# V. Mueller - AIP-Potsdam

## Contact Details

NameV. Mueller |
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AffiliationAIP-Potsdam |
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CityPotsdam |
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CountryGermany |
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## Pubs By Year |
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## Pub CategoriesAstrophysics (27) Cosmology and Nongalactic Astrophysics (5) Astrophysics of Galaxies (2) High Energy Physics - Theory (1) Physics - Disordered Systems and Neural Networks (1) Physics - Statistical Mechanics (1) |

## Publications Authored By V. Mueller

**Authors:**Sebastian E. Nuza

^{1}, Francisco-Shu Kitaura

^{2}, Steffen Hess

^{3}, Noam I. Libeskind

^{4}, Volker Mueller

^{5}

**Affiliations:**

^{1}AIP-Potsdam,

^{2}AIP-Potsdam,

^{3}AIP-Potsdam,

^{4}AIP-Potsdam,

^{5}AIP-Potsdam

We present, for the first time, a Local Universe (LU) characterization using high precision constrained $N$-body simulations based on self-consistent phase-space reconstructions of the large-scale structure in the Two-Micron All-Sky Galaxy Redshift Survey. We analyse whether we live in a special cosmic web environment by estimating cosmic variance from a set of unconstrained $\Lambda$CDM simulations as a function of distance to random observers. By computing volume and mass filling fractions for voids, sheets, filaments and knots, we find that the LU displays a typical scatter of about $1\sigma$ at scales $r>15\,h^{-1}\,{\rm Mpc}$, in agreement with $\Lambda$CDM, converging to a fair unbiased sample when considering spheres of about $60\,h^{-1}\,{\rm Mpc}$ radius. Read More

We present the first theoretical study of metals in damped Ly-alpha (DLA) systems at redshift z=7. The features of cold, primordial gas are studied by means of N-body, hydro, chemistry simulations, including atomic and molecular non-equilibrium chemistry, cooling, star formation for population III and population II-I regimes, stellar evolution, cosmic metal spreading according to proper yields (for He, C, O, Si, Fe, Mg, S, etc.) and lifetimes, and feedback effects. Read More

In this work we introduce a new method to perform the identification of groups of galaxies and present results of the identification of galaxy groups in the Seventh Data Release of the Sloan Digital Sky Survey (SDSS-DR7). Our methodology follows an approach that resembles the standard friends-of-friends (FoF) method. However, it uses assumptions on the mass of the dark matter halo hosting a group of galaxies to link galaxies in the group using a local linking length. Read More

A quantitative study of the clustering properties of the cosmic web as a function of absolute magnitude and colour is presented using the SDSS Data Release 7 galaxy survey. Mark correlations are included in the analysis. We compare our results with mock galaxy samples obtained with four different semi-analytical models of galaxy formation imposed on the merger trees of the Millenium simulation. Read More

**Affiliations:**

^{1}Leibniz-Institut Fuer Astrophysik Potsdam,

^{2}Leibniz-Institut Fuer Astrophysik Potsdam,

^{3}Leibniz-Institut Fuer Astrophysik Potsdam

**Category:**Cosmology and Nongalactic Astrophysics

We present the implementation of a halo based method for the reconstruction of the cosmic mass density field. The method employs the mass density distribution of dark matter haloes and its environments computed from cosmological N-body simulations and convolves it with a halo catalog to reconstruct the dark matter density field determined by the distribution of haloes. We applied the method to the group catalog of Yang etal (2007) built from the SDSS Data Release 4. Read More

We present a morphological study of the two richest superclusters from the 2dF Galaxy Redshift Survey (SCL126, the Sloan Great Wall, and SCL9, the Sculptor supercluster). We use Minkowski functionals, shapefinders, and galaxy group information to study the substructure of these superclusters as formed by different populations of galaxies. We compare the properties of grouped and isolated galaxies in the core region and in the outskirts of superclusters. Read More

**Authors:**Joerg M. Colberg

^{1}, Frazer Pearce

^{2}, Caroline Foster

^{3}, Erwin Platen

^{4}, Riccardo Brunino

^{5}, Mark Neyrinck

^{6}, Spyros Basilakos

^{7}, Anthony Fairall

^{8}, Hume Feldman

^{9}, Stefan Gottloeber

^{10}, Oliver Hahn

^{11}, Fiona Hoyle

^{12}, Volker Mueller

^{13}, Lorne Nelson

^{14}, Manolis Plionis

^{15}, Cristiano Porciani

^{16}, Sergei Shandarin

^{17}, Michael S. Vogeley

^{18}, Rien van de Weygaert

^{19}

**Affiliations:**

^{1}Carnegie-Mellon University,

^{2}University of Nottingham,

^{3}Bishop's University,

^{4}University of Groningen,

^{5}University of Nottingham,

^{6}University of Hawaii,

^{7}National Observatory Athens,

^{8}University of Cape Town,

^{9}University of Kansas,

^{10}Astrophysikalisches Institut Potsdam,

^{11}ETH Zurich,

^{12}Widener University,

^{13}Astrophysikalisches Institut Potsdam,

^{14}Bishop's University,

^{15}National Observatory Athens,

^{16}ETH Zurich,

^{17}University of Kansas,

^{18}Drexel University,

^{19}University of Groningen

**Category:**Astrophysics

Despite a history that dates back at least a quarter of a century studies of voids in the large--scale structure of the Universe are bedevilled by a major problem: there exist a large number of quite different void--finding algorithms, a fact that has so far got in the way of groups comparing their results without worrying about whether such a comparison in fact makes sense. Because of the recent increased interest in voids, both in very large galaxy surveys and in detailed simulations of cosmic structure formation, this situation is very unfortunate. We here present the first systematic comparison study of thirteen different void finders constructed using particles, haloes, and semi--analytical model galaxies extracted from a subvolume of the Millennium simulation. Read More

For the 2dFGRS we study the properties of voids and of fainter galaxies within voids that are defined by brighter galaxies. Our results are compared with simulated galaxy catalogues from the Millenium simulation coupled with a semianalytical galaxy formation recipe. We derive the void size distribution and discuss its dependence on the faint magnitude limit of the galaxies defining the voids. Read More

We investigate the origin and evolution of fossil groups in a concordance LCDM cosmological simulation. We consider haloes with masses between $(1-5)\times10^{13} \hMsun$ and study the physical mechanisms that lead to the formation of the large gap in magnitude between the brightest and the second most bright group member, which is typical for these fossil systems. Fossil groups are found to have high dark matter concentrations, which we can relate to their early formation time. Read More

**Authors:**Dominik Bomans

^{1}, Elvira Krusch

^{2}, Ralf-Juergen Dettmar

^{3}, Volker Mueller

^{4}, Chris Taylor

^{5}

**Affiliations:**

^{1}Astronomical Institute of the Ruhr-University Bochum,

^{2}Astronomical Institute of the Ruhr-University Bochum,

^{3}Astronomical Institute of the Ruhr-University Bochum,

^{4}Astrophysikalisches Institut Potsdam,

^{5}California State University, Sacramento

**Category:**Astrophysics

We observed 5 Hickson Compact Groups with the ESO/MPI 2.2m telescope and WFI to investigate the dwarf galaxy content and distribution in these galaxy groups. Our deep imaging and careful selection of the candidate galaxies revealed a rich population of mainly passively evolving dwarf galaxies, which is spatially much more extended than the originally defined Hickson Compact groups. Read More

The aim of the present work is to show that, contrary to popular belief, galaxy clusters are **not** expected to be self-similar, even when the only energy sources available are gravity and shock-wave heating. In particular, we investigate the scaling relations between mass, luminosity and temperature of galaxy groups and clusters in the absence of radiative processes. Theoretical expectations are derived from a polytropic model of the intracluster medium and compared with the results of high-resolution adiabatic gasdynamical simulations. Read More

We use the 2dF Galaxy Redshift Survey data to compile catalogues of superclusters for the Northern and Southern regions of the 2dFGRS, altogether 543 superclusters at redshifts 0.009 < z < 0.2. Read More

We study the contribution of stochastic motion of a domain wall (DW) to the dielectric AC susceptibility for low frequencies. Using the concept of waiting time distributions, which is related to the energy landscape of the DW in a disordered medium, we derive the power-law behavior of the complex susceptibility observed recently in some ferroelectrics below Curie temperature. Read More

**Affiliations:**

^{1}AIP Potsdam,

^{2}AIP Potsdam

**Category:**Astrophysics

We analyze quasi-2-dimensional slices of the SDSS EDR. Gaussian smoothing with weighting by the inverse of the selection function provides 2D density fields across the full survey depth. Superclusters (SC) are characterized by a percolation algorithm in the large-scale smoothed field. Read More

**Affiliations:**

^{1}University of Oxford,

^{2}Universidad Autonoma de Madrid,

^{3}Astrophysikalisches Institut Potsdam,

^{4}Astrophysikalisches Institut Potsdam

**Category:**Astrophysics

The radial mass distribution of dark matter haloes is investigated within the framework of the spherical infall model. We present a new formulation of spherical collapse including non-radial motions, and compare the analytical profiles with a set of high-resolution N-body simulations ranging from galactic to cluster scales. We argue that the dark matter density profile is entirely determined by the initial conditions, which are described by only two parameters: the height of the primordial peak and the smoothing scale. Read More

**Affiliations:**

^{1}University of Oxford,

^{2}Universidad Autonoma de Madrid,

^{3}Astrophysikalisches Institut Potsdam,

^{4}Astrophysikalisches Institut Potsdam

**Category:**Astrophysics

Simple self-consistent models of galaxy groups and clusters are tested against the results of high-resolution adiabatic gasdynamical simulations. We investigate two models based on the existence of a 'universal' dark matter density profile and two versions of the beta-model. The mass distribution of relaxed clusters can be fitted by phenomenological formulae proposed in the literature. Read More

**Affiliations:**

^{1}AIP,

^{2}LMU,

^{3}AIP,

^{4}AIP

**Category:**Astrophysics

The relative orientation of clusters' major elongation axes and clusters' angular momentum is studied using a large N-body simulation in a box of 500 Mpc/h base length for a standard LambdaCDM model. Employing the technique of mark correlation functions, we successfully separated the correlations in the orientation from the well known clustering signal traced by the two-point correlation function. The correlations in the orientation are highly significant for our sample of 3000 clusters. Read More

**Authors:**Stefan Gottloeber

^{1}, Martin Kerscher

^{2}, Andrey V. Kravtsov

^{3}, Andreas Faltenbacher

^{4}, Anatoly Klypin

^{5}, Volker Mueller

^{6}

**Affiliations:**

^{1}AIP,

^{2}LMU,

^{3}CfCP, U.Chicago,

^{4}AIP,

^{5}NMSU,

^{6}AIP

**Category:**Astrophysics

We use a novel statistical tool, the mark correlation functions (MCFs), to study clustering of galaxy-size halos as a function of their properties and environment in a high-resolution numerical simulation of the LambdaCDM cosmology. We applied MCFs using several types of continuous and discrete marks: maximum circular velocity of halos, merger mark indicating whether halos experienced or not a major merger in their evolution history, and a stripping mark indicating whether the halo underwent a tidal stripping. We find that halos which experienced a relatively early (z>1) major merger or mass loss (due to tidal stripping) in their evolution histories are over-abundant in halo pairs with separations < 3 Mpc/h. Read More

The cosmic star formation history in Cold Dark Matter dominated cosmological scenarios is studied by means of hydrodynamical numerical simulations. In particular, we explore a low density model with a Lambda-term and two high density models with different power spectra, all of them being spatially flat. Our simulations employ a fully nonlinear N-body and Eulerian hydrodynamics algorithm with a model for star formation and supernovae feedback that depends on two phenomenological parameters determined in agreement with previous papers. Read More

**Affiliations:**

^{1}Astrophysikalisches Institut Potsdam,

^{2}Astrophysikalisches Institut Potsdam

**Category:**Astrophysics

An analysis of voids using cosmological N-body simulations of cold dark matter models is presented. It employs a robust statistics of voids, that was recently applied to discriminate between data from the Las Campanas Redshift Survey and different cosmological models. Here we extend the analysis to 3D and show that typical void sizes D in the simulated galaxy samples obey a linear scaling relation with the mean galaxy separation lambda: D=D_0+nu*lambda. Read More

**Affiliations:**

^{1}Astroph. Inst. Potsdam,

^{2}Astroph. Inst. Potsdam

**Category:**Astrophysics

We have analyzed the size distribution of voids in 2D slices of the Las Campanas Redshift Survey (LCRS). The characteristic sizes show a scaling $D = D_0 + \nu\lambda$ with the mean galaxy separation $\lambda$. Comparison with mock samples of the LCRS in 2D and 3D, using various simulations, cosmologies and galaxy identification schemes, gives a similar scaling, but with steeper slope and a lack of large voids. Read More

We present a measure of the power spectrum on scales from 15 to 800 Mpc/h using the ROSAT-ESO Flux-Limited X-Ray(REFLEX) galaxy cluster catalogue. The REFLEX survey provides a sample of the 452 X-ray brightest southern clusters of galaxies with the nominal flux limit S=3.0 10^{-12}erg/s/cm2 for the ROSAT energy band (0. Read More

The large scale matter distribution in three different simulations of CDM models is investigated and compared with corresponding results of the Zel'dovich theory of nonlinear gravitational instability. We show that the basic characteristics of wall-like structure elements are well described by this theory, and that they can be expressed by the cosmological parameters and a few spectral moments of the perturbation spectrum. Therefore the characteristics of such elements provide reasonable estimates of these parameters. Read More

**Affiliations:**

^{1}Potsdam,

^{2}Potsdam,

^{3}Tartu,

^{4}Batavia

**Category:**Astrophysics

We have analyzed the distribution of void sizes in the two-dimensional slices of the Las Campanas Redshift Survey (LCRS). Fourteen volume-limited subsamples were extracted from the six slices to cover a large part of the survey and to test the robustness of the results against cosmic variance. Thirteen samples were randomly culled to produce homogeneously selected samples. Read More

**Affiliations:**

^{1}Oxford,

^{2}AIP Potsdam

**Category:**Astrophysics

Substructure in galaxy clusters can be quantified with the robust Delta statistics (Dressler and Shectman 1988) which uses velocity kinematics and sky projected positions. We test its sensitivity using dissipationless numerical simulations of cluster formation. As in recent observations, about 30 % of the simulated clusters show substructure, but the exact percentage depends on the chosen limit for defining substructure, and a better discriminator is the distribution function of the Delta statistics. Read More

**Affiliations:**

^{1}Ecole Polytechnique,

^{2}Universitaet Kaiserslautern

**Category:**High Energy Physics - Theory

The proof given in the paper was incomplete due to an omission in the proof of Lemma 2. A corrected and improved version of the paper is in arXiv:0902.2486. Read More

The formation, inner properties, and spatial distribution of galaxy groups and clusters are closely related to the background cosmological model. We use numerical simulations of variants of the CDM model with different cosmological parameters and distinguish relaxed objects from recent mergers using the degree of virialisation. Mergers occur mostly in deep potential wells and mark the most important structure formation processes. Read More

Using extensive N-body simulations we estimate redshift space power spectra of clusters of galaxies for different cosmological models (SCDM, TCDM, CHDM, Lambda-CDM, OCDM, BSI, tau-CDM) and compare the results with observational data for Abell-ACO clusters. Our mock samples of galaxy clusters have the same geometry and selection functions as the observational sample which contains 417 clusters of galaxies in a double cone of galactic latitude |b| > 30 degrees up to a depth of 240 Mpc/h. The power spectrum has been estimated for wave numbers k in the range 0. Read More

**Authors:**D. L. Tucker

^{1}, A. Oemler, Jr.

^{2}, R. P. Kirshner

^{3}, H. Lin

^{4}, S. A. Shectman

^{5}, S. D. Landy

^{6}, P. L. Schechter

^{7}, V. Mueller

^{8}, S. Gottloeber

^{9}, J. Einasto

^{10}

**Affiliations:**

^{1}FNAL/AIP,

^{2}OCIW/Yale,

^{3}CFA,

^{4}Toronto,

^{5}OCIW,

^{6}OCIW,

^{7}MIT,

^{8}AIP,

^{9}AIP,

^{10}Tartu

**Category:**Astrophysics

Presented are measurements of the observed redshift-space galaxy-galaxy autocorrelation function, xi(s), for the Las Campanas Redshift Survey (LCRS). For separations 2.0/h Mpc < s < 16. Read More

High resolution $N$-body simulations for variants of the CDM model are used to derive the redshift dependence of galaxy formation and of galaxy correlation functions. The reconstructed power spectra and clustering properties provide a sensible test for the underlying power spectra. We compare our simulations with new results of the analysis of recent redshift surveys. Read More

Standard inflation with one scalar field produces primordial perturbations with a nearly flat ('Harrison-Zeldovich') power spectrum. Here we consider first, a double inflation spectrum, and second, a massive scalar field with an interaction potential which mimics an early quartic interaction, but fading away at a characteristic scale. We solve numerically the linear perturbation equations with initial conditions due to scalar field quantum fluctuations at the initial horizon crossing. Read More

A double inflationary model provides perturbation spectra with enhanced power at large scales (Broken Scale Invariant perturbations -- BSI), leading to a promising scenario for the formation of cosmic structures. We describe a series of high-resolution PM simulations with a model for the thermodynamic evolution of baryons in which we are capable of identifying 'galaxy' halos with a reasonable mass spectrum and following the genesis of large and super-large scale structures. The power spectra and correlation functions of 'galaxies' are compared with reconstructed power spectra of the CfA catalogue and the correlation functions of the Las Campanas Deep Redshift Survey. Read More

A quantitative theory, based on the Zeldovich approximation, to provide an approximate description of the evolution of structure is presented. We give an expression for the characteristic scale of superlarge-scale structure which can also be applied to power spectra with a Harrison-Zeldovich asymptotic. The evolution of the characteristic scale of large-scale structure is described with an analytical expression. Read More

To test the primordial power spectra predicted by a double inflationary model with a break of amplitude $\Delta=3$ at a scale of $2\pi/k\approx 10 \hm$ and CDM as dominant matter content, we perform PM simulations with 128$^3$ particles on a 256$^3$ grid. The broken scale invariance of the power spectra explains the extra power observed in the large-scale matter distribution. COBE-normalized spectra and a linear biasing with $b\approx 2$ are shown to reproduce the reconstructed power spectra from the CfA catalog. Read More