3,022 research outputs found
The Standard Cosmology
These lectures provide an introductory review of big bang cosmology. I
discuss the expanding Friedmann-Robertson-Walker universe, summarizing the
observational evidence which has led to its adoption as the `standard'
cosmological model and reviewing its basic properties. Subsequent lectures
provide an overview of the early universe. The final lectures give an
introduction to the inflationary universe, beginning with the motivating
puzzles of the standard cosmology (the horizon and flatness problems) and
ending with the inflationary production of quantum field fluctuations and their
possible role in seeding the large-scale structure of the Universe.Comment: 49 pages, uuencoded postscript file (includes 7 figures),
Fermilab-Conf-94/090-
Perturbations in a coupled scalar field cosmology
I analyze the density perturbations in a cosmological model with a scalar
field coupled to ordinary matter, such as one obtains in string theory and in
conformally transformed scalar-tensor theories. The spectrum of multipoles on
the last scattering surface and the power spectrum at the present are compared
with observations to derive bounds on the coupling constant and on the
exponential potential slope. It is found that the acoustic peaks and the power
spectrum are strongly sensitive to the model parameters. The models that best
fit the galaxy spectrum and satisfy the cluster abundance test have energy
density and a scale factor expansion law .Comment: 13 pages, 9 figures, minor revision, now figures are embedded in tex
Loop Corrections in Non-Linear Cosmological Perturbation Theory
Using a diagrammatic approach to Eulerian perturbation theory, we
analytically calculate the variance and skewness of the density and velocity
divergence induced by gravitational evolution from Gaussian initial conditions,
including corrections *beyond* leading order. Except for the power spectrum,
previous calculations in cosmological perturbation theory have been confined to
leading order (tree level)-we extend these to include loop corrections. For
scale-free initial power spectra, the one-loop variance \sigma^2 = \sigma^2_l +
1.82 \sigma^4_l and the skewness S_3 = 34/7 + 9.8 \sigma^2_l, where \sigma_l is
the rms fluctuation of the linear density field. We also compute loop
corrections to the variance, skewness, and kurtosis for several non-linear
approximation schemes, where the calculation can be easily generalized to
1-point cumulants of higher order and arbitrary number of loops. We find that
the Zel'dovich approximation gives the best approximation to the loop
corrections of exact perturbation theory, followed by the Linear Potential
approximation (LPA) and the Frozen Flow approximation (FFA), in qualitative
agreement with the relative behavior of tree-level results. In LPA and FFA,
loop corrections are infrared divergent for spectral indices n < 0; this is
related to the breaking of Galilean invariance in these schemes.Comment: 53 pages, uuencoded and gzipped postscript file, 20 figures, 25
tables, also available at http://fnas08.fnal.gov/cumu.u
Loop Corrections in Non-Linear Cosmological Perturbation Theory II. Two-point Statistics and Self-Similarity
We calculate the lowest-order non-linear contributions to the power spectrum,
two-point correlation function, and smoothed variance of the density field, for
Gaussian initial conditions and scale-free initial power spectra, . These results extend and in some cases correct previous work in the
literature on cosmological perturbation theory. Comparing with the scaling
behavior observed in N-body simulations, we find that the validity of
non-linear perturbation theory depends strongly on the spectral index . For
, we find excellent agreement over scales where the variance \sigma^2(R)
\la 10; however, for , perturbation theory predicts deviations from
self-similar scaling (which increase with ) not seen in numerical
simulations. This anomalous scaling suggests that the principal assumption
underlying cosmological perturbation theory, that large-scale fields can be
described perturbatively even when fluctuations are highly non-linear on small
scales, breaks down beyond leading order for spectral indices . For
, the power spectrum, variance, and correlation function in the scaling
regime can be calculated using dimensional regularization.Comment: 48 pages, 19 figures, uses axodraw.sty; also available at
http://fnas08.fnal.gov
Lensing and high-z supernova surveys
Gravitational lensing causes the distribution of observed brightnesses of
standard candles at a given redshift to be highly non-gaussian. The
distribution is strongly, and asymmetrically, peaked at a value less than the
expected value in a homogeneous Robertson-Walker universe. Therefore, given any
small sample of observations in an inhomogeneous universe, the most likely
observed luminosity is at flux values less than the Robertson-Walker value.
This paper explores the impact of this systematic error due to lensing upon
surveys predicated on measuring standard candle brightnesses. We re-analyze
recent results from the high-z supernova team (Riess et al. 1998), both when
most of the matter in the universe is in the form of compact objects
(represented by the empty-beam expression, corresponding to the maximal case of
lensing), and when the matter is continuously distributed in galaxies. We find
that the best-fit model remains unchanged (at Omega_m=0, Omega_Lambda=0.45),
but the confidence contours change size and shape, becoming larger (and thus
allowing a broader range of parameter space) and dropping towards higher values
of matter density, Omega_m (or correspondingly, lower values of the
cosmological constant, Omega_Lambda). These effects are slight when the matter
is continuously distributed. However, the effects become considerably more
important if most of the matter is in compact objects. For example, neglecting
lensing, the Omega_m=0.5, Omega_Lambda=0.5 model is more than 2 sigma away from
the best fit. In the empty-beam analysis, this cosmology is at 1 sigma.Comment: 11 pages, 3 ps figures. uses aaspp4.sty. accepted to ApJ Letters.
includes analysis of lensing due to matter continuously distributed in
galaxie
Weak Gravitational Lensing by Voids
We consider the prospects for detecting weak gravitational lensing by
underdensities (voids) in the large-scale matter distribution. We derive the
basic expressions for magnification and distortion by spherical voids.
Clustering of the background sources and cosmic variance are the main factors
which limit in principle the detection of lensing by voids. We conclude that
only voids with radii larger than \hm have lensing signal to noise
larger than unity.Comment: 12 pages, 7 figures, uses mn-1_4.sty file, submitted to MNRA
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