Cosmology : Cosmic Microwave Background & Large scale structure & Large scale structure Cosmology : Cosmic Microwave Background & Large scale structure & Large scale structure Tarun Souradeep I.U.C.A.A. Cosmology IUCAA VSP program (May 18-22, 2012) Lec. 1: Background universe
Andromeda Galaxy The Realm of Cosmology Basic unit: Galaxy Size : kilo parsec (kpc.) Mass : 100 billion Stars Measure distances in light travel time 1 pc. (parsec) = 200,000 AU = 3.26 light yr. Measure Mass in Solar mass
The Realm of Cosmology 100 million Light years
The Realm of Cosmology 500 million Light years
The Realm of Cosmology 5 Billion Light years
The Realm of Cosmology
How can we even hope to comprehend this immensely large& complex Universe !?! Look for an appropriate simple model
Modeling nature Picasso: Steiren series
Lick Observatory survey North South The Isotropic Universe Distribution of galaxies on the sky is broadly isotropic Isotropy around every point implies Homogeneity Cosmological principle FLRW models
The Expanding Universe Leads to the Hubble’s law Recession velocity is Proportional to the distance Matter density: 1/V Radiation density: 1/(V L) Early Universe is radiation dominated E Einstein’s General relativity applied to an uniform distribution of matter on cosmic scales leads to a smooth expanding universe (FRW Cosmology) Fig.: Ned Wright
The Expanding Universe Fig.: Ned Wright
Space-time of the cosmos Fig.: Ned Wright
Space-time of the cosmos General relativity allows us to formulate physics in any coordinates Fig.: Ned Wright
Space-time of the cosmos Fig.: Ned Wright Comoving spatial coordinates
Space-time of the cosmos Fig.: Ned Wright Comoving spatial coordinates Conformal time
Observer Distant galaxy Equal time events at a distant galaxy appears time-dilated Cosmological Redshift Frequency of light from a distant galaxy is scaled by the expansion Redshift, z=v/c Redshift is related to distance Fig.: adapted from Ned Wright
Expanding Universe Hubble’s measurements in 1929 Hubble’s law: Recession velocity of galaxies is proportional to the distance Fig.: Ned Wright Frequency of light from a distant galaxy Redshift, z=v/c Redshift is related to distance
Expanding Universe Hubble’s Law: Current observational status Fig.: Ned Wright
Post-recombination :Freely propagating through (weakly perturbed) homogeneous & isotropic cosmos. Pre-recombination : Tightly coupled to, and in thermal equilibrium with, ionized matter. Pristine relic of a hot, dense & smooth early universe - Hot Big Bang model (text background: W. Hu) Cosmic Microwave Background
Cosmic “Super–IMAX” theater Transparent universe Opaque universe 43 Billion Light-years Here & Now (14 Giga-years) 0.5 Mega-years
The Isotropic Universe T 0 =2.725 (+/-0.002)K. Serendipitous discovery of the dominant Radiation content of the universe as an extremely isotropic, Black-body bath at temperature T 0 =2.725 (+/-0.002)K. “Clinching support for Hot Big Bang model” Nobel prize 1978 Cosmic Microwave Background
The dominant radiation component in the universe (D. Scott ’99) ~ 400 CMB photons per cubic cm. Cosmic Microwave Background
“Dust” in an expanding box Radiation in an expanding box Size = ½ Number density x 8 Energy density x 16 Temperature x 2 Size = ¼ Number density x 64 Energy density x 128 Temperature x 4 Size = ¼ Number density x 64 Energy density x 64 Size = ½ Number density x 8 Energy density x 8 time Matter density: 1/V Radiation density: 1/(V L) Early Universe is radiation dominated E
The most perfect Black-Body spectrum in nature COBE website COBE –FIRAS The CMB temperature – A single number characterizes the radiation content of the universe!! Cosmic Microwave Background
Baryons: Big Bang Nucleosynthesis
Flat Universe Hyperbolic Universe Constant negative curvature Spherical Universe Constant positive curvature Geometry of the Universe
Friedman equations
Evolution of density
`Standard’ cosmological model: Geometry, Expansion & Matter Clustering matter Non-Clustering matter
How much do we now know about this model Universe ? lots !!!
NASA/WMAP science team Age of the universe Dark energy density Dark matter density Expansion rate of the universe Good old Cosmology, … New trend ! Total energy density Baryonic matter density