Publications (7)27.94 Total impact
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ABSTRACT: We introduce and explore "paired" cosmological simulations. A pair consists of an A and B simulation with initial conditions related by the inversion $\delta_A(x, t_{initial})=\delta_B(x,t_{initial})$ (underdensities substituted for overdensities and vice versa). We argue that the technique is valuable for improving our understanding of cosmic structure formation. The A and B fields are by definition equally likely draws from {\Lambda}CDM initial conditions, and in the linear regime evolve identically up to the overall sign. As nonlinear evolution takes hold, a region that collapses to form a halo in simulation A will tend to expand to create a void in simulation B. Applications include (i) contrasting the growth of Ahalos and Bvoids to test excursionset theories of structure formation; (ii) crosscorrelating the density field of the A and B universes as a novel test for perturbation theory; and (iii) canceling error terms by averaging power spectra between the two boxes. Generalizations of the method to more elaborate field transformations are suggested. 
Article: Genetically modified halos: towards controlled experiments in $\Lambda$CDM galaxy formation
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ABSTRACT: We propose a method to generate `geneticallymodified' (GM) initial conditions for highresolution simulations of galaxy formation in a cosmological context. Building on the HoffmanRibak algorithm, we start from a reference simulation with fully random initial conditions, then make controlled changes to specific properties of a single halo (such as its mass and merger history). The algorithm demonstrably makes minimal changes to other properties of the halo and its environment, allowing us to isolate the impact of a given modification. As a significant improvement over previous work, we are able to calculate the abundance of the resulting objects relative to the $\Lambda$CDM reference cosmology. Our approach can be applied to a wide range of cosmic structures and epochs; here we study two problems as a proofofconcept. First, we investigate the change in density profile and concentration as the collapse time of three individual halos are varied at fixed final mass, showing good agreement with previous statistical studies using large simulation suites. Second, we modify the $z=0$ mass of halos to show that our theoretical abundance calculations correctly recover the halo mass function. The results demonstrate that the technique is robust, opening the way to controlled experiments in galaxy formation using hydrodynamic zoom simulations.  [Show abstract] [Hide abstract]
ABSTRACT: Galaxies and the dark matter halos that host them are not spherically symmetric, yet spherical symmetry is a helpful simplifying approximation for idealised calculations and analysis of observational data. The assumption leads to an exact conservation of angular momentum for every particle, making the dynamics unrealistic. But how much does that inaccuracy matter in practice for analyses of stellar distribution functions, collisionless relaxation, or dark matter corecreation? We provide a general answer to this question for a wide class of aspherical systems; specifically, we consider distribution functions that are "maximally stable", i.e. that do not evolve at first order when external potentials (which arise from baryons, large scale tidal fields or infalling substructure) are applied. We show that a sphericallysymmetric analysis of such systems gives rise to the false conclusion that the density of particles in phase space is ergodic (a function of energy alone). Using this idea we are able to demonstrate that: (a) observational analyses that falsely assume spherical symmetry are made more accurate by imposing a strong prior preference for nearisotropic velocity dispersions in the centre of spheroids; (b) numerical simulations that use an idealised sphericallysymmetric setup can yield misleading results and should be avoided where possible; and (c) triaxial dark matter halos (formed in collisionless cosmological simulations) nearly attain our maximallystable limit, but their evolution freezes out before reaching it.  [Show abstract] [Hide abstract]
ABSTRACT: We derive robust constraints on primordial nonGaussianity (PNG) using the clustering of 800,000 photometric quasars from the Sloan Digital Sky Survey in the redshift range $0.5<z<3.5$. These measurements rely on the novel technique of {\it extended mode projection} to control the impact of spatiallyvarying systematics in a robust fashion, making use of blind analysis techniques. This allows the accurate measurement of quasar halo bias at the largest scales, while discarding as little as possible of the data. When constraining the standard localtype PNG parameters $f_\mathrm{NL}$ and $g_\mathrm{NL}$ separately, we obtain (at 95\% CL) $49<f_\mathrm{NL}<31$ and $2.7\times10^5<g_\mathrm{NL}<1.9\times10^5$, while their joint constraints lead to $105<f_\mathrm{NL}<72$ and $4.0\times10^5<g_\mathrm{NL}<4.9\times10^5$. Introducing a running parameter $n_{f_\mathrm{NL}}$ for the effect of $f_\mathrm{NL}$ in the scaledependent quasar bias, we obtain $121<f_\mathrm{NL}<144$, and $0.32<n_{f_\mathrm{NL}}<0.9$. These results incorporate uncertainties in the cosmological parameters, redshift distributions, shot noise, and the bias prescription used to relate the quasar clustering to the underlying dark matter. These are the strongest constraints obtained to date on PNG using a single population of largescale structure tracers, and are already at the level of pre{\it Planck} constraints from the cosmic microwave background. They demonstrate the importance of robustly mitigating systematics in order to exploit upcoming large scale structure surveys to probe the initial conditions of the universe.  [Show abstract] [Hide abstract]
ABSTRACT: We present accurate measurements of the largescale clustering of photometric quasars from the Sloan Digital Sky Survey. These results, detailed in Leistedt & Peiris (2014), rely on a novel technique to identify and treat systematics when measuring angular power spectra, using nulltests and analytical marginalisation. This approach can be used to maximise the extraction of information from current and future galaxy or quasar surveys. For example, it enables to robustly constrain primordial nonGaussianity (PNG), which modifies the bias of galaxies and quasars on large scales – the most sensitive to observational systematics. The constraints on PNG obtained with the quasar power spectra are detailed in Leistedt, Peiris & Roth (2014); these are the most stringent constraints to date obtained with a single tracer of the largescale structure.  [Show abstract] [Hide abstract]
ABSTRACT: The scaledependent galaxy bias generated by primordial nonGaussianity (PNG) can be used to detect and constrain deviations from standard singlefield inflation. The strongest signal is expected in the local model for PNG, where the amplitude of nonGaussianity can be expressed by a set of parameters (ƒNL, gNL, etc.). Current observational constraints from galaxy clustering on ƒNL and gNL assume that the others PNG parameters are vanishing. Using two sets of cosmological Nbody simulations where both fNL and gNL are nonzero, we show that this strong assumption generally leads to biased estimates and spurious redshift dependencies of the parameters. Additionally, if the signs of ƒNL and gNL are opposite, the amplitude of the scaledependent bias is reduced, possibly leading to a false null detection. Finally, we show that model selection techniques like the Bayesian evidence can (and should) be used to determine if more than one PNG parameter is required by the data.  [Show abstract] [Hide abstract]
ABSTRACT: We test thirdorder standard perturbation theory (SPT) as an approximation to nonlinear cosmological structure formation. A novel approach is used to numerically calculate the threedimensional dark matter density field using SPT from the initial conditions of two highresolution cosmological simulations. The calculated density field is compared to the nonlinear dark matter field of the simulations both pointbypoint and statistically. For smoothing scales above 8 Mpc/h it shows a good agreement up to redshift 0. We present a simple fitting formula to relate the linear and nonlinear density contrast that accurately recovers the nonlinear time evolution for 0 <= z <= 10 at the per cent level. To address the problem of biasing between the matter field and the haloes identified in the simulation, we employ the Eulerian local bias model (ELB), including nonlinear bias up to the third order. The bias parameters are obtained by fitting a scatter plot of halo and matter density (both from the simulation and from SPT). Using these bias parameters, we can reconstruct the halo density field. We find that this reconstruction is not able to capture all the details of the halo distribution. We investigate how well the large scale bias can be described by a constant and if it corresponds to the linear bias parameter b_1 of the local bias model. We also discuss how well the halohalo power spectrum and the halomass cross spectrum from the reconstructed halo density field agree with the corresponding statistics from the simulation. The results show that while SPT is an excellent approximation for the matter field for suitably large smoothing scales even at redshift 0, the ELB model can only account for some of the properties of the halo density field.
Publication Stats
48  Citations  
27.94  Total Impact Points  
Top Journals
Institutions

20142015

University College London
 Department of Physics and Astronomy
Londinium, England, United Kingdom


20112012

University of Bonn
 ArgelanderInstitute of Astronomy
Bonn, North RhineWestphalia, Germany
