effects on halo properties MPPG对晕属性 MPPG重子的影响课件.ppt

The Baryonic Effects on the Properties of Dark Matter Haloes Weipeng Lin (Shanghai Astronomical Observatory,CAS) Collaborators: Shude Mao (Univ. of Manchester) Yipeng Jing(Shanghai Astro. Obs.) Liang Gao (NAOC) The 9th Sino-German Workshop on Galaxy Formation and Cosmology, 26-29 April, 2011@HangZhou Basic Facts of Baryon Universal baryon fraction of mass: ~16% (WMAP’s result) DM dominates on large scale, while on small scale, there are spaces (e.g. halo center) where baryon are dominated, and important. Baryon physics, 1st order: gas shock-heating, cooling, star formation, SN/AGN feedback, metal enrichment; 2nd order: heating by UV background cosmic ray, evaporation, ram pressure stripping, gravitational heating, magnetic field, tidal stripping, heat conduction, turbulence, convection, etc. Dynamics: AC effect, dynamical friction of sinking satellites, interaction between rotation disk/bars and halo matter, etc. What halo properties could be influenced by baryon physics? Matter distribution (DM, stellar components, cold/hot gas) of halo, especially at central part of halo Baryon/stellar fraction, temperature/entropy profiles Shape of halo: density or potential well, x-ray halo Properties of halo sub-structures Angular momentum distribution and alignment (of gas, stars and DM) Extended: Gravitational shear field Alignment of matter distribution in DM halo，…… The effects are important for precise cosmology! What we have done so far? We have done a set of N-body/SPH simulations and studied following baryonic effects: Clustering and weak lensing : Jing, et al. 2006, ApJ Galaxy HOD: Zhu, et al. 2006 Galaxy merging time-scale: Jiang et al. 2008 ApJ; AA 2010 Mass distribution and entropy profile: Lin et al. 2006, ApJ Sunyave-Zel’dovich Effect (thermal and kinetic): Shao, et al. 2011a,b Mass distribution, halo shape and alignment: Lin et al. , to be submitted Brief of simulations LCDM (WMAP parameters), Box：100 Mpc/h Gadget-v2 (Springel 2005) A set of simulations us