286 research outputs found
Imprint of DESI fiber assignment on the anisotropic power spectrum of emission line galaxies
The Dark Energy Spectroscopic Instrument (DESI), a multiplexed fiber-fed
spectrograph, is a Stage-IV ground-based dark energy experiment aiming to
measure redshifts for 29 million Emission-Line Galaxies (ELG), 4 million
Luminous Red Galaxies (LRG), and 2 million Quasi-Stellar Objects (QSO). The
survey design includes a pattern of tiling on the sky and the locations of the
fiber positioners in the focal plane of the telescope, with the observation
strategy determined by a fiber assignment algorithm that optimizes the
allocation of fibers to targets. This strategy allows a given region to be
covered on average five times for a five-year survey, but with coverage varying
between zero and twelve, which imprints a spatially-dependent pattern on the
galaxy clustering. We investigate the systematic effects of the fiber
assignment coverage on the anisotropic galaxy clustering of ELGs and show that,
in the absence of any corrections, it leads to discrepancies of order ten
percent on large scales for the power spectrum multipoles. We introduce a
method where objects in a random catalog are assigned a coverage, and the mean
density is separately computed for each coverage factor. We show that this
method reduces, but does not eliminate the effect. We next investigate the
angular dependence of the contaminated signal, arguing that it is mostly
localized to purely transverse modes. We demonstrate that the cleanest way to
remove the contaminating signal is to perform an analysis of the anisotropic
power spectrum and remove the lowest bin, leaving
modes accurate at the few-percent level. Here, is the cosine of the angle
between the line-of-sight and the direction of . We also investigate
two alternative definitions of the random catalog and show they are comparable
but less effective than the coverage randoms method.Comment: Submitted to JCA
Field Flows of Dark Energy
Scalar field dark energy evolving from a long radiation- or matter-dominated
epoch has characteristic dynamics. While slow-roll approximations are invalid,
a well defined field expansion captures the key aspects of the dark energy
evolution during much of the matter-dominated epoch. Since this behavior is
determined, it is not faithfully represented if priors for dynamical quantities
are chosen at random. We demonstrate these features for both thawing and
freezing fields, and for some modified gravity models, and unify several
special cases in the literature.Comment: 9 pages, 5 figure
Spin-Orbit and Tensor Forces in Heavy-quark Light-quark Mesons: Implications of the New Ds state at 2.32 GeV
We consider the spectroscopy of heavy-quark light-quark mesons with a simple
model based on the non-relativistic reduction of vector and scalar exchange
between fermions. Four forces are induced: the spin-orbit forces on the light
and heavy quark spins, the tensor force, and a spin-spin force. If the vector
force is Coulombic, the spin-spin force is a contact interaction, and the
tensor force and spin-orbit force on the heavy quark to order are
directly proportional. As a result, just two independent parameters
characterize these perturbations. The measurement of the masses of three p-wave
states suffices to predict the mass of the fourth. This technique is applied to
the system, where the newly discovered state at 2.32 GeV provides the
third measured level, and to the system. The mixing of the two
p-wave states is reflected in their widths and provides additional constraints.
The resulting picture is at odds with previous expectations and raises new
puzzles.Comment: 6 pages, 1 figur
Parity violations in hydrogen and the fundamental structure of the weak current
Experiments in progress with hydrogen and deuterium may in practice determine the fundamental parameters and constituents of the weak interaction within the framework of unified gauge theories. In particular, for SU (2) x U (1) theories, from the results of these experiments one can infer the masses of the charged and neutral weak vector bosons (and thus sin2[theta]W), and the isospin classification of the right-handed portions of the electron and the u- and d-quarks. Non-singlet assignments for eR, uR and dR would imply the existence of additional leptons and/or quarks. Hydrogen/deuterium data also may be used to discriminate between SU (2) x U (1) models and various models based on larger gauge groups.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/22810/1/0000368.pd
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Parameterized Beyond-Einstein Growth
A single parameter, the gravitational growth index gamma, succeeds in characterizing the growth of density perturbations in the linear regime separately from the effects of the cosmic expansion. The parameter is restricted to a very narrow range for models of dark energy obeying the laws of general relativity but can take on distinctly different values in models of beyond-Einstein gravity. Motivated by the parameterized post-Newtonian (PPN) formalism for testing gravity, we analytically derive and extend the gravitational growth index, or Minimal Modified Gravity, approach to parameterizing beyond-Einstein cosmology. The analytic formalism demonstrates how to apply the growth index parameter to early dark energy, time-varying gravity, DGP braneworld gravity, and some scalar-tensor gravity
Testing Standard Cosmology with Large Scale Structure
The galaxy power spectrum contains information on the growth of structure,
the growth rate through redshift space distortions, and the cosmic expansion
through baryon acoustic oscillation features. We study the ability of two
proposed experiments, BigBOSS and JDEM-PS, to test the cosmological model and
general relativity. We quantify the latter result in terms of the gravitational
growth index \gamma, whose value in general relativity is \gamma\approx 0.55.
Significant deviations from this value could indicate new physics beyond the
standard model of cosmology. The results show that BigBOSS (JDEM-PS) would be
capable of measuring \gamma with an uncertainty \sigma(\gamma) = 0.043 (0.054),
which tightens to \sigma(\gamma) = 0.031 (0.038) if we include Stage III data
priors, marginalizing over neutrino mass, time varying dark energy equation of
state, and other parameters. For all dark energy parameters and related figures
of merit the two experiments give comparable results. We also carry out some
studies of the influence of redshift range, resolution, treatment of
nonlinearities, and bias evolution to enable further improvement.Comment: 9 pages, 12 tables, 1 figure; v3 matches MNRAS accepted versio
Suppression of Heavy Ion gamma gamma Production of the Higgs by Coulomb Dissociation
Predicted two-photon Higgs production with heavy ions at LHC is shown to be
reduced due to the large Coulomb dissociation cross section. Incorporating the
effect of dissociation reduces the production of a 100 GeV Higgs by about a
factor of three compared to rates in the literature calculated without this
effect.Comment: 5 pages, latex, revtex source, two postscript figure
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