is related to the sneutrino density before its decay by

 Ω~Gh2=m˜Gm~νΩ~νh2+ΩT~Gh2, (11)

where is the contribution to the gravitino density from thermal production after reheating, which is sensitive to the unknown reheating temperature . We do not discuss this contribution here. The only constraint we impose is that the contribution to the gravitino relic density arising from sneutrino decay does not exceed the value suggested by WMAP [32] and other observations:

 ΩDMh2=0.1099±0.0062. (12)

Hence, we require that the first term on the right-hand side of (11) should not exceed (the 2- upper limit). Because of the scaling by the mass ratio , even a large sneutrino density after decoupling could still be compatible with the dark matter constraint if .

In this case, we must check whether gravitinos are non-relativistic at the time structure formation begins, roughly at  s, in which case they act in the same way as conventional cold dark matter. If , and scales subsequently as , where is the sneutrino lifetime. We can use Fig. 1 to estimate whether or not gravitinos will behave as cold dark matter. For example, at the left-most point of the lowest curve, gravitinos are produced relativistically with , but the decay occurs so early that they become non-relativistic well before structure formation begins. The same is also true for the two middle curves in Fig. 1. Only for the left part of the topmost curve (when GeV) is there a potential problem. However, in this case the sneutrino relic density is generally already small in the model considered here.

4 NUHM Parameter Space

In the CMSSM, the values of and are determined by the electroweak vacuum conditions for any given input values of and . However, the constraints on and are relaxed in the NUHM, with the values of these parameters being related to the degrees of non-universality assumed for the Higgs soft masses and . A general discussion of the parameter space of the NUHM was given in [11, 12, 13, 14], which we use here as a starting point for our discussion. Regions of the NUHM parameter space in which a sneutrino is the lightest spartner of any Standard Model particle were identified in [12], see for example the dark blue shaded regions in Figs. 2, 3, 4, 6, 8 and 9 of that paper. There, it was assumed that the LSP is the lightest neutralino , with the gravitino assumed to be heavy, so that these light-sneutrino regions were disallowed. However, in this paper we assume that the gravitino is the LSP, so the viability of these light-sneutrino regions must be re-evaluated. We focus our discussion here on planes of the types shown in Figs. 4 and 6 of [12], where the light-sneutrino region moves to lower as increases.

In general, keeping some sneutrino species light favours small values of and . However, there is an important lower limit on , in particular, due to the LEP lower bound on the mass of the lightest MSSM Higgs boson. A sneutrino NLSP region may be found by choosing a moderate value of  GeV while keeping relatively small, e.g.,  GeV. The resulting masses of the sparticles are shown in Fig. 2 assuming and , for various values of and 2000 GeV, in panels (a), (b), (c), and (d), respectively 999We use  GeV for our analysis [33]..

As noted earlier, in regions of the NUHM parameter plane (particularly when and are large), the masses-squared of the Higgs and left-sleptons have a tendency to run down to negative values at the GUT scale. This allows for the possibility that large scale vevs be excited along the or flat directions. One expects that these flat directions are lifted by some effective operator at or above the GUT scale. The vev along the flat direction is sensitive to the fundamental scale associated with this operator and clearly grows as that scale is increased above the GUT scale. The reliability of this high-scale vacuum depends also on the one-loop corrections to the scalar potential. This sensitivity can be characterized by the ratio of the tree-level vev to the renormalization scale, , at which the vev disappears (i.e., the masses-squared go positive). Here we adopt the most conservative set of assumptions, namely that the flat directions are lifted at the GUT scale and that the vev must be of order ( in the notation of [31]). This preserves the largest volume of the NUHM parameter space. Of course the GUT constraint itself is cosmology-dependent, and may not be important if the Universe starts out in the weak scale vacuum after inflation. For more details on this constraint see [31].

In the case of small  GeV, shown in panel (a) of Fig. 2, we see that the GUT stability constraint (represented by a couple of vertical black dotted lines) allows only small  TeV, far from the sneutrino NLSP region which appears when  GeV. We also see that the constraint (solid green line) allows only  GeV and the Higgs mass constraint (dashed red) allows only  GeV for this small value of . Note that a Higgs mass of 114.4 GeV is found around GeV (dot-dashed vertical line) for this value of , but current theoretical and experimental uncertainties only provide for the weaker bound shown by the dashed line. The anomalous magnetic moment of the muon, , is reconciled with experiment at the 95% CL for GeV, as shown by the light blue long-dashed line 101010We assume that the deviation of from the standard model is between 10.7 to , the 2 range according to [35].. Therefore, we do not have an allowed region in panel (a), assuming the GUT constraint holds. For larger , these constraints become more relaxed, and an allowed sneutrino NLSP region emerges.

For  GeV, shown in panel (b) of Fig. 2, the GUT stability constraint allows  TeV, the constraint allows , and the Higgs constraint is essentially unimportant, as a Higgs mass greater than 114.4 GeV occurs at  GeV. The constraint is satisfied in two regions: GeV and GeV. While the GUT constraint is relaxed, the sneutrino LSP region still requires  TeV , where we have degenerate NLSPs. We note that around  TeV several other sparticles are only slightly heavier than the , including the lightest neutralino , the and , the lighter and the . Thus, all these sparticles must be included in coannihilation calculations of the abundance. For larger , only and masses stay close to the NLSP mass, while the others get larger mass gaps.

When is increased to 1500 GeV, as shown in panel (c) of Fig. 2, the GUT constraint remains at  TeV, very close to the region when the sneutrino is the NLSP, which extends from  TeV to  TeV. The lightest sparticles are again the , with the and again slightly heavier. In this case, a theoretical upper limit on arises when the become tachyonic 111111Here and in panel (d), we truncate all the other sparticle lines at this boundary of the tachyonic region. Slightly more stringent upper limits on come from the lower limits on provided by LEP [36, 37].. In this case, the Higgs constraint requires only that GeV, and is satisfied when GeV or GeV. The constraint from is unimportant at this value of .

Finally, in panel (d) of Fig. 2 we display the sparticle masses for  GeV. In this case, the allowed sneutrino NLSP is the , for 200 GeV  TeV. The becomes the NLSP for smaller in the Higgsino region, and upper limits are provided by the LEP lower limits discussed above. For this value of , the differences in mass between the and the heavier sparticles are relatively large. Neither the Higgs mass nor provide a constraint, while requires GeV or GeV with the later has less than the LEP limit.

In these plots, we find that sneutrino NLSP has relic density of order which is well below the WMAP limit. This means that most of the gravitino dark matter must be produced by some other sources, e.g., by reheating. We take coannihilation effects into account for the relic density calculation. However, in contrast with the neutralino LSP case, coannihilations do not always reduce the final relic density. Sneutrino coannihilation with the lightest neutralino would indeed generally increase the relic density, while that with charged sleptons might reduce it. In the former (latter) case, the effective sneutrino cross section is averaged with the weaker (stronger) annihilation cross section of neutralinos (charged sleptons). The relatively small relic density of the sneutrino compared to that of the neutralino can be attributed generically to the fact that the sneutrino is a scalar particle, rather than a Majorana fermion. In Fig. 2(d), for example, since the mass gaps with other sparticles are relatively large, the coannihilation effects are not maximal, but the relic density is still small.

To get a more comprehensive view of the NUHM parameter space, we display in Fig. 3 some contour plots in selected planes. In panel (a), we choose ,  GeV,  GeV and . This panel therefore includes and extends the specific examples shown in Fig. 2. We plot the regions where the lighter stau, the right selectron, some sneutrino or the lightest neutralino is the NLSP. At large , the electron-sneutrino is the NSLP and is shown by the regions shaded dark blue. At large and smaller , the NLSP becomes the tau-sneutrino (shaded light blue). Above these regions, the white area corresponds to an unphysical region where one or more of the sparticles has a negative mass-squared at the weak scale. Below these regions, in most of the area, it is the lightest neutralino which is the NLSP. At lower and relatively small , we see regions where the lighter stau (shaded brick red), or the right selectron (shaded orange) is the NLSP. At even smaller the NLSP is a higgsino-like neutralino. The narrow turquoise shaded region is that in which is within two of the WMAP value. (Recall that, with the gravitino as the LSP, this is not the dark matter relic density.) Regions surrounded by the strip (which have higher ) might also be permitted if , and regions not surrounded by the strip (which have lower ) would certainly be permitted by the dark matter constraint. As one can see these regions track very closely the degeneracy lines between the neutralino and one of the four sparticles where the relic density is controlled by coannihilations or the funnel region where (The contour is shown by the thin blue line.).

The Higgs mass contour of 114.4 GeV (red dot-dashed line) excludes  GeV. However, if one uses a likelihood analysis for the Higgs mass and allows for theoretical uncertainties in the calculation of , this constraint is relaxed and most of the displayed region is allowed, as shown by red dashed line. The constraint (shaded green) excludes small and prefers positive . However, this constraint is unimportant in this panel at large . The GUT constraint is represented by a black dotted line: it excludes large and essentially all of the electron-sneutrino NLSP region for this set of parameters. Finally, the light pink shaded region bordered by a black solid line represents the region favored by . The vertical dashed black lines correspond to the chargino mass contours of 104 GeV and exclude very small values of .

In panel (b), we display a case with  GeV, with the other parameters chosen to be the same as in (a). We see that the stau NLSP region becomes bigger and there is no longer a right-selectron NLSP region. In the white region interior to the stau NLSP region, the stau has gone tachyonic at the weak scale, which is problematic. We also see that the constraint becomes stronger, especially for negative . However, the qualitative features of the sneutrino NLSP band at large and/or are similar. This feature is also retained in panel (c), where the larger value  GeV is chosen, and also in panel (d), in which a larger value is chosen. In panel (c) (which now extends to higher values of ), there is no longer a charged NLSP. In panel (d), we see again a region with a right selectron NLSP. The GUT constraint in this case constrains only the lower right corner of the plane shown, and allows part of the electron-sneutrino region. The constraint (orange dashed line) excludes a region with small [38].

We conclude that the possibility of a sneutrino NLSP is quite generic in the NUHM, and certainly not much less plausible than the lighter stau. This is in contrast to the CMSSM, where a stau NLSP is a generic feature at large and small , but there is no possibility of a sneutrino NLSP.

5 Cosmological Constraints on a Sneutrino NLSP

The cosmological impact of a long-lived sneutrino depends on its lifetime 121212See [19] and references therein.. If the sneutrino decays during or after Big-Bang Nucleosynthesis (BBN), it could alter predictions for the light-element abundances. If the sneutrino decays around or after the time of recombination, it could distort the blackbody spectrum of the CMB. If the sneutrino decays at a very late time, its effect might be seen on the diffuse neutrino and photon spectra. The production of relativistic neutrinos by sneutrino decays could also change the equation of state and therefore the evolution history of the Universe [39].

Although the sneutrino is neutral, and its dominant two-body decay channel produces only a neutrino and the gravitino, which are also neutral, there could still be a significant effect on BBN if the sneutrino decays during or round after the time of BBN [19, 20, 40, 41]. If the mass gap is sufficiently large, the decay of the sneutrino produces high-energy, non-thermal neutrinos. Through scattering processes with the background particles, such as , and , the energetic neutrinos transfer some parts of their energies to charged particles. The final-state particles may then photodissociate or hadrodissociate the elements already produced by standard BBN processes. In the case of the charged pion, it can alter the neutron-to-proton ratio if it occurs at the beginning of BBN. There can also be energy transfer through elastic scattering with electrons and positrons: , and the high-energy might then initiate electromagnetic showers. However, at the epoch of interest (when their energies are  MeV) the electron and positron number densities are already low. Therefore these processes can be neglected.

Subdominant three- and four-body sneutrino decay channels can also be important, even though their branching ratios are relatively small. This is because these decays produce charged and/or strongly-interacting particles directly. These effects had been studied in [19], where it was found that the effects of the three- and four-body decays are negligible if their collective branching ratio is less than about . To estimate this branching ratio, we calculate the decay rate for the following process

 ˜ν→˜G+ν+γ, (13)

which occurs through neutralinos exchange, with the photon produced via the photino content of the neutralinos. This provides an estimate of the total multi-body decay rate that should be accurate to within an order of magnitude. The detailed calculation can be found in the Appendix.

To gauge the possible impact of the BBN constraint, we examine the tau sneutrino NLSP region in Fig. 2(d), where the sneutrino mass varies from the LEP lower limit of about 40 GeV up to about 100 GeV. We first consider the case  GeV,  GeV, , and  GeV shown in the top two panels of Fig. 4. Panel (a) shows the three-body-decay branching ratio for various values of  GeV, corresponding to lifetimes  s. We see that the branching ratio is always very small, falling below throughout the range of parameter space considered. This is consistent with the results of [20] which also finds a small hadronic fraction when the sneutrino mass is GeV. Thus, according to the analysis of [19], the three-body decay is too small to affect significantly the successful results of BBN.

Although the hadronic branching ratio is expected to be small, BBN nevertheless sets a limit on the density of sneutrinos at the time of decay. For a 100 GeV sneutrino, all lifetimes are safe so long as the quantity

 Y~νM~ν=Ω~νh2×(3.65×10−9GeV) (14)

is less than GeV for and less than for where is the ratio of the number density of sneutrinos to entropy, . In panel (b) of Fig. 4, we display the sneutrino relic density following freeze-out but prior to decay as . We see that is always below about GeV, with a large dip at  GeV due to the resonance in sneutrino-pair annihilation (with a smaller dip at  GeV due to the resonance). Thus, the sneutrino density is far below the range where BBN constraints become important for the range of the three-body branching ratio shown in panel (a) of Fig. 4.

The lower panels of Fig. 4 display the three-body branching ratio and for another case:  GeV,  GeV, , and  GeV. We see in panel (c) that the three-body branching ratio is smaller than for  GeV, and always . Panel (d) shows that is, again, always below about GeV. In this case, the prominent dip due to the light resonance in sneutrino-pair annihilation, and the direct-channel resonance is less important. This difference from the previous case is due to the larger value of .

These examples are indicative that the sneutrino LSP regions in the NUHM parameter space are generally safe from BBN constraints. We next check other possible constraints on decaying sneutrinos.

When the high-energy decay neutrinos are thermalized, their energy is transferred and converted to radiation. If the sneutrinos decay after about (corresponding to a lifetime of s), then the photons produced might not have a chance to thermalize, and could show up as distortion of the CMB black-body radiation spectrum. These constraints were also considered in [19] where it was found that for lifetimes between and s, the upper limit on is roughly () GeV for . Thus in the parameter space we are interested in, this too is never a serious constraint.

When the sneutrino and gravitino mass are nearly degenerate, the sneutrino lifetime might be very long ( s as seen in Fig. 1). If the sneutrinos have decayed after the time of recombination, they will produce a diffuse neutrino and photon background. In principle, there is then a very strong constraint from water Cerenkov detectors placing an upper limit on of order GeV [40]. However, these detectors lose sensitivity for neutrino energies below about 10 GeV [42]. Thus we again do not expect a severe constraint placed on the parameter space of interest.

6 Signatures of Metastable Sneutrinos at Colliders

We have seen in the previous sections that a sneutrino NLSP is a generic possibility in the NUHM. It would be metastable, so that its decays would not be seen at colliders, but the late decays of relic sneutrinos are not excluded by the available cosmological constraints. The mass of such a sneutrino NLSP might be as low as the LEP lower limit [36, 37]. As a non-decaying neutral particle, the sneutrino would have a missing-energy signature at colliders. Distinguishing the sneutrino from other possible origins of such events would require a search for the heavier states that decay into the sneutrino inside the detector.

Covi and Kraml [21] have studied several scenarios with a sneutrino NLSP assuming the following mass hierarchies. (a) : in this case, neutralino decays into a neutrino and sneutrino are invisible, and the signatures of such decay chains resemble those in a conventional neutralino LSP scenario. However, if , the neutralino can decay into , where the pair is soft if the mass gap is small. (b) : in this case, besides the invisible decay mode, the neutralino can undergo cascade decays that might be detectable, such as . (c) : in this case, there are additional decay channels with neutralino decay into an electron and a selectron which subsequently decays into leptons and a tau-sneutrino. Heavier sparticles might decay via the lightest neutralino, but they might also decay directly into the , e.g., via , or via sleptons, e.g., .

We see from Fig. 2 that there are several possible scenarios for the sparticle mass spectrum in the NUHM, which are distinct from the standard CMSSM spectrum as we now enumerate.

1. :

This is the mass hierarchy seen in panel (d) of Fig. 2 for larger . The neutralino can decay into

 χ → (15) ~ντ+ντ

which, for the first mode, would be followed by

 ~eL → (16) ~ντ+νe+τ,

the second mode by

 ~νe → (17) ~ντ+e+τ,

and the third mode by

 ~τ1→~ντ+¯f′+f (18)

In the case of the two-body neutralino decay to stau and tau, the decay rate is

 Γ(χ→~τ1+τ) = , (19)

where , are the left and right couplings in the neutralino-tau-stau vertex. There are similar expressions are for the other two-body decay modes.

2. :
This hierarchy occurs for more intermediate values of when is large as seen in panels (b) and (c) of Fig. 2 131313The viability of such models would require some action to conform with the GUT constraint, e.g., by constraining inflationary cosmology.. The neutralino 2-body decay modes would be the same as in the previous case, although with different branching ratios. However, the cascade decays are in general different. In this case, we would have

 ~ντ → (20) ~ντ+e+τ
 ~τ → (21) ~νe+e+ντ

and

 ~eL→~νe+¯f′+f. (22)
3. For large , e.g. as shown in panel d of Fig. 3, and large , the third-generation sleptons get larger masses through the Yukawa couplings. Thus we have for the lightest sparticles. In this case, the neutralino cascade decays become simpler,

 χ → (23) ~νe+νe

which, for the first mode, would be followed by

 ~eL→~νe+¯f′+f, (24)

whilst the second mode is invisible.

4. There are also other possibilities for narrower region of parameter space, near where the masses cross each other in Fig. 2: (a) ; (b) ; and (c) .

We extract from these examples a few generic features. As in the cases of many other scenarios beyond the Standard Model, particularly within the general framework of supersymmetry, the most prominent signature of a sneutrino NLSP scenario is likely to be missing energy. However, there would in general be accompanying signatures that would enable a sneutrino NLSP scenario to be distinguished from other possibilities. Specifically, one expects to see also events with missing energy accompanied by leptons. The precise nature of this supplementary signature would, however, depend on the nature of the sneutrino: or , and on the hierarchy of heavier sparticle masses.

In particular, the relative multiplicities of different charged leptons would depend on the flavour of the invisible , and hence be a useful tool for identifying it. Concretely, in cases where the parent sparticle has no lepton flavour, as would normally be the case at the LHC, each NLSP would be accompanied by an unmatched or , and each NLSP would be accompanied by an unmatched electron, or corresponding neutrino. In general, there would be additional lepton-antilepton pairs with matched flavours.

7 Summary

We have analyzed in this paper the possibility of a sneutrino NLSP in NUHM models with a gravitino LSP. This possibility does not exist in the CMSSM, but is quite generic in the NUHM, as we have illustrated with various specific examples. The sneutrino might well be the , but the and are also possible candidates for the NLSP. A sneutrino NLSP would be metastable and subject to cosmological constraints on late-decaying particles, but we have shown that these are not difficult to respect. There are various different possible scenarios for the spectrum of sparticles heavier than the sneutrino, which would have distinctive signatures at colliders. In addition to events with missing energy carried away by the invisible , there would also be events with accompanying charged leptons. The flavours of such leptons would help identify the flavour of the sneutrino NLSP.

As particle physics embarks on the study of the TeV scale with the LHC, much unknown physics will surely be revealed. Supersymmetry is occasionally regarded as a ‘known unknown’ in the sense that, whereas we do not know whether it exists,we think we know what it would look like if it does exist. This paper reminds us that supersymmetry should rather be regarded as an ‘unknown unknown’, in the sense that not only do we not know whether it exists, but we also do not know what it would look like. In the conventional ‘known unknown’ scenario, the LSP is the lightest neutralino and supersymmetry would produce missing-energy events. The latter would also be the signature of a scenario with a gravitino LSP with a neutralino NLSP, at least in gravity-mediated scenarios. However, once the ‘Pandora’s box’ of a gravitino LSP has been opened, many other NLSP candidates fly out. In addition to the relatively familiar case of the lighter stau and the more radical case of the lighter stop, there are other possibilities including the sneutrino NLSP scenarios discussed here. All of these scenarios have distinctive features, as illustrated here, so the LHC and subsequent experiments have good prospects for detecting and distinguishing between the various ‘unknown unknowns’. No ‘unknown unknown’ stone should be left unturned in the search for supersymmetry.

Acknowledgments

The work of K.A.O. was supported in part by DOE grant DE–FG02–94ER–40823. Y.S. is grateful for the hospitality of CERN and University of Victoria where part of this work was done, and thanks Terrance Figy, Gudrun Heinrich, Stefan Hesselbach, Emerson Luna and Kazunori Kohri for useful discussions.

Appendix: Sneutrino Three-Body Decay

We calculate here the radiative sneutrino three-body decay

 ~ν(P)→ν(p)+γσ(k)+˜Gμ(PG) (25)

that may arise through the photino content of the neutralino, as illustrated in the diagram below.

The invariant amplitude for this decay is

 M=−iBiCi4MPl(q2−m2i)¯u(p)PR(to0.0pt/q+mi)γμ[to0.0pt/k,γσ]Ψμ(PG)ϵσ(k), (26)

where is the Planck mass, ,

 q≡k+PG (27)

and the dimensionless couplings are

 Bi ≡ −g2√2(O2i−tanθWO1i) (28) Ci ≡ O1icosθW+O2isinθW. (29)

Ignoring the neutrino mass, we get

 ¯¯¯¯¯¯¯¯¯¯¯¯|M|2 = 83k⋅PGM2Pl∑i,jC∗jCiB∗jBi(q2−m2i)(q2−m2j) (30) = {k⋅PGm2G[2(PG⋅q)(p⋅q)+(PG⋅p)(mimj−q2)] +2(k⋅q)(p⋅q)+(k⋅p)(mimj−q2)}.

Use the Dalitz parametrization , with , , , we get

 PG⋅k = 12(m212−m2G) (31) k⋅p = 12m223 (32) PG⋅p = 12(M2−m212−m223) (33) k⋅q = 12(m212−m2G) (34) p⋅q = 12(M2−m212) (35) PG⋅q = 12(m212+m2G) (36)

and

 q2=m212. (37)

Hereafter, we abbreviate our notation by defining and .

The resulting partial decay rate is [37]

 dΓ=1(2π)3132M3¯¯¯¯¯¯¯¯¯¯¯¯|M|2dm212dm223. (38)

This can be integrated analytically using the following integration boundaries - for : and , and for : to . The result is

 Γ=1768π3M2PlM3∑i,jC∗jCiB∗jBi2(Ia(i,j)+Ib(i,j)+Ic(i,j)+Id(i,j)), (39)

where

 Ia(i,j) ≡ m2i+m2jm2G(mimj)4[7∑a=1αa(i,j)a(M2a−m2aG)+α0(i,j)ln[M2m2G]], (40) Ib(i,j) ≡ 1m2G(mimj)2[6∑a=1αa+1(i,j)a(M2a−m2aG)+α1(i,j)ln[M2m2G] (41) −α0(i,j)(1M2−1m2G)], Ic(i,j)