Correlated adiabatic and isocurvature CMB fluctuations in the wake of the WMAP

Details Correlated adiabatic and isocurvature CMB fluctuations in the wake of the WMAP Correlated adiabatic and isocurvature CMB fluctuations in the wake of the WMAP

2003-04-10

arxiv.org/abs/astro-ph/0304175v2

Phys.Rev.Lett. 91 (2003) 131302

Astronomy and Astrophysics

Astrophysics

5 pages, 7 figures. V2: Added 2 figures and revised a bit the results section. This is a slightly longer version than the publ

Scientific paper

10.1103/PhysRevLett.91.131302

In general correlated models, in addition to the usual adiabatic component with a spectral index n_ad1 there is another adiabatic component with a spectral index n_ad2 generated by entropy perturbation during inflation. We extend the analysis of a correlated mixture of adiabatic and isocurvature CMB fluctuations of the WMAP group, who set the two adiabatic spectral indices equal. Allowing n_ad1 and n_ad2 to vary independently we find that the WMAP data favor models where the two adiabatic components have opposite spectral tilts. Using the WMAP data only, the 2-sigma upper bound for the isocurvature fraction f_iso of the initial power spectrum at k_0=0.05 Mpc^{-1} increases somewhat, e.g., from 0.76 of n_ad2 = n_ad1 models to 0.84 with a prior n_iso < 1.84 for the isocurvature spectral index. We also comment on a possible degeneration between the correlation component and the optical depth tau. Moreover, the measured low quadrupole in the TT angular power could be achieved by a strong negative correlation, but then one needs a large tau to fit the TE spectrum.

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