Angular Power Spectrum of the Microwave Background Anisotropy seen by the COBE Differential Microwave Radiometer

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dc.creatorWright, E. L.
dc.creatorBennett, C. L.
dc.creatorGorski, K.
dc.creatorHinshaw, G.
dc.creatorSmoot, G. F.
dc.date1996-01-12
dc.date.accessioned2026-07-07T11:46:07Z
dc.date.available2026-07-07T11:46:07Z
dc.descriptionThe angular power spectrum estimator developed by Peebles (1973) and Hauser & Peebles (1973) has been modified and applied to the 4 year maps produced by the COBE DMR. The power spectrum of the observed sky has been compared to the power spectra of a large number of simulated random skies produced with noise equal to the observed noise and primordial density fluctuation power spectra of power law form, with $P(k) \propto k^n$. The best fitting value of the spectral index in 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 spectral index $n_{pri} = 1$ The best fitting amplitude for $n_{app} = 1$ is $\langle Q_{RMS}^2\rangle^{0.5}$ = 18 uK.
dc.description17 pages including 3 PostScript figures. Submitted to The Astrophysical Journal (Letters)
dc.identifierhttps://arxiv.org/abs/astro-ph/9601059
dc.identifierhttp://arxiv.org/abs/astro-ph/9601059
dc.identifierAstrophys.J.464:L21-L24,1996
dc.identifierdoi:10.1086/310073
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/202112
dc.subjectAstrophysics
dc.titleAngular Power Spectrum of the Microwave Background Anisotropy seen by the COBE Differential Microwave Radiometer
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