5,555 research outputs found
What it takes to measure a fundamental difference between dark matter and baryons: the halo velocity anisotropy
Numerous ongoing experiments aim at detecting WIMP dark matter particles from
the galactic halo directly through WIMP-nucleon interactions. Once such a
detection is established a confirmation of the galactic origin of the signal is
needed. This requires a direction-sensitive detector. We show that such a
detector can measure the velocity anisotropy beta of the galactic halo.
Cosmological N-body simulations predict the dark matter anisotropy to be
nonzero, beta~0.2. Baryonic matter has beta=0 and therefore a detection of a
nonzero beta would be strong proof of the fundamental difference between dark
and baryonic matter. We estimate the sensitivity for various detector
configurations using Monte Carlo methods and we show that the strongest signal
is found in the relatively few high recoil energy events. Measuring beta to the
precision of ~0.03 will require detecting more than 10^4 WIMP events with
nuclear recoil energies greater than 100 keV for a WIMP mass of 100 GeV and a
32S target. This number corresponds to ~10^6 events at all energies. We discuss
variations with respect to input parameters and we show that our method is
robust to the presence of backgrounds and discuss the possible improved
sensitivity for an energy-sensitive detector.Comment: 15 pages, 8 figures, accepted by JCAP. Matches accepted versio
A Cosmological Three Level Neutrino Laser
We present a calculation of a neutrino decay scenario in the early Universe.
The specific decay is \nu_{2} \to \nu_{1} + \phi, where \phi is a boson. If
there is a neutrino mass hierarchy, m_{\nu_{e}} < m_{\nu_{\mu}} <
m_{\nu_{\tau}}, we show that it is possible to generate stimulated decay and
effects similar to atomic lasing without invoking new neutrinos, even starting
from identical neutrino distributions. Under the right circumstances the decay
can be to very low momentum boson states thereby producing something similar to
a Bose condensate, with possible consequences for structure formation. Finally,
we argue that this type of decay may also be important other places in early
Universe physics.Comment: 7 pages, RevTex, due for publication in Phys. Rev. D, April 15 issu
Stochastic optimization methods for extracting cosmological parameters from CMBR power spectra
The reconstruction of the CMBR power spectrum from a map represents a major
computational challenge to which much effort has been applied. However, once
the power spectrum has been recovered there still remains the problem of
extracting cosmological parameters from it. Doing this involves optimizing a
complicated function in a many dimensional parameter space. Therefore efficient
algorithms are necessary in order to make this feasible. We have tested several
different types of algorithms and found that the technique known as simulated
annealing is very effective for this purpose. It is shown that simulated
annealing is able to extract the correct cosmological parameters from a set of
simulated power spectra, but even with such fast optimization algorithms, a
substantial computational effort is needed.Comment: 7 pages revtex, 3 figures, to appear in PR
Stringent neutron-star limits on large extra dimensions
Supernovae (SNe) are copious sources for Kaluza-Klein gravitons which are
generic for theories with large extra dimensions. These massive particles are
produced with average velocities ~0.5 c so that many of them are
gravitationally retained by the SN core. Every neutron star thus has a halo of
KK gravitons which decay into nu bar-nu, e^+e^- and gamma gamma on time scales
\~10^9 years. The EGRET gamma-flux limits (E_gamma ~ 100 MeV) for nearby
neutron stars constrain the fundamental scale for n=2 extra dimensions to M
>500 TeV, and M>30 TeV for n=3. The upcoming GLAST satellite is a factor ~30
more sensitive and thus may detect KK decays, for example at the nearby neutron
star RX J185635--3754. The requirement that neutron stars are not excessively
heated by KK decays implies M>1700 TeV for n=2, and M>60 TeV for n=3.Comment: Minor changes, matches version to appear in PR
Reconstructing the primordial power spectrum - a new algorithm
We propose an efficient and model independent method for reconstructing the
primordial power spectrum from Cosmic Microwave Background (CMB) and large
scale structure observations. The algorithm is based on a Monte Carlo principle
and therefore very simple to incorporate into existing codes such as Markov
Chain Monte Carlo. The algorithm has been used on present cosmological data to
test for features in the primordial power spectrum. No significant evidence for
features is found, although there is a slight preference for an overall bending
of the spectrum, as well as a decrease in power at very large scales. We have
also tested the algorithm on mock high precision CMB data, calculated from
models with non-scale invariant primordial spectra. The algorithm efficiently
extracts the underlying spectrum, as well as the other cosmological parameters
in each case. Finally we have used the algorithm on a model where an artificial
glitch in the CMB spectrum has been imposed, like the ones seen in the WMAP
data. In this case it is found that, although the underlying cosmological
parameters can be extracted, the recovered power spectrum can show significant
spurious features, such as bending, even if the true spectrum is scale
invariant.Comment: 22 pages, 12 figures, matches JCAP published versio
Strong constraint on large extra dimensions from cosmology
We have studied cosmological constraints on the number and radii of possible
large extra dimensions. If such dimensions exist, Kaluza-Klein (KK) modes are
copiously produced at high temperatures in the early universe, and can
potentially lead to unacceptable cosmological effects. We show that during
reheating, large numbers of KK modes are produced. These modes are not diluted
completely by the entropy production during reheating because they are produced
non-relativistically. This means that the modes produced during reheating can
easily be the dominant component. For instance, for two extra dimensions the
bound on their radii from considering only the thermally produced KK modes is R
< 1.1 x 10^-4 mm. If the modes produced during reheating are also accounted
for, the bound is strengthened to R < 2.2 x 10^-5 mm. This bound is stronger
than all other known astrophysical or laboratory limits.Comment: 6 pages, 3 figures, matches version to appear in Phys Rev
Probing neutrino decays with the cosmic microwave background
We investigate in detail the possibility of constraining neutrino decays with
data from the cosmic microwave background radiation (CMBR). Two generic decays
are considered \nu_H -> \nu_L \phi and \nu_H -> \nu_L \nu_L_bar \nu_L. We have
solved the momentum dependent Boltzmann equation in order to account for
possible relativistic decays. Doing this we estimate that any neutrino with
mass m > 1 eV decaying before the present should be detectable with future CMBR
data. Combining this result with other results on stable neutrinos, any
neutrino mass of the order 1 eV should be detectable.Comment: 8 pages, 4 figures, to appear in Phys. Rev.
Neutrino masses and cosmic radiation density: Combined analysis
We determine the range of neutrino masses and cosmic radiation content
allowed by the most recent CMB and large-scale structure data. In contrast to
other recent works, we vary these parameters simultaneously and provide
likelihood contours in the two-dimensional parameter space of N_eff}, the usual
effective number of neutrino species measuring the radiation density, and \sum
m_nu. The allowed range of \sum m_nu and N_eff has shrunk significantly
compared to previous studies. The previous degeneracy between these parameters
has disappeared, largely thanks to the baryon acoustic oscillation data. The
likelihood contours differ significantly if \sum m_nu resides in a single
species instead of the standard case of being equally distributed among all
flavors. For \sum m_nu=0 we find 2.7 < N_eff < 4.6 at 95% CL while \sum m_nu <
0.62 eV at 95% CL for the standard radiation content.Comment: 8 pages, 2 figure
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