Connecting Quarks to the Cosmos. Inflationary Cosmology I
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Connecting Quarks to the Cosmos Institute for Nuclear Theory 29 June to 10 July 2009 Inflationary Cosmology I Michael S. Turner Kavli Institute for Cosmological Physics The University of Chicago Michael S Turner Quarks and the Cosmos: Convergence of Frontiers of Particle Physics, Nuclear Physics and Astrophysics/Cosmology • What is the dark matter particle? • How did neutrinos shape the Universe and what are they telling us about the unification of forces? • What is the dark energy that is causing the Universe to accelerate? • What are Nature’s highest energy particles and how are they accelerated? • How did the chemical elements originate? • How are quantum mechanics and gravity reconciled? • What happens when black holes collide? • What are space and time and where did they come from? • What was the dynamite behind the big bang? Michael S Turner Cosmology is a young science its story only begins 60 years after Darwin, 300 years after the invention of the telescope Michael S Turner 1916-1918: General Relativity & Λ PS: Never mind Λ Michael S Turner 1929: Just One Number K (error bars not needed, velocity in km) H 0) ( K 50 5 = Hubble & Humanson: Michael S Turner c p s/M / km few 100 galaxies, z < 0.1 Cosmology: The Search for Two Numbers … Sandage 1970 Michael S Turner Landau on Cosmologists Often in Error, Never in Doubt! Michael S Turner and at U Mass The Redbook, a manual for faculty members that explained what a university was, and what it wasn't. It cited two courses one wouldn't find in a curriculum of higher education: witchcraft and cosmology. Michael S Turner Discovery of Cosmic Microwave Background, 1964 Michael S Turner Michael S Turner “The Standard Model” Hot Big Bang (circa 1972) “Reality (physics) Based” • BBN (nuclear physics) • CMB (atomic physics) • Structure Formation (grav. physics) • Begins at 0.01 sec • Ω0 ~ 0.1 (baryons) Big Questions • “The naughts”: H0, t0, Ω0 • Large entropy per baryon • Hadron Wall • Origin of density perturbations Michael S Turner 1980s: The Go Go Junk Bond Days of Early Universe Cosmology “Creativity Based” • Inflation • Cosmic Strings • Baryogenesis • Magnetic Monopoles • Phase Transitions • Hot and Cold Dark Matter • Decaying Particles • Kaluza-Klein Michael S Turner 1990s: Beginning of Data-driven Cosmology • • • • • COBE! and CMB experiments Redshift surveys (CfA, IRAS, 2dF, SDSS) Large-scale velocity field measurements Gravitational lensing Big telescopes (Keck, …) with big CCD cameras • HST, X-ray, gamma-ray, IR, … Michael S Turner Big Glass on the Ground: 4 VLT, 2 Kecks, 2 Geminis and 2 Magellans Great Observatories in Space: Hubble, Spitzer, Chandra, and Fermi Giant CCD Cameras Gigapixel 100 Megapixel How far can you see on a clear day? Back to the birth of galaxies How far can you see on a clear day with x-ray eyes? To supermassive black holes at the edge of the Universe! Swift GRB 090423 z = 8.2 GROND photo-z Birth of a Black Hole at the Edge of the Universe Greiner et al. 2000s: Era of Precision Cosmology • • • • • “Fisher Based” Cosmological parameters Tests of inflation, CDM Correlating large, complex data sets Cosmological Consistency Physical parameters (e.g., neutrino mass) Michael S Turner In the midst of a revolutionary period of discovery -- powerful ideas and instruments Michael S Turner Quarks and the Cosmos Two Really Important Ideas That Changed Cosmology with deep connections between quarks and the cosmos Inflation: brief period of rapid (accelerated) expansion accounts for smoothness, flatness; heat of the big bang; and seed inhomogeneities Particle dark matter: bulk of the dark matter that holds the Universe together resides in a sea of elementary particles left over from the big bang Michael S Turner H0 = 70 ± 7 km/s/Mpc … and Dr. Sandage, H0 is now measured and q0 is negative! Decoding the Cosmic Rosetta Stone COBE DASI ACBAR ACBAR CBI Maxima BOOMERanG Michael S Turner CBI The Universe circa 380,000 yrs WMAP Michael S Turner ±0.001% Fluctuations Michael S Turner Curve = concordance cosmology Michael S Turner Sloan Digital Sky Survey sdss.org Large-scale structure: Distribution of 106 galaxies Michael inS Turner the Universe today Tracing the history from a slightly lumpy Universe to galaxies ablaze Michael S Turner Today’s “Consensus Cosmology” based upon precision measurements • From quark soup to nuclei and atoms to galaxies and large-scale structure • Flat, accelerating Universe • Atoms, exotic dark matter & dark energy • Consistent with inflation • Precision cosmo parameters –Ω0 = 1.005 ± 0.006 (uncurved) –ΩM = 0.280 ± 0.013 –ΩB = 0.045 ± 0.0015Consistent with –ΩDE = 0.72 ± 0.015 –H0 = 70 ± 1.3 km/s/Mpc all data, laboratory and –t0 = 13.73 ± 0.12 Gyr –Nν = 4.4 ± 1.5 cosmological! Michael S Turner Michael S Turner The Universe Observed Michael S Turner A Universe Full of Galaxies and Clusters of Galaxies • • • • 1011 galaxies! Density of galaxies: ~0.001/Mpc3 Typical mass 1012 solar mass (2 x 1045 g) Range: 106 to 1013 solar masses Michael S Turner Michael S Turner Clusters of Galaxies: Largest Bound and Relaxed Objects Michael S Turner Perseus Cluster Coma Cluster of Galaxies • Masses from 1013 to 1016 solar masses • X-ray bright (hot gas) Michael S Turner • 5% of galaxies are found in rich clusters Isotropy (same in all directions): Galaxy Distribution on Sky Michael S Turner Isotropy & Homogeneity: at 400,000 yrs CMB Intensity Scale: ±0.01% Michael S Turner Homogeneity (same everywhere): Galaxy Distribution 2dF Michael S Turner Sloan Digital Sky Survey sdss.org Michael S Turner •Expansion = Scaling up •Single “Cosmic Scale Factor” R(t) Summarizes Expansion Michael S Turner Our Universe Michael S Turner Cosmological Redshift All physical distances get stretched with cosmic scale factor, Rtoday = 1.0 • Wavelength of a photon (redshift z) • Momenta of particles too: p ~ 1/R • Distance between galaxies NB: but not the size of self-bound objects (from atoms to starsMichael to Sgalaxies & clusters) Turner UV light (1216 Å) from the early Universe redshifted to near IR. The Universe was ~7 times smaller! Michael S Turner 1992: COBE Maps & Blackbody Spectrum Michael S Turner Giant Dipole in the Sky: Milky Way is Michael S Turner moving toward Leo at 600 km/sec COBE Proves Copernicus Right! Michael S Turner Sloan Digital Sky Survey sdss.org Michael S Turner Cosmological Parameters Michael S Turner Precision Cosmology Indeed! CMB (first to second peak) Ωbh2 = 0.0225 ± 0.0006 vs. BBN (Deuterium) Ωbh2 = 0.0213 ± 0.0013 ~5% agreement Michael S Turner h = H0/100 km/s/Mpc ~ 0.7 Ωb = 0.044 ± 0.002 Friedmann Equations Matter tells space how to bend (“flat”, Euclidean Universe) • H = expansion rate (“Hubble constant”) • Total energy density ρ and total pressure p • Solutions: Michael S Turner Evolution of Matter/Energy space tells matter how to move Michael S Turner Three Epochs Dominated by Different Forms of Energy 1. Rad dominated R ~ t1/2 thermal bath R < 10-4, t < 104 yrs 2. Matter dominated R ~ t2/3 struc. forms t ~ 104 yrs – 1010 yrs Michael S Turner 3. Dark Energy R ~ eHt accelerated expansion t > 1010 yrs Structure Formation Gravitational amplification of small (few parts in 105) density inhomogeneities to the structure seen today during matter dominated epoch, δρ/ρ α R(t) Michael S Turner Thermal Bath For most of its early history: thermal equilibrium (departures are very important – not all Fe today!) • For kT > mc2 particle/antiparticle pairs as abundant as photons • Energy density: ρ = g*π2T4/30 g* counts dof Michael S Turner Michael S Turner Relativistic Degrees of Freedom All SM Particles γ/neutrinos Quark/Hadron e± pairs Michael S Turner Radiation-dominated Universe Michael S Turner
