Barthelemy, Alexandre Codis, Sandrine Bernardeau, Francis

Weak lensing of galaxies and CMB photons through the large-scale structure of the Universe is one of the most promising cosmological probes with upcoming experiments dedicated to its measurements such as Euclid/LSST and CMB Stage 4 experiments. With increasingly precise measurements, there is a dire need for accurate theoretical predictions. In thi...

Lund, K. Jardine, M. Lehmann, L. T. Mackay, D. H. See, V. Vidotto, A. A. Donati, J. -F. Fares, R. Folsom, C. P. Jeffers, S. V.
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Helicity is a fundamental property of a magnetic field but to date it has only been possible to observe its evolution in one star - the Sun. In this paper we provide a simple technique for mapping the large-scale helicity density across the surface of any star using only observable quantities: the poloidal and toroidal magnetic field components (wh...

Lacasa, Fabien

As galaxy surveys become more precise and push to smaller scales, the need for accurate covariances beyond the classical Gaussian formula becomes more acute. Here, I investigate the analytical implementation and impact of non-Gaussian covariance terms that I previously derived for galaxy clustering. Braiding covariance is such a class of terms and ...

Pasquato, M.

ABSTRACT The Alessandrini A+ indicator is a measure of star cluster dynamical evolution based on the mass-segregation of blue straggler stars. A+ is defined as the integral of the cumulative distribution of blue stragglers over log radius, minus a term related to the reference population used. In a companion paper I introduced a model of dynamical ...

Uhlemann, Cora Friedrich, Oliver Villaescusa-Navarro, Francisco Banerjee, Arka Codis, Sandrine

We comprehensively analyse the cosmology dependence of counts-in-cell statistics. We focus on the shape of the one-point probability distribution function (PDF) of the matter density field at mildly nonlinear scales. Based on large-deviation statistics, we parametrise the cosmology dependence of the matter PDF in terms of the linear power spectrum,...

Munshi, D. Namikawa, T. Kitching, T. D. McEwen, J. D. Takahashi, R. Bouchet, F. R. Taruya, A. Bose, B.

Recent studies have demonstrated that {\em secondary} non-Gaussianity induced by gravity will be detected with a high signal-to-noise (S/N) by future and even by on-going weak lensing surveys. One way to characterise such non-Gaussianity is through the detection of a non-zero three-point correlation function of the lensing convergence field, or of ...

Taruya, Atsushi Saga, Shohei Breton, Michel-Andrès Rasera, Yann Fujita, Tomohiro

Redshift-space distortions (RSD) in galaxy redshift surveys generally break both the isotropy and homogeneity of galaxy distribution. While the former aspect is particularly highlighted as a probe of growth of structure induced by gravity, the latter aspect, often quoted as wide-angle RSD but ignored in most of the cases, will become important and ...

Visser, P.M. (author) Mol, M.A. (author)

Context. A double planet system or planet binary undergoes eclipses that modify the reflective light curve. In the time domain, the eclipse events are fast and weak. This would make their signal difficult to find and recognize in the phase light curve, even for small inclinations when eclipses happen frequently. However, due to the quasiperiodic na...

Pasquato, M.

ABSTRACT Blue straggler stars are more massive than the average star in globular clusters, as they originate from the merger of two stars. Consequently, they experience dynamical friction, progressively sinking to the cluster center. Recently, several indicators of the degree of dynamical relaxation of a globular cluster have been proposed, based o...

Castorina, E White, M

This is an erratum to the paper 'The Zeldovich approximation and wide-angle redshift-space distortions' by Castorina & White (2018). There is a mistake in equation (37) which should read (Equation Presented) where Σ2 and ξij are defined in the main text. The figures and the conclusions are all unchanged, however this mistake propagates to equation ...