The power spectrum implied by COBE and the matter correlation function
| dc.creator | Torres, S. | |
| dc.creator | Fabbri, R. | |
| dc.creator | Ruffini, R. | |
| dc.date | 1993-11-28 | |
| dc.date | 1993-12-01 | |
| dc.date.accessioned | 2026-07-07T08:58:13Z | |
| dc.date.available | 2026-07-07T08:58:13Z | |
| dc.description | A phenomenological power spectrum of primordial density perturbations has been constructed by using both COBE data to probe the large wavelength region, and a double power law, locally deduced from galaxy catalogs, which describes the matter correlation function up to tens of Megaparsec. The shape of the spectrum P(k) of density fluctuations exhibits a peak that singles out a characteristic wavelength proportional to the cutoff radius R0 in the matter distribution (comparable to the distance at which matter becomes anticorrelated). {}From a least squares fit to COBE's angular correlation function we obtain R0 = 35 +- 12 Mpc/h for the correlation length, and n = 0.76 +- 0.3 for the spectral index of P(k) in the large wavelength region. The inferred scale in the spectrum is 51 +- 18 Mpc/h. This number agrees with that derived from the analysis of the correlation function of matter and with a preferred scale identified in IRAS PSC. | |
| dc.description | 5, Latex, ICRA31-5-93 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9311068 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9311068 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/147236 | |
| dc.subject | Astrophysics | |
| dc.title | The power spectrum implied by COBE and the matter correlation function | |
| dc.type | text |