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 2 year maps produced by theCOBE DMR. The power spectrum of the real 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 $P(k) \propto k^n$. Within the limited range of spatial scalescovered by the COBE DMR, corresponding to spherical harmonic indices $3 \leq\ell \lsim 30$, the best fitting value of the spectral index is $n =1.25^{+0.4}_{-0.45}$ with the Harrison-Zeldovich value $n = 1$ approximately0.5$\sigma$ below the best fit. For $3 \leq \ell \lsim 19$, the best fit is $n= 1.46^{+0.39}_{-0.44}$. Comparing the COBE DMR $\Delta T/T$ at small $\ell$ tothe $\Delta T/T$ at $\ell \approx 50$ from degree scale anisotropy experimentsgives a smaller range of acceptable spectral indices which includes $n = 1$.Comment: 22 pages of LaTex using aaspp.sty and epsf.sty with appended  Postscript figures, COBE Preprint 94-0

Angular power spectrum of the microwave background anisotropy seen by the COBE differential microwave radiometer