Presentation on theme: "References: López-Corredoira & Gabrielli, 2013, Physica A, 392, 474"— Presentation transcript:
1 Peaks in the CMBR power spectrum: Physical interpretation for any cosmological scenario References:López-Corredoira & Gabrielli, 2013, Physica A, 392, 474López-Corredoira, 2013, Int. J. Mod. Phys. D, 22(7), idMartín López-CorredoiraInstituto de Astrofísica de CanariasTenerife, Spain
2 Origin of theoscillationsTwo-point correlation function (Transform: Fourier/Legendre) Power spectrum
3 Origin of theoscillations- If 𝐶 𝜃 has some non-continuous derivative at some point, then Cl [or P(k)] presents oscillations. (see mathematical demonstration in López-Corredoira & Gabrielli 2013) - These kinds of discontinuities do not need to be abrupt in an infinitesimal range of angular distances but may also be smooth. - The positions, widths, amplitudes of the peaks are not independent, but they depend only on the position of the point with the abrupt transition in 𝐶 𝜃 and its derivatives.
4 How to generate abrupt changes in the correlation function? Toy ModelHow to generate abrupt changes in the correlation function?Filled disks of contantradius R=1o with a Poissonian distribution
5 How to generate abrupt changes in the correlation function? Toy ModelHow to generate abrupt changes in the correlation function?Filled disks of contantradius R=1o with a random distribution but disks do not intersect
6 How to generate abrupt changes in the correlation function? Toy ModelHow to generate abrupt changes in the correlation function?Filled disks of contantradius R=1o with a non-Poissonian distribution
7 How to generate abrupt changes in the correlation function? Toy ModelHow to generate abrupt changes in the correlation function?Filled disks of variable (finite) radius with any distribution inside, and distribution of disks
8 A model to generate CMBR power spectrum PhysicalinterpretationA model to generate CMBR power spectrumDisks may represent a projection of spherical regions in 3D space.The standard cosmological model is a particular case in which the radius of the disk is constant representing the size of the acoustic horizon (diameter of the acoustic horizon region at recombination epoch: 1.2 degrees). Photon-baryon fluid compressed by gravitational attraction produced by local density fluctuations.Non-standard cosmological models: any fluid with clouds of overdensities that emits/absorbs radiation or interact gravitationally with the photons. Different radii is possible when the 3D distribution projects clouds from different distances.
9 Caveats of an alternative model of CMBR PhysicalinterpretationCaveats of an alternative model of CMBRBlack body shape.(Almost) Gaussian fluctuations.Only 6 free parameters to fit the power spectrum.
10 WMAP-7yr data How many free Parameters? Dip = anticorrelation of disks f6: set of polynomial functions with continuous derivative with 6 free parameters: χred2=3.0f4: set of polynomial functions with continuous derivative with 4 free parameters.g4: set of polynomial / logarithmic functions with 4 free parameters.
11 WMAP-7yr + ATACAMA/ACT data How many freeParameters?WMAP-7yr + ATACAMA/ACT dataf6,A: set of polynomial functions with continuous derivative with 6 free parameters: χred2=1.4
12 Power spectrum How many free Parameters? Peaks 3rd. and beyond are not fitted with the sets of polynomials (possibly because we have not used ѳ<0.2 deg.)
13 Power spectrum How many free Parameters? Narlikar et al. (2007): WMAP-3yr data.Solid line: QSSC and clusters of galaxies with 6 parameters;Dashed line: standard model.Angus & Diaferio (2011): WMAP-7yr+ACT+ACBAR data.Blue line: MOND, with sterile neutrinos with 6 free parameters;Red line: standard model.
14 Success of standard cosmological model? DiscussionSuccess of standard cosmological model?Wrong predictions which were corrected ad hoc:Temperature TCMBR=50 K (Gamow 1961) or 30 K (Dicke et al. 1965)Amplitude of the anisotropies (ΔT/T ~ ; Sachs & Wolfe 1967)Position of the first peak at l≈200 (measured for the first time in the middle 90s [White et al. 1996] and contradicting the preferred cosmological model at that time Ω=Ωm≈0.2)Amplitude of the second peak as high as the first peak (Bond & Efstathiou 1987)Etc.Succesful predictions:IsotropyBlack body radiationPeaks in CMBR power spectrum (Peebles & Yu 1970)Etc.Dark matter ad hocDark energy ad hoc
15 FURTHER RESEARCH IS NEEDED DiscussionRecipe to cook CMBR in an alternative cosmologyGeneral features of CMBR and its power spectrum/two-point correlation function:Temperature TCMBR=3 KIsotropyBlack body radiationGaussian fluctuationsPeaks in CMBR power spectrum6 free parameters should fit itOthers (polarization,…)Explanations which do not require the standard model:Several ideas (e.g., stellar radiation)Radiation coming from all directionsThermalization of radiation? Not clear yetThere are many processes in Nature which generate Gaussian fluctuations; but, there may be non-Gaussianity tooAbrupt transition of emission/absorption inside and outside some clouds/regionsA simple set of polynomials produce a quite good fit of the 2-point corr.func., but do not explain 3rd peak ≈ 2nd peak amplitudeFURTHER RESEARCH IS NEEDEDPendingMajor problemReferences: López-Corredoira & Gabrielli, 2013, Physica A, 392, 474López-Corredoira, 2013, Int. J. Mod. Phys. D, 22(7), id
16 Science is in decline.Facts and challenging ideas about the exhaustion of our culture in The Twilight of the Scientific AgePublisher: BrownWalker PressYear: 2013Book available at: BrownWalker Press, Amazon, Barnes & Noble,…
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