Observational Matter Power Spectrum and the Height of the Second Acoustic Peak | Zendy

F. AtrioBarandela | Zendy; J. Einasto | Zendy; V. Müller | Zendy; J. P. Mücket | Zendy; Alexei A. Starobinsky | Zendy

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Observational Matter Power Spectrum and the Height of the Second Acoustic Peak

Author(s) -

F. AtrioBarandela,

J. Einasto,

V. Müller,

J. P. Mücket,

Alexei A. Starobinsky

Publication year - 2001

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 - 10.1086/322280

Subject(s) - physics , hubble's law , cosmic microwave background , matter power spectrum , big bang nucleosynthesis , astrophysics , spectral density , amplitude , nucleosynthesis , maxima , dark matter , cosmology , cold dark matter , dark energy , supernova , statistics , quantum mechanics , art , mathematics , anisotropy , performance art , art history

We show that the amplitude of the second acoustic peak in the newly releasedBOOMERANG-98 and MAXIMA-I data is compatible with the standard primordialnucleosynthesis and with the locally broken-scale-invariant matter powerspectrum suggested by recent measurements of the power spectrum in the range$20 - 200$ Mpc. If the slope of matter density perturbations on large scales is$n \approx 1$, the Hubble constant is $0.5< h < 0.75$, and r.m.s. massfluctuations at 8 Mpc are $0.65 \le \sigma_8 \le 0.75$, then for a Universeapproximately 14 Gyr old our best fit within the nucleosynthesis bound$\Omega_Bh^2= 0.019 \pm 0.0024$ requires $0.3 \le \Omega_m \le 0.5$. Clusterabundances further constraint the matter density to be $\Omega_m \approx 0.3$.The CMB data alone are not able to determine the detailed form of the matterpower spectrum in the range $0.03

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