127 research outputs found
Small steps towards Grand Unification and the electron/positron excesses in cosmic-ray experiments
We consider a small extension of the standard model by adding two Majorana
fermions; those are adjoint representations of the SU(2)_L and SU(3)_c gauge
groups of the standard model. In this extension, the gauge coupling unification
at an energy scale higher than 10^{15} GeV is realized when the masses of the
triplet and the octet fermions are smaller than 10^4 GeV and 10^{12} GeV,
respectively. We also show that an appropriate symmetry ensures a long lifetime
of the neutral component of the triplet fermion whose thermal relic density
naturally explains the observed dark matter density. The electron/positron
excesses observed in recent cosmic-ray experiments can be also explained by the
decay of the triplet fermion.Comment: 11 pages, 5 figure
PAMELA, DAMA, INTEGRAL and Signatures of Metastable Excited WIMPs
Models of dark matter with ~ GeV scale force mediators provide attractive
explanations of many high energy anomalies, including PAMELA, ATIC, and the
WMAP haze. At the same time, by exploiting the ~ MeV scale excited states that
are automatically present in such theories, these models naturally explain the
DAMA/LIBRA and INTEGRAL signals through the inelastic dark matter (iDM) and
exciting dark matter (XDM) scenarios, respectively. Interestingly, with only
weak kinetic mixing to hypercharge to mediate decays, the lifetime of excited
states with delta < 2 m_e is longer than the age of the universe. The
fractional relic abundance of these excited states depends on the temperature
of kinetic decoupling, but can be appreciable. There could easily be other
mechanisms for rapid decay, but the consequences of such long-lived states are
intriguing. We find that CDMS constrains the fractional relic population of
~100 keV states to be <~ 10^-2, for a 1 TeV WIMP with sigma_n = 10^-40 cm^2.
Upcoming searches at CDMS, as well as xenon, silicon, and argon targets, can
push this limit significantly lower. We also consider the possibility that the
DAMA excitation occurs from a metastable state into the XDM state, which decays
via e+e- emission, which allows lighter states to explain the INTEGRAL signal
due to the small kinetic energies required. Such models yield dramatic signals
from down-scattering, with spectra peaking at high energies, sometimes as high
as ~1 MeV, well outside the usual search windows. Such signals would be visible
at future Ar and Si experiments, and may be visible at Ge and Xe experiments.
We also consider other XDM models involving ~ 500 keV metastable states, and
find they can allow lighter WIMPs to explain INTEGRAL as well.Comment: 22 pages, 7 figure
Conservative Constraints on Dark Matter from the Fermi-LAT Isotropic Diffuse Gamma-Ray Background Spectrum
We examine the constraints on final state radiation from Weakly Interacting
Massive Particle (WIMP) dark matter candidates annihilating into various
standard model final states, as imposed by the measurement of the isotropic
diffuse gamma-ray background by the Large Area Telescope aboard the Fermi
Gamma-Ray Space Telescope. The expected isotropic diffuse signal from dark
matter annihilation has contributions from the local Milky Way (MW) as well as
from extragalactic dark matter. The signal from the MW is very insensitive to
the adopted dark matter profile of the halos, and dominates the signal from
extragalactic halos, which is sensitive to the low mass cut-off of the halo
mass function. We adopt a conservative model for both the low halo mass
survival cut-off and the substructure boost factor of the Galactic and
extragalactic components, and only consider the primary final state radiation.
This provides robust constraints which reach the thermal production
cross-section for low mass WIMPs annihilating into hadronic modes. We also
reanalyze limits from HESS observations of the Galactic Ridge region using a
conservative model for the dark matter halo profile. When combined with the
HESS constraint, the isotropic diffuse spectrum rules out all interpretations
of the PAMELA positron excess based on dark matter annihilation into two lepton
final states. Annihilation into four leptons through new intermediate states,
although constrained by the data, is not excluded.Comment: 11 pages, 5 figures. v3: minor revisions, matches version to appear
in JCA
Dark matter and sub-GeV hidden U(1) in GMSB models
Motivated by the recent PAMELA and ATIC data, one is led to a scenario with
heavy vector-like dark matter in association with a hidden sector
below GeV scale. Realizing this idea in the context of gauge mediated
supersymmetry breaking (GMSB), a heavy scalar component charged under
is found to be a good dark matter candidate which can be searched for direct
scattering mediated by the Higgs boson and/or by the hidden gauge boson. The
latter turns out to put a stringent bound on the kinetic mixing parameter
between and : . For the typical range
of model parameters, we find that the decay rates of the ordinary lightest
neutralino into hidden gauge boson/gaugino and photon/gravitino are comparable,
and the former decay mode leaves displaced vertices of lepton pairs and missing
energy with distinctive length scale larger than 20 cm for invariant lepton
pair mass below 0.5 GeV. An unsatisfactory aspect of our model is that the
Sommerfeld effect cannot raise the galactic dark matter annihilation by more
than 60 times for the dark matter mass below TeV.Comment: 1+15 pages, 4 figures, version published in JCAP, references added,
minor change
Two component dark matter
We explain the PAMELA positron excess and the PPB-BETS/ATIC e+ + e- data
using a simple two component dark matter model (2DM). The two particle species
in the dark matter sector are assumed to be in thermal equilibrium in the early
universe. While one particle is stable and is the present day dark matter, the
second one is metastable and decays after the universe is 10^-8 s old. In this
model it is simple to accommodate the large boost factors required to explain
the PAMELA positron excess without the need for large spikes in the local dark
matter density. We provide the constraints on the parameters of the model and
comment on possible signals at future colliders.Comment: 6 pages, 2 figures, discussion clarified and extende
Kaluza-Klein Dark Matter, Electrons and Gamma Ray Telescopes
Kaluza-Klein dark matter particles can annihilate efficiently into
electron-positron pairs, providing a discrete feature (a sharp edge) in the
cosmic spectrum at an energy equal to the particle's mass (typically
several hundred GeV to one TeV). Although this feature is probably beyond the
reach of satellite or balloon-based cosmic ray experiments (those that
distinguish the charge and mass of the primary particle), gamma ray telescopes
may provide an alternative detection method. Designed to observe very
high-energy gamma-rays, ACTs also observe the diffuse flux of electron-induced
electromagnetic showers. The GLAST satellite, designed for gamma ray astronomy,
will also observe any high energy showers (several hundred GeV and above) in
its calorimeter. We show that high-significance detections of an
electron-positron feature from Kaluza-Klein dark matter annihilations are
possible with GLAST, and also with ACTs such as HESS, VERITAS or MAGIC.Comment: 10 pages, 2 figure
Gamma-ray and radio tests of the e+e- excess from DM annihilations
PAMELA and ATIC recently reported an excess in e+e- cosmic rays. We show that
if it is due to Dark Matter annihilations, the associated gamma-ray flux and
the synchrotron emission produced by e+e- in the galactic magnetic field
violate HESS and radio observations of the galactic center and HESS
observations of dwarf Spheroidals, unless the DM density profile is
significantly less steep than the benchmark NFW and Einasto profiles.Comment: 16 pages, 4 figures; v2: normalizations fixed in Table 2 and typos
corrected (no changes in the analysis nor the results), some references and
comments added; v3: minor additions, matches published versio
PAMELA/ATIC Anomaly from Exotic Mediated Dark Matter Decay
We discuss dark matter decay mediated by exotically charged particles
("exotics") in a supersymmetric model with two dark matter (DM) components: One
is the (bino-like) lightest supersymmetric particle (LSP) \chi, and the other
is a newly introduced meta-stable neutral singlet . decays to \chi
e^+e^- via a dimension 6 operator induced by a penguin-type one loop diagram
with the life time of 10^{26} sec., explaining energetic cosmic e^\pm excess
observed recently by PAMELA and ATIC/PPB-BETS. The superheavy masses of exotics
(\sim 10^{15-16} GeV) are responsible for the longevity of . The
superpartner of develops the vacuum expectation value (VEV) of order TeV so
that the DM achieves the desired mass of 2 TeV. By the VEV, the U(1)_R
symmetry is broken to the discrete Z_2 symmetry, which is identified with the
matter parity in the minimal supersymmetric standard model (MSSM). Since we
have the two DM components, even extremely small amount of [O(10^{-10}) <
(n_N/n_\chi)] could account for the observed positron flux with relatively
light exotics' masses [10^{12} GeV < M_{exo.} < 10^{16} GeV].Comment: 1+7 pages, version to appear in JHE
The Leptonic Higgs as a Messenger of Dark Matter
We propose that the leptonic cosmic ray signals seen by PAMELA and ATIC
result from the annihilation or decay of dark matter particles via states of a
leptonic Higgs doublet to leptons, linking cosmic ray signals of dark
matter to LHC signals of the Higgs sector. The states of the leptonic Higgs
doublet are lighter than about 200 GeV, yielding large and
event rates at the LHC. Simple models are
given for the dark matter particle and its interactions with the leptonic
Higgs, for cosmic ray signals arising from both annihilations and decays in the
galactic halo. For the case of annihilations, cosmic photon and neutrino
signals are on the verge of discovery.Comment: 34 pages, 9 figures, minor typos corrected, references adde
Pulsars as the Sources of High Energy Cosmic Ray Positrons
Recent results from the PAMELA satellite indicate the presence of a large
flux of positrons (relative to electrons) in the cosmic ray spectrum between
approximately 10 and 100 GeV. As annihilating dark matter particles in many
models are predicted to contribute to the cosmic ray positron spectrum in this
energy range, a great deal of interest has resulted from this observation.
Here, we consider pulsars (rapidly spinning, magnetized neutron stars) as an
alternative source of this signal. After calculating the contribution to the
cosmic ray positron and electron spectra from pulsars, we find that the
spectrum observed by PAMELA could plausibly originate from such sources. In
particular, a significant contribution is expected from the sum of all mature
pulsars throughout the Milky Way, as well as from the most nearby mature
pulsars (such as Geminga and B0656+14). The signal from nearby pulsars is
expected to generate a small but significant dipole anisotropy in the cosmic
ray electron spectrum, potentially providing a method by which the Fermi
gamma-ray space telescope would be capable of discriminating between the pulsar
and dark matter origins of the observed high energy positrons.Comment: 10 pages, 5 figures; updated to include published Pamela results;
version to appear in JCA
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