Xiaohu Yang (SJTU/SHAO) With: H. Wang, H.J. Mo, Y.P. Jing, F.C van den Bosch, W.P. Lin, D. Tweed… 2014.11.04, KIAS Exploring the Local Universe with re-

Xiaohu Yang (SJTU/SHAO)

With: H. Wang, H.J. Mo, Y.P. Jing, F.C van den Bosch, W.P. Lin, D. Tweed2014.11.04, KIASExploring the Local Universe with re-Constructed Initial Density fields ELUCID

Motivation

Shortcomings in comparing theory (simulations) with data in a statistical way: (1) cosmic variance (environmental effects); (2) only part of information is used.

If we can accurately reconstruct the initial condition of the local Universe, we can compare data and theory directly.

The ELUCID Project

Finding galaxy groups in SDSS DR7Sky coverage: 7748 deg^2

Galaxies with redshifts: 639359

Groups are found and assigned with halo masses

Reconstruct the current density fieldusing halos above a certain mass

Method:(1) Each point in space is assigned to its nearest halo according to distance scaled by halo virial radius;

(2) The density at the point is given by the cross-correlation between halos and mass given by the chosen cosmological model.

Test with mock catalogssimulation + halo occupation + SDSS selection function + redshift space + group finder

The SDSS MTV

First, the linear density field (k) should obey the following distribution:

Second, the density field, mod, evolved from (k), should match a given final density field f. We seek the appropriate (k) to minimize a cost parameter:

Assuming that the likelihood of mod given f is exp(-2), the posterior probability distribution for (k) given f can be written as:

We seek the solutions for (k) that maximize this posterior probability distribution function or sample the distribution.Hamiltonian Markov Chain Monte Carlo Method(prior)(likelihood)

Phase correlationK95: the k that haveCp=0.95

ZA: k95~0.3 h/Mpc (Nusser & Dekel 1992; many previous works)MZA: k95=0.33 h/Mpc (Wang et al. 2013)2LPT: k95=0.37 h/Mpc (Jasche & Wandelt 2013; Kitaura 2013)ALPT: k95=0.45 h/Mpc (He et al. 2013)Particle-Mesh dynamics

Checking the properties of the halos2-way halo matching: halos in catalog A and B:halos are associated by tracing particles ids only, NOT halo positionswhen comparing A to B, several halos in A can be associated to a single halo in Bwhen comparing B to A, several halos in B can be associated to a single halo in AWe consider halos in A and B to be a "match", if only the association is consistent when I compare A to B and B to A.We consider halos in one catalog to be a "double", if the association only goes one way.

Test with SDSS Mock Catalogs

Application to SDSS

Formation of Coma Cluster

Velocity field

In a void region

Coherent motionNo tracers here

Model:Galaxy properties: galaxy redshift survey;ISM properties: 21cm emission, millimeter/submillimeter emissions;IGM properties: quasar absorption line systems; X-ray observations; Sunyaev-Zeldovich effect.N-body+ hydrodynamics simulation of local Universe (including radiative cooling, star formation and feedback)Semi-analytical model of galaxy formation Observation: