Inflation, large-scale structure, and COBE

Details Inflation, large-scale structure, and COBE Inflation, large-scale structure, and COBE

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aipc..272.1602f&link_type=abstract

Proceedings of the XXVI International Conference on High Energy Physics. Vol. II. AIP Conference Proceedings, Volume 272, pp. 1

Physics

High Energy Physics

Unified Theories And Models Of Strong And Electroweak Interactions, Perturbative Calculations

Scientific paper

In several versions of the inflationary scenario, such as natural, extended, and power law inflation, the spectrum of density perturbations generated can differ significantly from the scale-invariant (SI) Harrison-Zeldovich form. In these models, the primordial power spectrum is a power law in wavenumber k, P(k)=||δk||2~kns, with spectral index ns<=1, leading to more relative power on large scales than the ns=1 SI spectrum. In the context of the cold dark matter (CDM) model, such a `tilted' spectrum with ns<~0.6-0.7 can help explain the otherwise puzzling large-scale clustering of galaxies. However, the microwave background anisotropies recently detected by COBE severely constrain this possibility: when combined with the requirement that galaxies form sufficiently early, COBE implies that ns>~0.6. For extended and power law inflation, which produce a significant gravity wave background, the constraint is even tighter, ns>~0.76.

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