Light Higgsino for Gauge Coupling Unification

TL;DR

This paper investigates how light higgsinos in high-scale supersymmetry can enable precise gauge coupling unification and provide dark matter candidates, with implications for supersymmetry breaking mechanisms.

Contribution

It demonstrates that light higgsinos allow gauge coupling unification at high scales and connects this to dark matter and specific supersymmetry breaking models.

Findings

Gauge couplings unify as precisely as in low-energy supersymmetry.

Dark matter can be explained by neutral higgsino or gravitino.

High scale supersymmetry with light higgsinos is naturally realized in anomaly and gauge mediation models.

Abstract

We explore gauge coupling unification and dark matter in high scale supersymmetry where the scale of supersymmetry breaking is much above the weak scale. The gauge couplings unify as precisely as in low energy supersymmetry if the higgsinos, whose mass does not break supersymmetry, are much lighter than those obtaining masses from supersymmetry breaking. The dark matter of the universe can then be explained by the neutral higgsino or the gravitino. High scale supersymmetry with light higgsinos requires a large Higgs mixing parameter for electroweak symmetry breaking to take place. It is thus naturally realized in models where superparticle masses are generated at loop level while the Higgs mixing parameter is induced at tree level, like in anomaly and gauge mediation of supersymmetry breaking.

Equations

$$|\mu |\ll m_{\mathrm{susy}},$$

$$(m_{H_u}^2+|\mu {|}^2)|H_u^0{|}^2+(m_{H_d}^2+|\mu {|}^2)|H_d^0{|}^2$$

$$-(B\mu H_u^0{H}_d^0+h.c.),$$

$$|B\mu {|}^2>(m_{H_u}^2+|\mu {|}^2)(m_{H_d}^2+|\mu {|}^2),$$

$$2|B\mu |$$

$$|\mu |\sim |B|\sim \sqrt{m_{H_d}^2}\sim m_{\mathrm{susy}},$$

$$\sin 2\beta$$

$$\frac{1}{2}{m}_Z^2$$

$$|\mu |\ll m_{\mathrm{susy}}\ll |B|\approx \frac{m_{\mathrm{susy}}^2}{|\mu |\tan \beta },$$

$$m_{H_d}^2{|}_{\mathrm{AM}}$$

$$B{|}_{\mathrm{AM}}$$

$$f(X)H_u{H}_d,$$

$$m_{H_d}^2{|}_{\mathrm{GM}}$$

$$B{|}_{\mathrm{GM}}$$

$$m_{3/2}\gtrsim \frac{M}{M_{Pl}}F/M,$$

$$|B|\lesssim 8{\pi }^2{m}_{\mathrm{susy}}.$$

$$\frac{1}{g_{\mathrm{GUT}}^2{|}_{\mathrm{TeV}}}$$

$$M_{\mathrm{GUT}}{|}_{\mathrm{TeV}}$$

$$m_{\ast }$$

$$m_{\ast }\approx 1\mathrm{TeV},$$

$$\frac{1}{g_{\mathrm{GUT}}^2}$$

$$\frac{|\mu |}{m_{\ast }}{\left(\frac{m_H}{m_{\ast }}\right)}^{\frac{1}{4}}{\left(\frac{M_2}{m_{\ast }}\right)}^{\frac{1}{3}}{\left(\frac{M_2}{M_3}\right)}^{\frac{7}{3}}{\left(\frac{m_{\tilde{\ell }}}{m_{\tilde{q}}}\right)}^{\frac{1}{4}}=1,$$

$$\frac{1}{g_{\mathrm{GUT}}^2}=\frac{1}{g_{\mathrm{GUT}}^2{|}_{\mathrm{TeV}}}$$

$$+\frac{1}{8{\pi }^2}\ln \left[{\left(\frac{|\mu |}{m_H}\right)}^{\frac{10}{19}}{\left(\frac{M_2}{|\mu |}\right)}^{\frac{12}{19}}{\left(\frac{m_{\tilde{\ell }}}{|\mu |}\right)}^2\right]$$

$$+\frac{1}{8{\pi }^2}\ln \left[{\left(\frac{M_3}{M_2}\right)}^{\frac{125}{19}}{\left(\frac{m_{\tilde{q}}}{m_{\tilde{\ell }}}\right)}^{\frac{173}{76}}\right],$$

$$M_{\mathrm{GUT}}$$

$${\left(\frac{g_{\mathrm{GUT}}^2}{0.5}\right)}^{-1}{\left(\frac{M_{\mathrm{GUT}}}{2\times 10^{16}\mathrm{GeV}}\right)}^2\gtrsim 0.1,$$

$$\frac{m_{\mathrm{susy}}}{|\mu |}\lesssim 0.6\times 10^4{\left(\frac{M_3}{M_2}\right)}^{-\frac{25}{8}},$$

$$m_{\mathrm{susy}}\approx {\left(\frac{m_{\ast }}{|\mu |}\right)}^{\frac{12}{7}}{\left(\frac{M_3}{M_2}\right)}^4{m}_{\ast },$$

$${\frac{M_a}{g_a^2}|}_{m_{\mathrm{susy}}}\propto 1+b_a\alpha ,$$

$$\frac{M_3}{M_2}=\frac{1+b_3\alpha }{1+b_2\alpha }\frac{g_3^2}{g_2^2},$$

$$|\alpha |\le \mathcal{O}(1),$$

$$\frac{|B|}{m_{H_d}^2}=\frac{\kappa }{m_{\mathrm{susy}}},$$

$$0<\kappa \lesssim 8{\pi }^2.$$

Full text

††preprint: PNUTP-17/A11

Supersymmetry (SUSY) is a theoretically well-motivated framework for extending the Standard Model (SM), and can be realized in various ways. Taken as a theoretical guiding principle to physics beyond the SM, naturalness suggests low energy SUSY spontaneously broken at a TeV scale or below, for which the minimal supersymmetric SM (MSSM) becomes compatible with gauge unification Dimopoulos:1981yj and provides a viable candidate for cold dark matter Jungman:1995df . However, the observation of the SM-like Higgs boson with mass near 125 GeV and non-observation of new physics signals at the LHC seem to indicate that the scale of SUSY breaking is around multi TeV or higher. One may then need a different approach to the naturalness problem, like for instance the dynamical relaxation of the weak scale Graham:2015cka . If realized at a high energy scale, SUSY would play only a partial role in stabilizing the weak scale against quantum corrections.222 In SUSY relaxion models Batell:2015fma ; Choi:2015fiu ; Evans:2016htp , the higgsino mass parameter $\mu$ receives two or more contributions whose relative phase is determined by the relaxion, generating the weak scale via cosmological evolution. This mechanism would work also in high scale SUSY with light higgsinos because $|B\mu|^{2}$, on which the determinant of the Higgs mass matrix depends, still varies along the relaxion direction. Here $B$ denotes the Higgs mixing parameter.

Nonetheless it still remains attractive, in particular from the viewpoint of grand unification and dark matter.

In this letter we examine if SUSY broken much above the weak scale can account for the dark matter of the universe, and retain the unification of gauge couplings in the absence of high scale threshold corrections so that extension towards a grand unified theory (GUT) is possible.333See, for instance, Ref. Hisano:2013cqa for threshold corrections at the GUT scale in the high scale SUSY scenario. Interestingly, gauge couplings unify as precisely as in low energy SUSY if the higgsinos, whose mass is not directly connected to SUSY breaking, are much lighter than other sparticles and the heavy Higgs doublet ArkaniHamed:2005yv ; Hall:2011jd . That is, if

[TABLE]

where $\mu$ is the higgsino mass parameter, and $m_{\rm susy}$ denotes the scale of SUSY breaking. The lightest sparticle is then the neutral higgsino or the gravitino, which can make up all the dark matter if produced non-thermally or from thermal scatterings of sparticles.

High scale SUSY with light higgsinos can have interesting phenomenology ArkaniHamed:2005yv ; Hall:2011jd ; Cheung:2005pv ; Beylin:2009wz ; Fox:2014moa ; Nagata:2014wma ; Chun:2016cnm , but needs to address how to achieve electroweak symmetry breaking (EWSB) that requires a Higgs mixing parameter $B$ much larger than $m_{\rm susy}$. We stress that a natural framework for large $B$ is provided by models where sparticle masses are generated at loop level while $B$ is induced at tree level, like in anomaly Randall:1998uk ; Giudice:1998xp or gauge mediation Dine:1994vc ; Dine:1995ag . We examine the relation between $m_{\rm susy}$ and $\mu$ required for EWSB and gauge unification in the scenario where anomaly or gauge mediation is sizable, and estimate the value and scale at which the gauge couplings unify.

How light can the higgsinos be compared to other sparticles? The most important theoretical constraint on $\mu$ comes from EWSB. In the MSSM scalar potential, the squared-mass terms of the neutral Higgs fields read

[TABLE]

including SUSY breaking terms associated with the Higgs doublet fields. Thus EWSB occurs if

[TABLE]

where the involved parameters should satisfy

[TABLE]

for the scalar potential to be stable along the $D$-flat direction, $|H^{0}_{u}|=|H^{0}_{d}|$. It is obvious that the above condition cannot be satisfied if $\mu$ is much larger than $m_{\rm susy}$ as inferred from that it gives a supersymmetric mass to the Higgs bosons. For the conventional scenario with

[TABLE]

EWSB is triggered when renormalization group (RG) flow drives $m^{2}_{H_{u}}$ to negative or small values at low energy, which is possible as it is considerably affected by loop effects associated with the large top Yukawa coupling.

It is remarkable that EWSB is possible also for $|\mu|\ll m_{\rm susy}$ if the Higgs mixing parameter $B$ has a large value around $m^{2}_{\rm susy}/\mu$. To be in more detail, the minimization condition

[TABLE]

shows that EWSB can be achieved when the higgsinos are relatively light and the Higgs sector parameters have the hierarchy Jeong:2011sg ,

[TABLE]

for moderate and large $\tan\beta$, while $m^{2}_{H_{u}}$ is negative or much smaller than $m^{2}_{\rm susy}$ in size as in the conventional scenario. Here $\tan\beta=\langle|H^{0}_{u}|\rangle/\langle|H^{0}_{d}|\rangle$, and $m_{Z}$ is the $Z$-boson mass.

The hierarchy between the Higgs mixing parameter and sparticle masses is naturally realized in a class of SUSY breaking models where sparticles obtain masses at loop level, that is, for instance, models in which anomaly or gauge mediation is sizable. A large $B$ in such models has been regarded as problematic in low energy SUSY because it makes EWSB difficult unless $\mu$ is below 100 GeV, which is in conflict with the LEP bound on the chargino mass. The situation however changes in high scale SUSY.

In supergravity, anomaly mediation always induces sparticle masses radiatively, but the Higgs mixing parameter associated with $\mu$ arises at tree-level:

[TABLE]

where $m_{3/2}$ is the gravitino mass. Hence $m_{\rm susy}\ll|B|$ is obtained in models where anomaly mediation is sizable to other mediations in size. In such a case, the gravitino is quite heavy as would be required to make the gravitino decay before big bang nucleosynthesis (BBN). Note also that the higgsino is likely the lightest supersymmetric particle (LSP) because EWSB requires $|\mu|\ll m_{\rm susy}$.

Another possible way to get a large Higgs mixing parameter is to consider models with sizable gauge mediation where $\mu$ is dynamically generated from the superpotential term

[TABLE]

for some function $f$. Here $X$ is the SUSY breaking field that provides masses to messengers. One may instead consider $f(X,X^{*})H_{u}H_{d}$ in the K$\ddot{\rm a}$hler potential. The sparticles then obtain masses at loop level, while the Higgs mixing parameter is generated at tree level:

[TABLE]

for $\langle X\rangle=M+\theta^{2}F$. On the other hand, the vanishing cosmological constant puts a lower bound on the gravitino mass

[TABLE]

with $M_{Pl}$ being the reduced Planck mass. The gravitino can be the LSP if the messenger scale $M$ is intermediate or low.

To summarize, there naturally arises a hierarchy between the Higgs mixing parameter and the sparticle masses:

[TABLE]

in models where anomaly or gauge mediation gives sizable contributions to sparticle masses. For large $B$, we need $|\mu|\ll m_{\rm susy}$ to trigger EWSB. In this class of models, therefore, the lightest ordinary supersymmetric particle would be a nearly pure higgsino, while the gravitino can be very heavy or light.

Let us now turn to the issue of gauge coupling unification. The MSSM leads to quantitative unification of gauge couplings for low scale SUSY where the sparticles are around TeV. The unified gauge coupling and unification scale are approximately given by

[TABLE]

Let us consider a simple case in which all the sparticles and the heavy Higgs doublet have a common mass. Then, there exists a value of the common sparticle mass

[TABLE]

at which the three gauge couplings meet exactly at one point within the MSSM. The value of $m_{\ast}$ is estimated to be

[TABLE]

where the dependence on $\tan\beta$, which arises at the two-loop level, is very mild.

To see how gauge coupling unification is affected by sparticle masses, we use one-loop RG evolution of gauge couplings in the dimensional reduction scheme under the assumption, for simplicity, that the sleptons (squarks) have a universal mass $m_{\tilde{\ell}}$ ($m_{\tilde{q}}$). From the fact that gauge unification works in low scale SUSY, the unified gauge coupling is found to be

[TABLE]

for $a=1,2,3$ and summing over the sparticles and heavy Higgs doublet. Here $b_{a}$ denotes the $\beta$ function coefficient in the MSSM, and $b^{\phi}_{a}$ is the contribution of the particle $\phi$ to it. Using the above relations, one finds that successful unification is maintained for a sparticle spectrum satisfying

[TABLE]

with $m_{\ast}\approx 1$ TeV Langacker:1992rq ; Carena:1993ag ; Roszkowski:1995cn ; Raby:2009sf ; Krippendorf:2013dqa . Here $M_{2}$ and $M_{3}$ are the wino and gluino mass, respectively, and $m_{H}$ is the heavy Higgs doublet mass. The unification condition is sensitive to the masses of the higgsino, wino and gluino. But it is relatively insensitive to the masses of the heavy Higgs doublet and sfermions. In particular, gauge unification becomes independent of the sfermion spectrum if the squarks and sleptons have a common mass, which reflects the fact that they form complete SU$(5)$ multiplets. This implies that unification works even when the sfermions are very heavy while other sparticles are around $m_{\ast}$ as in the split SUSY ArkaniHamed:2004fb . It is also worth noting that the inclusion of two-loop corrections leads to small shift of the scale $m_{\ast}$, and does not change the qualitative features.

Under the condition Eq. (17), the three gauge couplings converge to a common value

[TABLE]

at a GUT scale

[TABLE]

For higgsinos much lighter than other sparticles, the GUT scale and the value of unified gauge coupling will get smaller. If the MSSM is embedded in a GUT, operators mediated by heavy gauge bosons around $M_{\rm GUT}$ would induce proton decay mainly via $p\to\pi^{0}e^{+}$ Hisano:2000dg . The experimental limits on proton lifetime are evaded for

[TABLE]

which is combined with the relations, Eqs. (Light Higgsino for Gauge Coupling Unification) and (19), to put an upper bound on the ratio between $m_{\rm susy}$ and $\mu$:

[TABLE]

for a simplified case where the wino, sfermions and heavy Higgs doublet have a similar mass about $m_{\rm susy}$. The constraint is satisfied in most of the parameter region of our interest. The gauge coupling at $M_{\rm GUT}$ increases if there are gauge messengers, enhancing the proton decay rate Hisano:2012wq ; Hisano:2015ala . As a consequence, the upper bound on $m_{\rm susy}/|\mu|$ presented above is reduced, for instance, by a factor of about 0.6 (0.2) for $N_{\rm mess}=1$ (3) and $M_{\rm mess}=10^{8}$ GeV. Here $N_{\rm mess}$ is the number of gauge messengers in ${\mathbb{5}}+\bar{\mathbb{5}}$ of SU$(5)$, and $M_{\rm mess}$ is their mass. Note that there are also model-dependent dimension-five operators leading to proton decay mainly via $p\to K^{+}\bar{\nu}$, which are induced by the exchange of colored Higgs multiplets Murayama:2001ur . The lifetime is approximately proportional to $\frac{M^{2}_{\rm GUT}}{\tan^{2}\beta}\frac{m^{4}_{\rm susy}}{M^{2}_{2}+\mu^{2}}$ for sfermions around $m_{\rm susy}$, and it follows that high scale SUSY with $m_{\rm susy}$ above 10 TeV and low $\tan\beta$ is favored to evade the experimental bound Hisano:2013exa .

For gauginos, sfermions and the heavy Higgs doublet around $m_{\rm susy}$, the unification condition Eq. (17) is reduced roughly to

[TABLE]

where we have kept the dependence on the ratio between the wino and gluino mass as it can be important. The above shows that the sparticle masses $m_{\rm susy}$ can be larger than $m_{\ast}$, i.e. above TeV, if the higgsinos are much lighter than other sparticles. The value of $m_{\rm susy}$ consistent with unification is further pushed up if the gluino is heavier than the wino Wells:2004di .

Let us examine if gauge unification works for the Higgs sector with the hierarchy of Eq. (7). Combined with gauge unification, the low energy gaugino masses have a distinctive and robust pattern Choi:2007ka in many mediation schemes including anomaly, gauge, gravity mediation and mixed mediations,

[TABLE]

at the one-loop level, whereas scalars have a quite model-dependent mass pattern. Here $\alpha$ represents the relative importance of anomaly-mediated contributions, and it is positive in many mixed mediation models Pomarol:1999ie ; Rattazzi:1999qg ; Choi:2011xt . Negative $\alpha$ is also possible but in rather involved models Okada:2002mv . From the gaugino mass pattern, it follows

[TABLE]

where one would need

[TABLE]

because pure anomaly mediation suffers from the tachyonic slepton problem. The gauge coupling ratio $g^{2}_{3}/g^{2}_{2}$ is equal to 3 around TeV, and it decreases to 1 as energy scale increases. For other soft SUSY breaking parameters, one obtains

[TABLE]

for $\kappa$ lying in the range

[TABLE]

The parameter $\kappa$ is much larger than order unity if anomaly and/or gauge mediation provide sizable masses to sparticles while generating $B$ at tree level. Finally, from the minimization condition, the value of $\mu$ appropriate for EWSB reads

[TABLE]

and it should not exceed much $m_{\rm susy}$. As noticed above, the value of $m_{\rm susy}$ consistent with gauge unification becomes higher than TeV for $|\mu|\ll m_{\rm susy}$, and is further pushed up if the gluino is heavy relative to the wino.

We now perform a simple numerical discussion of the sparticle spectrum required for EWSB and gauge unification. The EWSB relation Eq. (28) is combined with the unification condition Eq. (17) to uniquely fix the values of $\mu$ and $m_{\rm susy}$:

[TABLE]

for $\kappa\tan\beta\gtrsim 1$, and $\alpha$ of order unity. Here we have taken into account that low $\tan\beta$ is favored to accommodate the 125-GeV Higgs boson in high scale SUSY, for instance, $\tan\beta$ smaller than $4$ for $m_{\rm susy}$ above a few tens TeV Bagnaschi:2014rsa , and that one has $g^{2}_{3}/g^{2}_{2}=2$ around 100 TeV. We emphasize that high scale SUSY can be reconciled with gauge unification when the higgsinos are much lighter than other sparticles. For instance, EWSB and unification are achieved for $\mu$ around a few hundred GeV and $m_{\rm susy}=10\,$–$\,100$ TeV. If $M_{3}/M_{2}$ gets larger, the required value of $\mu$ and $m_{\rm susy}$ increase by the same factor.

Fig. 1 shows RG flow of gauge couplings in the MSSM. High scale SUSY with light higgsinos can lead to gauge coupling unification, where the three gauge coupling unify as precisely as in the conventional TeV SUSY. In Fig. 2, the shaded region is compatible with gauge unification. Here we have used the fact that the SUSY particle mass $m_{\rm susy}$ and the higgsino mass parameter $\mu$ are fixed according to Eq. (Light Higgsino for Gauge Coupling Unification) once the EWSB and unification conditions are imposed.

Finally we discuss dark matter and collider signs in high scale SUSY under consideration. The LSP, which is stable under $R$-parity conservation, is the higgsino or the gravitino. For $|\mu|\ll m_{\rm susy}$, the lightest neutralino and chargino are mostly pure higgsino, and are nearly mass degenerate:

[TABLE]

where the tree-level contribution is due to mixing with the bino and wino, and is positive unless the bino and wino mass have a different sign

[TABLE]

while the radiative mass difference comes mainly from gauge boson loops Thomas:1998wy , and is approximated by

[TABLE]

for $\mu$ below about TeV. Hence, the mass difference is expected to be positive and larger than the pion mass, for which the lightest chargino dominantly decays to the lightest neutralino and the charged pion. The decay time of the lightest chargino is about $0.3\times 10^{-10}{\rm sec}\times(\Delta m/300{\rm MeV})^{-3}$ for $\Delta m$ not close to the pion mass. It would thus be difficult to probe at the LHC, but $e^{+}e^{-}\to\gamma\chi^{0}_{1}\chi^{0}_{2}$ or $\gamma\chi^{+}_{1}\chi^{-}_{1}$ mediated by virtual $Z$ boson may provide a visible signal in future linear colliders.

We first examine the gravitino LSP case, $m_{3/2}<|\mu|$. In this case, the gravitino production from thermal scatterings can generate the right dark matter density. If the freeze-out temperature of the gravitino Fujii:2002fv

[TABLE]

is higher than the reheating temperature $T_{\rm reh}$ after inflation, the gravitino relic abundance is determined by

[TABLE]

where the gravitino should be heavier than about $100$ keV to be a cold dark matter Bolz:2000fu . The reheating temperature producing the observed dark matter density can be higher than about $10^{9}$ GeV as required for standard thermal leptogenesis Fukugita:1986hr . One should however note that the next to lightest supersymmetric particle (NLSP), which is the neutral higgsino, decays into the gravitino and ordinary particles with a width

[TABLE]

and so it occurs during or after the BBN epoch in the parameter region of our interest while producing high energetic electromagnetic and hadronic showers. Such late-time decay of the NLSP can significantly alter the abundances of light elements, spoiling the success of BBN. A simple way to avoid this cosmological difficulty is to consider $R$-parity violation. One possibility is to add $R$-parity violating terms that violate the lepton number as well but preserve the baryon number to forbid dangerous proton decay operators Takayama:2000uz ; Buchmuller:2007ui . For instance, $\Delta W=\mu_{i}L_{i}H_{u}$ with $\frac{\mu_{i}}{\mu}\tan\beta$ larger than about $10^{-12}$ can allow the NLSP to decay very shortly into ordinary particles while making the gravitino live long enough to make up the dark matter of the universe. Note that one needs $\frac{\mu_{i}}{\mu}\tan\beta\lesssim 10^{-5}$ to avoid washout of baryon asymmetry before the electroweak phase transition Buchmuller:2007ui ; Endo:2009cv .

Let us move on to the case of $m_{3/2}>|\mu|$ with $R$-parity conservation, for which the LSP is the neutral higgsino. The LSP thermal relic density is significant only for $\mu$ above 1 TeV. For smaller $\mu$, the right dark matter density can be generated via non-thermal LSP production. Here we consider a scenario where gravitinos are abundantly produced from the decay of a heavy scalar field such as inflaton, Polonyi field, or string moduli. The gravitino decay width reads

[TABLE]

for $m_{3/2}\gg m_{\rm susy}$, and it corresponds to the decay temperature

[TABLE]

where $g_{\ast}$ counts the effective number of relativistic degrees of freedom. Thus, LSPs are produced below the LSP freeze-out temperature $\sim|\mu|/20$. If the gravitino abundance is large enough to make annihilation among produced LSPs effective, the LSP relic density becomes independent of the initial gravitino abundance Jeong:2011sg ; Olive:1990qm :

[TABLE]

where $c_{Z}\equiv(1-m^{2}_{Z}/|\mu|^{2})^{3/2}/(2-m^{2}_{Z}/|\mu|^{2})^{2}$, and $c_{W}$ is similarly defined by taking $m_{Z}\to m_{W}$. Note that the gravitino should be heavier than about 40 TeV to decay before nucleosynthesis, and its mass is bounded from above, $m_{3/2}\lesssim 8\pi^{2}m_{\rm susy}$, because anomaly mediation is a model-independent source of sparticle masses. The direct detection of the higgsino dark matter would be challenging since it has only small couplings to the SM Higgs boson and $Z$ boson suppressed by $m_{W}/M_{1,2}$, making both spin-dependent and independent scatterings too small to be detected by current experiments. However, indirect detection via the process $\chi^{0}_{1}\chi^{0}_{1}\to\gamma\gamma$ or $\gamma Z$ may be possible in future experiments.

Fig. 3 shows the region where the right dark matter density $\Omega_{\rm DM}h^{2}=0.12$ is obtained. If the neutral higgsino is the LSP, one can consider non-thermal production of higgsinos from heavy gravitino decays. On the other hand, in the case of a gravitino LSP, gravitino production by thermal scatterings can yield the right relic density.

We have studied gauge coupling unification and dark matter in high scale SUSY where sparticles have masses much higher than the weak scale as would be indicated by tensions between low energy SUSY and the LHC results. High scale SUSY admits gauge coupling unification as exactly as in low energy SUSY if the higgsinos are much lighter than those obtaining SUSY breaking masses. In this scenario, the LSP is the neutral higgsino or the gravitino, which can make up all the dark matter of the universe if produced non-thermally in the former case and thermally from sparticle scatterings in the latter case. A large Higgs mixing parameter required for EWSB is naturally obtained in models where sparticle masses are generated at loop level while the Higgs mixing parameter arises at tree level, as is the case in anomaly and gauge mediation. Then, gauge coupling unification and dark matter would indicate high scale SUSY around 10 TeV – a PeV and light higgsinos below a few TeV.

Acknowledgment

The author thanks to Bumseok Kyae and Fuminobu Takahashi for useful discussions. This work is supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MSIP) (NRF-2015R1D1A3A01019746).