Effects of neutrino inverse seesaw mechanism on the sparticle spectrum in CMSSM and NUHM2

We study the implications of the inverse seesaw mechanism (ISS) on the sparticle spectrum in the Constrained Minimal Supersymmetric Standard Model (CMSSM) and Non-Universal Higgs Model (NUHM2). Employing the maximal value of the Dirac Yukawa coupling involving the up type Higgs doublet provides a 2–3 GeV enhancement of the lightest CP-even Higgs boson mass. This effect permits one to have lighter colored sparticles in the CMSSM and NUHM2 scenarios with LSP neutralino, which can be tested at LHC14. We present a variety of LHC testable benchmark points with the desired LSP neutralino dark matter relic abundance.

The current LHC lower bounds on the colored sparticle masses from LHC data are mg 1.5 TeV (for mg ∼ mq), and mg 0.9 TeV (for mg mq) [26,27], and it is expected that the LHC14 can test squarks and gluinos with masses up to 3.5 TeV [28]. In order to be able to reduce the sparticle masses to more accessible values in models with universal sfermion and gaugino masses, we require additional contributions from new physics, which preserves gauge coupling unification. Solar and atmospheric neutrino oscillation experiments have established that at least two neutrino states are massive [29]. On the theoretical side the nature of the physics responsible for neutrino masses and flavor properties remains largely unknown and is a JHEP05(2014)078 subject of extensive investigations [30]. Since our goal is to lower the sparticle mass spectrum while preserving gauge coupling unification, we utilize in this paper the inverse seesaw mechanism (ISS) for generating the light neutrino masses [31,32]. Introducing only SM singlet fields allows one to realize the ISS mechanism, and all new fields can be below the TeV scale. In addition, we can have O(1) Dirac Yukawa couplings involving the up type Higgs doublet. It has been shown in refs. [33][34][35] that the Dirac Yukawa coupling can impact the lightest CP-even Higgs boson mass through radiative corrections and increase it by 2-3 GeV when the additional new fields are SM singlets. The ISS mechanism can also be realized using SU(2) W weak triplets [33,34], and in this case the Higgs mass can be enhanced by more than 10 GeV.
In this paper we restrict ourselves to the case of SM singlet fields since we do not want to disturb gauge coupling unification. An enhancement by 2-3 GeV of the CP-even SM-like Higgs boson mass, as we will show, can yield significant reductions of sparticle masses in the Constrained Minimal Supersymmetric Standard Model (CMSSM) [21][22][23][24][25] and Non-Universal Higgs Model with m 2 Hu = m 2 H d (NUHM2) [36][37][38]. Here m 2 Hu and m 2 H d denote the SSB mass square terms for the up and down type MSSM Higgs doublets respectively.
The outline for the rest of the paper is as follows. In section 2 we briefly describe the model including the SSB parameters, the range of values employed in our scan, and the scanning procedure. The relevant experimental constraints that we have employed are described in section 3. The results pertaining to CMSSM, CMSSM-ISS and NUHM2-ISS are discussed in section 4, and our conclusions are summarized in section 5.

Inverse seesaw mechanism and Higgs boson mass
In order to explain non-zero neutrino masses and mixings by the ISS mechanism [31,32], we supplement the MSSM field content with three pairs of MSSM singlet chiral superfields (N c i + N i ), i = 1, 2, 3, and a singlet chiral superfield S which develops a vacuum expectation value (VEV) comparable to or less than the electroweak scale. The part of the renormalizable superpotential involving only the new chiral superfields is given by Here Y N ij and λ N ij are dimensionless couplings and m ij is a mass term. A non-zero VEV for the scalar component of S generates the lepton-number-violating term µ s N i N j ≡ λ N ij S N i N j and, as a result, Majorana masses for the observed neutrinos can be generated. The coupling λ N ij SN i N j is preferred over the direct mass term µN i N j , with the former yielding the desired mass terms for the N fields with a non-zero S . A singlet chiral superfield S can make it easier to find extension of the SM gauge group with help from a suitable symmetry (see, for instance, refs. [33,34,[39][40][41][42][43][44][45][46][47]), and avoid terms which otherwise may spoil the ISS mechanism. The SSB terms pertaining to the fields N c i and N i are given by Figure 1. Supergraph leading to dimension six operator for neutrino masses.
where the SSB parameters are prescribed at the TeV SUSY breaking scale. In the ISS case there are regions of the SSB parameter space for which one of the sneutrinos can be the lightest supersymmetric particle (LSP). The phenomenology of models of this kind has been studied in refs. [39][40][41][42][43][44][45][46][47]. In our present work we assume that the lightest neutralino is the LSP, and a spectrum of this nature can be realized both in the CMSSM and NUHM2 if we assume that all sfermions, including the N c i and N i fields, have universal SSB mass terms at M GUT .
According to the superpotential in eq. (2.1), after integrating out the (N c i + N i ) fields, the neutrino mass arises from the effective dimension six operator (figure 1): We assume here that M 6 δ ij ≡ m ij is larger than the electroweak scale. Also, in eq. (2.3) the family and SU(2) W gauge indices are omitted. Following the electroweak symmetry breaking, the neutrino Majorana mass matrix is generated: For simplicity, we set Y N ≡ Y N ij and λ N ≡ λ N ij , and v u , S are the VEVs of H u , and the S field. Eq. (2.4) implies that even if we require Y N ∼ O(1) and M 6 ∼ 1 TeV, the correct mass scale for the light neutrinos can be reproduced by suitably adjusting λ N S . Keeping Y N ∼ O(1) will provide sizable contribution to the lightest CP-even Higgs mass, which is given by [48,49] [ where and

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We incorporate the ISS mechanism in CMSSM and NUHM2 and scan the SUSY parameter space using the ISAJET 7.84 package [50]. We modify the code by including the additional contributions from eq. (2.5) to the lightest CP-even Higgs boson mass.

Phenomenological constraints and scanning procedure
We employ the ISAJET 7.84 package [50] to generate sparticle spectrum over the fundamental parameter space. In this package, the weak scale values of the gauge, third generation Yukawa couplings, including the Yukawa coupling N c i H u L j from ISS, are evolved to M GUT via the MSSM renormalization group equations (RGEs) in the DR regularization scheme. With the boundary conditions given at M GUT , all of the SSB parameters, along with the gauge and Yukawa couplings, are evolved back to the weak scale M Z . The data points collected all satisfy the requirement of radiative electroweak symmetry breaking condition with the neutralino in each case being the LSP.
We have performed Markov-chain Monte Carlo (MCMC) scans for the following CMS-SM parameter range: with µ > 0 and m t = 173.3 GeV [51]. We use m DR b (M Z ) = 2.83 GeV which is hard-coded into ISAJET. Here m 0 is the universal SSB mass parameter for MSSM sfermions, Higgs and additional N c , N and S fields, m 1/2 is the gaugino mass parameter, tan β is the ratio of the VEVs of the two MSSM Higgs doublets, and A 0 is the MSSM universal SSB trilinear scalar coupling. In order to maximize the contribution from the ISS mechanism to the Higgs boson mass, we setX Y N = 4, following refs. [33,34].
In the case of NUHM2, in addition to the above mentioned parameters we have two additional independent mass parameters m H d and m Hu . We use the following parameter range for them: To maximize the impact of ISS on the sparticle spectrum, we set λ N = 0.7. This is the maximal value of λ N at low scale that remains perturbative up to M GUT . We also assume that M 6 is larger than M S , in order that the neutralino rather than sneutrino is the LSP.
After collecting the data, we impose the mass bounds on all the particles [52] and use the IsaTools package [53,54] and ref. [55] to implement the following phenomenological JHEP05(2014)078 constraints: As far as the muon anomalous magnetic moment a µ is concerned, we require that the benchmark points are at least as consistent with the data as the SM.
For the benchmark points presented in table 1 and 2, we require that the neutralino LSP relic abundance lies in the interval 0.0913 ≤ Ω CDM h 2 ≤ 0.1363 measured by WMAP for the Cold Dark Matter (CDM) abundance [60].
Finally we implement the following following bounds on the sparticle masses: mg 1.5 TeV (for mg ∼ mq) and mg 0.9 TeV (for mg mq) [26,27]. 4 Results

CMSSM and inverse seesaw
In this section we present our results for the CMSSM and the CMSSM with additional ISS contribution (CMSSM-ISS). The main idea behind the presentation of these results is to show that these two scenarios have quite distinct features as far as choice for the fundamental parameters of the models is concerned. In figure 2, the left panels represent our results for the CMSSM, while the right panels display our results for the CMSSM-ISS.
Here grey points satisfy REWSB and the LSP neutralino requirement. The orange points represent solutions which satisfy the mass bounds and B-physics bounds from section 3. Solutions in blue color are a subset of orange points and satisfy the requirement 123 GeV m h 127 GeV. We display our results for a wider range of neutralino LSP relic abundance, Ωh 2 , keeping in mind that one can always find points within the WMAP range with dedicated scans within the orange regions. For instance, the graph in m 0 -m 1/2 plane shows that for the CMSSM case, the Higgs mass bounds excludes simultaneously small values for m 0 and m 1/2 , while in the CMSSM-ISS case, we can have relatively small values for m 1/2 (< 800 GeV) and m 0 (< 400 GeV), consistent with all constraints given in section 3. There is also noticeable difference between CMSSM and CMSSM-ISS in the A 0 /m 0 -m 0 plane. In the CMSSM case, for instance, we find the minimal values m 0 ∼ 700 GeV for A 0 /m 0 = −3, and for A 0 /m 0 = 3 we have m 0 ∼ 1.3 TeV. In CMSSM-ISS, on the other hand, the corresponding minimum m 0 values vary from 400 GeV to 1.1 TeV. In the m 0 -tan β plane too, considering the blue points, we see in the left panel that for a minimum value m 0 ∼ 700 GeV, the corresponding tan β value is around 16. In the right panel, on the other hand, tan β is again around 16 but now the minimum value of m 0 is ∼ 300 GeV.
In figure 3 we show plots of m 0 versus µ. The color coding is the same as in figure 2 with the left and right panels representing CMSSM and CMSSM-ISS respectively. This JHEP05(2014)078  in addition to the top quark loop, which makes µ relatively heavy. Thus, in the CMSSM-ISS case we do not have the so-called focus point/hyperbolic branch scenario [61][62][63][64] while it is still a viable solution in the CMSSM case.
In figure 4, we show graphs in mχ0 1 -mt 1 and mχ0 1 -mτ 1 planes. The color coding is the same as in figure 2, except that the solutions in red are a subset of solutions in blue and also satisfy the relic abundance bound 0.001 ≤ Ωh 2 ≤ 1. These graphs show that despite the fact that there are differences in the space of fundamental parameters, the mass spectrum for χ 0 1 ,t 1 andτ 1 turn out to be more or less identical. For instance, in the mχ0 1 -mt 1 plane we see that we have NLSPt 1 in the mass range of ∼ 260-500 GeV in both cases. Similar results were also reported in [65,66] in the case of b-τ Yukawa coupling unification in CMSSM and SU (5). It was shown in [67,68] that the region of parameter space with stop-neutralino mass difference of 20% is ruled out for mt 1 140 GeV. In the mχ0 1 -mτ 1 plane, we note that NLSPτ 1 has the same mass range in CMSSM and CMSSM-ISS. The reason why we have comparable intervals for mt 1 and mτ 1 in CMSSM and CMSSM-ISS is that low values for both sparticle masses are acheived via fine tuning involving the trilinear SSB terms, while the addition of ISS to CMSSM mostly affects the first two generation sparticle masses.
In figure 5, we present graphs in mχ0 1 -m A and mχ0 1 -mχ± 1 planes, with color coding the same as in figure 4. The graphs in mχ0 1 -m A plane show that we do not have the A-resonance solution [69][70][71][72][73][74], and the reason can be understood from the following equation:  the black line. In the right panel, which represents the CMSSM-ISS case, we note that both the orange and blue points are further away from the solid black line. This is because of two reasons. Firstly, as stated earlier, µ is larger because of extra contributions from the N c i H u L j Yukawa coupling, and so the orange points move away from the solid black line. Secondly, as explained, in the CMSSM case the m h constraint makes solutions move away from the solid black line as m A becomes larger.
A more distinctive figure concerning the sparticle spectra in CMSSM and CMSSM-ISS is presented in the mχ0 1 -mχ± 1 plane. In contrast to CMSSM (left panel), the figure for CMSSM-ISS is quite different. This is due to the fact that in CMSSM-ISS, the LSP neutralino is mostly a bino and the chargino mostly wino. Therefore, the ratio mχ0 1 /mχ± 1 is close to the ratio of U(1) and SU(2) gauge couplings, g 1 /g 2 ≈ 1/2, and the points form a narrow strip. In figure 6 we show mq versus mg for CMSSM (left panel) and CMSSM-ISS (right panel). The color coding is the same as in figure 2, except that the orange points do not include mass bounds for gluinos and the first two generation squarks. Dashed vertical and horizontal lines represent current squark and gluino mass bounds. We note that especially JHEP05(2014)078 in the CMSSM the gluino mass bound excludes a significant portion of the parameter space which otherwise is consistent with the experimental data. The location of blue points relative to the orange points shows how the lower bounds on the squark and gluino masses are pushed up by m h . It is interesting to observe that there are no red points with neutralino LSP dark matter within the reach of LHC14. Comparing results from mg-mq panel with the results from figures 4 and 5, we conclude that in the CMSSM, the solution which yields the correct dark matter relic abundance predicts gluino and squarks masses that lie beyond the reach of the LHC14 [28].
On the other hand, comparison of left and right panels in figure 6 shows the impact of the ISS mechanism on the sparticle masses. We can see from the mg-mq plot in the right panel that plenty of blue points are left after we apply the Higgs mass constraint 123 GeV m h 127 GeV. This means that in the presence of the ISS mechanism, most points satisfying all experimental constraints lie in the Higgs mass range 123 GeV m h 127 GeV, which is very different from the CMSSM case. There are also red points in the right panel which shows that we can have LHC testable solutions with the correct relic abundance of dark matter.  In the left panel we see from the blue points that ml > 1.4 TeV, which may be difficult to test at the LHC. On the other hand, we see in the right panel solutions in blue and red colors around ml 500 GeV, which provides a glimmer of hope that sleptons employing the CMSSM-ISS mechanism may be found at the LHC.

NUHM2 and inverse seesaw
In this subsection we present the results of our scan for NUHM2 with ISS contributions (NUHM2-ISS). In figure 8 we present graphs in m 0 -m 1/2 and m 0 -µ planes, with color coding the same as in figure 2. In the m 0 -m 1/2 plane we see that the results are similar to what we found in CMSSM-ISS. Again we can have solutions compatible with all experimental constraints presented in section 3. We note that the Higgs mass constraint 123 GeV m h 127 GeV provides the lower bounds m 1/2 ≈ 500 GeV and m 0 ≈ 1 TeV. Since µ is a free parameter in NUHM2, we can find solutions with any value of µ compatible with the experimental data (see m 0 -µ plot). As shown in [86,87], a relatively small µ term is necessary, but not sufficient, to be consistent with natural supersymmetry (little hierarchy problem) criteria. We find that it is hard to fully resolve the little hierarchy problem in this scenario. The sparticle spectrum for NUHM2-ISS is shown in figure 9, In the bottom right panel we plot mχ± 1 versus mχ0 1 . This graph is very different from the corresponding one for CMSSM-ISS. In NUHM2-ISS scenario, because of low µ values, the chargino can be Higgsino-like, which yields bino-Higgsino mixed dark matter. This type of solution can be seen along the solid back line. In those cases where µ is heavy, the chargino will be wino-like as in the CMSSM-ISS case. Such solutions can are displayed in the second strip in the graph. We also display a plot in the mχ0 1 -mν 3 plane where we show a minimum value mν 3 ≈ 250 GeV, which is also consistent with the results reported in ref. [88].

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In figure 10 we show graphs in mq-mg and mχ± 1 -ml planes. In the left panel, the orange points do not satisfy the mass bounds for gluinos and first two generation squarks. The color coding otherwise is the same as in the previous figures. Dashed vertical and horizontal lines display the current squark and gluino mass bounds.
Comparing results from figures 10 and 7, we see very small changes on the lower mass bounds for the first two generation squarks, and sleptons as well as gluinos, which is what we expected. But there are many more red points in figure 10, because in the NUHM2-ISS case, we have the additional A-resonance and bino-Higgsino dark matter solutions for the JHEP05(2014)078 LSP neutralino relic abundance. As in the CMSSM-ISS case, we can have squarks and gluinos in a mass range which can be explored at LHC14.
In table 2 we present five benchmark points for NUHM2-ISS case which satisfy the phenomenological constraints discussed in section 3. Points 1, 2, 3, 4 and 5 are chosen, respectively, from the stau-neutralino coannihilation region, the bino-Higgsino mixed dark JHEP05(2014)078 matter region, the A-resonance region, the sneutrino-neutralino coannihilation region, and the stop-neutralino coannihilation region. In all the five benchmark points the first two generation squarks are in the mass range 2.4-3.5 TeV, while the first two generation sleptons lie around 1.6-3 TeV. Note that for the bino-Higgsino mixed dark matter point the spin independent cross section is 6.83 × 10 −9 pb, which is below the current XENON100 bounds [89], but within the reach of XENON1T [90] and SuperCDMS [91].

Conclusions
The recent discovery at the LHC of a SM-like Higgs boson with mass m h 125 GeV puts considerable stress on the MSSM. With m h M Z at tree level, large radiative corrections are required. Such corrections can be achieved in the MSSM either with multi-TeV stops, or with a large stop trilinear coupling and stop masses around 1 TeV. In models with universal sfermion masses at M GUT , such as CMSSM and NUHM2, this leads to heavy sleptons and 1st/2nd generation squarks which are near or beyond the ultimate LHC reach. Various MSSM extensions have been proposed to allow lighter sfermions via additional contributions to the lightest CP-even Higgs boson mass. In this paper we explored the impact of the inverse seesaw mechanism on the sparticle mass spectrum.
The ISS mechanism allows an increase of m h by a few GeV, while simultaneously generating mass for neutrinos via dimension six operators. With a maximal value of the Dirac Yukawa coupling involving the up-type Higgs doublet, m h is increased by 2-3 GeV. As we have shown, this effect allows one to have lighter colored sparticles in CMSSM and NUHM2 scenarios which can be tested at LHC14. For example, in CMSSM-ISS the minimal value of m 0 consistent with all mass and B-physics bounds is ∼ 400 GeV, compared to CMSSM where m 0 800 GeV. Furthermore, requiring neutralino LSP to be the cold dark JHEP05(2014)078  Table 2. Masses (in GeV units) and ohter parameters for NUHM2-ISS benchmark points satisfying all phenomenological constraints discussed in section 3. Points 1-5 are chosen, respectively, from the stau-neutralino coannihilation, the bino-Higgsino mixed dark matter, the A-resonance, the sneutrino-neutralino coannihilation, and the stop-neutralino coannihilation regions.
matter pushes m 0 to 10-20 TeV range in CMSSM, whereas in CMSSM-ISS m 0 ∼ 400 GeV are compatible with the CDM constraint. This means that squarks and gluinos in CMSSM-ISS lie within the reach of LHC14. Similarly, in NUHM2-ISS squarks and gluinos in 1.5-3 TeV range are consistent with neutralino CDM. We have presented several LHC testable benchmark points with the desired neutralino dark matter relic abundance.