arXiv subjects

Edmund Bertschinger

Publications and source records attributed to Edmund Bertschinger.

At least 55 records · Page 3Linked to original sources

arXiv1995

COSMICS: Cosmological Initial Conditions and Microwave Anisotropy Codes

COSMICS is a package of fortran programs useful for computing transfer functions and microwave background anisotropy for cosmological models, and for generating gaussian random initial conditions for nonlinear structure formation simulations of such models. Four programs are provided: {\bf linger\_con} and {\bf linger\_syn} integrate the linearized equations of general relativity, matter, and radiation in conformal Newtonian and synchronous gauge, respectively; {\bf deltat} integrates the photon transfer functions computed by the linger codes to produce photon anisotropy power spectra; and {\bf grafic} tabulates normalized matter power spectra and produces constrained or unconstrained samples of the matter density field. Version 1.0 of COSMICS is available at http://arcturus.mit.edu/cosmics/ . The current release gives fortran-77 programs that run on workstations and vectorized supercomputers. Unix makefiles are included that make it simple to build and test the package. A future release will include portable parallel versions of the linger codes using standard message-passing libraries.

astro-ph↗

arXiv1995

Parallel Linear General Relativity and CMB Anisotropies

We have developed a code which links scalar-mode fluctuations in the early universe with those observable at the present time by integrating the coupled, linearized, Einstein, Boltzmann, and fluid equations in a perturbed flat Robertson-Walker spacetime. The results are useful both for calculations of the cosmic microwave background anisotropy and the linear power spectrum of matter fluctuations. This paper introduces the serial and parallel codes, presents timing results, and gives sample output in graphical and animated form. This is a latex version containing most of an HTML-format technical paper submitted for Supercomputing '95. The preferred method of viewing is to point your WWW client to http://arcturus.mit.edu/SC95/

astro-ph↗

arXiv1995

Cosmological Dynamics

This is a set of lecture notes basd on the lectures on cosmological dynamics given by E. Bertschinger at Les Houches in August 1993. The contents include elementary mechanics in cosmology, Eulerian and Lagrangian fluid dynamics, hot dark matter, and relativistic cosmological perturbation theory. To typeset the notes one must first obtain the style files and figures in file figmac.uu sent separately. Place all the files in one directory, run latex three times, and run dvips or equivalent to produce a postscript file.

astro-ph↗

arXiv1995

A Parallel Processing Algorithm for Computing Short-Range Particle Forces with Inhomogeneous Particle Distributions

We present a computational algorithm for computing short range forces between particles. The algorithm has two distinguishing features. First, it is optimized for multi-processor computers, and will use as many processors as are available. Second, it is optimized for inhomogeneous, dynamic particle distributions; for any distribution the computational load is distributed evenly to all processors, and the communication time is less than 15\% of the total run time. In this talk we present our new algorithm. We developed the program for a grand-challenge problem in cosmology, simulation of the formation of large-scale structure in the universe. This simulation, run on the Thinking Machines Corporation CM-5, uses the particle-particle/particle-mesh (PPPM) \cite{hock_east} algorithm. The particle-particle phase is computed using the algorithm we describe in this paper. We discuss this and other applications.

astro-ph↗

arXiv1995

Self-Similar Evolution of Cosmological Density Fluctuations

The gravitational evolution of scale free initial spectra $P(k)\propto k^n$ in an Einstein-de Sitter universe is widely believed to be self-similar for $-3<n<4$. However, for $-3<n<-1$ the existence of self-similar scaling has not been adequately demonstrated. Here we investigate the possible breaking of self-similar scaling due to the nonlinear contributions of long wave modes. For $n<-1$ the nonlinear terms in the Fourier space fluid equations contain terms that diverge due to contributions from wavenumber $k\to 0$ (the long wave limit). To assess the possible dynamical effects of this divergence the limit of long wave contributions is investigated in detail using two different analytical approaches. Perturbative contributions to the power spectrum are examined. It is shown that for $n<-1$ there are divergent contributions at all orders. However, at every order the leading order divergent terms cancel out exactly. This does not rule out the existence of a weaker but nevertheless divergent net contribution. The second approach consists of a non-perturbative approximation, developed to study the nonlinear effects of long wave mode coupling. A solution for the phase shift of the Fourier space density is obtained which is divergent for $n<-1$. A kinematical interpretation of the divergence of the phase shift, related to the translational motion induced by the large-scale bulk velocity, is given. Our analysis indicates that the amplitude of the density is {\it not} affected by the divergent terms. Thus both analytical approaches lead to the conclusion that the self-similar scaling of physically relevant measures of the growth of density perturbations is preserved.

astro-ph↗

arXiv1994

Cold Dark Matter I: The Formation of Dark Halos

We use numerical simulations of critically-closed cold dark matter (CDM) models to study the effects of numerical resolution on observable quantities. We study simulations with up to $256^3$ particles using the particle-mesh (PM) method and with up to $144^3$ particles using the adaptive particle-particle --particle-mesh (P$^3$M) method. Comparisons of galaxy halo distributions are made among the various simulations. We also compare distributions with observations and we explore methods for identifying halos, including a new algorithm that finds all particles within closed contours of the smoothed density field surrounding a peak. The simulated halos show more substructure than predicted by the Press-Schechter theory. We are able to rule out all $Ω=1$ CDM models for linear amplitude $σ_8\gsim 0.5$ because the simulations produce too many massive halos compared with the observations. The simulations also produce too many low mass halos. The distribution of halos characterized by their circular velocities for the P$^3$M simulations is in reasonable agreement with the observations for $150\kms\lsim V_{\rm circ} \lsim 350\kms$.}}

astro-ph↗

arXiv1994

Cold Dark Matter II: Spatial and Velocity Statistics

We examine high-resolution gravitational N-body simulations of the $Ω=1$ cold dark matter (CDM) model in order to determine whether there is any normalization of the initial density fluctuation spectrum that yields acceptable results for galaxy clustering and velocities. Dense dark matter halos in the evolved mass distribution are identified with luminous galaxies; the most massive halos are also considered as sites for galaxy groups, with a range of possibilities explored for the group mass to light ratios. We verify the earlier conclusions of White et al. (1987) for the low amplitude (high bias) CDM model --- the galaxy correlation function is marginally acceptable but that there are too many galaxies. We also show that the peak biasing method does not accurately reproduce the results obtained using dense halos identified in the simulations themselves. The COBE anisotropy implies a higher normalization, resulting in problems with excessive pairwise galaxy velocity dispersion unless a strong velocity bias is present. Although we confirm the strong velocity bias of halos reported by Couchman \& Carlberg (1992), we show that the galaxy motions are still too large on small scales. We find no amplitude for which the CDM model can reconcile simultaneously the galaxy correlation function, the low pairwise velocity dispersion, and the richness distribution of groups and clusters. With the normalization implied by COBE, the CDM spectrum has too much power on small scales if $Ω=1$.

astro-ph↗

arXiv1994

Do Galactic Systems Form Too Late in Cold+Hot Dark Matter Models?

The abundance of galactic systems at high redshifts can impose a strong constraint on the cold+hot dark matter (CDM+HDM) models. The hot component reduces the excessive small-scale power in the COBE-normalized CDM model but also delays the epoch of galaxy formation. We present results from the first numerical simulations that have enough dynamic range to address accurately the issue of high-redshift halo abundances in CDM+HDM models. Equivalent high-resolution particle-particle/particle-mesh $N$-body simulations are performed for spatially flat models with $Ω_ν=0.3$ and 0.2 (with $H_0=50$ km s$^{-1}$ Mpc$^{-1}$ and $Ω_b=0.05$). We study the constraints placed on the models by the high-redshift quasar space density and by the mass fraction in neutral dense gas associated with damped Ly$α$ systems. We find that even with optimistic assumptions, the much-studied $Ω_ν=0.3$ model does not produce enough massive halos to account for the observed abundance of quasars at $z>4$. The model passes this test if $Ω_ν$ is decreased to 0.2. Both models do not produce enough high column-density halos to account for the amount of gas in damped Ly$α$ systems at $z\go 3$: the $Ω_ν=0.3$ model falls short by a factor $\sim$80; the $Ω_ν=0.2$ model by a factor $\sim$3. We conclude that only CDM+HDM models with $Ω_ν\lo 0.2$ can match observations at high redshift, implying an upper bound of 4.7 eV on the most massive light neutrino (presumably the $τ$).

astro-ph↗

arXiv1994

Lagrangian Evolution of the Weyl Tensor

We derive the evolution equations for the electric and magnetic parts of the Weyl tensor for cold dust from both general relativity and Newtonian gravity. In a locally inertial frame at rest in the fluid frame, the Newtonian equations agree with those of general relativity. We give explicit expressions for the electric and magnetic parts of the Weyl tensor in the Newtonian limit. In general, the magnetic part does not vanish, implying that the Lagrangian evolution of the fluid is not purely local.

astro-ph↗

arXiv1994

Gravitational Instability of Cold Matter

We solve the nonlinear evolution of pressureless, irrotational density fluctuations in a perturbed Robertson-Walker spacetime using a new Lagrangian method based on the velocity gradient and gravity gradient tensors. Borrowing results from general relativity, we obtain a set of Newtonian ordinary differential equations for these quantities following a given mass element. Using these Lagrangian fluid equations we prove the following results: (1) The spherical tophat perturbation, having zero shear, is the slowest configuration to collapse for a given initial density and growth rate. (2) Initial density maxima are not generally the sites where collapse first occurs. (3) Initially underdense regions may undergo collapse if the shear is not too small. If the magnetic part of the Weyl tensor vanishes, the nonlinear evolution is described purely locally by our equations; this condition holds for spherical, cylindrical, and planar perturbations and may be a good approximation in other circumstances. Assuming the vanishing of the magnetic part of the Weyl tensor, we compute the exact nonlinear gravitational evolution of cold matter. We find that 56\% of initially underdense regions collapse in an Einstein-de Sitter universe for a homogeneous and isotropic random field. We also show that, given this assumption, the final stage of collapse is generically two-dimensional, leading to strongly prolate filaments rather than Zel'dovich pancakes. While this result may explain the prevalence of filamentary collapses in N-body simulations, it is not true in general, suggesting that the magnetic part of the Weyl tensor need not vanish in the Newtonian limit.

astro-ph↗

arXiv1994

Cosmological Perturbation Theory in the Synchronous vs. Conformal Newtonian Gauge

We present a systematic treatment of the linear theory of scalar gravitational perturbations in the synchronous gauge and the conformal Newtonian (or longitudinal) gauge. We first derive the transformation law relating the two gauges. We then write down in parallel in both gauges the coupled, linearized Boltzmann, Einstein and fluid equations that govern the evolution of the metric perturbations and the density fluctuations of the particle species. The particle species considered include cold dark matter (CDM), baryons, photons, massless neutrinos, and massive neutrinos (a hot dark matter or HDM candidate), where the CDM and baryon components are treated as fluids while a detailed phase-space description is given to the photons and neutrinos. The linear evolution equations presented are applicable to any $Ω=1$ model with CDM or a mixture of CDM and HDM. Isentropic initial conditions on super-horizon scales are derived. The equations are solved numerically in both gauges for a CDM+HDM model with $Ω_{\rm cold}=0.65,$ $Ω_{\rm hot}=0.3$, and $Ω_{\rm baryon}=0.05$. We discuss the evolution of the metric and the density perturbations and compare their different behaviors outside the horizon in the two gauges. In a companion paper we integrate the geodesic equations for the neutrino particles in the perturbed conformal Newtonian background metric computed here. The purpose is to obtain an accurate sampling of the neutrino phase space for the HDM initial conditions in $N$-body simulations of the CDM+HDM models.

astro-ph↗

arXiv1993

Cosmic Structure Formation

This article reviews the prevailing paradigm for how galaxies and larger structures formed in the universe: gravitational instability. Basic observational facts are summarized to motivate the standard cosmological framework underlying most detailed investigations of structure formation. The observed universe approaches spatial uniformity on scales larger than about $10^{26}$ cm. On these scales gravitational dynamics is almost linear and therefore relatively easy to relate to observations of large-scale structure. On smaller scales cosmic structure is complicated not only by nonlinear gravitational clustering but also by nonlinear nongravitational gas dynamical processes. The complexity of these phenomena makes galaxy formation one of the grand challenge problems of the physical sciences. No fully satisfactory theory can presently account in detail for the observed cosmic structure. However, as this article summarizes, significant progress has been made during the last few years.

astro-ph↗

arXiv1993

Amplitude of Primeval Fluctuations from Cosmological Mass Density Reconstructions

We use the POTENT reconstruction of the mass density field in the nearby universe to estimate the amplitude of the density fluctuation power spectrum for various cosmological models. We find sigma_8Ω_m^{0.6}= 1.3^{+0.4}_{-0.3}, almost independently of the power spectrum. This value agrees well with the COBE normalization for the standard CDM model, while some alternative models predict an excessive amplitude compared with COBE. Flat low Ω_m models and tilted models with spectral index n<0.8 are particularly discordant.

astro-ph↗

arXiv1993

Second Order Power Spectrum and Nonlinear Evolution at High Redshift

The Eulerian cosmological fluid equations are used to study the nonlinear mode coupling of density fluctuations. We evaluate the second-order power spectrum including all four-point contributions. In the weakly nonlinear regime we find that the dominant nonlinear contribution for realistic cosmological spectra is made by the coupling of long-wave modes and is well estimated by second order perturbation theory. For a linear spectrum like that of the cold dark matter model, second order effects cause a significant enhancement of the high $k$ part of the spectrum and a slight suppression at low $k$ near the peak of the spectrum. Our perturbative results agree well in the quasilinear regime with the nonlinear spectrum from high-resolution N-body simulations. We find that due to the long-wave mode coupling, characteristic nonlinear masses grow less slowly in time (i.e., are larger at higher redshifts) than would be estimated using the linear power spectrum. For the cold dark matter model at $(1+z)=(20,10,5,2)$ the nonlinear mass is about $(180,8,2.5,1.6)$ times (respectively) larger than a linear extrapolation would indicate, if the condition rms $δρ/ρ=1$ is used to define the nonlinear scale. At high redshift the Press-Schechter mass distribution significantly underestimates the abundance of high-mass objects for the cold dark matter model. Although the quantitative results depend on the definition of the nonlinear scale, these basic consequences hold for any initial spectrum whose post-recombination spectral index $n$ decreases sufficiently rapidly with increasing $k$, a feature which arises quite generally during the transition from a radiation- to matter-dominated universe.

astro-ph↗

arXiv1993

Evolution of One-Point Distributions from Gaussian Initial Fluctuations

We study the quasilinear evolution of the one-point probability density functions (PDFs) of the smoothed density and velocity fields in a cosmological gravitating system beginning with Gaussian initial fluctuations. Our analytic results are based on the Zel'dovich approximation and laminar flow. A numerical analysis extends the results into the multistreaming regime using the smoothed fields of a CDM N-body simulation. We find that the PDF of velocity, both Lagrangian and Eulerian, remains Gaussian under the laminar Zel'dovich approximation, and it is almost indistinguishable from Gaussian in the simulations. The PDF of mass density deviates from a normal distribution early in the quasilinear regime and it develops a shape remarkably similar to a lognormal distribution with one parameter, the \rms density fluctuation $σ$. Applying these results to currently available data we find that the PDFs of the velocity and density fields, as recovered by the \pot\ procedure from observed velocities assuming $Ω=1$, or as deduced from a redshift survey of \iras\ galaxies assuming that galaxies trace mass, are consistent with Gaussian initial fluctuations.

astro-ph↗

arXiv1993

Particle-Mesh Methods on the Connection Machine

We describe an efficient Particle-Mesh algorithm for the Connection Machine CM-5. Our particular method parallelizes well and the computation time per time step decreases as the particles become more clustered. We achieve floating-point computation rates of 4--5 MFlops/sec/processing node and total operations (the sum of floating-point and integer arithmetic plus communications) of 5--10 MOps/sec/processing node. The rates scale almost linearly from 32 to 256 processors. Although some of what we discuss is specific to the CM-5, many aspects (e.g., the computation of the force on a mesh) are generic to all implementations, and other aspects (e.g., the algorithm for assignment of the density to the mesh) are useful on any parallel computer.

comp-gas↗

arXiv1993

Nonlinear Effects due to the Coupling of Long-Wave Modes

The cosmological fluid equations are used to study the nonlinear mode coupling of density fluctuations. We find that for realistic cosmological spectra there is a significant contribution to the nonlinear evolution on scales of interest to large-scale structure from the long-wave part of the initial spectrum. A consequence of this mode coupling is that at high redshift, $z$, the nonlinear scale [defined by $σ(z)=1$] can be significantly larger than a linear extrapolation would indicate. For the standard CDM spectrum with a $σ_8=1$ normalization the mass corresponding to the nonlinear scale at $z=20, 10, 5$ is about $100, 10, 3$ times (respectively) larger than the linearly extrapolated value. We also investigate the possibility of divergent contributions to the density field from long-wave modes if the spectral index of the power spectrum $\ n<-1$. Using an approximate non-perturbative approach we find that for $n>-3\,$ the divergent contribution appears only in the phase. This can be related to the large-scale bulk velocity, and clarifies previous results from N-body simulations.

astro-ph↗

arXiv1993

Kinematical and Dynamical Approaches to Gravitational Instability

This paper reviews the essential physics of gravitational instability in a Robertson-Walker background spacetime. Three approaches are presented in a pedagogical manner, based on (1) the Eulerian fluid equations, (2) the Lagrangian description of trajectories, and (3) the Lagrangian fluid equations. Linear and nonlinear limits are discussed for each case. Shear and tides are shown to play a key role in nonlinear gravitational instability. The Lagrangian fluid approach is used to show that several widely held beliefs about gravitational instability are false. The following collapse theorem is proven: for a given initial density fluctuation and growth rate, the spherical tophat perturbation collapses more slowly than any other configuration. We also show that density maxima are not the first points to collapse and that underdense regions may collapse if their initial shear is sufficiently high. The Lagrangian fluid approach leads to an almost closed set of local evolution equations for individual mass elements. The magnetic part of the Weyl tensor, which may be present even in the nonrelativistic (Newtonian) limit, may prevent a purely local description. However, neglecting the magnetic part of the Weyl tensor, we obtain predictions for high-redshift collapse that are in good agreement with a high-resolution cold dark matter N-body simulation.

astro-ph↗