SuperWIMP Cosmology and Collider Physicsa
ABSTRACT Dark matter may be composed of superWIMPs, superweakly-interacting mas- sive particles produced in the late decays of other particles. We focus here on the well-motivated supersymmetric example of gravitino LSPs. Gravitino su- perWIMPs share several virtues with the well-known case of neutralino dark matter: they are present in the same supersymmetric frameworks (supergravity with R-parity conservation) and naturally have the desired relic density. In con- trast to neutralinos, however, gravitino superWIMPs are impossible to detect by conventional dark matter searches, may explain an existing discrepancy in Big Bang nucleosynthesis, predict observable distortions in the cosmic microwave background, and imply spectacular signals at future particle colliders.
arXiv:hep-ph/0410178v1 12 Oct 2004
SuperWIMP Cosmology and Collider Physicsa
JONATHAN L. FENG∗, ARVIND RAJARAMAN∗, BRYAN T. SMITH∗,
SHUFANG SU†, FUMIHIRO TAKAYAMA∗
∗Department of Physics and Astronomy, University of California
Irvine, CA 92697, USA
†Department of Physics, University of Arizona
Tucson, AZ 85721, USA
Dark matter may be composed of superWIMPs, superweakly-interacting mas-
sive particles produced in the late decays of other particles. We focus here on
the well-motivated supersymmetric example of gravitino LSPs. Gravitino su-
perWIMPs share several virtues with the well-known case of neutralino dark
matter: they are present in the same supersymmetric frameworks (supergravity
with R-parity conservation) and naturally have the desired relic density. In con-
trast to neutralinos, however, gravitino superWIMPs are impossible to detect by
conventional dark matter searches, may explain an existing discrepancy in Big
Bang nucleosynthesis, predict observable distortions in the cosmic microwave
background, and imply spectacular signals at future particle colliders.
In recent years, there has been tremendous progress in understanding the universe on
the largest scales. In particular, the energy density in non-baryonic dark matter is known
to be 
ΩDM= 0.23 ± 0.04
in units of the critical density. At the same time, we have no idea what the microscopic
identity of non-baryonic dark matter is. The dark matter problem therefore provides
precise, unambiguous evidence for new physics and has motivated new particles such
as axions [2,3,4], neutralinos [5,6], Q balls , wimpzillas , axinos , self-interacting
dark matter , annihilating dark matter , Kaluza-Klein dark matter [12,13], bra-
nons [14,15], and many others.
Here we review a new class of dark matter candidates: superWIMPs, superweakly-
interacting massive particles produced in the late decays of other particles [16,17,18].
SuperWIMPs have several strong motivations:
• They are present in well-motivated frameworks for new physics, including models
with supersymmetry (supergravity with R-parity conservation) and extra dimen-
sions (universal extra dimensions with KK-parity conservation).
• Their relic density is naturally in the right range to be dark matter without the
need to introduce and fine-tune new energy scales.
aPlenary talk given by JLF at SUSY2004, the 12th International Conference on Supersymmetry and
Unification of Fundamental Interactions, Tsukuba, Japan, 17-23 June 2004.
• They can explain an existing anomaly, namely the observed underabundance of7Li
relative to the prediction of standard Big Bang nucleosynthesis.
• They have rich implications for early universe cosmology and imply spectacular
signals at the Large Hadron Collider (LHC) and the International Linear Collider
2. The Basic Idea
As noted above, superWIMPs exist in theories with supersymmetry and in models
with extra dimensions. We concentrate on the supersymmetric scenarios here. Details of
the extra dimensional realizations may be found in Refs. [16,17,18].
In the simplest supersymmetric models, supersymmetry is transmitted to standard
model superpartners through gravitational interactions, and supersymmetry is broken at
a high scale. The mass of the gravitino˜G is
and the masses of standard model superpartners are
˜ m ∼
where M∗ = (8πGN)−1/2≃ 2.4 × 1018GeV is the reduced Planck scale and F ∼
(1011GeV)2is the supersymmetry breaking scale squared. The precise ordering of masses
depends on unknown, presumably O(1), constants in Eq. (3). Most supergravity studies
assume that the lightest supersymmetric particle (LSP) is a standard model superpartner,
such as the neutralino. In this case, it is well-known that the neutralino naturally freezes
out with a relic density that is in the right range to account for dark matter .
The gravitino may be the LSP, however [16,17,18,20,21,22,23,24,25,26,27,28]. In su-
pergravity, the gravitino has weak scale mass Mweak∼ 100 GeV and couplings suppressed
by M∗. The gravitino’s extremely weak interactions imply that it is irrelevant during ther-
mal freeze out. The next-to-lightest supersymmetric particle (NLSP) therefore freezes out
as usual, and if the NLSP is a slepton, sneutrino, or neutralino, its thermal relic density is
again ΩNLSP∼ 0.1. However, eventually the NLSP decays to its standard model partner
and the gravitino. The resulting gravitino relic density is
In supergravity, where m˜G∼ mNLSP, the gravitino therefore inherits a relic density of the
right order to be much or all of non-baryonic dark matter. The superWIMP gravitino
scenario preserves the prime virtue of WIMPs, namely that they give the desired amount
of dark matter without relying on the introduction of new, fine-tuned energy scales.b
Because superWIMP gravitinos interact only gravitationally, with couplings suppressed
by M∗, they are impossible to detect in conventional direct and indirect dark matter search
experiments. At the same time, the extraordinarily weak couplings of superWIMPs imply
other testable signals. The NLSP is a weak-scale particle decaying gravitationally and so
has a natural lifetime of
This decay time, outlandishly long by particle physics standards, implies testable cosmo-
logical signals, as well as novel signatures at colliders.
∼ 104− 108s . (5)
The most sensitive probes of late decays with lifetimes in the range given in Eq. (5)
are from Big Bang nucleosynthesis (BBN) and the Planckian spectrum of the cosmic
microwave background (CMB). The impact of late decays to gravitinos on BBN and
the CMB are determined by only two parameters: the lifetime of NLSP decays and
the energy released in these decays. The energy released is quickly thermalized, and so
the cosmological signals are insensitive to the details of the energy spectrum and are
determined essentially only by the total energy released.
The width for the decay of a slepton to a gravitino is
Γ(˜l → l˜G) =
assuming the lepton mass is negligible. (Similar expressions hold for the decays of a
neutralino NLSP.) This decay width depends on only the slepton mass, the gravitino mass,
and the Planck mass. In many supersymmetric decays, dynamics brings a dependence on
many supersymmetry parameters. In contrast, as decays to the gravitino are gravitational,
dynamics is determined by masses, and so no additional parameters enter. In particular,
there is no dependence on left-right mixing or flavor mixing in the slepton sector. For
m˜G/m˜l≈ 1, the slepton decay lifetime is
τ(˜l → l˜G) ≃ 3.6 × 108s
This expression is valid only when the gravitino and slepton are nearly degenerate, but it
is a useful guide and verifies the rough estimate of Eq. (5).
The energy release is conveniently expressed in terms of
produced either thermally, with Ω˜ G∼ 0.1 obtained by requiring m˜ G∼ keV, or through reheating, with
Ω˜ G∼ 0.1 obtained by tuning the reheat temperature to TRH∼ 1010GeV.
Previously, however, gravitinos were expected to be
for electromagnetic energy, with a similar expression for hadronic energy. Here ǫEMis the
initial EM energy released in NLSP decay, and BEMis the branching fraction of NLSP
decay into EM components. YNLSP≡ nNLSP/nγis the NLSP number density just before
NLSP decay, normalized to the background photon number density nγ= 2ζ(3)T3/π2. It
can be expressed in terms of the superWIMP abundance:
YNLSP≃ 3.0 × 10−12
Once an NLSP candidate is specified, and assuming superWIMPs make up all of the
dark matter, with Ω˜G= ΩDM= 0.23, the early universe signals are completely determined
by only two parameters: m˜Gand mNLSP.
3.1. BBN Electromagnetic Constraints
BBN predicts primordial light element abundances in terms of one free parameter, the
baryon-to-photon ratio η ≡ nB/nγ. In the past, the fact that the observed D,4He,3He,
and7Li abundances could be accommodated by a single choice of η was a well-known
triumph of standard Big Bang cosmology.
More recently, BBN baryometry has been supplemented by CMB data, which alone
yields η10 = η/10−10= 6.1 ± 0.4 . This value agrees precisely with the value of η
determined by D, considered by many to be the most reliable BBN baryometer. However,
it highlights slight inconsistencies in the BBN data. Most striking is the case of7Li. For
η10= 6.0±0.5, the value favored by the combined D and CMB observations, the standard
BBN prediction is 
7Li/H = 4.7+0.9
at 95% CL. This contrasts with observations. Three independent studies find
7Li/H = 1.5+0.9
−0.22× 10−10(1σ + sys) 
−0.32× 10−10(stat + sys, 95% CL)  ,
(95% CL) (11)
7Li/H = 1.72+0.28
7Li/H = 1.23+0.68
where depletion effects have been estimated and included in the last value. Within the
published uncertainties, the observations are consistent with each other but inconsistent
with the theoretical prediction of Eq. (10), with central values lower than predicted by a
factor of 3 to 4.
for example, by rotational mixing in stars that brings Lithium to the core where it may
be burned [45,46], but it is controversial whether this effect is large enough to reconcile
observations with the BBN prediction .
We now consider the effects of NLSP decays to gravitinos. For WIMP NLSPs, that
is, sleptons, sneutrinos, and neutralinos, the energy released is dominantly deposited
in electromagnetic cascades. For the decay times of Eq. (5), mesons decay before they
interact hadronically. The impact of EM energy on the light element abundances has been
7Li may be depleted from its primordial value by astrophysical effects,
Figure 1: Predicted and excluded regions of the (τ,ζEM) plane in the superWIMP dark matter scenario,
where τ is the lifetime for˜l → l˜G, and ζEMis the normalized electromagnetic energy release. The grid gives
predicted values for m˜ G= 100 GeV−3 TeV (top to bottom) and ∆m ≡ m˜l−m˜ G= 600 GeV−100 GeV
(left to right), assuming Ω˜ G= 0.23. BBN constraints exclude the shaded regions; the circle indicates the
best fit region where7Li is reduced to observed levels without upsetting other light element abundances.
Contours of CMB µ distortions indicate the current bound (µ < 0.9 × 10−4) and the expected future
sensitivity of DIMES (µ ∼ 10−6). From Ref. .
studied in Refs. [47,48,49,50]. The results of Ref.  are given in Fig. 1. The shaded
regions are excluded because they distort the light element abundances too much. The
predictions of the superWIMP scenario for a stau NLSP with m˜Gand mNLSPvarying over
weak scale parameters are given in Fig. 1 by the grid.
We find that the BBN constraint excludes some weak scale parameters. However,
much of the weak scale parameter space remains viable. Note also that, given the7Li
discrepancy, the best fit is not achieved at ξEM= 0, but rather for τ ∼ 3 × 106s and
ξEM∼ 10−9GeV, where7Li is destroyed by late decays without changing the other relic
abundances. This point is marked by the circle in Fig. 1. The energy release predicted
in the superWIMP scenario naturally includes this region. The7Li anomaly is naturally
resolved in the superWIMP scenario by a stau NLSP with mNLSP∼ 700 GeV and m˜G∼
3.2. BBN Hadronic Constraints
Hadronic energy release is also constrained by BBN [51,52,53,54,55,56,57]. In fact,
constraints on hadronic energy release are so severe that even subdominant contributions
to hadronic energy may provide stringent constraints.
Slepton and sneutrino decays contribute to hadronic energy through the higher order