1• Type Ia Supernovae as “standard candles” accelerating expansion qo= m/2 - • CMB anisotropy total= m+ • Can solve for m, = Cosmological Constantm= matter density/critical densityThe “Concordance” Cosmology (or CDM)Another independent measure:Rate of galaxy cluster evolution[CO 30.22]Position & height of first peak also depend on m, b, hHeight of peak• Larger m all peaks have smaller amplitudes. – Through change in matter/radiation density ratio during radiation-dominated phase.– Through effect on when universe becomes matter dominated.Position of Peakmh3/4Calculated for tot= 12So use constraints from other measurements:Position of Peakmh3/4Calculated for tot= 1Galaxy cluster evolutionfb= baryon fraction in clusters= minimum ageof universeBBN resultsPosition & height of first peak also depend on m, b, hHSTWMAP also measured second peak• Due to rarefaction of an acoustic wave.• Larger b smaller amplitude of second peak.– greater inertial mass in oscillating plasma.3Print-through of spectrum of primordial fluctuations(Sachs-Wolfe effect)Photon diffusion(Silk damping)bCurvatureResults:• Total density: o= tot= 1.02 0.02• Age of Universe: to= 13.7 0.2 Gyr• Matter density: mh2= 0.135 +0.008/-0.009 m= 0.27• Baryon density: bh2 = 0.0224 0.009 b= 0.04473% Dark Energy, 22% Dark Matter, 4.4% Baryonic MatterFlat Universe with density fluctuations P(k) ~ kn, n ~ 1 INFLATIONAstrophysical Journal Supplement 148, pg. 1 (September 2003)Astrophysical Journal Supplement 148, pg. 233 (September 2003)4Power spectrum measures many things[CO 30.22]But still needs to be combined with other measurements.Appendix N --- WMAP dataThe Syllabus:Quasars & Active galactic Nuclei (AGN)[28.2] Unified model of AGN …(Skip [28.1], [28.3]) [18.2] Accretion Disk description pp. 661-666[24.4] The Galactic CenterDec 7,9,11[26.2] The formation of galaxiesNov 30, Dec 2,4Thanksgiving HolidayFri Nov 27[26.1] Interaction of galaxiesNov 23,25What is dark matter?[30.2] The origin of structure; WMAP measurements.Nov 16,18,20The Structure of the Universe & Evolution of Galaxies[27.3] Clusters of galaxies[28.4] Using quasars to probe the universe (gravitational lenses) Nov 9,11,13• Present-day structure.• Evidence for Dark Matter.• Gravitational lenses.• What is Dark Matter?• Hot vs. cold DM• The growth of structure.• Initial fluctuations.• WMAP.• Bottom-up structureformation.( turkey break)• The Quasar Era.• Evolution to modern-day galaxies.• Chemical enrichmentrevisited.• The first stars.The agenda:Final Exam: in BPS 1420, at 3PM Monday, Dec
View Full Document
Unlocking...