English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The angular power spectrum estimator developed by Peebles (1973) and Hauser &Peebles (1973) has been modified and applied to the 4 year maps produced by theCOBE DMR. The power spectrum of the observed sky has been compared to the powerspectra of a large number of simulated random skies produced with noise equalto the observed noise and primordial density fluctuation power spectra of powerlaw form, with $P(k) \propto k^n$. The best fitting value of the spectral indexin the range of spatial scales corresponding to spherical harmonic indices $3\leq \ell \lesssim 30$ is an apparent spectral index $n_{app}$ = 1.13 (+0.3)(-0.4) which is consistent with the Harrison-Zel'dovich primordial spectralindex $n_{pri} = 1$ The best fitting amplitude for $n_{app} = 1$ is $\langleQ_{RMS}^2\rangle^{0.5}$ = 18 uK.Comment: 17 pages including 3 PostScript figures. Submitted to The  Astrophysical Journal (Letters

Angular Power Spectrum of the Cosmic Microwave Background Anisotropy Seen by the [ITAL]COBE[/ITAL] DMR