Multiple Peaks in the Angular Power Spectrum of the Cosmic Microwave Background: Significance and Consequences for Cosmology

By P. Bernardis, P. Ade, J. Bock, J. Richard Bond, J. Borrill, A. Boscaleri, K. Coble, C. Contaldi, B. Crill, G. Troia and 25 more. 2001

296 citations recorded by the source corpus.

Three peaks and two dips have been detected in the power spectrum of the cosmic microwave background by the BOOMERANG experiment, at l = (213), (541), (845) and l = (416), (750), respectively. Using model-independent analyses, we find that all five features are statistically significant, and we measure their location and amplitude. These are consistent with the adiabatic inflationary model. We also calculate the mean and variance of the peak and dip locations and amplitudes in a large seven-dimensional parameter space of such models, which gives good agreement with the model-independent estimates. We forecast where the next few peaks and dips should be found if the basic paradigm is correct. We test the robustness of our results by comparing Bayesian marginalization techniques on this space with likelihood maximization techniques applied to a second seven-dimensional cosmological parameter space, using an independent computational pipeline, and find excellent agreement: Ωtot = 1.02 versus 1.04 ± 0.05, Ωbh2 = 0.022 versus 0.019, and ns = 0.96 versus 0.90 ± 0.08. The determination of the best fit by the maximization procedure effectively ignores nonzero optical depth of reionization τC > 0, and the difference in primordial spectral index ns between the two methods is thus a consequence of the strong correlation of ns with the τC.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/02cd966a9e98d1befdcd96a275e6b416eb2e8ffa

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In Astronomy and Astrophysics

1. Simon D. M. White
2. F. V. D. Bosch
3. Volker Springel
4. C. Baugh
5. P. Hopkins
6. L. Hernquist
7. H. Mo
8. Xiaohu Yang

In Nuclear and High Energy Physics

1. F. V. D. Bosch
2. Andrei Linde
3. H. Mo
4. Xiaohu Yang
5. R. Kallosh
6. Zong-hong Zhu
7. C. Baugh
8. Carlos S. Frenk

Citations in the corpus

• The shear power spectrum from the COMBO-17 survey (2002, methodology): “Firstly, we consider only flat Universe models c© 2003 RAS, MNRAS341, 100–118 (ΩΛ + Ωm = 1) as compelling evidence for a flat Universe has already been found from the CMB data (e.g. de Bernardis et al. 2002; Pryke et al. 2002; Lewis & Bridle 2002).”
• The 2dF Galaxy Redshift Survey: The Amplitudes of fluctuations in the 2dFGRS and the CMB, and implications for galaxy biasing (2001, methodology): “The latest CMB measurements from Boomerang (Netterfield et al. 2001, de Bernardis et al. 2002), Maxima (Lee et al. 2001; Stomper et al. 2001) and DASI (Halverson et al. 2002; Pryke et al. 2002) suggest three acoustic peaks.”
• Cosmological Results from High-z Supernovae (2003, background): “Confidence that the universe is dominated by dark energy has been boosted by recent observations of the power spectrum of fluctuations in the cosmic microwave background (de Bernardis et al. 2002; Spergel et al. 2003).”
• Latest supernova data in the framework of the generalized Chaplygin gas model (2004, methodology): “The tightest constraints were obtained by Bento et al. (2003a) using the CMBR power spectrum measurements from BOOMERANG (de Bernardis et al. 2002) and Archeops (Benoit et al. 2002), together with the SNe Ia constraints.”
• How do galaxies get their gas (2002, methodology): “For the baryonic density we adopt b = 0.02 h−2, a value consistent both with the deuterium abundance in high-redshift Lyman-limit systems (Burles & Tytler 1998) and the value derived from cosmic microwave background (CMB) anisotropy measurements (de Bernardis et al. 2002).”
• Fast-Roll Inflation (2001, background): “One of the problems of the modern cosmology is to find a proper mechanism which drives the present stage of the accelerated expansion/inflation of the universe [7, 11].”
• Constraining galaxy formation and cosmology with the conditional luminosity function of galaxies (2002, background): “These cosmological parameters are consistent with a wide range of observations, and so this cosmology has become known as the “concordance” model (e.g., Perlmutter et al. 1999; Riess et al. 1998, 2001; Melchiorri et al. 2000; de Bernardis et al. 2002).”
• SNLS3: CONSTRAINTS ON DARK ENERGY COMBINING THE SUPERNOVA LEGACY SURVEY THREE-YEAR DATA WITH OTHER PROBES (2011, background): “…structure (Cole et al. 2005; Eisenstein et al. 2005; Percival et al. 2007; Reid et al. 2010) and the cosmic microwave background (CMB; e.g., de Bernardis et al. 2002; Bennett et al. 2003; Larson et al. 2011), this dark energy emerges as the dominant component of the Universe responsible for…”
• Hubble Space Telescope and Ground-based Observations of Type Ia Supernovae at Redshift 0.5: Cosmological Implications (2005, background): “The former favors a universe with total ¼ 1:0 0:02 (de Bernardis et al. 2002; Spergel et al. 2003), while the latter indicates that M 0:3 (Peacock et al. 2001) or perhaps even lower ( M 0:19; Bahcall et al. 2003).”
• String theory and hybrid inflation / acceleration (2001, methodology): “By making this connection we may constrain parameters of the brane model using the recent cosmological observations [10, 11, 12].”