Polarizing bubble collisions

Czech, Bartłomiej; Kleban, Matthew; Larjo, Klaus; Levi, Thomas S.; Sigurdson, Kris

doi:10.1088/1475-7516/2010/12/023

Cited by 35 publications

(50 citation statements)

References 47 publications

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“…However, several non-standard physical mechanisms have been proposed as possible explanations. These include the gravitational effect produced by a collapsing cosmic texture (Cruz et al 2007), the linear and nonlinear ISW effect caused by a void in the large-scale structure (e.g., Tomita 2005;Inoue & Silk 2006;Rudnick et al 2007;Tomita & Inoue 2008;Finelli et al 2016), a cosmic bubble collision within the eternal inflation framework (Czech et al 2010;Feeney et al 2011;McEwen et al 2012), and a localized version of the inhomogeneous reheating scenario within the inflationary paradigm (Bueno Sanchez 2014).…”

Section: Commandermentioning

confidence: 99%

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Planck2015 results

Ade

Aghanim

Akrami

et al. 2016

A&A

364

192

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We test the statistical isotropy and Gaussianity of the cosmic microwave background (CMB) anisotropies using observations made by the Planck satellite. Our results are based mainly on the full Planck mission for temperature, but also include some polarization measurements. In particular, we consider the CMB anisotropy maps derived from the multi-frequency Planck data by several component-separation methods. For the temperature anisotropies, we find excellent agreement between results based on these sky maps over both a very large fraction of the sky and a broad range of angular scales, establishing that potential foreground residuals do not affect our studies. Tests of skewness, kurtosis, multi-normality, N-point functions, and Minkowski functionals indicate consistency with Gaussianity, while a power deficit at large angular scales is manifested in several ways, for example low map variance. The results of a peak statistics analysis are consistent with the expectations of a Gaussian random field. The "Cold Spot" is detected with several methods, including map kurtosis, peak statistics, and mean temperature profile. We thoroughly probe the large-scale dipolar power asymmetry, detecting it with several independent tests, and address the subject of a posteriori correction. Tests of directionality suggest the presence of angular clustering from large to small scales, but at a significance that is dependent on the details of the approach. We perform the first examination of polarization data, finding the morphology of stacked peaks to be consistent with the expectations of statistically isotropic simulations. Where they overlap, these results are consistent with the Planck 2013 analysis based on the nominal mission data and provide our most thorough view of the statistics of the CMB fluctuations to date.

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Section: Commandermentioning

confidence: 99%

“…For example, no polarization signal would be expected in those models producing secondary anisotropies due to a gravitational effect, whereas a specific pattern might be expected in a bubble collision scenario (Czech et al 2010). Appropriate tests will be pursued in future work, once the large-scale polarization data are available.…”

Section: Commandermentioning

confidence: 99%

Planck2015 results

Ade

Aghanim

Akrami

et al. 2016

A&A

364

192

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“…Considering CMB observations first, the increased angular resolution of upcoming experiments such as Planck will improve constraints on the step model, but not on the ramp model where the signal is weighted toward large scales that are already sample variance limited in WMAP. Future measurements of CMB polarization may eventually improve constraints on both models [13]. Looking beyond the CMB, large-scale structure can potentially provide interesting constraints on bubble collisions, e.g.…”

Section: Discussionmentioning

confidence: 99%

“…Our observable Hubble volume is a smaller region given by taking the intersection with the past lightcone of a present-day observer. If there is a second bubble nucleation, and its future lightcone intersects our observable Hubble volume, then the metric will be perturbed, and this will generate a disc-shaped CMB temperature perturbation [10][11][12][13][14].…”

Section: Mini-summary Of the Theory Of Bubble Collisionsmentioning

confidence: 99%

Optimal analysis of azimuthal features in the CMB

Osborne

Senatore

Smith

2013

J. Cosmol. Astropart. Phys.

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We present algorithms for searching for azimuthally symmetric features in CMB data. Our algorithms are fully optimal for masked all-sky data with inhomogeneous noise, computationally fast, simple to implement, and make no approximations. We show how to implement the optimal analysis in both Bayesian and frequentist cases. In the Bayesian case, our algorithm for evaluating the posterior likelihood is so fast that we can do a brute-force search over parameter space, rather than using a Monte Carlo Markov chain. Our motivating example is searching for bubble collisions, a pre-inflationary signal which can be generated if multiple tunneling events occur in an eternally inflating spacetime, but our algorithms are general and should be useful in other contexts.

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“…Alternative proposals include cosmic texture [37,38], chaotic post-inflationary preheating [39], cosmic bubble collisions (e.g., [40]), and nothing less than a gate to extra dimensions [41].…”

Section: Cold Spot and Proposed Explanationsmentioning

confidence: 99%

A theory of a spot

Afshordi

Slosar

Wang

2011

J. Cosmol. Astropart. Phys.

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We present a simple inflationary scenario that can produce arbitrarily large spherical underdense or overdense regions embedded in a standard Λ cold dark matter paradigm, which we refer to as bubbles. We analyze the effect such bubbles would have on the Cosmic Microwave Background (CMB). For super-horizon sized bubble in the vicinity of the last scattering surface, a signal is imprinted onto CMB via a combination of SachWolfe and an early integrated Sach-Wolfe (ISW) effects. Smaller, sub-horizon sized bubbles at lower redshifts (during matter domination and later) can imprint secondary anisotropies on the CMB via Rees-Sciama, late-time ISW and Ostriker-Vishniac effects. Our scenario, and arguably most similar inflationary models, produce bubbles which are over/underdense in potential: in density such bubbles are characterized by having a distinct wall with the interior staying at the cosmic mean density. We show that such models can potentially, with only moderate fine tuning, explain the cold spot, a non-Gaussian feature identified in the Wilkinson Microwave Anisotropy Probe (WMAP) data by several authors. However, more detailed comparisons with current and future CMB data are necessary to confirm (or rule out) this scenario.

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Polarizing bubble collisions

Cited by 35 publications

References 47 publications

Planck2015 results

Planck2015 results

Optimal analysis of azimuthal features in the CMB

A theory of a spot

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