Neutrino Fluxes from NUHM LSP Annihilations in the Sun
Abstract
We extend our previous studies of the neutrino fluxes expected from neutralino LSP annihilations inside the Sun to include variants of the minimal supersymmetric extension of the Standard Model (MSSM) with squark, slepton and gaugino masses constrained to be universal at the GUT scale, but allowing one or two nonuniversal supersymmetrybreaking parameters contributing to the Higgs masses (NUHM1,2). As in the constrained MSSM (CMSSM) with universal Higgs masses, there are large regions of the NUHM parameter space where the LSP density inside the Sun is not in equilibrium, so that the annihilation rate may be far below the capture rate, and there are also large regions where the capture rate is not dominated by spindependent LSPproton scattering. The spectra possible in the NUHM are qualitatively similar to those in the CMSSM. We calculate neutrinoinduced muon fluxes above a threshold energy of 10 GeV, appropriate for the IceCube/DeepCore detector, for points where the NUHM yields the correct cosmological relic density for representative choices of the NUHM parameters. We find that the IceCube/DeepCore detector can probe regions of the NUHM parameter space in addition to analogues of the focuspoint strip and the tip of the coannihilation strip familiar from the CMSSM. These include regions with enhanced Higgsinogaugino mixing in the LSP composition, that occurs where neutralino mass eigenstates cross over. On the other hand, rapidannihilation funnel regions in general yield neutrino fluxes that are unobservably small.
CERNPHTH/2011025, KCLPHTH/201103, SU–ITP–11/04,
UMN–TH–2936/11, FTPI–MINN–11/03, SLACPUB14372
I Introduction
One of the most actively pursued strategies for detecting supersymmetric dark matter particles (LSPs) is the search for signatures of the annihilations of LSPs inside the Sun or Earthindirectdet:solar (); indirectdet:earth (). The principle for detection is to search for the passage through a large detector in ice or water of muons produced by the interactions of energetic neutrinos released in the LSP dark matter annihilation process. There have been extensive studies of this potential experimental signature in many variants of the MSSM, and experiments such as IceCube/DeepCore Ahrens:2003ix (); Achterberg:2006md (); Resconi:2008fe (); Abbasi:2009uz () are starting to chip away at the MSSM parameter space.
We recently reanalyzed EOSSnu () this potential signature in the framework of the MSSM with all the supersymmetrybreaking spin1/2 and 0 mass parameters constrained to be universal at the GUT scale (the CMSSM) cmssm (), imposing the requirement that the LSP should provide the density of dark matter inferred from WMAP Komatsu:2010fb () and other experiments. In the CMSSM, where the supersymmetry breaking trilinear mass parameters, are also taken to be universal at the GUT scale, the resulting relic density is found to lie in the WMAP range only along relatively narrow strips in the plane for fixed and eoss (); cmssmwmap (). These correspond to the coannihilation strip, where the mass of the lightest neutralino is close to the mass of the lightest charged slepton (usually the mostly righthanded stau); the heavy Higgs funnel, found at large and large , where the neutralino mass is close to half the heavy Higgs mass and rapid annihilations of neutralinos are mediated by the schannel exchange of heavy Higgs scalars and pseudoscalars; and the focuspoint region which is typically found at very large values of when the parameter (an output of the minimization of the Higgs potential in the CMSSM) is driven to small values and the neutralino picks up a more significant Higgsino component.
In our previous work EOSSnu (), we found that the LSP capture rate was not in general dominated by scattering on protons inside the Sun via spindependent couplings, but that an important role was often played by spinindependent scattering on heavier nuclides. We also found that, in many regions of the CMSSM parameter space, LSP capture and annihilation would not be in equilibrium, and that the annihilation rate would be correspondingly reduced. We also analyzed the uncertainties in the magnitude of the potential muonneutrino signal due to uncertainties in the composition of the Sun and in the scattering matrix elements. We found that the CMSSM might be detectable in IceCube/DeepCore along (some part of) the WMAP strip in the focuspoint region of the plane, and near the low tip of the WMAP strip in the coannihilation region cmssmnu (); EOSSnu ().
In this paper we extend these previous studies to models with one or two degrees of nonuniversality in the soft supersymmetrybreaking contributions to the Higgs doublets, the NUHM1 nuhm1 (); nuhm12 () and NUHM2 nonu (); nuhm2 (); nuhm12 (). One of our primary objectives is to understand the circumstances under which such relatively high neutrino fluxes may be attained in these models and, conversely, whether the relatively low rates usually found in the CMSSM are specific to that model. More generally, we seek to lay a basis for systematic comparisons of the physics capabilities of different detection strategies in (relatively) simple variants of the MSSM.
Supersymmetric dark matter searches Ahmed:2009zw (); Aprile:2010um (); Abbasi:2009uz () are complementary to searches for supersymmetry at accelerators CMSsusy (); ATLASsusy (). At the moment, the latter are sensitive primarily to the spin1/2 and 0 mass parameters and , and are less sensitive to the nonuniversality parameters that appear in the NUHM1,2. For example, global likelihood fits mc3 () currently yield similar 68 and 95% confidencelevel preferred regions in the planes of the CMSSM and NUHM1. It is therefore particularly interesting to know whether direct and indirect dark matter searches offer ways to differentiate between these models.
The NUHM1,2 offer additional mechanisms to bring the relic LSP density into the WMAP range, in addition to the coannihilation, rapidannihilation and focuspoint possibilities mentioned above in the context of the CMSSM. For example, there are distinctive regions of NUHM parameter space where Higgsinogaugino mixing in the LSP is enhanced by levelcrossing in the neutralino mass matrix, bringing the relic density into the WMAP range. Alternatively, the LSPs may annihilate rapidly through directchannel heavy Higgs poles even if and are relatively small. It was shown in mc3 () that the collider prospects for sparticle detection are rather different in the NUHM1 lowmass rapidannihilation region than they are in the CMSSM, whereas the favoured rates for direct LSP detection via scattering on nuclei were broadly similar in the CMSSM and the NUHM1 (though the uncertainties were greater in the latter case). Therefore, it is interesting to study the prospects in this region for LSP detection via the energetic neutrinos produced by annihilation inside the Sun.
The layout of this paper is as follows. In Section II we recall briefly some general features of the NUHM1,2 and discuss other inputs into the rate calculations. Then, in Section III we explore the solar annihilation rates in some generic slices through the NUHM1 parameter space, finding that they are enhanced in regions with relatively large Higgsino components in the LSP as may occur for specific relations between and where there is level crossing. In Section IV we extend our analysis to slices through the NUHM2 parameter space. Section V summarizes our conclusions.
We find that whereas the neutrino flux may be observable in regions with enhanced Higgsinogaugino mixing, analogously to the enhancement along the focuspoint WMAP strip in the CMSSM, the flux is generically unobservably low in the rapidannihilation funnels. This suggests that the observation of a highenergy solar neutrino flux in the IceCube/DeepCore experiment is a potential diagnostic for large mixing and level crossing in the neutralino mass matrix, and specifically of the relation between and , which is a potential tool for identifying nonuniversal Higgs mass parameters.
Ii Preamble
ii.1 The NUHM1 and NUHM2 Parameter Spaces
In the CMSSM, the free parameters are the supposedly universal supersymmetrybreaking parameters and , as well as . The Higgs mixing superpotential parameter and the bilinear supersymmetrybreaking parameter , and hence the pseudoscalar Higgs mass , are then determined using the electroweak vacuum conditions, with a sign ambiguity in . The sign of the discrepancy between the experimental value of and the value calculated within the Standard Model suggests that , and CMSSM analyses are often presented in planes for and fixed values of and . Although much of our NUHM analysis is for , we also consider the possibility of a negative sign. The value of is notoriously unconstrained, see, e.g., mcmSUGRA (), and for definiteness we set it to zero in what follows.
In the NUHM1, the soft supersymmetrybreaking contributions to the masses of the two MSSM Higgs doublets, and , are assumed to be equal, but are allowed to differ from . The extra degree of freedom may be used to treat either or as a free parameter. On the other hand, in the NUHM2, the two soft supersymmetrybreaking contributions to the masses of the MSSM Higgs doublets are allowed to vary independently, and the two extra degrees of freedom may be used to treat both and as free parameters. Analyses of the NUHM1 and NUHM2 parameter spaces are often presented in planes spanned by pairs of the quantities and for some fixed values of and the other parameters, and we present some examples below which are selected from the analysis in nuhm12 (). Since a frequentist likelihood analysis favours relatively small values of and in both the CMSSM and NUHM1 mc3 (), we concentrate here on NUHM1 and NUHM2 planes with relatively low values of either and . We note, however, that a complete likelihood analysis of the NUHM2 is yet to be performed.
ii.2 SpinDependent and Independent Scattering Rates
When calculating the LSP annihilation rates inside the Sun, the key particle physics inputs—apart from the choice of supersymmetric model—are the matrix elements for dark matter scattering on the nuclides inside the Sun. It is often assumed that LSP capture in the Sun is dominated by spindependent scattering on hydrogen but, as discussed in EOSSnu (), spinindependent scattering on heavier nuclei actually dominates in generic regions of the CMSSM parameter space. Figure 1 displays contours of the ratio of the solar dark matter annihilation rate calculated using only spindependent scattering to the total annihilation rate including also spinindependent scattering in (left) the CMSSM plane for , and , and (right) the NUHM1 plane for , and GeV. Regions excluded because there is no consistent electroweak symmetry breaking (EWSB) have dark pink shading, those with a charged LSP have brown shading, and those in conflict with bsgex () measurements have green shading. Regions to the left of the black dashed (red dashdotted) line are inconsistent with the absence at LEP of charginos (a Higgs boson) LEPsusy (); LEPHiggs (); FeynHiggs (). We recall that there is a theoretical uncertainty GeV in the calculation of in the CMSSM, which induces an uncertainty GeV in values of along the red dashdotted line. The recent LHC direct exclusion regions in the CMSSM plane CMSsusy (); ATLASsusy () are somewhat weaker than the indirect LEP Higgs constraint shown here. The pale pink band is favoured by the BNL measurement of Bennett:2006fi (); g2babar (); newg2 (), at the level along the dashed (solid) lines, but we do not impose this as a constraint on our analysis. In the CMSSM case (left panel), we see that spindependent scattering is dominant only at small and large . In the NUHM1 case (right panel), we see that spindependent scattering is subdominant at small , becoming more important along the WMAPcompatible strip with GeV. However, spinindependent scattering is important even here, and in the following analysis all calculations of the annihilation rates include the contributions from both spindependent and independent scattering.
The uncertainties in the spinindependent scattering matrix element include those in the ratios of the light quark masses, the octet contribution, , to the pionnucleon term, , and the value of itself Bottino:1999ei (); Accomando:1999eg (); Ellis:2005mb (); Ellis:2008hf (); Niro:2009mw (). The largest uncertainty is due to , for which we used the value 64 MeV as our default in EOSSnu (), whilst also exploring the implications of other values. The secondlargest uncertainty is due to that in , for which we used the value 36 MeV as our default. We assume the same default values in this analysis. As discussed in more detail in Refs. Ellis:2008hf (); EOSSnu (), different measurements for and lead to variations in the spinindependent scattering crosssection by a factor of 2–3 and the choice of experimental values for these two parameters significantly impacts the spinindependent scattering contribution to capture in the Sun. If were smaller, the total annihilation rate would decrease, and the ratio of the solar dark matter annihilation rate calculated using only spindependent scattering to the total annihilation rate including also spinindependent scattering shown in Figure 1 would increase. By comparison, the uncertainties in the light quark mass ratios are much less significant.
The principal uncertainty in the spindependent matrix element is the contribution of strange quarks to the nucleon spin, , with the uncertainties due to and the SU(3)octet nucleon matrix elements being significantly smaller. The range was considered in EOSSnu (), and was found to induce an uncertainty in the annihilation rate that was %, considerably smaller than the others considered. In the following we take the central value Alekseev:2007vi (), which was adopted in EOSSnu () as the default value.
ii.3 Capture/Annihilation Rates and Neutrino/Muon Fluxes
We compared in EOSSnu () the rates estimated in various alternative solar models. We found that there was at most a 4% difference in the annihilation rates between the two models of Serenelli et al. Serenelli:2009yc () (AGSS09 and AGSS09ph) based upon recent abundance estimates Asplund:2009fu (), and assumed the AGSS09 model as our default. We do the same here, performing a full numerical integration over the radial profile of the Sun when determining the capture rates ^{1}^{1}1Using the simpler Gould approximation Gould:1992xx () would have yielded rates differing from the exact results by at most 6%, as was shown in EOSSnu (). .
In modelling the dark matter halo, we assume a nonrotating isothermal sphere with an rms speed of 270 km/s, a disk rotation speed of 220 km/s, and a local dark matter density of 0.3 GeV/cm. If the calculated neutralino relic density is below the WMAP observed relic density, we assume that only a fraction of the local dark matter density, equal to the ratio of the neutralino and WMAP dark matter relic densities, is attributable to neutralinos. As in EOSSnu (), we do not address other halo models in this paper, but note that our results would scale linearly with the local dark matter density as equilibrium between capture and annihilation is approached.
However, as discussed extensively in EOSSnu (), equilibrium is not in general reached in the CMSSM, and an example is shown in the left panel of Figure 2, namely the plane for and . The dark blue contours are for different ratios of the annihilation and capture rates, and we see that equilibrium is reached only for small and large . The right panel of Figure 2 shows the corresponding contours in the NUHM1 plane for and GeV, where we see that equilibrium is approached only near a vertical strip with GeV. In the following we calculate annihilation rates without relying on the assumption of equilibrium.
The neutralino annihilations produce highenergy neutrinos which, through interactions with matter, will induce muons in or around a detector such as IceCube/DeepCore Ahrens:2003ix (); Achterberg:2006md (); Resconi:2008fe (); Abbasi:2009uz (). The IceCube detector has outfitted 1 km of ice at the South Pole with optical sensors to observe the Cerenkov light produced by the passage of muons through the ice. The large volume allows for sensitivity to very low neutrino fluxes. However, the relatively large spacing between sensors severely limits the sensitivity to lower energy muons (below 100 GeV) which are the largest portion of the neutrinoinduced muon spectra arising from annihilations in the Sun. To improve the sensitivity to these important lowerenergy muons, a portion of the IceCube volume, referred to as DeepCore, has been outfitted with more densely packed sensors.
The ability of IceCube/DeepCore to detect the flux from a given supersymmetric model depends on various factors such as the muon spectra, the neutrino backgrounds, and the method by which IceCube/DeepCore will analyze their results. However, to a very rough approximation, IceCube can detect muon fluxes on the order of 10 or 10 /km/yr above 100 GeV and DeepCore can detect muon fluxes on the order of 10 or 10 /km/yr above 10 GeV. In this paper, we primarily examine the latter case: total fluxes above 10 GeV. DeepCore can detect muons down 10 GeV; however, the analysis threshold may turn out to be somewhat higher: Ref. Barger:2011em () suggests an analysis threshold of 35 GeV is reasonable, while Ref. Danninger:2011pc () suggests 25–30 GeV is more likely (but possibly as low as 20 GeV) ^{2}^{2}2Triggering of two of IceCube/DeepCore’s optical modules—which is possible for muons with energies as low as 10 GeV—is sufficient to detect a muon. However, twomodule events suffer from extremely poor angular resolution. Muons that trigger three optical modules (which requires somewhat higher muon energies) yield much better track reconstruction and allow the analysis to be restricted to muons consistent with neutrinos coming from the direction of the Sun. . In addition, the efficiency of detecting muons (or, equivalently, the effective area of the detector) falls with decreasing muon energy. Our results are not significantly affected by our choice of a 10 GeV threshold as we use only an orderofmagnitude estimate of the IceCube/DeepCore sensitivity to the total muon flux above this energy. Our results are only affected if the flux is predominantly just above threshold (e.g. between 10 and 25 GeV), which is only expected to be the case for very light neutralinos ( GeV or GeV) ^{3}^{3}3The 10 GeV threshold was chosen and the bulk of the work done in this paper was performed prior to the availability of threshold estimates from Refs. Barger:2011em (); Danninger:2011pc (). As this choice does not significantly affect our results, we have chosen to keep the current threshold in our analysis. .
We use the results of the WimpSim simulation wimpsim () (as used within DarkSUSY darksusy ()) to calculate the spectra of the neutrinos produced by the annihilations and the corresponding spectra of neutrinoinduced muons in IceCube/DeepCore. More details of the neutralino capture/annihilation processes and the determination of the neutrino/muon fluxes may be found in Ref. EOSSnu ().
Iii Representative Studies in the NUHM1
iii.1 Comparison with the CMSSM in the Plane
The left panel of Figure 3 displays the neutrinoinduced muon fluxes calculated in the plane for the typical CMSSM scenario with and introduced above. We recall that this plane has two narrow strips where the LSP density falls within the range allowed by WMAP and other measurements Komatsu:2010fb (), which are coloured turquoise. One is the coannihilation strip close to the boundary of the forbidden chargedLSP region at low , and the other is the focuspoint strip close to the EWSB boundary at large .
As was discussed extensively in EOSSnu () and shown in the left panel of Figs. 1 & 2, at large it is usually not appropriate to assume that the LSP capture crosssection is dominated by spindependent interactions, nor that there is equilibrium between capture and annihilation. Accordingly, as already mentioned, neither assumption is made in this and subsequent plots. The solid (blue) lines are contours of the neutrinoinduced muon fluxes above 10 GeV in units of events/km/yr. As seen in the left panel of Figure 3, the neutrino rate is potentially detectable in IceCube/DeepCore along a significant stretch of the focuspoint strip, but apparently undetectable along the portion of the coannihilation strip that is compatible with the LEP Higgs constraint. As discussed in EOSSnu (), the neutrino fluxes in the CMSSM are generally larger for along the coannihilation strip (though still not observable in IceCube/DeepCore), and smaller along the focuspoint strip than they are for the case shown. We also recall that when , there is also a third region compatible with the dark matter density constraint, namely a rapidannihilation funnel at large , where the rate is far too small to be detectable by IceCube/DeepCore.
The right panel of Figure 3 displays the neutrinoinduced muon fluxes to be expected in a sample plane in the NUHM1, again with and , but now with fixed GeV. In this case, an excluded charged LSP region again appears at small though with a different shape from the CMSSM, and the EWSB boundary has moved to small and . Here it is that is driven negative rather than as in the CMSSM. There is a region favoured by that is almost excluded by the LEP Higgs constraint, and there is a coannihilation strip, as in the CMSSM, that follows the EWSB boundary. There is also a nearvertical extension of the coannihilation strip at GeV, that appears thanks to the freedom in the NUHM1 of independently adjusting the parameter. It occurs along a line where a particular relation between and induces level crossing in the neutralino mass matrix as is increased relative to , and thereby leads to increased Higgsinogaugino mixing that brings the LSP density down into the WMAP range. To the right of this strip, the relic density falls below the WMAP range. This strip is the only part of this particular NUHM1 plane where the neutrinoinduced muon flux approaches detectability in IceCube/DeepCore, rising above 30 /km/yr, thanks to the enhanced Higgsinogaugino mixing.
One of the key questions in our analysis will be the extent to which the freedom in the NUHM1,2 to vary and/or provides this and other opportunities for IceCube/DeepCore detection of neutrinos that are absent in the CMSSM.
iii.2 Nuhm1 Planes
We now illustrate further the behaviour of this IceCube/DeepCorefriendly WMAP strip with enhanced Higgsinogaugino mixing, first in some representative planes. Figure 4 displays planes for with (upper left) GeV and (upper right) GeV: both values of are in the range favoured by a frequentist analysis of the NUHM1 parameter space mc3 (). In each case we see EWSB boundaries at large and small where , and regions with that are disfavoured by . In the upper left panel, we also see charged LSP regions at large and . In each case, there is a pair of diagonal WMAPcompatible strips visible at where the Higgsinogaugino mixing is enhanced, which are only weakly dependent on and are compatible with the LEP Higgs constraint for large enough . The neutrinoinduced muon flux above 10 GeV is potentially detectable along essentially all of these diagonal WMAPcompatible strips in both panels, though decreasing as and increase. These strips constitute extensions of the IceCube/DeepCorefriendly strip seen in the right panel of Figure 3, which has GeV and GeV, to different values of these NUHM1 parameters. The red dotdashed curve is the contour for GeV and one should preferably lie above this curve, though one should recall that there is a 1.5 GeV uncertainty in the theoretical calculation of . Nevertheless, fluxes above the Higgs limit still reach above 500 /km/yr. For GeV, the constraint would prefer lower values of in potential conflict with the Higgs bound – though the muon fluxes are quite large where both constraints are satisfied. At GeV, the is not satisfied within 2 anywhere on the plot. We note that there is another WMAP strip slightly above the region with no EWSB. This strip corresponds to the heavy Higgs funnel where and would not be present in the CMSSM at . However, neutrinoinduced muon fluxes are too small along these strips to be observed in IceCube/DeepCore.
Similar diagonal strips with enhanced Higgsinogaugino mixing are seen in the lower left panel of Figure 4 for and GeV, though the muon fluxes are generally smaller. However, the diagonal strip for has a part where lies within the favoured range and the muon flux is /km/yr. As in the previous panels of Figure 4, the WMAPcompatible strips corresponding to the funnel and close to the EWSB boundary have muon fluxes which are unobservably low. In the lower right panel of Figure 4 for and GeV we see that, whilst the EWSB boundary is located similarly to the previous panels, the charged LSP region has advanced considerably, as has the region excluded by . At this value of , is not consistent with RGE running. We also note that the diagonal strip with enhanced Higgsinogaugino mixing has merged with the rapidannihilation funnel, with both sides of the funnel now easily discernible. The muon fluxes where is acceptable are /km/yr and large enough to be detectable by IceCube/DeepCore in the lower part of the transition strip, for values of above the bounds imposed by the LEP Higgs constraints and well with the 1 bounds from (denoted by the dashed black curves). The entire region with below 700800 GeV yields values of in the range favoured by experiment. In contrast to the cases with lower , the funnel region now also has neutrino fluxes that are sufficiently large to be observable ^{4}^{4}4We note that equilibrium is established along the transition strip in all cases, but not along the funnel except at very large . We also note that spindependent scattering is dominant at low for and 20, but subdominant at larger for all values of . .
iii.3 Nuhm1 Planes
In order to explore further the IceCube/DeepCorefriendly region, in Figure 5 we display NUHM1 planes for with (upper left) GeV and (upper right) GeV (again, both values of are in the range favoured by a frequentist analysis of the NUHM1 parameter space mc3 ()), and for GeV with (lower left) and (lower right) . We see in both the upper panels EWSB boundaries at large and small , charged LSP regions at smaller and , and regions excluded by when . When GeV, there is a small region (shaded black) between the stau LSP region and the EWSB boundary where the LSP is a righthanded selectron (or smuon). As in the right panel of Figure 3, we see in both of the upper panels WMAPcompatible strips at roughly fixed values of related to the values of , along which the muon flux above 10 GeV is potentially detectable: above 500 events/km/yr for (upper left) GeV and GeV, and above 100 events/km/yr for (upper right) GeV and GeV. As already commented, along these strips the fluxes are enhanced by Higgsinogaugino mixing. We note that only part of the strip for GeV is compatible with the LEP Higgs constraint, whereas all the GeV strip is compatible. There are no parts of the IceCube/DeepCorefriendly strips in regions favoured by . In both panels, there are WMAPcompatible extensions of these strips to larger at GeV, due to coannihilation, which segue into funnel strips close to the EWSB boundary. However, these do not yield neutrino fluxes interesting for IceCube/DeepCore. In both upper panels, equilibrium is established and spindependent scattering is dominant along the transition strip, whilst the opposite is true along the funnel.
Turning now to the lower panels in Figure 5, we see that as increases with fixed GeV the EWSB boundary moves away to larger , the charged LSP region rises to larger and (for ) the exclusion extends to as well as the visible parts of the halfplane with . In the lower left panel for GeV and we see nearvertical WMAPcompatible strips with GeV where Higgsinogaugino mixing is enhanced and the neutrino flux is favourable for IceCube/DeepCore, and part of the strip for is also favoured by . This interesting region then bends into a nearhorizontal coannihilation strip, resembling those in the upper panels, where the neutrinoinduced muon flux is mostly unfavourable. As increases at low , the LSP changes from a mostly righthanded stau to a righthanded . The muon flux is also small in the funnel that follows the stau LSP boundary. Turning finally to the lower right panel in Figure 5, we clearly see a twosided diagonal funnel where the rapid annihilation via directchannel heavy Higgs poles brings the relic density into the WMAPcompatible range, albeit with a relatively low muon flux. We also see that the strip with enhanced Higgsinogaugino mixing is less vertical and with a lower flux than previously, though still IceCube/DeepCorefriendly. In this case, the constraint is satisfied over much of the plane.
iii.4 Nuhm1 Planes
Figure 6 displays some representative planes in the NUHM1 for and with (upper left) GeV and (upper right) GeV. In both cases, we see that the EWSB requirement excludes a triangular region at large and small where is driven negative, whereas excludes a band at small . There is a region favoured by in the left plane that is again almost excluded by the LEP Higgs constraint. In each case, a WMAPcompatible strip runs parallel to the EWSB boundary, extending to small at GeV. There is also a diagonal funnel where LSPs annihilate rapidly though directchannel Higgs poles, because , and there are WMAP strips on either side of this funnel. The neutrino flux is very unfavourable along the funnel, since the neutrinoinduced muon flux above 10 GeV is events/km/yr. However, a signal may be observable in IceCube/DeepCore along the EWSB boundary, where the muon flux above 10 GeV lies in the range 10 to 100 events/km/yr. As we have seen before, equilibrium is established and spindependent scattering is dominant along the transition strip near the EWSB boundary, in contrast to the funnel regions where equilibrium is not established and spinindependent scattering is dominant.
Turning now to the lower row of plots in Figure 6 for (left) and (right) , both with GeV, we see that the EWSB boundary is broadly similar, whereas the region forbidden by is much reduced. The WMAPcompatible rapidannihilation funnel is clearly visible for , but folds into the EWSB boundary strip for . As in the previous cases, the neutrino flux is unobservably small along the rapidannihilation funnel, but may be observable along the EWSB boundary strip for . We note that a portion of the IceCube/DeepCorefriendly region for is favoured by . For , muon fluxes are /km/yr for GeV along the transition/funnel and compatible with . We note that this case is also interesting because in much of the allowable plane capture is dominated by spinindependent scattering.
iii.5 Nuhm1 Planes
Figure 7 shows some sample NUHM1 planes with fixed that exhibit rapidannihilation funnels. In these cases, the funnels appear as essentially vertical double strips on either side of the line where . In each case, we also note the presences of WMAPcompatible strips close to the EWSB boundary where . The two are attached by coannihilation strips at GeV. When GeV, coannihilation to the left of the funnel at low is dominated by selectrons/smuons which are the LSPs in the lower left corners. In the upper left panel for and GeV, we also see a region at low that is favoured by , but this is in a region disfavoured by the LEP Higgs limit. In this plane, the only WMAPcompatible region allowed by the other constraints is up the funnel at large , where the neutrino flux in unobservably low. In the upper right panel for GeV, the Higgs constraint is irrelevant, but the neutrino flux is still very low in all the WMAPcompatible region except along the strip close to the EWSB boundary. The same is true in the lower left plot for and GeV, where we note that a part of this strip is inside the region favoured by . However, as shown in the lower right plot, when is increased to 55 with the same value of , the EWSB boundary moves so close to the rapidannihilation funnel that there is no IceCube/DeepCorefriendly region.
iii.6 NUHM1 Summary
We have found in the above analysis that interesting neutrino fluxes may arise from enhanced Higgsinogaugino mixing. This possibility arose in the CMSSM in the focuspoint region along the EWSB boundary, but may arise in regions of the NUHM1 parameter space that are far from this boundary, corresponding in general to larger values of . The EWSB boundary region may also yield interesting fluxes when at the boundary. One of the other mechanisms present in the NUHM1 for bring the relic LSP density into the WMAPcompatible range is rapid annihilation through directchannel Higgs poles. However, we have found that this region generally yields low neutrino fluxes.
Iv Representative Studies in the NUHM2
As discussed earlier, in the NUHM2 we are free to adjust both soft Higgs masses independently and as a consequence we can study models for which both and are free parameters Ajaib:2011ab (). We first consider some planes for GeV and GeV as shown in Figure 8. In each case, we see a WMAPcompatible rapidannihilation funnel at GeV as the neutralino mass is roughly 0.43 and therefore roughly half the pseudoscalar mass across the plane. In addition there is an arc at relatively large and due to the coannihilations between the neutralino and sneutrinos. The dark blue shaded regions have a sneutrino LSP and are excluded snu (). In the left panel for , we also see a nearvertical strip at low where the LSP has a substantial Higgsino component, which extends downwards in a stau coannihilation strip almost parallel to the charged dark LSP boundary. The half of the plane is consistent with the constraint. As we have seen before, equilibrium is in this case well established along the vertical transition strip, partially established along the horizontal funnel, and not at all along the arcing coannihilation strip. While scattering is heavily dominated by the spindependent crosssection along the transition strip, spinindependent scattering is significant along the other two strips. In the right panel for , the charged LSP boundary is present at lower and more prevalent at large . Both the stau and sneutino LSP regions are again parallelled by WMAPcompatible coannihilation strips. The supersymmetric contribution to in the right panel exceeds the 2 bound.
In the left plane, the only region with an IceCube/DeepCorefriendly neutrino flux is the vertical strip with a substantial Higgsino content, analogous to those seen previously in our NUHM1 analysis. Here fluxes are in excess of 500 /km/yr. On the other hand, in the right panel where this strip has disappeared, the only IceCube/DeepCorefriendly region is at small and , below the rapidannihilation funnel. We further note that, in both planes, the Higgs mass falls below 114 GeV.
Similar trends can be seen in Figure 9 for GeV and GeV. In the left panel for , we see a nearvertical strip where the LSP has an enhanced Higgsino component, split in two by a nearhorizontal rapidannihilation funnel. This funnel is also present in the right panel for , and splits a diagonal coannihilation strip close to the charged LSP boundary. Again, as in the previous case for smaller and , the only IceCube/DeepCorefriendly regions are in the Higgsinolike strip at small for , and for very small and for . Spinindependent scattering becomes dominant for GeV when and is dominant everywhere in the displayed plane for . In this case, the Higgs mass is above 114 GeV everywhere above the red dot dashed curved found at low . For , the supersymmetric contribution to is too small across the plane, whereas for it lies within the experimental range.
Finally, we present some planes in Figs. 10 and 11, for GeV, GeV and GeV, GeV, respectively. In each case, we assume and the left panel is for and the right panel for . The ranges of and are symmetric GeV, except for the right panel of Figure 10, where asymmetric ranges GeV are chosen so as to display better the regions not excluded by the EWSB constraint (pink) and the sneutrino LSP regions (blue) or the chargedLSP constraint (brown). The signs shown for actually refer to the sign of as they are run in the RGEs. As these are GUT scale parameters, negative values may indicate a cosmological issue with broken symmetric vacua. For a recent discussion of this issue in the NUHM, see Ellis:2008mc ().
In the left panel of Figure 10 for , we see two narrow WMAP strips following the top left and bottom right boundaries of the allowed lozenge of the plane. Of these, the former has an IceCube/DeepCorefriendly neutrinoinduced muon flux over most of its length, rising to events/km/yr for GeV. Note that the nearly horizontal part of the strip corresponds again to the transition strip where a there significant Higgsino contribution to the neutralino composition. The more vertical part of the strip corresponds to the rapid annihilation funnel. On the other hand, the bottom right WMAP strip corresponding to neutralinosneutrino coannihilation generally has an unobservably small neutrino flux, except for positive values of , where the muon flux may reach events/km/yr. As usual, the larger neutrino fluxes are reached when the Higgsino component of the LSP is enhanced. In this plane the constraint is satisfied, though the Higgs mass is low.
In the right panel of Figure 10 for , the allowed region of the plane has receded to more negative values of and , and the two narrow WMAP strips are squeezed closer together. Additionally, we note that the top left strip has bifurcated along the two sides of a rapidannihilation funnel, whereas the lower right strip follows either the stau or sneutrino coannihilation boundaries. As in the left panel of Figure 10, the neutrino fluxes are generally more favourable along the top left strip, though they also become more IceCube/DeepCorefriendly towards the upper end of the other strip, near their junction. Neither or the Higgs mass constraints are satisfied in this plane.
In the left panel of Figure 11 for , we see a single narrow WMAP strip following the top boundary of the allowed region of the plane corresponding to the transition strip. As in the corresponding panel of Figure 10, the neutrinoinduced muon flux is largest, exceeding events/km/yr and hence quite IceCube/DeepCorefriendly, in the top part of the strip close to the EWSB boundary where GeV and the LSP has an enhanced Higgsino component. The left boundary corresponds to the the funnel region where there are two strips, one of which continues on to the vertical transitions strip. The upper part of the funnel still has observable fluxes, but these quickly drop as is decreased. Here, and in the right panel as well, equilibrium is established along all WMAP strips, however spindependent scattering is subdominant almost everywhere in the plane.
In the right panel of Figure 11 for , the previous single narrow WMAP strip has again bifurcated along the two sides of a rapidannihilation funnel, and has moved away from the boundaries of the allowed region of the plane. Once again, the neutrino flux is largest for , though generally lower than in the left panel of Figure 11 (where is smaller) or in the right panel of Figure 10 (where and are smaller), and only barely IceCube/DeepCorefriendly. In this plane, both the and Higgs mass constraints are satisfied.
V Summary
In our previous analysis of the CMSSM, we found that the flux of highenergy neutrinos from LSP annihilations inside the Sun was likely to be observable along the focuspoint WMAP strip, where the Higgsino component of the LSP is enhanced, and at the tip of the coannihilation WMAP strip where the LSP is relatively light. On the other hand, there were significant portions of the WMAPcompatible strips in parameter space, particularly along the coannihilation strip and heavyHiggs rapidannihilation funnels, where the the neutrino flux was not IceCube/DeepCorefriendly.
We find some similar features in our analyses of the NUHM1 and NUHM2. Specifically, there are significant portions of the WMAP strips where the highenergy solar neutrino flux is unlikely to be observable with IceCube/DeepCore. In these models, IceCube/DeepCorefriendly fluxes are often found in regions where the LSP has an enhanced Higgsino component, and this occurs under circumstances that cannot be realized in the CMSSM. Specifically, it may occur for larger LSP masses than along the focuspoint strip of the CMSSM: see, for example, the right panel of Figure 3, the first three panels of Figure 4, and the first three panels of Figure 5.
We conclude, therefore, that IceCube/DeepCore has interesting prospects for probing aspects of the NUHM1 and NUHM2 parameter spaces. However, it seems clear that a more complete exploration of these models, capable of measuring a highenergy neutrino flux when the LSP is relatively heavy and/or does not have a large Higgsino component, would require a subsequent generation of experiment. On the other hand, one may hope that forthcoming LHC results and/or direct searches for LSP scattering could provide more encouraging indications on the prospects for searches for supersymmetric dark matter via annihilation into highenergy solar neutrinos.
Acknowledgements.
The work of KAO was supported in part by DOE Grant No. DEFG0294ER40823. KAO also thanks SLAC (supported by the DOE under contract number DEAC0276SF00515) and the Stanford Institute for Theoretical Physics for their hospitality and support while this work was being finished. C.S. is grateful for financial support from the Swedish Research Council (VR) through the Oskar Klein Centre and thanks the William I. Fine Theoretical Physics Institute at the University of Minnesota, where part of this work was performed, for its hospitality. C.S. also thanks M. Danninger for useful discussions regarding IceCube/DeepCore. The work of V.C.S. was supported by Marie Curie International Reintegration grant SUSYDMPHEN, MIRGCT2007203189.References
 (1) J. Silk, K. A. Olive and M. Srednicki, Phys. Rev. Lett. 55, 257 (1985); M. Srednicki, K. A. Olive and J. Silk, Nucl. Phys. B 279, 804 (1987); J. S. Hagelin, K. W. Ng and K. A. Olive, Phys. Lett. B 180, 375 (1986); K. W. Ng, K. A. Olive and M. Srednicki, Phys. Lett. B 188, 138 (1987); T. K. Gaisser, G. Steigman and S. Tilav, Phys. Rev. D 34, 2206 (1986); F. Halzen, T. Stelzer and M. Kamionkowski, Phys. Rev. D 45, 4439 (1992); L. Bergstrom, J. Edsjo and P. Gondolo, Phys. Rev. D 55, 1765 (1997) [arXiv:hepph/9607237]; K. Freese and M. Kamionkowski, Phys. Rev. D 55, 1771 (1997) [arXiv:hepph/9609370].
 (2) K. Freese, Phys. Lett. B 167, 295 (1986); L. M. Krauss, M. Srednicki and F. Wilczek, Phys. Rev. D 33, 2079 (1986).
 (3) J. Ahrens et al. [IceCube Collaboration], Astropart. Phys. 20, 507 (2004) [arXiv:astroph/0305196].
 (4) A. Achterberg et al. [IceCube Collaboration], Astropart. Phys. 26, 155 (2006) [arXiv:astroph/0604450].
 (5) E. Resconi, for the IceCube Collaboration, Nucl. Instrum. Meth. A 602, 7 (2009) [arXiv:0807.3891 [astroph]].
 (6) R. Abbasi et al. [IceCube Collaboration], Phys. Rev. Lett. 102, 201302 (2009) [arXiv:0902.2460v2 [astroph.CO]]; the combined IceCube/DeepCore flux sensitivities are found in Figure 3 of the arXiv version 2.
 (7) J. Ellis, K. A. Olive, C. Savage and V. C. Spanos, Phys. Rev. D 81, 085004 (2010) [arXiv:0912.3137 [hepph]].
 (8) M. Drees and M. M. Nojiri, Phys. Rev. D 47, 376 (1993) [arXiv:hepph/9207234]; H. Baer and M. Brhlik, Phys. Rev. D 53, 597 (1996) [arXiv:hepph/9508321]; H. Baer and M. Brhlik, Phys. Rev. D 57, 567 (1998) [arXiv:hepph/9706509]; J. R. Ellis, T. Falk, K. A. Olive and M. Schmitt, Phys. Lett. B 388, 97 (1996) [arXiv:hepph/9607292]; J. R. Ellis, T. Falk, K. A. Olive and M. Schmitt, Phys. Lett. B 413, 355 (1997) [arXiv:hepph/9705444]; J. R. Ellis, T. Falk, G. Ganis, K. A. Olive and M. Schmitt, Phys. Rev. D 58, 095002 (1998) [arXiv:hepph/9801445]; V. D. Barger and C. Kao, Phys. Rev. D 57, 3131 (1998) [arXiv:hepph/9704403]; J. R. Ellis, T. Falk, G. Ganis and K. A. Olive, Phys. Rev. D 62, 075010 (2000) [arXiv:hepph/0004169]; J. R. Ellis, T. Falk, G. Ganis, K. A. Olive and M. Srednicki, Phys. Lett. B 510, 236 (2001) [arXiv:hepph/0102098]; V. D. Barger and C. Kao, Phys. Lett. B 518, 117 (2001) [arXiv:hepph/0106189]; L. Roszkowski, R. Ruiz de Austri and T. Nihei, JHEP 0108, 024 (2001) [arXiv:hepph/0106334]; A. B. Lahanas and V. C. Spanos, Eur. Phys. J. C 23, 185 (2002) [arXiv:hepph/0106345]; A. Djouadi, M. Drees and J. L. Kneur, JHEP 0108, 055 (2001) [arXiv:hepph/0107316]; U. Chattopadhyay, A. Corsetti and P. Nath, Phys. Rev. D 66, 035003 (2002) [arXiv:hepph/0201001]; J. R. Ellis, K. A. Olive and Y. Santoso, New J. Phys. 4, 32 (2002) [arXiv:hepph/0202110]; H. Baer, C. Balazs, A. Belyaev, J. K. Mizukoshi, X. Tata and Y. Wang, JHEP 0207, 050 (2002) [arXiv:hepph/0205325]; R. Arnowitt and B. Dutta, arXiv:hepph/0211417.
 (9) E. Komatsu et al. [WMAP Collaboration], Astrophys. J. Suppl. 192 (2011) 18 [arXiv:1001.4538 [astroph.CO]].
 (10) J. R. Ellis, K. A. Olive, Y. Santoso and V. C. Spanos, Phys. Lett. B 565, 176 (2003) [arXiv:hepph/0303043];
 (11) H. Baer and C. Balazs, JCAP 0305, 006 (2003) [arXiv:hepph/0303114]; A. B. Lahanas and D. V. Nanopoulos, Phys. Lett. B 568, 55 (2003) [arXiv:hepph/0303130]; U. Chattopadhyay, A. Corsetti and P. Nath, Phys. Rev. D 68, 035005 (2003) [arXiv:hepph/0303201]; C. Munoz, Int. J. Mod. Phys. A 19, 3093 (2004) [arXiv:hepph/0309346]; R. L. Arnowitt, B. Dutta and B. Hu, arXiv:hepph/0310103.
 (12) A. Corsetti and P. Nath, Int. J. Mod. Phys. A 15, 905 (2000) [arXiv:hepph/9904497]; J. L. Feng, K. T. Matchev and F. Wilczek, Phys. Rev. D 63, 045024 (2001) [arXiv:astroph/0008115]; V. D. Barger, F. Halzen, D. Hooper and C. Kao, Phys. Rev. D 65, 075022 (2002) [arXiv:hepph/0105182]; H. Baer, A. Belyaev, T. Krupovnickas and J. O’Farrill, JCAP 0408, 005 (2004) [arXiv:hepph/0405210]; R. Trotta, R. R. de Austri and C. P. d. Heros, JCAP 0908, 034 (2009) [arXiv:0906.0366 [astroph.HE]].
 (13) H. Baer, A. Mustafayev, S. Profumo, A. Belyaev and X. Tata, Phys. Rev. D 71, 095008 (2005) [arXiv:hepph/0412059]; H. Baer, A. Mustafayev, S. Profumo, A. Belyaev and X. Tata, JHEP 0507, 065 (2005) [arXiv:hepph/0504001].
 (14) J. R. Ellis, K. A. Olive and P. Sandick, Phys. Rev. D 78, 075012 (2008) [arXiv:0805.2343 [hepph]].
 (15) D. Matalliotakis and H. P. Nilles, Nucl. Phys. B 435, 115 (1995) [arXiv:hepph/9407251]; M. Olechowski and S. Pokorski, Phys. Lett. B 344, 201 (1995) [arXiv:hepph/9407404]; V. Berezinsky, A. Bottino, J. R. Ellis, N. Fornengo, G. Mignola and S. Scopel, Astropart. Phys. 5, 1 (1996) [arXiv:hepph/9508249]; M. Drees, M. M. Nojiri, D. P. Roy and Y. Yamada, Phys. Rev. D 56, 276 (1997) [Erratumibid. D 64, 039901 (2001)] [arXiv:hepph/9701219]; M. Drees, Y. G. Kim, M. M. Nojiri, D. Toya, K. Hasuko and T. Kobayashi, Phys. Rev. D 63, 035008 (2001) [arXiv:hepph/0007202]; P. Nath and R. L. Arnowitt, Phys. Rev. D 56, 2820 (1997) [arXiv:hepph/9701301]; J. R. Ellis, T. Falk, G. Ganis, K. A. Olive and M. Schmitt, Phys. Rev. D 58, 095002 (1998) [arXiv:hepph/9801445]; J. R. Ellis, T. Falk, G. Ganis and K. A. Olive, Phys. Rev. D 62, 075010 (2000) [arXiv:hepph/0004169]; A. Bottino, F. Donato, N. Fornengo and S. Scopel, Phys. Rev. D 63, 125003 (2001) [arXiv:hepph/0010203]; S. Profumo, Phys. Rev. D 68, 015006 (2003) [arXiv:hepph/0304071]; D. G. Cerdeno and C. Munoz, JHEP 0410, 015 (2004) [arXiv:hepph/0405057].
 (16) J. R. Ellis, K. A. Olive and Y. Santoso, Phys. Lett. B 539, 107 (2002) [arXiv:hepph/0204192]; J. R. Ellis, T. Falk, K. A. Olive and Y. Santoso, Nucl. Phys. B 652, 259 (2003) [arXiv:hepph/0210205].
 (17) Z. Ahmed et al. [The CDMSII Collaboration], Science 327, 1619 (2010) [arXiv:0912.3592 [astroph.CO]].
 (18) E. Aprile et al. [XENON100 Collaboration], Phys. Rev. Lett. 105, 131302 (2010) [arXiv:1005.0380 [astroph.CO]].
 (19) V. Khachatryan et al. [CMS Collaboration], Phys. Lett. B 698, 196 (2011) [arXiv:1101.1628 [hepex]].

(20)
G. Aad et al. [ATLAS Collaboration],
in preparation;
see
https://twiki.cern.ch/twiki/bin/view/AtlasPublic/SusyPublicResults.  (21) O. Buchmueller et al., JHEP 0809, 117 (2008) [arXiv:0808.4128 [hepph]]; O. Buchmueller et al., Eur. Phys. J. C 64, 391 (2009) [arXiv:0907.5568 [hepph]].
 (22) O. Buchmueller et al., Eur. Phys. J. C 71, 1583 (2011) [arXiv:1011.6118 [hepph]].
 (23) S. Chen et al. [CLEO Collaboration], Phys. Rev. Lett. 87, 251807 (2001) [arXiv:hepex/0108032]; P. Koppenburg et al. [Belle Collaboration], Phys. Rev. Lett. 93, 061803 (2004) [arXiv:hepex/0403004]; B. Aubert et al. [BaBar Collaboration], arXiv:hepex/0207076; E. Barberio et al. [Heavy Flavor Averaging Group (HFAG)], arXiv:hepex/0603003.
 (24) Joint LEP 2 Supersymmetry Working Group, Combined LEP Chargino Results up to 208 GeV, http://lepsusy.web.cern.ch/lepsusy/www/inos_moriond01/charginos_pub.html.
 (25) R. Barate et al. [ALEPH, DELPHI, L3, OPAL Collaborations: the LEP Working Group for Higgs boson searches], Phys. Lett. B 565, 61 (2003) [arXiv:hepex/0306033]; D. ZerZion, Prepared for 32nd International Conference on HighEnergy Physics (ICHEP 04), Beijing, China, 1622 Aug 2004, World Scientific, Hackensack (2005); ALEPH, DELPHI, L3, OPAL Collaborations: the LEP Working Group for Higgs boson searches, LHWGNOTE200401, ALEPH2004008, DELPHI2004042, L3NOTE2820, OPALTN744, http://lephiggs.web.cern.ch/LEPHIGGS/papers/August2004_MSSM/index.html.
 (26) S. Heinemeyer, W. Hollik and G. Weiglein, Comput. Phys. Commun. 124, 76 (2000) [arXiv:hepph/9812320]; S. Heinemeyer, W. Hollik and G. Weiglein, Eur. Phys. J. C 9, 343 (1999) [arXiv:hepph/9812472]; G. Degrassi, S. Heinemeyer, W. Hollik, P. Slavich and G. Weiglein, Eur. Phys. J. C 28, 133 (2003) [arXiv:hepph/0212020]; M. Frank, T. Hahn, S. Heinemeyer, W. Hollik, H. Rzehak and G. Weiglein, JHEP 0702, 047 (2007) [arXiv:hepph/0611326]; http://www.feynhiggs.de/
 (27) G. W. Bennett et al. [Muon G2 Collaboration], Phys. Rev. D 73, 072003 (2006) [arXiv:hepex/0602035].
 (28) B. Aubert et al. [BABAR Collaboration], Phys. Rev. Lett. 103, 231801 (2009) [arXiv:0908.3589 [hepex]].
 (29) M. Davier, A. Hoecker, B. Malaescu and Z. Zhang, Eur. Phys. J. C 71, 1515 (2011) [arXiv:1010.4180 [hepph]].
 (30) A. Bottino, F. Donato, N. Fornengo and S. Scopel, Astropart. Phys. 13, 215 (2000) [arXiv:hepph/9909228].
 (31) E. Accomando, R. L. Arnowitt, B. Dutta and Y. Santoso, Nucl. Phys. B 585, 124 (2000) [arXiv:hepph/0001019].
 (32) J. R. Ellis, K. A. Olive, Y. Santoso and V. C. Spanos, Phys. Rev. D 71, 095007 (2005) [arXiv:hepph/0502001].
 (33) J. R. Ellis, K. A. Olive and C. Savage, Phys. Rev. D 77, 065026 (2008) [arXiv:0801.3656 [hepph]].
 (34) V. Niro, A. Bottino, N. Fornengo and S. Scopel, Phys. Rev. D 80, 095019 (2009) [arXiv:0909.2348 [hepph]].
 (35) M. Alekseev et al. [COMPASS Collaboration], Phys. Lett. B 660, 458 (2008) [arXiv:0707.4077 [hepex]].
 (36) A. Serenelli, S. Basu, J. W. Ferguson and M. Asplund, Astrophys. J. 705, L123 (2009) [arXiv:0909.2668 [astroph.SR]].
 (37) M. Asplund, N. Grevesse, A. J. Sauval and P. Scott, Ann. Rev. Astron. Astrophys. 47, 481 (2009) [arXiv:0909.0948 [astroph.SR]].
 (38) A. Gould, Astrophys. J. 388, 338 (1992).
 (39) V. Barger, Y. Gao and D. Marfatia, Phys. Rev. D 83, 055012 (2011) [arXiv:1101.4410 [hepph]].
 (40) M. Danninger, private correspondence.
 (41) M. Blennow, J. Edsjo and T. Ohlsson, JCAP 0801, 021 (2008) [arXiv:0709.3898 [hepph]]; J. Edsjo, WimpSim Neutrino Monte Carlo, http://www.physto.se/~edsjo/wimpsim/
 (42) P. Gondolo, J. Edsjo, P. Ullio, L. Bergstrom, M. Schelke and E. A. Baltz, JCAP 0407, 008 (2004) [arXiv:astroph/0406204]; P. Gondolo, J. Edsjo, P. Ullio, L. Bergstrom, M. Schelke, E. A. Baltz, T. Bringmann and G. Duda, http://www.physto.se/~edsjo/darksusy/
 (43) For a recent study within the NUHM2, see: M. A. Ajaib, I. Gogoladze and Q. Shafi, arXiv:1101.0835 [hepph].
 (44) T. Falk, K. A. Olive and M. Srednicki, Phys. Lett. B 339, 248 (1994) [arXiv:hepph/9409270]; C. Arina and N. Fornengo, JHEP 0711, 029 (2007) [arXiv:0709.4477 [hepph]].
 (45) J. R. Ellis, J. Giedt, O. Lebedev, K. Olive and M. Srednicki, Phys. Rev. D 78, 075006 (2008) [arXiv:0806.3648 [hepph]].