ELUCID simulation data

SDSS-ELUCID matched data available now. 

Introduction

In order to make full use of the potential of the observational data, one has to develop or make use of optimal strategies. One of the most efficient ways of using the observational data is to carry out constrained simulations where the initial density field is extracted from the observations, which is the basic idea of our ELUCID (Exploring the Local Universe with reConstructed Initial Density field ) project. Based on the SDSS DR7 observatoin, we constructed the group catalogs where galaxy groups are closly associated with dark matter halos (Yang et al. 2007, 2012). The group (halo) catalog is then used to creat the mass density field of our local Universe (Wang et al. 2012). Using a method combining the Bayesian reconstruction approach with an accurate dynamic model of structure evolution, the Particle Mesh (PM) model, Wang et al. (2014) reproduced the initial density field of our local Universe. We run N-body simulation with this set of initial conditions using 3072^3 particles in a cubic box with side length L=500Mpc/h at SJTU HPC.

N-body simulation data

Shown in the left to right panels are the projected distributions of groups in real space, the mass density and ELUCID simulation density fields, respectively.

Cubic box cordinates Readme 0.1% DM particles subhalos host halos

SDSS cordinates Readme subhalos host halos

References

Galaxy Groups in the SDSS DR4. I. The Catalogue and Basic Properties
Yang X., Mo H.J., van den Bosch F.C., Pasquali A., Li C., Barden M., 2007, ApJ, 671, 153

Evolution of the Galaxy-Dark Matter Connection and the Assembly of Galaxies in Dark Matter Halos
Yang X., Mo H.J., van den Bosch F.C.,Zhang, Youcai; Han, Jiaxin 2012, ApJ, 752, 41

Reconstructing the cosmic density field with the distribution of dark matter haloes
Wang H., Mo H.J., Jing Y.P., Guo Y. , van den Bosch F.C., Yang X., 2009, MNRAS, 394, 398

Reconstructing the Cosmic Velocity and Tidal Fields with Galaxy Groups Selected from the Sloan Digital Sky Survey
Wang H., Mo H.J., Yang X., van den Bosch F.C., 2012, MNRAS, 420, 1809

ELUCID-Exploring the Local Universe with the Reconstructed Initial Density Field. I. Hamiltonian Markov Chain Monte Carlo Method with Particle Mesh Dynamics
Wang H., Mo H.J., Yang X., Jing Y.P., Lin W.P., 2014, ApJ, 794, 94

ELUCID - Exploring the Local Universe with ReConstructed Initial Density Field III: Constrained Simulation in the SDSS Volume
Wang H., Mo H.J., Yang X., Zhang Y., Shi J., Jing Y.P., Liu C., et al., 2016, ApJ, 831, 164

SDSS galaxies matched with subhalos

Shown in the below plot from left to right panels are the distributions of SDSS galaxies, the density field and the reconstructed density field, respectively. Here we use a neighborhood abundance matching method to light the dark matter halos and subhalos in the reconstructed region in the simulation with galaxies in the SDSS observations (Yang et al. 2018).

SDSS DR7 matched subhalos Readme Galaxy-subhalo match halo and galaxy properties

References

ELUCID. V. Lighting Dark Matter Halos with Galaxies
Yang X., Zhang Y., Wang H., Liu C., Lu T., Li S., Shi F., et al., 2018, ApJ, 860, 30.

ELUCID. VI. Cosmic Variance of the Galaxy Distribution in the Local Universe
Chen Y., Mo H.J., Li C., Wang H., Yang X., Zhou S., Zhang Y., 2019, ApJ, 872, 180

Connections between galaxy properties and halo formation time in the cosmic web
Zhang Y., Yang X., Guo H., 2021, MNRAS, 507, 5320

Comments to:  xyang@sjtu.edu.cn