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The Big Bang• Hubble expansion law depends on the amount of
matter and energy (both are equivalent!) in the Universe; more precisely, on the
matter and energy density (and ??)• Define density parameter, and Critical Density • Just after the BB the Universe must have been
extremely hot and dense; as it expands it cools• Initially, radiation and matter are coupled together
in a hot, dense soup; Universe is opaque• Later, atoms form and radiation can escape –
Recombination Epoch Dark Ages
Background radiation and temperature of the Universe
• Radiation from the Hot Big Bang must fill the whole universe
• As the universe expands, the temperature must decrease
• Must be able to detect this background radiation – signature of the Big Bang
• Penzias and Wilson detected this Cosmic Microwave Background Radiation (CMBR)
Discovery of Cosmic Microwave Background
Microwave antenna used by Penzias and Wilson to detect the CMBR
Black-Body radiation curve at 2.7 K peak wavelength ~ 1 mm
Cosmic Microwave Background Radiation (CMBR)
COBE Results for the CMBR: The Universe is a perfect blackbody at a radiation temperature of 2.7 K
Hubble Parameter H_o and Redshifts• Measure redshifts of spectra and calibrate by all
known steps using ‘standard candles’• Distance to LMC is calibrated with Cepheid P-L
relation
• Best estimate of H_o = 67 +/- 8 km/sec/Mpc
• Expansion history of the Universe; ‘look-back’ time to the Big Bang: Age T_o = 1/H_o ~ 13-14 Gyr
• Cosmological Principle: Universe is uniform and isotropic (same in every direction) on large-scales (not locally !)
How rapid is the Expansion of the Universe? Was it the same always?
The answer depends on the matter/energy density of the Universe, which will slow the expansion due to gravity. But what could causethe observed acceleration ?
The Cosmological Constant • Einstein introduced an ‘arbitrary’ parameter, called the
“Cosmological Constant” into General Relativity to obtain a ‘static’ universe (the Hubble expansion had not been observed then) – Einstein’s ‘greatest blunder’ (as he called it himself) ??
• The cosmological constant counteracts gravity• Quantum effects in gravity – vacuum energy – could
also play the same role Dark Energy ; density denoted
as (Capital Greek )
• Recent data suggest Einstein may have been right !• But what is the shape of space-time in the universe ?• It is determined by the path light rays would follow
• Universe: Space-time, Matter, Energy
• Very little matter-energy is observable
Critical matter-energy density balances expansion and gravitational collapse
Mass Density/Critical Density:Density Parameter
Critical density is the density of matter required to just ‘close’ the Universe; if < 1 then Universe will go on expanding; if >1, it will stop expanding and will contract back (the Big Crunch!).
And Curvature of the Universe
• Density determines shape of the Universe
Flat (matter + energy density c)
Closed (spherical) Open (hyperbolic)
• Visible matter + energy (0.05) + dark matter
(0.25) , dark energy (0.7), i.e. m~ 0.3 + 0.7 = 1
How rapid is the Expansion of the Universe? Was it the same always?
The answer depends on the matter/energy density of the Universe, which will slow the expansion due to gravity. But what could causethe observed acceleration ?
Flat Euclidean - Triangle 180o
Matter-Energy densityand the “shape” of theUniverse
Matter + energy density just right to balance expansion
Large-Scale structure of the Universe• Galaxies group into Clusters• Milky Way is part of the Local Group: 39 galaxies
out to ~ 1 Mpc• Large-Scale Structure: - Groups: 3 to 30 bright galaxies - Clusters: > 30 (up to 1000’s) of bright galaxies; often with many more dwarf galaxies, 1 – 10 Mpc across; ~ 3000 clusters known - Superclusters: Clusters of Clusters - Voids, filaments, & Walls
Galactic Dynamics• Nearest comparable cluster to the Local Group is the Virgo
Cluster at about ~ 18 Mpc, size ~ 2 Mpc, ~ 2500 galaxies (mostly dwarfs), Mass ~ 100 trillion times M(Sun)
• Galaxies are large compared to distance between them; most galaxies within a group are separated by only ~ 20 times their diameter (by comparison most stars are separated by 10 million times the diameter)
• Tidal interactions, collisions, cannibalisation, splash encounters, starbursts, mergers, etc.
• The MW and Andromeda are moving towards each other at ~120 Km/sec, and might have a close encounter in ~3-4 Gyr; tidal distortion and merger after 1-2 Gyr
• Eventually only one galaxy might remain, most likely a medium-sized Elliptical
Large-Scale Structure• How did matter distribute on a universal scale?
• How did the galaxies form and evolve?
• How do we detect imprints of early universe?
WMAP
• How do we determine large-scale structure?
Galaxy Redshift Surveys, e.g. SDSS (Sloan Digital Sky Survey)
How did galaxies evolve?• Baryon-to-photon ratio increases with time
• Quantum fluctuations lead to inhomogeneity in the primordial radiation background
• Amplitude of fluctuations grows, manifest in temperature variations or power spectrum
• Oscillations imprinted on the radiation background
• Observed in present-day CMB PLANCK Satellite
Matter and Energy Density Dominated Expansion
• Primordial radiation dominated Universe• As the Universe expands: V ~ R3
• Density = M/V• Matter density falls off as ~ M/R3
• But energy density falls of as ~ E/R4
• Photons redshift to lower energies as ~1/R• But “dark energy” may trump both
End of Dark Ages: Reionization
• Dark Ages: Following atomic recombination, radiation and matter decoupled and radiation escaped leaving material universe unobservable or dark
• Until the first stars lit up and formed galaxies, at a redshift of about
Reionization: Formation of firststars and galaxiesIonizedneutral atomsto ion-plasma at about 500million years afterBig Bang orat z ~ 10
Lyman-alpha clouds: Red-shifted light absorption by neutralHydrogen of light from distant galaxies up to Reionization
(observed) = (1+ z) (rest)rest (Lyman alpha) emitted by distant galaxy is absorbed at > 1215 A by H-clouds at various redshifts, resulting in a Lyman-alpha “forest” of lines at different obs > 1215 A.