Astro/Physics 224 Winter 2008Origin and Evolution of the UniverseStructure FormationFriday, February 8Joel PrimackUniversity of California, Santa CruzThe Initial Fluctuations rms perturbation: At Inflation: Gaussian, adiabatic Fourier transform:xkikkexrrrrr⋅∑=δδ)(Power Spectrum:nkkkP ∝><≡2|)(~|)(rδScale-Invariant Spectrum (Harrison-Zel’dovich)massttimeMδMGravitational InstabilitySmall fluctuations: Continuity: Euler: Poisson: comoving coordinates matter era growing mode: irrotational, potential flow: Linear approximation:Thus far, we have considered only the evolution of fluctuations in the dark matter. But of course we have to consider also the ordinary matter, known in cosmology as “baryons” (implicitly including the electrons). See Madau’s lectures “The Astrophysics of Early Galaxy Formation (http://arxiv.org/abs/0706.0123v1 ) for a recent summary. We have already seen that the baryons are primarily in the form of atoms after z ~ 1000, with a residual ionization fraction of a few x 10-4. They become fully reionized by z ~ 6, but they were not reionized at z~20 since the COBE satellite found that “Compton parameter” y ≤ 1.5 x 10-5, where This implies that Thus, for example, a universe that was reionized and reheated at z = 20 to (xe, Te) = (1, > 4×105 K) would violate the COBE y-limit.The figure at right shows the evolution of the radiation (dashed line, labeled CMB) and matter (solid line, labeled GAS) temperatures after recombination, in the absence of any reheating mechanism. (From Madau’s lectures.)The linear evolution of sub-horizon density perturbations in the dark matter-baryonfluid is governed in the matter-dominated era by two second-order differential equations:for the dark matter, andfor the baryons, where dm(k) and b(k) are the Fourier components of the densityfluctuations in the dark matter and baryons,† fdm and fb are the corresponding massfractions, cs is the gas sound speed, k is the (comoving) wavenumber, and the derivatives are taken with respect to cosmic time. Here† For each fluid component (i = b, dm) the real space fluctuation in the density field,can be written as a sum over Fourier modes,is the time-dependent matter density parameter, and ρ(t) is the total backgroundmatter density. Because there is ~5 times more dark matter than baryons, it is the formerthat defines the pattern of gravitational wells in which structure formation occurs. Inthe case where fb ≃ 0 and the universe is static (H = 0), equation (1) above becomes(1)(2)“Hubble friction”After a few dynamical times, only the exponentially growing term is significant: gravity tends to make small density fluctuations in a static pressureless medium grow exponentially with time. Sir James Jeans (1902) was the first to discuss this. The additional term ∝ H present in an expanding universe can be thought as a “Hubble friction” term that acts to slow down the growth of density perturbations. Equation (1) admits the general solution for the growing mode:where tdyn denotes the dynamical timescale. This equation admits solutionso that an Einstein-de Sitter universe gives the familiar scaling δdm(a) = a with coefficient unity. The right-hand side of equation (3) is called the linear growth factor D(a) = D+(a). Different values of Ωm, ΩΛ lead to different linear growth factors. Growing modes actually decrease in density, but not as fast as the average universe. Note how, in contrast to the exponential growth found in the static case, the growth of perturbations even in the case of an Einstein-de Sitter (Ωm =1) universe is just algebraic. This was discovered by the Russian physicist Lifshitz (1946).(3)The consequence is that dark matter fluctuations grow proportionally to the scale factor a(t) when matter is the dominant component of the universe, but only logarithmically when radiation is dominant. Thus there is not much difference in the amplitudes of fluctuations of mass M < 1015 Msun, which enter the horizon before zmr ~ 4 ×103, while there is a stronger dependance on M for fluctuations with M > 1015 Msun. There is a similar suppression of the growth of matter fluctuations once the gravitationally dominant component of the universe is the dark energy, for example a cosmological constant. Lahav, Lilje, Primack, & Rees (1991) showed that the growth factor in this case is well approximated by Here is again given byCDM Power SpectrumδMeqmassCDM HDM free streamingmassttimeteqδ growth when matter is self-gravitatingPkkpeak ∝ Ωm hkCDMHDMFormation of Large-Scale StructureM10CDM: bottom-upFluctuation growth in the linear regime:HDM: top-downM10free streamingrms fluctuation at mass scale M:Galaxies Clusters Superclusters Galaxies Clusters SuperclustersAn approximate fitting function for T(k) in a ΛCDM universe is (Bardeen et al. 1986)where (Sugayama 1995)For accurate work, for example for starting high-resolution N-body simulations, it is best to use instead of fitting functions the numerical output of highly accurate integration of the Boltzmann equations, for example from CMBFast http://cfa-www.harvard.edu/~mzaldarr/CMBFAST/cmbfast.html W e l c o m e to the CMBFAST Website!This is the most extensively used code for computing cosmic microwave background anisotropy, polarization and matter power spectra. The code has been tested over a wide range of cosmological parameters. We are continuously testing and updating the code based on suggestions from the cosmological community. Do not hesitate to contact us if you have any questions or suggestions.U. Seljak & M. ZaldarriagaFrom Peter Schneider, Extragalactic Astronomy and Cosmology (Springer, 2006)From Peter Schneider, Extragalactic Astronomy and Cosmology (Springer, 2006)On large scales (k small), the gravity of the dark matter dominates. But on small scales, pressure dominates and growth of baryonic fluctuations is prevented. Gravity and pressure are equal at the Jeans scaleThe Jeans mass is the dark matter + baryon mass enclosed within a sphere of radius πa/kJ, where µ is the mean molecular weight. The evolution of MJ is shown below, assuming that reionization occurs at z=15:Jeans-type analysis for HDM, WDM, and CDMGRAVITY – The Ultimate Capitalist PrincipleThe early universe expands almost perfectly uniformly. But there are small differences in density from place to place (about 30 parts per million). Because of gravity, denser