1、宇宙微波背景辐射,郭宗宽,中国科学院研究生院2012.06.26,宇宙学基本假设和理论基础宇宙学原理（无边，无中心）爱因斯坦引力理论宇宙物质（重子+光子+中微子+暗物质+暗能量）观测实验的重要性超新星，大尺度结构，宇宙微波背景辐射宇宙射线，21厘米谱线，射电波，弱引力透镜，引力波，中微子目前的进展和存在的问题宇宙加速膨胀（暴涨，暗能量，修改引力，非均匀宇宙）宇宙大尺度结构形成（冷/温/热暗物质，暗物质粒子的性质，暗物质分布）,交叉学科-宇宙学,内容,宇宙微波背景（CMB）辐射的形成CMB的发现和探测实验CMB的数据分析CMB各向异性的物理起源CMB的宇宙学解释展望,1. CMB的形成,reco
2、mbination decoupling,2. CMB的发现和探测实验,the first discovery of CMB radiation in 1964-1965the Nobel Prize in Physics 1978: A.A. Penzias and R.W. Wilson,CMB was predicted by G. Gamow et al. in 1948 T5 K,interpreted by P.J.E. Peebles, D.T. Wilkinson, et al. in 1965,COBE (Cosmic Background Explorer) - the f
3、irst generation CMB experiment, launched on 18 Nov. 1989, 4 yearsthe Nobel Prize in Physics 2006: J.C. Mather and G.F. Smoot,J.C. Mather G.F. Smoot (DMR),Hot big bang,isotropy,the Far InfraRed Absolute Spectrophotometer (FIRAS) teamthe Differential Microwave Radiometer (DMR) team,no atmospheric ther
4、mal emission full-sky map,advantages of satellite experiments:,the COBE satellite experiments:,141,WMAP (Wilkinson Microwave Anisotropy Probe) - the second generation CMB experiment, launched on 30 June 2001, 9 years,free-free emission: electron-ion scattering synchrotron emission: the acceleration
5、of cosmic ray electrons in magnetic fields thermal emission from dust,23 GHz,33 GHz,41 GHz,61 GHz,94 GHz,angular power spectrum of CMB,foreground mask,We have entered a new era of precision cosmology.!?,Planck - the third generation CMB experiment, launched on 14 May 2009, 30 months, 5 full-sky surv
6、eys,LFI: 30, 44, 70 GHz HFI : 100, 143, 217, 353, 545, 857 GHz,NASA: CMBPol,ESA: COrE,next generation CMB experiment,Other experiments: ground based experiments (QUaD, BICEP, ACT, ACTPol from 2013, SPT, SPTpol from 2012) balloon borne experiments (BOOMRANG, MAXIMA),10 meter telescope,South Pole Tele
7、scope (SPT),150 and 220 GHz in 200895, 150 and 220 GHz in 2009,Atacama Cosmology Telescope (ACT),6 meter telescope,3 frequencies (148, 218, and 277 GHz),3. CMB的数据分析, the temperature anisotropies can be expanded in spherical harmonics,time-ordered data,full sky map,spectrum,parameter estimates, time-
8、ordered data, for Gaussian random fluctuations, the statistical properties of thetemperature field are determined by the angular power spectrum,For a full sky, noiseless experiments, cosmological parameter estimationlikelihood function for a full sky:,the sky-cut, MCMC,4. CMB各向异性的物理起源,primary CMB an
9、isotropies (at recombination),inflation model (Alan H. Guth in 1981) primordial power spectrum of curvature perturbations angular power spectrum of CMB anisotropies,V (),inflation,reheating,for slow-roll inflation, the primordial power spectra of scalar/tensor perturbations:,the coupled, linearized
10、Boltzmann, Einstein and fluid equations:,spherical harmonics,Fourier space,the linearized Einstein equations:,the Einstein equations:,reionization thermal Sunyaev-Zeldovich effect lensing effect integrated Sachs-Wolf effect,secondary CMB anisotropies (after recombination),large angular scalesintegra
11、ted SZ effect (1000)Silk damping: the dissipation of small-scale perturbations caused by photons random walking out of overdense regions.,features of spectrum,For full accuracy, the Boltzmann equation must be solved to follow the evolution of the photon distribution function.,5. CMB的宇宙学解释,precision
12、cosmology,the content of our Universe,The stronger the contraction, the higher these peaks should be.,the shape of the primordial power spectrum of curvature perturbationsdetection of the primordial power spectrum of tensor perturbationsnon-adiabaticitynon-Gaussianity,6. 展望,Thank you for your attent
13、ion.,a main-sequence star (hydrogen)red giant (helium carbon, oxygen)white dwarf (carbon, oxygen): electron degeneracy pressure, 1.4 solar massesType Ia supernova,a main-sequence star (hydrogen, carbon, oxygen)Type Ib, Ic, II supernova (a line of hydrogen)neutron star (including pulsar): neutron degeneracy pressure, 12 solar masses,a main-sequence star (hydrogen, carbon, oxygen)Type Ib, Ic, II supernovablack hole: 3.2 solar masses,Adam G. Riess (High-Z),Saul Perlmutter (leader of SCP),Brian P. Schmidt (leader of High-Z),
