Future Experimental Programs
Hitoshi Murayama
Department of Physics, University of California, Berkeley, California 94720, USA
Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley,
California 94720, USA
Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai
Institutes for Advanced Study, University of Tokyo, Kashiwa 277-8583, Japan
E-mail: hitoshi@berkeley.edu, murayama@lbl.gov, hitoshi.murayama@ipmu.jp
Abstract. I was asked to discuss future experimental programs even though I’m atheorist. As a result, I present my own personal views on where the field is, and where
it is going, based on what I myself have been working on. In particular, I discuss why
we need expeditions into high energies to find clues to where the relevant energy scale
is for dark matter, baryon asymmetry, and neutrino mass. I also argue that the nextenergy frontier machine should be justified on the basis of what we know, namely themass of the Higgs boson, so that we will learn what energy we should aim at once wenail the Higgs sector. Finally I make remarks on dark energy.

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1. Introduction
The discovery of a “Higgs-like particle” on July 4, 2012 was a truly historic momentin the history of science [1, 2]. Many of us in the United States watched the seminarat CERN over webcast in the midnight hours. Given that it was announced on the
Independence Day of the United States, we celebrated the Higgsdependence Day in theearly morning.
So far, what we’ve seen looks minimal . Later, a CERN announcement made inMarch 2013 said it is a Higgs boson. Indeed, the newly discovered particle looks verymuch like the Standard Model Higgs boson. We’ve been after this particle ever since
1933 when Fermi wrote his theory of nuclear beta decay. There, he introduced a constantG ≈ 10−5 m−2
p which we now call the Fermi constant GF . It corresponds to the energy−1/2≈ 300 GeV, and we learned from him that something is going on at thisscale GF
energy scale. It took a whopping eighty years to come to the point where we now
have a UV-complete theory of strong, weak, and electromagnetic forces with all of theparameters measured. In fact, it is a renormalizable and consistent theory that may bevalid all the way up to the Planck scale. Coincidentally, even cosmology looks minimal
given the Planck data [3], which suggests a minimal single-field inflation. Maybe theyear 2013 will be remembered in history as the year of elementary scalars.
Despite this achievement, or rather because of it, there is a building anxiety in thecommunity. How come we don’t see anything else? Will the progress stop? There is nosign of physics beyond the Standard Model in the LHC data. For a typical search forsupersymmetric particles, for example, squarks and gluinos are excluded up to 1.3 TeV
or so. On the other hand, the conventional arguments based on the naturalness concept
suggested that we should have new particles that stabilize the electroweak scale below
TeV. It appears that “natural and simple” models have been excluded (Fig. 1). Then
we have two directions to go in: the less natural, namely fine-tuned, or the less simple,
namely contrived. At the same time, theorists are trying to come up with models thatcan evade the current experimental limits, pushing back on this problem. See Appendix
A for my own recent attempts.
I have to point out, however, that certain levels of fine-tuning do occur in nature.
All examples I’m aware of, with the glaring exception of the cosmological constant, areat most at the level of a few per-mille. The current LHC limit has not quite reachedthat level; the next runs at 13–14 TeV may well reveal new physics as we hoped for. I
will come back to this question later in this talk.
In any case, it is true that experimental limits have started to haunt theorists.
Theorists used to complain that the experiments had a hard time keeping up with their
new ideas. Now the tide has reversed. Theorists are being threatened by new data. I
believe this is quite a healthy field!
Nonetheless, having a fully UV-complete theory of the Minimal Standard Model,
now supported by the new particle that has been discovered, makes us ask the following
question:3

per-mille
theoristsedludnatural& simpleexc

fine-tuned

Future Experimental Programs Murayama

contrived
Figure 1. Schematic constraints on space of theories.

2. Is particle physics over?
On this question, fortunately, the answer is a resounding no. Since 1998, we havediscovered five pieces of empirical evidence for physics beyond the Standard Model
thanks to tremendous progress in experiments.
First, non-baryonic dark matter. Even though dark matter had been discussed since1930’s by Fritz Zwicky, it was not clear whether dark matter would be dark astronomical
objects or hidden baryons. This issue was completely settled in 2003. The search fordark astronomical objects (MACHOs = Massive Compact Halo Objects) excludes thepossibility that Galactic halo consists solely of MACHOs between about ×10−7 M and
10M [4]. On the other hand, the power spectrum in the Cosmic Microwave Background(CMB) anisotropy by WMAP (Wilkinson Microwave Anisotropy Probe) excludes thebaryonic dark matter completely as a discrepancy between the overall matter densityΩM h2 = 0.14 ± 0.02 and the baryon density Ωb h2 = 0.024 ± 0.001 [5]. We are learning
what dark matter is not, but not what it is. In fact, we know so little that the only
model-independent lower limit on the dark matter mass comes from the requirementthat its “Bohr radius” in the gravitational potential must fit within the galactic scale[6]. Combined with the MACHO search, we managed to narrow down its mass from10−31 GeV to 1050 GeV, i.e., to within 81 orders of magnitude. Zwicky must be happy
to see our progress! Thus, we need to keep our minds very open about the nature ofdark matter.
The flavor oscillation of neutrinos, and hence their finite masses, is not a part of
the Minimal Standard Model either, arguably the first established physics beyond theStandard Model in 1998 [7], revealing the mixing angle θ23 . Later on, the oscillation (orrather lack of it as a result of the matter effect) of solar neutrinos [8] and oscillation ofreactor neutrinos [9] pointed to the same parameter set (and the angle θ12 ) in 2002
resolving a puzzle that goes back half a century. The final mixing angle θ13 wasdiscovered in 2012 [10]. Some people think it is only a minor extension of the Standard
Model, but it should be emphasized that we don’t yet know how it should be extended.

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The accelerated expansion of the Universe came as a big surprise to all of us [11, 12].
Its cause is now called dark energy, even though we are very far away from understanding
what it is. It may be cosmological constant, due to a miraculous cancellation between
quantum fluctuation of the vacuum and a classical constant energy density for 120 digits.
It may be some dynamical substance called quintessence. Either way, it is very difficult
to understand its overall amount.
At the same time, the observed apparently acausal density fluctuations in the CMB
cannot be explained by the Standard Model. The CMB photons that came from one
end of the Universe have just reached us; they seem to be correlated with the CMB
photons that came from the other end, when they have had no chance to meet and set
up their temperatures. This is what I mean by acausal . The best explanation is thatthey were in fact in causal contact early on because the entire visible Universe was muchsmaller than a nucleus; it was later stretched to a macroscopic size by an exponential
expansion called inflation. The latest Planck data strongly supports this idea [3]. We
normally assume that it was caused by a scalar field called the inflaton rolling slowly
down the hill, but we don’t know what it is, nor how it couples to the Standard Modelparticles.
Finally, once we accept the inflationary paradigm, the cosmic baryon asymmetry
ηb = nb /nγ ≈ 5 × 10−10 cannot be assumed to be the initial condition of the
Universe. This is because the enormous exponential expansion (normally assumed
to be more than e60 ) wipes out any pre-existing asymmetry. This implies that thebaryon asymmetry needs to be created after the inflation by a microphysical process.
On the other hand, the CP violation in the Standard Model is now known to beincapable of producing enough baryon asymmetry. This is because that we now haveunderstood the known CP violating phenomena by the Kobayashi–Maskawa theory
thanks to the B-factory experiments starting in 2001 [13, 14]. This means that
the Standard Model cannot generate the baryon asymmetry larger than the Jarlskog
invariant J = =m(T r[Yu† Yu , Yd† Yd ]) ≈ 10−20 [15], further suppressed by small efficiencies
or powers of coupling constants in known mechanisms.
So, it is clear that particle physics is far from over. There are at least five importantpieces of data that are crying out to be explained and understood. The catch is that
we don’t know the energy scale of physics relevant to these mysteries. Right now weare on fishing expeditions. In particular, we are and will continue to be looking for new
phenomena and new sources of CP violation in the quark sector (LHCb, SuperKEKB,
rare kaon decays), lepton sector (neutrino oscillations, neutrinoless double-beta decay,
and electric dipole moments), and their combination (proton decay). We try to cast awide net, hoping to catch any interesting fish, so that we learn where the next importantenergy scale is. In a sense, this is what Fermi succeeded in doing; by observing rare
phenomena of nuclear β-decays, which violate conservation law of neutron and proton
numbers that all other known forces respect, they were caught in the net and we learned
about the Fermi scale.
Whatever the next energy scale beyond the Standard Model is, it plays the role

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lepton flavor
quark flavor
dark matter
LHC
Tevatron
102

104

UnifiedTheories

proton deay
neutrino

106 108 1010 1012 1014 1016 1018
experimental reach [GeV](with significant simplifying assumptions)Figure 2. Approximate energy reach for expeditions. Solid arrows indicate the current
reach, while the dashed arrows anticipated improvements by proposed experiments [16].

of the UV cutoff of the Standard Model as a low-energy effective field theory. And
the effects of the UV cutoff can be parametrized by higher dimension operators power
suppressed by ΛU V added to the Standard Model,
11
L5 + 2 L6 + · · ·L = LSM +
(1)
ΛU V
ΛU V
We need to first look at the Standard Model Lagrangian LSM which has the structure
as shown on T-shirts from CERN designed by John Ellis,
1 2θLSM = − 2 Fµν+ ψ̄i6Dψ + |Dµ H|2 − y ψ̄ψH +F F̃ − λ(H † H)2
g64π 2+ µ2 H † H − ΛCC .
(2)
The first line here has only dimensionless parameters and is only logarithmically sensitive
to the physics at ΛU V . On the other hand, the last line has two parameters µ2 (massdimension 2) and ΛCC (4) and remember physics at ΛU V , the origin of the naturalness
problems we will come back to later.
On the other hand, the power-suppressed operators come in a great variety. For
instance, those suppressed by two powers can be
L6 = QQQL, L̄σ µν Wµν Hl, abc Wνaµ Wλbν Wµcλ , (H † Dµ H)2 , Bµν H † W µν H, · · ·(3)They may be seen in proton decay, gµ −2, triple gauge boson vertex, T and S-parametersin the precision EW observables, respectively.
It is interesting to note that there is actually only one-type of operator we can write
suppressed by a single power,
L5 = (LH)(LH).

(4)

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After substituting the expectation values for the Higgs field, it is nothing but the
Majorana neutrino mass operator,
v2
1
L5 =
νν.
(5)
ΛU V
ΛU V
In other words, the neutrino mass can be viewed as the leading order effect of the physics
beyond the Standard Model!
The neutrino mass is actually a tiny effect. Any kinematic effect is suppressed by
2mν /Eν2 ≈ (0.1eV/GeV)2 ≈ 10−20 ! Normally we don’t think we can be sensitive to sucha small number in experiments. However, there is one known technique that is sensitive
to very small numbers: interferometry, like in the Michaelson–Morley experiment. For
this to be possible, there are three conditions: a coherent source, a long baseline, andinterference. For some unknown reason, nature was kind enough to provide us with all of
the three necessary conditions. Because neutrinos interact so little, neutrinos maintaintheir coherence after propagation over long distances, coming from the Sun, cosmic
rays, supernovae, accelerators, and reactors. These sources are naturally associatedwith rather long baselines. And most remarkably, significant interference effects requirelarge mixing angles, which happened to be the case with neutrinos! Looking at it
this way, it may not be a huge surprise that the neutrino oscillation was the firstconcrete evidence for physics beyond the Standard Model. In other words, the neutrino
interferometry (a.k.a. neutrino oscillation) is a unique tool for studying physics at very
high energies, already probing up to Λ ≈ 1014 GeV. Because of this line of argument,
I’m a big fan of neutrino physics–so much so that I participated in the KamLAND
experiment [17] spending some time building the detector, taking shifts, and serving on
paper committees.
One sometimes hears the criticism that flavor physics experiments, quark, charged
lepton, or neutrinos, have done little to improve our understanding of the underlying
physics, compared to those experiments that focused on forces that led to the gauge
theory and the Englert–Brout–Higgs mechanism. Indeed, we’ve known the pattern ofquark masses and mixing angles already for some time, with no clear standard theory
behind them.
We can, however, at least ask a question: does the patten of masses and mixings
require a new structure or symmetries beyond what we know? I claim that we cananswer this question.
I proposed the idea called anarchy, namely that the neutrino masses and mixings do
not require any new symmetries to be understood, with Lawrence Hall and Neal Weiner[18]. If there are no symmetries or quantum numbers that distinguish three generationsof neutrinos, the neutrino mass matrix would consist of nearly random comparable
numbers without a particular structure. We can understand their consequences basicallyby throwing dice. It actually leads to a definite prediction for the mixing angles: theprobability distributions are given by the Haar measure of the compact groups, theunique measure that is invariant under both left- and right-translations [19]. Thenthe distributions in xij = sin2 2θij turn out to be the same for all three angles,

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θ23

θ12
θ13

0.2

0.4

0.6

0.8

1

sin2 2θFigure 3. Left: Prediction of random matrices for the neutrino mixing angles. Right:
consequence of anarchy on the baryon asymmetry of the Universe via the thermal
leptogenesis scenario.

, peaked at the maximal mixing x = 1. Given this, it is not surprising
P (x)dx = 12 √dx
1−xthat the neutrino oscillation was first discovered at the peak x23 ≈ 1, then somewherearound the middle of the distribution x12 ≈ 0.86, and finally somewhat down the tailx13 ≈ 0.09 (Fig. 3 Left). In fact, André de Gouvêa and I did a Kolgomov–Smirnov test[20] to see if the one draw made by nature is consistent with this probably distribution,and found that it is 47% probable [21]! So we learned indeed that the neutrino masses
and mixings do not require any deeper symmetries or new quantum numbers. On theother hand, quarks clearly do need additional input, which is yet to be understood.
The idea can be extended to the sector of right-handed neutrinos by assuming thatthey have a hierarchy akin to those in the charged leptons or quarks, 2 :  : 1. We take ≈ 0.1. With this structure, we can randomly generate the full left- and right-handed
neutrino mass matrices. Xiaochuan Lu and I identified that the Gaussian measure is theunique choice based on a certain set of criteria, and found that the baryon asymmetry
comes out extremely well (Fig. 3 Right) [22]. This is encouraging; in particular it ispromising that the anarchy predicts that the distribution in the CP-violating effectwould peak at sin δ = ±1 (or flat in δ).
In fact, the CP violation in neutrino oscillation is the holy grail in neutrino
experiments currently being planned and discussed. A possible CP violation (assuming
no matter effect) is given in terms of a product of many factors,
P (νµ → νe ) − P (ν̄µ → ν̄e ) = − 16s12 c12 s13 c213 s23 c23∆m212 L
∆m213 L∆m223 Lsin δ sin
sin
sin
. (6)
4E
4E
4E
It is remarkable that all factors are now found to be large enough to make this searchfeasible, the only unknown being the size of the CP violation sin δ itself. Nature seems
kind to us once again! It was also interesting to learn at this symposium that beyond the
LBNE in the US and HyperK in Japan, there is a new discussion to use the European
Spallation Source in Sweden with a much shorter baseline to look for CP violation [23].
Coming back to dark matter, there is a big ongoing effort on Weakly Interacting

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Massive Particle dark matter experiments from underground, cosmic, and accelerator
experiments [24]. If the bet is right, we may see great discoveries sometime soon!
I argued that expeditions are needed to find where the next important energy scale
is to solve the five mysteries. On the other hand, so-called energy frontier experiments,
namely those that rely on high-energy colliders, target a rather specific energy scale.
This leads us to ask the next question.
3. Is the Energy Frontier Dead?
The mantra in particle physics is to go to as high energy as technology (and money)
allows. We are indeed going up a notch in 2015, restarting the LHC at 13–14 TeV.
This is already exciting, improving reach on new particles by a factor of two. HighLuminosity LHC (HL-LHC) would further improve the reach by 20–30%. We still havequite a bit of room for discoveries. More recently, there are discussions about a potential
100 TeV pp collider with a much bigger tunnel around CERN.
However, I see a problem arguing for the next much higher energy machine now.
Given that the discovery of the Higgs boson made the theory apparently complete, andthe five mysteries I discussed have not yet set particular energy scales, I don’t know how
we can justify the energy of the next machine. Does this mean that there is no case we
can make to build another high-energy collider? Is Energy Frontier dead?
It remains true that the best argument we have right now to expect new physics in
the TeV range is the naturalness: we would like to avoid fine-tuning between the barem2h and the radiative correction (see, e.g., [25] for a plot). Even though many in thecommunity are ditching the naturalness altogether, I still take the argument seriously
because it has worked many times before.
One example I always bring up is the discovery of the positron [26, 27]. Inclassical electrodynamics, the Coulomb self-energy of the electron is linearly divergent,2∆me c2 ∼ ere , where re is the “size” of the electron. It would have required a finecancellation between the “bare” mass of the electron (which must be negative by theway) and the correction to yield a small mass me c2 = 0.511 MeV. However, the discoveryof the positron and quantum mechanics told us that the vacuum is always fluctuating,producing a pair of e+ e− , that annihilates back to the vacuum within the time allowedby the uncertainty principle ∆t ∼ h̄/∆E = h̄/2me c2 . When you place an electron inthis fluctuating vacuum, it may find a (virtual) positron near it and decide to annihilate
it. Then the other electron that was originally in the vacuum fluctuation is now leftout and becomes a “real” particle. It turns out that this process cancels the linear
divergence exactly, leaving only a logarithmic divergence ∆me c2 = 3αlog meh̄cre . Even
4π
for an electron as small as the Planck distance, it amounts to only 9% correction. The
cancellation is guaranteed by a (softly broken) chiral symmetry. You can see that thenaturalness problem was solved by doubling the number of particles!
The idea of supersymmetry was pushed to repeat the history. Because the Higgs
2
boson must repel itself, it also has a divergent self-repulsion energy ∆m2H ∼ λ/rH.

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But by doubling the number of particles (namely introducing superpartners), there is acancellation between the self-repulsion among Higgs bosons, and the induced attraction
arising from the loop of higgsinos (fermionic partner of the Higgs boson). Again, theh̄
12
correction is down to a logarithmic divergence, ∆m2H ∼ (4π)
2 mSU SY log( m cr ).
H H
In the case of the electron, new physics (positron) appears “early” at the Compton
wave length h̄/me c ≈ 400 fm well before we get down to the smaller “classical radiusof electron” rc = e2 /me c2 ≈ 1 fm where the theory becomes fine-tuned. In anotherwell-known case, however, nature did fine-tune it so that the discovery was delayed.
The example is COBE (Cosmic Background Explorer) [28] that discovered the CMB
anisotropy. People expected anisotropy at the level of 10−5 so that the observed largescale structure can be explained. But the search went on, so much so that people started
writing articles questioning the inflationary cosmology itself. When COBE discovered
the quadrupole moment, it was small. Actually, compared to our best prediction today
based on the WMAP data, it was nearly an order of magnitude smaller than theory.
This is usually understood today as a consequence of cosmic variance, namely that thequadrupole moment has only 2l + 1 = 5 numbers to be measured and hence is subject√
to a statistical uncertainty of O(1/ 5). I find the observed quadrupole moment to befine-tuned at the 2% level.
Note that the inflation was invented to solve the naturalness problems, horizon
problem and flatness problem of the standard Big Bang cosmology. It worked: thecurrent data beautifully confirm predictions of inflation. But it was a little fine-tuned
and it required patience and more work.
So the moral I draw from these examples is that the naturalness argument generally
does work. But there are cases where fine-tuning at the level of a few percent or evenfew per-mille (some examples in nuclear physics are well-known, see [29]). Looking backat Fig. 1, we have not fully explored down to that level of not-that-fine-tuning yet. And
it took ten years for Tevatron to discover top. Patience pays, hence my optimism.
But it is true that it is a slippery slope how much fine tuning we tolerate. Percent?
Per-mille? 10−6 ? It is quite subjective or matter of taste, and we cannot firmly set theenergy for the next collider based on this argument with any confidence. Back to thequestion again: is there any justification for the next high-energy collider?
I believe there is. The Higgs boson is the only newly discovered particle at the LHC
so far, but it is clearly an unusual particle. And we know what energy is required to
study it already, because we know its mass. We know where to look.
What is unusual about the particle discovered? To the extent ATLAS and CMS
have managed to study it so far, it is consistent with J P C = 0++ . It has no spin! We
have never seen an elementary spinless particle before, so this looks like a new breed.
Matter particles like quarks and leptons come in three generations, and we seem tounderstand their context. That is, they look familiar, they are siblings, and are a partof a big family. Same with the force particles. They all belong to some kind of gauge
group. Even though the groups differ, they follow the same principle. Again, they haverelatives, and have context. But the Higgs boson is totally different. It is one of its

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10kind, with no context within the Standard Model. That means that we introduced akind of particle nobody has seen before. It is a faceless (spinless) intruder to our happy
family. Yet it is supposed to do the most important job in the theory. The whole idea
looks so artificial!
In fact, I couldn’t believe the artificial aspect of the Standard Model at all when
I studied it back in grad school, so I became one of the guilty ones to propose the
Higgsless theories [30]. But this idea now appears dead .
Facing its existence, we are still puzzled by another question. The closest analogy wehave in familiar systems is the superconductivity we can study in the laboratory. Insteadof giving mass to W and Z-bosons, superconductivity gives mass to the photon. In otherwords, due to the Meissner effect, the magnetic field is repelled by the superconductor,
allowing it to enter only by a finite distance (the penetration depth). The magnetic field
is short-ranged inside the superconductor! This case, however, is well understood. It iscaused by the instability of Fermi surface when electrons are attracted to each other by
a weak force from the phonon exchange. Cooper pairs condense, making the magnetism
short-ranged. On the other hand, the Standard Model does not tell us why the Higgs
boson condenses in our Universe. This is not only artificial, it is unsatisfying.
There are ideas to give context to the spinless Higgs boson. There may be many
siblings and relatives. The Higgs boson is just one among the big spinless tribe, ome
which happens to condense because of an attractive force induced by the top-quark
loops. This idea is known as supersymmetry. An additional Higgs doublet is its sibling,
and there are many other spinless squarks and sleptons, that are its relatives. On theother hand, it may be composite, just like spinless pions are made of spin 1/2 quarks.
In this case a new dynamics would be required to bind the constituents together. Or
the Higgs boson may actually be spinning, but if it does in extra dimensions we cannot
see, so we perceive it to be spinless. In such a case, the Higgs boson may actually bea gauge boson or even graviton. These are all familiar ideas we discussed for solving
the naturalness problem. Here I’m not using the naturalness argument at all; but I
still come back to a similar set of ideas, namely that there are good reasons to continue
discussing these ideas.
Then, what should we do? Of course, we should study this intruder as much as wecan! If we look closely enough, maybe we can tell it it has siblings or relatives. We mayfind it has a finite size. Or we may bring it back to spin in our dimensions.
Fortunately, the observed mass of 125 GeV is the best case scenario. It allows us
to measure branching fractions to bb̄, W W ∗ , ZZ ∗ , gg, τ + τ − , cc̄, γγ, Zγ, possibly evenµ+ µ− . Some of them would not be accessible if the Higgs were lighter or heavier by justa few tens of GeV. It is actually a dream case for experiments!
Looking back at the history of collider experiments, precision measurements using
leptons often revealed the next energy scale; we went up there with hadrons, and weindeed found new things, which we further studied with lepton probes. One full cycle isthe precision measurements of neutral currents in polarized electron deuteron scattering
at SLAC. The measured sin2 θW predicted the masses of W and Z. Spp̄S was built toFuture Experimental Programs Murayama

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discover them, which indeed did. After that LEP was built to study them precisely andwe nailed the gauge sector of the Standard Model.
The next cycle starts with LEP predicting the top quark and Higgs boson masses.
Tevatron and LHC were built for this purpose, and as we know, thy did discover thepredicted particles. The obvious thing to do next is to study them precisely to nail the
top and Higgs sector at another lepton machine.
If the history is any guide, the future precision measurement of the top and Higgs
sector would tell us the next energy scale we should go after. We are on a scavenger
hunt. The Higgs boson discovered is a lamp post, we need to look carefully at what’s
under it, and hope to find a clue to the next destination.
Another reason why the precision study of the Higgs boson is exciting is that the
Higgs boson may be a portal to a new sector outside the Standard Model. It may, forexample, be a sector of the dark matter particle. To probe an operator O (with massdimension d) in the new sector, we need its coupling to the Standard Model particles. As
we discussed before, all operators in the Standard Model are of dimension four, except
2,
for the Higgs mass-squared. Therefore the couping is suppressed as e.g., Λd1 OFµν
UV

1OH † H. Thus the coupling to the Higgs iswhile the coupling to the Higgs goes as Λd−2
UVenhanced by Λ2U V relative to other operators. The Higgs boson may be the window to
the new world.
In addition, once we build a new lepton collider to study Higgs and top precisely, we
can still hope that it discovers new particles directly. It is not true that LHC excluded
everything below TeV. Even a slepton of, say, 150 GeV is still allowed if it decays intoa neutralino heavier than 80 GeV or so. LHC will improve limits to heavier sleptons,
but not much to close the gap when their masses are close.
Given this, I’d think the strategy is clear. We start with what we have got. We
build a lepton collider that can study the top quark and Higgs boson precisely. This
will be an evolutionary program, starting with the Zh threshold, measuring branching
fractions and couplings to Z, W , b, c, τ , g, γ, even the decay into invisible particles.
Then on to the tt̄ threshold to study the top quark compositeness, say, going up further
in energies to make use of new processes such as W W -fusion, tt̄h production for ytth ,and multiple Higgs production for λhhh . But we should keep our eyes open to thepossibility that we may also discover new particles along the way. Just in case we
obtain a new piece of information on new particles from the LHC, the lepton collider
should be extendable. If we do see new particles, we should have the capability of
studying them in model-independent way, and to determine their quantum numbers,
spins, masses, and couplings. The machine should be one that we know how to build,so that we can propose it as soon as an opportunity presents itself.
The planned International Linear Collider (ILC) fits this bill very nicely, and its
scientific case was judged very strong in the European Strategy document adopted by
CERN Council in May [31]. The technology required for this is mature, thanks to the
Global Design Effort (GDE) led by Barry Barish that finished the Technical Design

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Figure 4. Top: The cross sections for producing pairs of right-handed slectron vs lefthanded selectron for various beam polarizations [34]. Bottom: s-channcel production
processes for new particles with polarized electrons.

Report (TDR) this year [32]. It is extendable, so that we can increase the energy
if needed and affordable. In addition, the longitudinal beam polarization provides a
crucial tool. The bottom diagrams in Fig. 4 show that different electron polarization
has different gauge bosons in the s-channel. At these energies, we can neglect m2Z  s
as an approximation. Then the gauge bosons exchanged are either U (1)Y gauge boson
Bµ , or the neutral SU (2)L gauge boson Wµ0 . The right-handed electron is a singlet underSU (2)L (the subscript L stands for left-handed), and does not couple to Wµ0 . Therefore,
the s-channel production goes as |g 0 Yf |2 and directly measures the hypercharge Yf of
the new particle f . On the other hand, the left-handed electron couples to both, andthe cross section goes as |g 0 Yf + gI3f |2 . Knowing Yf , we can determine I3f modelindependently. One can see how much the cross sections vary depending on the beampolarization in the top plot of Fig. 4.
There are many studies of spin and mass measurements, which can be done evenwhen particles decay into invisible particles. Combination of the LHC and ILC data may
allow us to even compute the cosmological abundance of the invisible particle, possibly
verifying that it is the dark matter of the Universe [33].
But isn’t ILC too expensive to be ever built? Through some miracle, many
politicians in Japan are interested in hosting the ILC as a global project. They would
like to open up the country to talented, intellectual people from abroad. They would
like to find prestige in hosting highly visible large international project. They also
want to use the ILC to build up infrastructure, a technological base, and they hope toFuture Experimental Programs Murayama

13

find economic benefits. More than 20% of the Diet members signed up to support the
ILC, in a group named Federation of Diet Members for Promotion of the ILC . When
Lyn Evans visited Japan in March, the prime minister Shinzo Abe agreed to meethim [35], and he said that he appreciated the significance of the ILC as “a dream forhumankind.” His opening address in the 183rd session of the Diet mentioned advanced
accelerator technology as one of the innovation areas in which he wants Japan to excel[36]. There are many industry associations actively supporting the ILC; the media ishighly interested as well. And the discovery of the Higgs boson has fueled interest evenfurther. I’d think there is a high enough level of interest for the Japanese government toinitiate discussions with other potentially interested countries to form an internationalframework for a global ILC project hosted in Japan. I am not absolutely sure; but it
doesn’t look impossible so far.
Having discussed expeditions to high-energy scales, and precision studis of the Higgs
and top to identify the next energy scale(s), there are plenty of things that we can andwill do in the near future in our field. However, it still leaves one question that has beenhaunting me.
4. Do we ever understand Dark Energy?
Dark Energy is such a big mystery that I cannot gauge how we may ever understand it.
Does this mean that it is useless to try to measure its properties precisely?
I don’t know. But all I can say is that a percent-level or better measurement iswhat I consider precise. If the equation of state parameter w ≡ p/ρ = 0 ± 0.01, I may
give up and say it is the cosmological constant, accidentally small in a landscape of 10500
universes. But it may turn out to be w = 0.05 ± 0.01, pointing us in a new direction. I
believe that it is worth the try.
I lead a major dark energy experiment called SuMIRe (Subaru Measurement of
Images and Redshifts) [37]. It combines imaging and spectroscopy on the 8.2m-diameter
Subaru telescope, a major step up from the wildly successful SDSS (Sloan Digital Sky
Survey) [38]. The first stage is the approved imaging survey with Hyper Suprime-Camfor 300 nights, with nearly 0.9 billion pixels with a field of view of 1.7 square degrees.
It will image hundreds of millions of galaxies. The next stage is a spectroscopic survey
with the Prime Focus Spectrograph for (hopefully) 300 nights, with 2400 optical fibers,
controlled robotically, being targeted at galaxies chosen from the imaging survey. For
instance, it will yield a model-independent measurement of the evolution of the darkenergy fractions as a function of the redshift (left Fig. 5) and provide a test of generalrelativity at cosmological distances (right Fig. 5).
We should do what we can do, and we will see what we find!

Future Experimental Programs Murayama

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Figure 5. Left: Projected accuracy in measuring ΩDE (z) using PFS on Subaru
telescope. Right: Test of general relativity on cosmological distances using the growthrate of structure. Both taken from [39].

Appendix A. Pushing back on fine-tuning
Take supersymmetry. There are two issues facing the experimental data. The first one
is that the mass of the discovered Higgs boson mh is a little too high within the MSSM,
which predicts mh ≤ mZ at the tree-level. Even though the Higgs mass can be pushed
up by the radiative correction as
m m
3 4 2
ht v log t̃1 2 t̃2 ,(A.1)
m2h ' m2Z +4π
mt
it would require a large scalar top mass, which would feed into the radiative correction
to the Higgs mass-squared term
h2t
ΛU V
m2t̃ log
.
(A.2)
2
16π
µIR
Therefore, a larger physical Higgs mass in the MSSM indirectly implies exponentiallyworse fine-tuning in m2Hu between the bare parameter in the Lagrangian and theradiative correction above.
This can be avoided if there is an additional contribution to the Higgs self-coupling,such as in the massive NMSSM W = λSHu Hd + 21 M S 2 . However the contribution
decouples in the limit M  mh as∆m2Hu ' −12

λ2 = 1 −M2.
M 2 + m2S

(A.3)

This can be prevented for a large soft mass m2S  M 2 as a non-decoupling effect [40],
ΛU V
1
2 2
but m2S then feeds into ∆m2Hu = 16π, re-introducing the fine-tuning.
2 2λ mS log µIR
Together with Xiaochuan Lu, Josh Ruderman, and Kohsaku Tobioka, we’ve
come up with an idea that we call semi-soft supersymmetry breaking [41]. Using
the NMSSM (Next-to-Minimal Supersymmetric Standard Model) of the Dirac-type,W = λSHu Hd + M S S̄, the singlet field S̄ couples to the rest of the model only
through a dimensionful coupling M . It can then be proven that the limit m2S̄ → ∞Future Experimental Programs Murayama

15

Figure A1. Degree of fine-tuning in Dirac NMSSM that shows it can be as good asa factor of six even when mS̄  mh . Taken from [41].

does not re-introduce fine-tuning (Fig. A1) even though it looks like a hard breaking ofsupersymmetry, hence semi-soft.
The second problem with supersymmetry is its non-observation in direct searches.
It is well-known that a quasi-degenerate spectrum among supersymmetric particles
makes the search difficult because of small Q-values in decays and hence small E
6 T(see, e.g., [42]). However, such a spectrum lacked theoretical motivation: in particular,
why should scalars and gauginos be degenerate?
Together with Yasunori Nomura, Satoshi Shirai, Kohsaku Tobioka, I proposed thatsupersymmetry broken by boundary conditions in extra dimensions would automaticallygive the same mass to all gauginos and sfermions at the tree-level split only by loop
effects [43], similar to the Universal Extra Dimension (UED) [44]. Correspondingly, theexperimental limit is weaker. A dedicated search with ISR should improve the limit likein the UED case [45].
This work was supported in part by the U.S. DOE under Contract No. DEAC0376SF00098, by the NSF under Grant No. PHY-1002399, by the JSPS Grant (C)No. 23540289, by the FIRST program Subaru Measurements of Images and Redshifts(SuMIRe), CSTP, and by WPI, MEXT, Japan.
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