A Measurement by BOOMERANG of Multiple Peaks in the Angular Power Spectrum of the Cosmic Microwave Background

Netterfield, C. B.; Ade, Peter A. R.; Bock, J. J.; Bond, J. R.; Borrill, J.; Boscaleri, A.; Coble, K.; Contaldi, C. R.; Crill, B. P.; Bernardis, P. de; Farese, P.; Ganga, K.; Giacometti, M.; Hivon, E.; Hristov, V. V.; Iacoangeli, A.; Jaffe, A. H.; Jones, W. C.; Lange, A. E.; Martinis, L.; Masi, S.; Mason, P.; Mauskopf, Philip Daniel; Melchiorri, A.; Montroy, T. E.; Pascale, Enzo; Piacentini, F.; Pogosyan, D.; Pongetti, F.; Prunet, S.; Romeo, G.; Ruhl, J. E.; Scaramuzzi, F.

doi:10.1086/340118

Cited by 811 publications

(580 citation statements)

References 35 publications

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“…After a correction of the first results from BOOMER-ANG (de Bernardis et al 2000) by Netterfield et al (2002), these measurements are in astounding agreement with the simplest flat adiabatic purely scalar model of structure formation. The best-fit cosmological parameters obtained coincide with other, completely independent determinations, like, for example, the baryon density parameter predicted by nucleosynthesis (Burles, Nollet, & Turner 2001).…”

Section: Introductionsupporting

confidence: 54%

“…The new data on the cosmic microwave background (CMB) temperature anisotropy obtained in the BOOMER-ANG (de Bernardis et al 2000;Netterfield et al 2002), MAXIMA-1 (Hanany et al 2000;Lee et al 2001), and DASI experiments provide relatively accurate measurements of the CMB anisotropies up to l $ 1000. BOOMERANG is a long-duration balloon (LDB) flight around the South Pole, MAXIMA is a balloon flight from Palestine, Texas, and DASI is an interferometer experiment.…”

Section: Introductionmentioning

confidence: 99%

“…The outline of the paper is as follows: In x 2 we determine the locations and amplitudes of the first, second, and third acoustic peak as well as first and second dip and their confidence levels (CLs) using the published data on the CMB angular power spectrum from BOOMERANG (Netterfield et al 2002), MAXIMA-1 (Lee et al 2001), and DASI . Analytical approximations for the positions and amplitudes of the acoustic peaks and dips are described in x 3.…”

Section: Introductionmentioning

confidence: 99%

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Acoustic Peaks and Dips in the Cosmic Microwave Background Power Spectrum: Observational Data and Cosmological Constraints

Durrer¹,

Novosyadlyj²,

Apunevych³

2003

ApJ

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The locations and amplitudes of three acoustic peaks and two dips in the BOOMERANG, MAXIMA, and DASI measurements of the cosmic microwave background (CMB) anisotropy power spectra as well as their statistical confidence levels are determined in a model-independent way. It is shown that the BOOMERANG 2001 data from Netterfield and coworkers fix the location and amplitude of the first acoustic peak at more than 3 confidence. The next two peaks and dips are determined at a confidence level above 1 but below 2 . The locations and amplitudes of the first three peaks and two dips are l p 1 ¼ 212 AE 17,(1 errors include statistical and systematic errors). The MAXIMA and DASI experiments give similar values for the extrema that they determine. For MAXIMA these are the first and third peaks, for DASI the first and second peaks and the first dip. Moreover, the locations and amplitudes of the extrema determined from the combined data of all experiments are quite close to the corresponding values extracted from the BOOMERANG data alone. In order to use these data in a fast search for cosmological parameters, an accurate analytic approximation to calculate CMB peak and dip positions and amplitudes in mixed dark matter models with cosmological constant and curvature is derived and tested. The determined cosmological parameters from the CMB acoustic extrema data show good agreement with other determinations, especially with the baryon content as deduced from standard nucleosynthesis constraints, as shown by Burles and coworkers. These data supplemented by constraints from direct measurements of some cosmological parameters and data on large-scale structure lead to a best-fit model that agrees with practically all the used experimental data within 1 . The best-fit parameters are Ã ¼ 0

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Section: Introductionsupporting

confidence: 54%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Acoustic Peaks and Dips in the Cosmic Microwave Background Power Spectrum: Observational Data and Cosmological Constraints

Durrer¹,

Novosyadlyj²,

Apunevych³

2003

ApJ

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“…Here we take the latest bound from WMAP, Ωh 2 < .128 and also compare with the old limit (of 2001) from BOOMERANG [47], MAXIMA [48] and DASI [49] with Ωh 2 < 0.3. We will refer to this limit as pre-WMAP.…”

Section: Relic Density Of Neutralinosmentioning

confidence: 99%

Lower limit on the neutralino mass in the general MSSM

Bélanger¹,

Boudjema²,

Cottrant³

et al. 2004

J. High Energy Phys.

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We discuss constraints on SUSY models with non-unified gaugino masses and R P conservation. We derive a lower bound on the neutralino mass combining the direct limits from LEP, the indirect limits from (g − 2) µ , b → sγ, B s → µ + µ − and the relic density constraint from WMAP. The lightest neutralino mχ0 1 ≈ 6 GeV is found in models with a light pseudoscalar with M A < 200 GeV and a large value for tan β. Models with heavy pseudoscalars lead to mχ0 1 > 18(29) GeV for tan β = 50(10). We show that even a very conservative bound from the muon anomalous magnetic moment can increase the lower bound on the neutralino mass in models with µ < 0 and/or large values of tan β. We then examine the potential of the Tevatron and the direct detection experiments to probe the SUSY models with the lightest neutralinos allowed in the context of light pseudoscalars with high tan β. We also examine the potential of an e + e − collider of 500 GeV to produce SUSY particles in all models with neutralinos lighter than the W . In contrast to the mSUGRA models, observation of at least one sparticle is not always guaranteed.

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“…The first analyses of the BOO-MERANG and MAXIMA experiments implied a low second peak in the CMB power spectrum, which could be explained by a higher baryon density b h 2 % 0:03 (Lange et al 2000;Jaffe et al 2001;Padmanabhan & Sethi 2001). Results from the more recent analysis of BOOMERANG (including more of the data) and from the Degree Angular Scale Interferometer experiment show a stronger second peak that is consistent with the b h 2 values inferred from the deuterium abundance (Netterfield et al 2002;Pryke et al 2002). It is tempting to conclude, therefore, that the baryon density is now known to be b ¼ 0:022h À2 with an uncertainty of $10%.…”

Section: Introductionmentioning

confidence: 61%

The Influence of \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10

Gardner¹,

Katz²,

Hernquist³

et al. 2003

ApJ

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We analyze high-redshift structure in three hydrodynamic simulations that have identical initial conditions and cosmological parameters and differ only in the value of the baryon density parameter, b ¼ 0:02, 0.05, and 0.125. Increasing b does not change the fraction of baryons in the diffuse (unshocked) phase of the intergalactic medium, but it increases cooling rates and therefore transfers some baryons from the shocked intergalactic phase to the condensed phase associated with galaxies. Predictions of Ly forest absorption are almost unaffected by changes in b at velocity scales greater than 5 km s À1 (our resolution limit), provided that the UV background intensity is adjusted so that the mean opacity of the forest matches the observed value. The required UV background intensity scales as 1:7 b , and the higher photoionization rate increases the gas temperature in low-density regions. Damped Ly absorption and Lyman limit absorption both increase with increasing b , although the impact is stronger for damped absorption and is weaker at z ¼ 4 than at z ¼ 2 3. The mass of cold gas and stars in high-redshift galaxies increases faster than b but slower than 2 b , and the global star formation rate scales approximately as 1:5 b . In the higher b models, the fraction of baryonic material within the virial radius of dark matter halos is usually higher than the universal fraction, indicating that gasdynamics and cooling can lead to an overrepresentation of baryons in virialized systems. On the whole, our results imply a fairly intuitive picture of the influence of b on high-redshift structure, and we provide scalings that can be used to estimate the impact of b uncertainties on the predictions of hydrodynamic simulations.

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A Measurement by BOOMERANG of Multiple Peaks in the Angular Power Spectrum of the Cosmic Microwave Background

Cited by 811 publications

References 35 publications

Acoustic Peaks and Dips in the Cosmic Microwave Background Power Spectrum: Observational Data and Cosmological Constraints

Acoustic Peaks and Dips in the Cosmic Microwave Background Power Spectrum: Observational Data and Cosmological Constraints

Lower limit on the neutralino mass in the general MSSM

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