Cosmology

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Cosmology Astrophysics with the Once Future
Microwave Background

• Theoretical Background
• Overview of MAXIMA BOOMERANG experiments and
  analyses
• Pitfalls, problems
• Solutions, successes
• Cosmological Parameters from the CMB
• Concordance? Confirmation? Bugs?
• The future

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References

• BOOMERanG
• P. deBernardis et al, Nature, 404, 955.
• A.E. Lange et al, PRD, Submitted,
  astro-ph/0005004
• MAXIMA
• S. Hanany et al, Ap. J., 545, L5, 2000,
  astro-ph/0005123
• A. Balbi et al, Ap. J., 545, L1, 2000,
  astro-ph/0005124
• BOOMERanG MAXIMA
• A.H. Jaffe et al, PRL, to appear, astro-ph/000733

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Measuring W L

• Wi is defined as a density Wi
  8pGri/3H02
• imatter, radiation, L, n, curvature...

• Wi determines
• distancescale factor, a(t)
• kinematics a?(t)
• curvature
• dynamics linear growth mode D(a)

• Different cosmological tests measure different
  aspects of W
• Difficult to get Wi alone Instead, measure (Wm
  WL), (Wm - WL), s8Wm0.6, ...

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Kinematics

• determines the "Hubble Diagram"
• relates observed distance to redshift.
• Comoving distance along a line of sight

Other cosmological distances (luminosity,
angular-diameter, etc.) are in turn determined by
Dw, z, and the cosmology. nb. Quintessence just
adds terms in E(z)2
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The CMB

• As Universe cools, peH
• ionizedneutral, opaquetransparent
• Sound Horizon at last-scattering surface is a
  standard ruler
• (degree-scale fluctuations)
• angular diameter distance at z1300,
• total curvature
• hence WL (1-Wk)

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Measuring Curvature with the CMB
Flat
W1
Us!
Last Scattering Surface
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Measuring Curvature with the CMB
Closed
Wgt1
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Measuring Curvature with the CMB
Open
Wlt1
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WGeometry is Density Destiny

• Also corresponds to density of stuff
• Normal matter (baryons) dark matter
  cosmological constant ...
• Determines evolution and ultimate fate of the
  Universe
• Is the Universe accelerating?

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Inflation Predicts

• Flat
• Wtot Wm WL 1
• Approximately scale-invariant adiabatic initial
  spectrum of density fluctuations
• P(k) µ kns
• Gravity waves
• Need polarization

• Corollaries
• Dark baryons, dark matter
• Caveats
• Open inflation
• Quintessence
• Isocurvature fluctuations
• Trace defects

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CMB statistics
z1300 peH Universe becomes transparent.
Determined by temperature, velocity and metric
on the last scattering surface.
Power Spectrum
Multipole l Û angular scale 180 /l
For a Gaussian theory, Cl completely determines
the statistics of the temperature.
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CMB Power Spectrum
Cl measures statistical properties of
fluctuations on angular scale 180/l
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