Cosmic Microwave Background Radiation Power Spectrum in Cold Dark Matter Open Universes Up to Second-Order Perturbations

1996 ◽  
Vol 467 ◽  
pp. 485 ◽  
Author(s):  
Jose Luis Sanz ◽  
Enrique Martinez-Gonzalez ◽  
Laura Cayon ◽  
Joseph Silk ◽  
Naoshi Sugiyama
Keyword(s):  
Dark Matter ◽  
Power Spectrum ◽  
Cosmic Microwave Background ◽  
Cold Dark Matter ◽  
Background Radiation ◽  
Radiation Power ◽  
Cosmic Microwave Background Radiation ◽  
Second Order ◽  
Microwave Background ◽  
Microwave Background Radiation

scholarly journals Microwave Background Anisotropies in a Baryon-Dominated Universe

1988 ◽  
Vol 130 ◽  
pp. 513-513
Author(s):  
Yasushi Suto ◽  
Naoteru Gouda ◽  
Misao Sasaki
Keyword(s):  
Power Spectrum ◽  
Cosmic Microwave Background ◽  
Background Radiation ◽  
Cosmic Microwave Background Radiation ◽  
Microwave Background ◽  
Gauge Invariant ◽  
Invariant Method ◽  
Angular Scale ◽  
Microwave Background Radiation ◽  
Image Position

We have calculated the anisotropies of the cosmic microwave background radiation in a baryon-dominated model (BDM), using a gauge invariant method. The results on a 4.5′ angular scale are as follows (h = 0.5 and initially Zel'dovich power spectrum assumed):

scholarly journals Current Status of the Cosmic Microwave Background Radiation

1999 ◽  
Vol 183 ◽  
pp. 74-87
Author(s):  
R. B. Partridge
Keyword(s):  
Power Spectrum ◽  
Cosmic Microwave Background ◽  
Background Radiation ◽  
Cosmological Parameters ◽  
Theoretical Description ◽  
Cosmic Microwave Background Radiation ◽  
Current Status ◽  
Next Generation ◽  
Microwave Background ◽  
Microwave Background Radiation

My goal is to summarize our understanding of the cosmic microwave background radiation (CMBR) at this interesting moment after the detection of fluctuations in the background and before the next generation of satellite experiments. I begin by listing recent reviews and papers on the spectrum of the CMBR. I then sketch the current theoretical description of the power spectrum of fluctuations in the CMBR. Astronomical foregrounds and the nature of secondary fluctuations are treated next. Then I turn to observations, with special emphasis on the final results of the COBE–DMR experiment, on the growing evidence for ΔT/T = 2–3 × 10−5 fluctuations at degree scales, and on what they tell us about cosmological parameters.

DYNAMICS AND THE SECOND PEAK: COLD DARK MATTER?

2001 ◽  
Vol 16 (supp01c) ◽  
pp. 1031-1033 ◽  
Author(s):  
STACY MCGAUGH
Keyword(s):  
Dark Matter ◽  
Power Spectrum ◽  
Cold Dark Matter ◽  
Background Radiation ◽  
Angular Spectrum ◽  
Microwave Background ◽  
Λcdm Model ◽  
Microwave Background Radiation ◽  
Second Peak ◽  
Modified Dynamics

The amplitude of the second peak in the angular spectrum of the cosmic microwave background radiation is constrained to be small by recent experiments like Boomerang. This is surprising in the context of the ΛCDM model, which predicted a large second peak. However, this result is expected if CDM does not exist. The observed shape of the power spectrum was accurately predicted (before the fact) by a model motivated by the surprising recent successes of the modified dynamics (MOND) hypothesized by Milgrom.

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