Conventional meta-analytic techniques rely on the assumption that effect size estimates from different studies are independent and have sampling distributions with known conditional variances. The independence assumption is violated when studies produce several estimates based on the same individuals or there are clusters of studies that are not independent (such as those carried out by the same investigator or laboratory). This paper provides an estimator of the covariance matrix of meta-regression coefficients that are applicable when there are clusters of internally correlated estimates. It makes no assumptions about the specific form of the sampling distributions of the effect sizes, nor does it require knowledge of the covariance structure of the dependent estimates. Moreover, this paper demonstrates that the meta-regression coefficients are consistent and asymptotically normally distributed and that the robust variance estimator is valid even when the covariates are random. The theory is asymptotic in the number of studies, but simulations suggest that the theory may yield accurate results with as few as 20-40 studies. Copyright © 2010 John Wiley & Sons, Ltd.

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Several statistics have been proposed for measuring the kSZ effect by combining the small-scale CMB with galaxy surveys. We review five such statistics, and show that they are all mathematically equivalent to the optimal bispectrum estimator of type ggT . Reinterpreting these kSZ statistics as special cases of bispectrum estimation makes many aspects transparent, for example optimally weighting the estimator, or incorporating photometric redshift errors. We analyze the information content of the bispectrum and show that there are two observables: the small-scale galaxy-electron power spectrum Pge(kS), and the large-scale galaxy-velocity power spectrum Pgv(k). The cosmological constraining power of the kSZ arises from its sensitivity to fluctuations on large length scales, where its effective noise level can be much better than galaxy surveys. Contents I. Introduction II. Definitions and notation III. The δ g δ g T bispectrum A. Mathematical representation of the bispectrum B. Optimal bispectrum estimator and Fisher matrix C. The tree-level kSZ bispectrum D. Squeezed limit IV. Equivalence with other formalisms A. Equivalence between the bispectrum and pair sum B. Equivalence between the bispectrum and kSZ template formalisms C. Equivalence between the bispectrum and velocity matched filter D. Equivalence between the bispectrum and the velocity growth method E. Equivalence between the bispectrum and long-wavelength velocity reconstruction V. Forecasts and phenomenology A. Total signal-to-noise ratio B. What does kSZ tomography actually measure? C. Constraining cosmology: the large-scale power spectrum P gv (k L ) D. Constraining astrophysics: the small-scale power spectrum P ge (k S ) E. More on the optical depth degeneracy F. Including kSZ tomography in larger cosmological analyses VI. Photometric redshift errors and redshift space distortions A. Modelling photo-z errors and RSD B. The kSZ bispectrum with photo-z's and RSD C. Constraining astrophysics using P ge (k S ), with photo-z's and RSD D. Constraining cosmology with photo-z's and RSD

Ordered two-dimensional arrays such as S-layers 1 , 2 and designed analogues 3 – 5 have intrigued bioengineers, 6 , 7 but with the exception of a single lattice formed with flexible linkers, 8 they are constituted from just one protein component. For modulating assembly dynamics and incorporating more complex functionality, materials composed of two components would have considerable advantages. 9 – 12 Here we describe a computational method to generate co-assembling binary layers by designing rigid interfaces between pairs of dihedral protein building-blocks, and use it to design a p6m lattice. The designed array components are soluble at mM concentrations, but when combined at nM concentrations, rapidly assemble into nearly crystalline micrometer-scale arrays nearly identical (based on TEM and SAXS) to the computational design model in vitro and in cells without the need for a two-dimensional support. Because the material is designed from the ground up, the components can be readily functionalized, and their symmetry reconfigured, enabling formation of ligand arrays with distinguishable surfaces which we demonstrate can drive extensive receptor clustering, downstream protein recruitment, and signaling. Using AFM on supported bilayers and quantitative microscopy on living cells, we show that arrays assembled on membranes have component stoichiometry and structure similar to arrays formed in vitro, and thus that our material can impose order onto fundamentally disordered substrates like cell membranes. In sharp contrast to previously characterized cell surface receptor binding assemblies such as antibodies and nanocages, which are rapidly endocytosed, we find that large arrays assembled at the cell surface suppress endocytosis in a tunable manner, with potential therapeutic relevance for extending receptor engagement and immune evasion. Our work paves the way towards a synthetic cell biology, where a new generation of multi-protein macroscale materials is designed to modulate cell responses and reshape synthetic and living systems.

The statistics of primordial curvature fluctuations are our window into the period of inflation, where these fluctuations were generated. To date, the cosmic microwave background has been the dominant source of information about these perturbations. Large scale structure is however from where drastic improvements should originate. In this paper, we explain the theoretical motivations for pursuing such measurements and the challenges that lie ahead. In particular, we discuss and identify theoretical targets regarding the measurement of primordial non-Gaussianity. We argue that when quantified in terms of the local (equilateral) template amplitude f loc NL (f eq NL ), natural target levels of sensitivity are ∆f loc,eq. NL 1. We highlight that such levels are within reach of future surveys by measuring 2-, 3-and 4-point statistics of the galaxy spatial distribution. This paper summarizes a workshop held at CITA (University of Toronto) on October 23-24, 2014 [Link]. BNL-1124147-2014-IR Contents 4 Beyond the Halo Power Spectrum 4.1 State of Bispectrum Observations 4.