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

E. L. Wright | Zendy; C. L. Bennett | Zendy; K. M. Górski | Zendy; G. Hinshaw | Zendy; G. F. Smoot | Zendy

AI Assistant Blog Pricing

Home ZAIA Blog

Open Access

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

Author(s) -

E. L. Wright,

C. L. Bennett,

K. M. Górski,

G. Hinshaw,

G. F. Smoot

Publication year - 1996

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/310073

Subject(s) - spectral density , cosmic microwave background , spectral index , anisotropy , physics , amplitude , spectral line , noise (video) , estimator , astrophysics , sky , computational physics , range (aeronautics) , optics , statistics , astronomy , mathematics , materials science , composite material , artificial intelligence , computer science , image (mathematics)

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

The content you want is available to Zendy users.

Already have an account? Click here to sign in.

Having issues? You can contact us here

Accelerating Research