التفاصيل البيبلوغرافية
| العنوان: |
The Cosmic Microwave Background & Inflation, Then & Now. |
| المؤلفون: |
Bond, J. Richard, Contaldi, Carlo, Pogosyan, Dmitry, Mason, Brian, Myers, Steve, Pearson, Tim, Pen, Ue-Li, Prunet, Simon, Readhead, Tony, Sievers, Jonathan |
| المصدر: |
AIP Conference Proceedings; 2002, Vol. 646 Issue 1, p15, 19p |
| مصطلحات موضوعية: |
COSMIC background radiation, INFLATIONARY universe |
| مستخلص: |
The most recent results from the Boomerang, Maxima, DASI, CBI and VSA CMB experiments significantly increase the case for accelerated expansion in the early universe (the inflationary paradigm) and at the current epoch (dark energy dominance). This is especially so when combined with data on high redshift supernovae (SN1) and large scale structure (LSS), encoding information from local cluster abundances, galaxy clustering, and gravitational lensing. There are "7 pillars of Inflation" that can be shown with the CMB probe, and at least 5, and possibly 6, of these have already been demonstrated in the CMB data: (1) the effects of a large scale gravitational potential, demonstrated with COBE/DMR in 1992-96; (2) acoustic peaks/dips in the angular power spectrum of the radiation, which tell about the geometry of the Universe, with the large first peak convincingly shown with Boomerang and Maxima data in 2000, a multiple peak/dip pattern shown in data from Boomerang and DASI (2nd, 3rd peaks, first and 2nd dips in 2001) and from CBI (2nd, 3rd, 4th, 5th peaks, 3rd, 4th dips at 1-sigma in 2002); (3) damping due to shear viscosity and the width of the region over which hydrogen recombination occurred when the universe was 400000 years old (CBI 2002); (4) the primary anisotropies should have a Gaussian distribution (be maximally random) in almost all inflationary models, the best data on this coming from Boomerang; (5) secondary anisotropies associated with nonlinear phenomena subsequent to 400000 years, which must be there and may have been detected by CBI and another experiment, BIMA. Showing the 5 "pillars" involves detailed confrontation of the experimental data with theory; e.g., (5) compares the CBI data with predictions from two of the largest cosmological hydrodynamics simulations ever done. DASI, Boomerang and CBI in 2002, AMiBA in 2003, and many other experiments have the sensitivity to demonstrate the next pillar, (6) polarization, which must be there at the... [ABSTRACT FROM AUTHOR] |
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| قاعدة البيانات: |
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