Genetics of Personality Disorders

Reichborn‐Kjennerud, Ted

doi:10.1002/9780470015902.a0022415

Cited by 28 publications

(34 citation statements)

References 39 publications

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“…7. Current efforts to measure B-mode polarization (ACTpol [396], SPTpol [397], PolarBear [398], BICEP3 [399], SPIDER [400], EBEX [401], ABS [402]) and the next generation of CMB experiments (CLASS [403], PIPER [404], LSPE [405], LiteBird [406], Core+ [407]) will be able to further constrain the tensor-to-scalar ratio, r, with a possibility to probe values of r as small as ∼ 10 −3 (subject to the complexity of the foreground contamination [408]). One can consider which inflationary models can be probed in the future, given the current measurements of the scalar spectral index n s , by the standard approach of selecting a potential, or alternatively by using families of parameterizations for the slow-roll parameters [409].…”

Section: Parametermentioning

confidence: 99%

BeyondΛCDM: Problems, solutions, and the road ahead

Bull

Akrami

Adamek

et al. 2016

Physics of the Dark Universe

441

210

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Despite its continued observational successes, there is a persistent (and growing) interest in extending cosmology beyond the standard model, ΛCDM. This is motivated by a range of apparently serious theoretical issues, involving such questions as the cosmological constant problem, the particle nature of dark matter, the validity of general relativity on large scales, the existence of anomalies in the CMB and on small scales, and the predictivity and testability of the inflationary paradigm. In this paper, we summarize the current status of ΛCDM as a physical theory, and review investigations into possible alternatives along a number of different lines, with a particular focus on highlighting the most promising directions. While the fundamental problems are proving reluctant to yield, the study of alternative cosmologies has led to considerable progress, with much more to come if hopes about forthcoming high-precision observations and new theoretical ideas are fulfilled.Keywords: cosmology -dark energy -cosmological constant problem -modified gravitydark matter -early universe Cosmology has been both blessed and cursed by the establishment of a standard model: ΛCDM. On the one hand, the model has turned out to be extremely predictive, explanatory, and observationally robust, providing us with a substantial understanding of the formation of large-scale structure, the state of the early Universe, and the cosmic abundance of different types of matter and energy. It has also survived an impressive battery of precision observational tests -anomalies are few and far between, and their significance is contentious where they do arise -and its predictions are continually being vindicated through the discovery of new effects (B-mode polarization [1] and lensing [2,3] of the cosmic microwave background (CMB), and the kinetic Sunyaev-Zel'dovich effect [4] being some recent examples). These are the hallmarks of a good and valuable physical theory.On the other hand, the model suffers from profound theoretical difficulties. The two largest contributions to the energy content at late times -cold dark matter (CDM) and the cosmological constant (Λ) -have entirely mysterious physical origins. CDM has so far evaded direct detection by laboratory experiments, and so the particle field responsible for it -presumably a manifestation of "beyond the standard model" particle physics -is unknown. Curious discrepancies also appear to exist between the predicted clustering properties of CDM on small scales and observations. The cosmological constant is even more puzzling, giving rise to quite simply the biggest problem in all of fundamental physics: the question of why Λ appears to take such an unnatural value [5,6,7]. Inflation, the theory of the very early Universe, has also been criticized for being fine-tuned and under-predictive [8], and appears to leave many problems either unsolved or fundamentally unresolvable. These problems are indicative of a crisis.From January 14th-17th 2015, we held a conference in Oslo, Norway to surve...

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Section: Parametermentioning

confidence: 99%

BeyondΛCDM: Problems, solutions, and the road ahead

Bull

Akrami

Adamek

et al. 2016

Physics of the Dark Universe

441

210

View full text Add to dashboard Cite

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“…First, we consider a part of the sky, which is typical of small-scale experiments, inspired by the design study of the ebex experiment [47] and very similar to the patch and noise level used in Ref. [48] mimicking current ground-based efforts such as ACTpol or polarbear.…”

Section: Measuring the Tensor-to-scalar Ratio: Selected Examplesmentioning

confidence: 99%

Detecting the tensor-to-scalar ratio with the pure pseudospectrum reconstruction ofB-mode

Ferté¹,

Peloton²,

Grain³

et al. 2015

Phys. Rev. D

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B-mode of polarized anisotropies of the cosmic microwave background is a unique and nearly direct probe of primordial inflation, which can constrain the amplitude of the primordial gravity waves. However, its detection and precise measurement is made difficult by a minute amplitude of the signal, which has to be discerned from many contributions of non-cosmological origin and reliable estimated in the presence of numerous sources of statistical uncertainties. Among these latter, the Eto-B leakage, arising as a result of partial sky coverage, has been found to play a key and potentially fundamental role in determining the possible statistical significance with which the primordial Bmode signal can be detected. In this work we employ the pure-pseudo formalism devised to minimise the effects of the leakage on the variance of power spectrum estimates and discuss the limits on the tensor-to-scalar ratio, r, that could be realistically set by current and forthcoming measurements of the B-mode angular power spectrum. We compare those with the results obtained using other approaches: naïve mode-counting, minimum-variance quadratic estimators, and re-visit the question of optimizing the sky coverage of small-scale, suborbital experiments in order to maximize the statistical significance of the detection of r. We show that the optimized sky coverage is largely insensitive to the adopted approach at least for reasonably compact sky patches. We find, however, that the mode-counting overestimates the detection significance by a factor ∼ 1.17 as compared to the lossless maximum variance approach and by a factor ∼ 1.25 as compared to the lossy pure pseudospectrum estimator. In a second time, we consider more realistic experimental configurations. With a pure pseudospectrum reconstruction of B-modes and considering only statistical uncertainties, we find that a detection of r ∼ 0.11, r ∼ 0.0051 and r ∼ 0.0026 at 99% of confidence level is within the reach of current sub-orbital experiments, future arrays of ground-based telescopes and a satellite mission, respectively. This means that an array of telescopes could be sufficient to discriminate between large-and small-field models of inflation, even if the E-to-B leakage is consistently included but accounted for in the analysis. However, a satellite mission will be required to distinguish between different small-field models depending on the number of e-folds.

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“…Current experiments already deploy several hundreds to thousands of detectors, making them ideal candidates for the algorithm, e.g., SPTpol (about 800 pixels, Austermann et al 2012), POLARBEAR (about 1300 pixels, Kermish et al 2012), EBEX (about 1400 pixels, Reichborn-Kjennerud et al 2010), Spider (about 2600 pixels, Filippini et al 2010), ACTPol (about 3000 pixels, Niemack et al 2010). For future experiments, the number of detectors can be expected to increase further, e.g., for PIPER (about 5000 pixels, Lazear et al 2013), the Cosmic Origins Explorer (about 6000 pixels, The COrE Collaboration 2011), or POLARBEAR-2 (about 7500 pixels Tomaru et al 2012), making the application of the algorithm even more rewarding.…”

Section: Scope Of the Algorithmmentioning

confidence: 99%

Compressed convolution

Elsner

Wandelt

2014

A&A

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We introduce the concept of compressed convolution, a technique to convolve a given data set with a large number of non-orthogonal kernels. In typical applications our technique drastically reduces the effective number of computations. The new method is applicable to convolutions with symmetric and asymmetric kernels and can be easily controlled for an optimal trade-off between speed and accuracy. It is based on linear compression of the collection of kernels into a small number of coefficients in an optimal eigenbasis. The final result can then be decompressed in constant time for each desired convolved output. The method is fully general and suitable for a wide variety of problems. We give explicit examples in the context of simulation challenges for upcoming multi-kilo-detector cosmic microwave background (CMB) missions. For a CMB experiment with O(10 000) detectors with similar beam properties, we demonstrate that the algorithm can decrease the costs of beam convolution by two to three orders of magnitude with negligible loss of accuracy. Likewise, it has the potential to allow the reduction of disk space required to store signal simulations by a similar amount. Applications in other areas of astrophysics and beyond are optimal searches for a large number of templates in noisy data, e.g. from a parametrized family of gravitational wave templates; or calculating convolutions with highly overcomplete wavelet dictionaries, e.g. in methods designed to uncover sparse signal representations.

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Genetics of Personality Disorders

Cited by 28 publications

References 39 publications

BeyondΛCDM: Problems, solutions, and the road ahead

BeyondΛCDM: Problems, solutions, and the road ahead

Detecting the tensor-to-scalar ratio with the pure pseudospectrum reconstruction ofB-mode

Compressed convolution

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