1994/08/01 by Edward L. Wright, E. L. Wright, Wright, Edward L.
Physics and Astronomy · #Astrophysics (astro-ph) #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #FOS: Physical sciences #Scientific Research and Discoveries #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9408003
presented at the CWRU CMB conference, April 1994, 11 pages of LaTex using aaspp.sty and epsf.sty with appended Postscript figures, UCLA-ASTRO-ELW-94-02
arxiv created 1994/08/01 · openalex publication_date 1994/08/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The index n of a power law power spectrum of primordial density fluctuations, P(k) ∝ kn, has been estimated using many different techniques. The most precise compare the COBE DMR large angular scale ΔT to the amplitude of the large scale structure, but these are also the most model-dependent. The COBE DMR ΔT has also been compared to the degree-scale ΔT from several experiments. And finally, a relatively model-independent value of n can derived from the COBE data alone, but the small range of angular scales covered by COBE limits the precision of these methods.