492 research outputs found
Structure Formation With a Long-Range Scalar Dark Matter Interaction
Numerical simulations show that a long-range scalar interaction in a single
species of massive dark matter particles causes voids between the
concentrations of large galaxies to be more nearly empty, suppresses accretion
of intergalactic matter onto galaxies at low redshift, and produces an early
generation of dense dark matter halos. These three effects, in moderation, seem
to be improvements over the Lambda CDM model predictions for cosmic structure
formation. Because the scalar interaction in this model has negligible effect
on laboratory physics and the classical cosmological tests, it offers an
observationally attractive example of cosmology with complicated physics in the
dark sector, notably a large violation of the weak equivalence principle.Comment: 10 pages, 7 figures, revtex4. v2: minor improvements, refs added,
version to appear in PR
Galaxy Satellites and the Weak Equivalence Principle
Numerical simulations of the effect of a long-range scalar interaction (LRSI)
acting only on nonbaryonic dark matter, with strength comparable to gravity,
show patterns of disruption of satellites that can agree with what is seen in
the Milky Way. This includes the symmetric Sagittarius stellar stream. The
exception presented here to the Kesden and Kamionkowski demonstration that an
LRSI tends to produce distinctly asymmetric streams follows if the LRSI is
strong enough to separate the stars from the dark matter before tidal
disruption of the stellar component, and if stars dominate the mass in the
luminous part of the satellite. It requires that the Sgr galaxy now contains
little dark matter, which may be consistent with the Sgr stellar velocity
dispersion, for in the simulation the dispersion at pericenter exceeds virial.
We present other examples of simulations in which a strong LRSI produces
satellites with large mass-to-light ratio, as in Draco, or free streams of
stars, which might be compared to "orphan" streams.Comment: 14 pages, accepted for publication in PR
Using Perturbative Least Action to Reconstruct Redshift Space Distortions
In this paper, we present a redshift space reconstruction scheme which is
analogous to and extends the Perturbative Least Action (PLA) method described
by Goldberg & Spergel (2000). We first show that this scheme is effective in
reconstructing even nonlinear observations. We then suggest that by varying the
cosmology to minimize the quadrupole moment of a reconstructed density field,
it may be possible to lower the errorbars on the redshift distortion parameter,
as well as to break the degeneracy between the linear bias parameter,
, and . Finally, we discuss how PLA might be applied to realistic
redshift surveys.Comment: 34 Pages LaTeX, including 10 postscript figures. Submitted to
Astrophysical Journa
Maximum-Likelihood Comparisons of Tully-Fisher and Redshift Data: Constraints on Omega and Biasing
We compare Tully-Fisher (TF) data for 838 galaxies within cz=3000 km/sec from
the Mark III catalog to the peculiar velocity and density fields predicted from
the 1.2 Jy IRAS redshift survey. Our goal is to test the relation between the
galaxy density and velocity fields predicted by gravitational instability
theory and linear biasing, and thereby to estimate where is the linear bias parameter for IRAS galaxies.
Adopting the IRAS velocity and density fields as a prior model, we maximize the
likelihood of the raw TF observables, taking into account the full range of
selection effects and properly treating triple-valued zones in the
redshift-distance relation. Extensive tests with realistic simulated galaxy
catalogs demonstrate that the method produces unbiased estimates of
and its error. When we apply the method to the real data, we model the presence
of a small but significant velocity quadrupole residual (~3.3% of Hubble flow),
which we argue is due to density fluctuations incompletely sampled by IRAS. The
method then yields a maximum likelihood estimate
(1-sigma error). We discuss the constraints on and biasing that follow
if we assume a COBE-normalized CDM power spectrum. Our model also yields the
1-D noise noise in the velocity field, including IRAS prediction errors, which
we find to be be 125 +/- 20 km/sec.Comment: 53 pages, 20 encapsulated figures, two tables. Submitted to the
Astrophysical Journal. Also available at http://astro.stanford.edu/jeff
Einstellungen und Selbstwirksamkeit von Lehrerinnen und Lehrern zur schulischen Inklusion in Deutschland - eine Analyse mit Daten des Nationalen Bildungspanels Deutschlands (NEPS)
In Deutschland wird der gemeinsame Unterricht von SchĂŒlerinnen und SchĂŒlern mit und ohne sonderpĂ€dagogischem Förderbedarf im Schulsystem stark ausgebaut. Als eine wichtige Voraussetzung fĂŒr eine gelungene Umsetzung des gemeinsamen Unterrichts wird in der Forschung die Einstellungen der beteiligten Lehrerinnen und Lehrer zur Inklusion gesehen. Der vorliegende Bei- trag berichtet ĂŒber die Selbstwirksamkeit und die allgemeine Einstellung zur Inklusion bei 130 KlassenlehrkrĂ€ften in der der 2. Welle der Startkohorte 3 (6. Jahrgangsstufe) des Nationalen Bildungspanels (NEPS). Insgesamt haben die RegelschullehrkrĂ€fte eine positive Einstellung gegenĂŒber der Inklusion, jedoch ist die Selbstwirksamkeit in Bezug auf Inklusion eher gering ausgeprĂ€gt. Die befragten KlassenlehrkrĂ€fte in Förderschulen trauen sich dagegen die Umsetzung des gemeinsamen Unterrichts eher zu. GegenĂŒber der Inklusion haben sie jedoch Bedenken und halten die Förderschule fĂŒr den optimaleren Förderort fĂŒr SchĂŒlerinnen und SchĂŒler mit sonderpĂ€dagogischem Förderbedarf
Reconstruction Analysis of Galaxy Redshift Surveys: A Hybrid Reconstruction Method
In reconstruction analysis of galaxy redshift surveys, one works backwards
from the observed galaxy distribution to the primordial density field in the
same region, then evolves the primordial fluctuations forward in time with an
N-body code. This incorporates assumptions about the cosmological parameters,
the properties of primordial fluctuations, and the biasing relation between
galaxies and mass. These can be tested by comparing the reconstruction to the
observed galaxy distribution, and to peculiar velocity data. This paper
presents a hybrid reconstruction method that combines the `Gaussianization''
technique of Weinberg(1992) with the dynamical schemes of Nusser & Dekel(1992)
and Gramann(1993). We test the method on N-body simulations and on N-body mock
catalogs that mimic the depth and geometry of the Point Source Catalog Redshift
Survey and the Optical Redshift Survey. This method is more accurate than
Gaussianization or dynamical reconstruction alone. Matching the observed
morphology of clustering can limit the bias factor b, independent of Omega.
Matching the cluster velocity dispersions and z-space distortions of the
correlation function xi(s,mu) constrains the parameter beta=Omega^{0.6}/b.
Relative to linear or quasi-linear approximations, a fully non-linear
reconstruction makes more accurate predictions of xi(s,mu) for a given beta,
thus reducing the systematic biases of beta measurements and offering further
scope for breaking the degeneracy between Omega and b. It also circumvents the
cosmic variance noise that limits conventional analyses of xi(s,mu). It can
also improve the determination of Omega and b from joint analyses of redshift
& peculiar velocity surveys as it predicts the fully non-linear peculiar
velocity distribution at each point in z-space.Comment: 72 pages including 33 figures, submitted to Ap
Evidence for a Positive Cosmological Constant from Flows of Galaxies and Distant Supernovae
Recent observations of high-redshift supernovae seem to suggest that the
global geometry of the Universe may be affected by a `cosmological constant',
which acts to accelerate the expansion rate with time. But these data by
themselves still permit an open universe of low mass density and no
cosmological constant. Here we derive an independent constraint on the lower
bound to the mass density, based on deviations of galaxy velocities from a
smooth universal expansion. This constraint rules out a low-density open
universe with a vanishing cosmological constant, and together the two favour a
nearly flat universe in which the contributions from mass density and the
cosmological constant are comparable. This type of universe, however, seems to
require a degree of fine tuning of the initial conditions that is in apparent
conflict with `common wisdom'.Comment: 8 pages, 1 figure. Slightly revised version. Letter to Natur
The end of the Dark Ages in MOND
We study the evolution of a spherically symmetric density perturbation in the
Modified Newtonian Dynamics (MOND) model applied to the net acceleration over
Hubble flow. The background cosmological model is a -dominated,
low- Friedmann model with no Cold Dark Matter. We include thermal
processes and non-equilibrium chemical evolution of the collapsing gas. We find
that under these assumptions the first low-mass objects () may collapse already for , which is in quite good
agreement with the recent WMAP results. A lower value of would lead to
much slower collapse of such objects.Comment: 6 pages, 11 figures, LaTeX 2e with MN2e, MNRAS submitte
Comparison of the ENEAR Peculiar Velocities with the PSCz Gravity Field
We present a comparison between the peculiar velocity field measured from the
ENEAR all-sky catalog and that derived from the galaxy
distribution of the IRAS PSCz redshift survey. The analysis is based on a modal
expansion of these data in redshift space by means of spherical harmonics and
Bessel functions. The effective smoothing scale of the expansion is almost
linear with redshift reaching 1500km/s at 3000km/s. The general flow patterns
in the filtered ENEAR and PSCz velocity fields agree well within 6000km/s,
assuming a linear biasing relation between the mass and the PSCz galaxies. The
comparison allows us to determine the parameter , where
is the cosmological density parameter and is the linear biasing
factor. A likelihood analysis of the ENEAR and PSCz modes yields , in good agreement with values obtained from Tully-Fisher surveys.Comment: Submitted to MNRA
Observational Constraints on a Variable Dark Energy Model
We study the effect of a phenomenological parameterized quintessence model on
low, intermediate and high redshift observations. At low and intermediate
redshifts, we use the Gold sample of supernova Type Ia (SNIa) data and recently
observed size of baryonic acoustic peak from Sloan Digital Sky Survey (SDSS),
to put constraint on the parameters of the quintessence model. At the high
redshift, the same fitting procedure is done using WAMP data, comparing the
location of acoustic peak with that obtain from the dark energy model. As a
complementary analysis in a flat universe, we combine the results from the
SNIa, CMB and SDSS. The best fit values for the model parameters are (the present matter content) and
(dark energy equation of state). Finally we
calculate the age of universe in this model and compare it with the age of old
stars and high redshift objectsComment: 10 pages, 12 figures, accepted in PR
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