ELUCID - Exploring the Local Universe with reConstructed Initial Density field I: Hamiltonian Markov Chain Monte Carlo Method with Particle Mesh Dynamics

Abstract

Simulating the evolution of the local universe is important for studying galaxies and the intergalactic medium in a way free of cosmic variance. Here we present a method to reconstruct the initial linear density field from an input non-linear density field, employing the Hamiltonian Markov Chain Monte Carlo (HMC) algorithm combined with Particle Mesh (PM) dynamics. The HMC+PM method is applied to cosmological simulations, and the reconstructed linear density fields are then evolved to the present day with N-body simulations. The constrained simulations so obtained accurately reproduce both the amplitudes and phases of the input simulations at various $z$. Using a PM model with a grid cell size of 0.75 Mpc/h and 40 time-steps in the HMC can recover more than half of the phase information down to a scale k~0.85 h/Mpc at high z and to k~3.4 h/Mpc at z=0, which represents a significant improvement over similar reconstruction models in the literature, and indicates that our model can reconstruct the formation histories of cosmic structures over a large dynamical range. Adopting PM models with higher spatial and temporal resolutions yields even better reconstructions, suggesting that our method is limited more by the availability of computer resource than by principle. Dynamic models of structure evolution adopted in many earlier investigations can induce non-Gaussianity in the reconstructed linear density field, which in turn can cause large systematic deviations in the predicted halo mass function. Such deviations are greatly reduced or absent in our reconstruction.

45 pages, 16 figures, accepted for publication in ApJ

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Cited by in corpus (17)

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• ELUCID - Exploring the Local Universe with reConstructed Initial Density field III: Constrained Simulation in the SDSS Volume
• SDSS-IV MaNGA: environmental dependence of stellar age and metallicity gradients in nearby galaxies
• Galaxy groups in the low-redshift Universe
• Simulations of ultra-high Energy Cosmic Rays in the local Universe and the origin of Cosmic Magnetic Fields
• ELUCID IV: Galaxy Quenching and its Relation to Halo Mass, Environment, and Assembly Bias
• SIBELIUS-DARK: a galaxy catalogue of the Local Volume from a constrained realisation simulation
• Impacts of the physical data model on the forward inference of initial conditions from biased tracers
• Galaxy groups in the 2MASS Redshift Survey
• Halo intrinsic alignment: dependence on mass, formation time and environment
• The Local Group in the cosmic web
• SDSS-IV MaNGA: Environmental dependence of the Mgb/<Fe>-sigma_* relation for nearby galaxies
• Connections between galaxy properties and halo formation time in the cosmic web
• Virgo: an unlikely cluster of galaxies because of its environment
• Predicting Structures in the Zone of Avoidance
• Efficiently estimating mean, uncertainty and unconstrained large scale fraction of local Universe simulations with paired fixed fields
• The Impact of Baryons on the Large-Scale Structure of the Universe