The dual parameterization of the proton generalized parton distribution functions H and E and description of the DVCS cross sections and asymmetries

We develop the minimal model of a new leading order parameterization of GPDs introduced by Shuvaev and Polyakov. The model for GPDs H and E is formulated in terms of the forward quark distributions, the Gegenbauer moments of the D-term and the forward limit of the GPD E. The model is designed primarely for small and medium-size values of x_B, x_B \leq 0.2. We examined two different models of the t-dependence of the GPDs: The factorized exponential model and the non-factorized Regge-motivated model. Using our model, we successfully described the DVCS cross section measured by H1 and ZEUS, the moments of the beam-spin A_{LU}^{\sin \phi}, beam-charge A_{C}^{\cos \phi} and transversely-polarized target A_{UT}^{\sin \phi \cos \phi} DVCS asymmetries measured by HERMES and A_{LU}^{\sin \phi} measured by CLAS. The data on A_{C}^{\cos \phi} prefers the Regge-motivated model of the t-dependence of the GPDs. The data on A_{UT}^{\sin \phi \cos \phi} indicates that the u and d quarks carry only a small fraction of the proton total angular momentum.Comment: 33 pages, 11 figure

Dinâmica de crescimento de angico (Anadenanthera colubrina var. cebil) no Pantanal Mato-Grossense.

bitstream/CNPF-2009-09/41784/1/circ-tec102.pd

Growth dynamics of Anadenanthera colubrina var. cebil and Tabebuia impetiginosa from Pantanal Mato-grossense, Brazil.

O uso de informações obtidas por estudos com anéis de crescimento é cada vez mais freqüente e são muito importantes para florestas naturais tropicais onde a demanda por madeira é grande, mas geralmente não existem dados disponíveis sobre o crescimento das espécies arbóreas para a estruturação de programas de manejo. O Pantanal da Nhecolândia, sub-região do Pantanal Mato-Grossense, pode ser visto como uma dessas regiões onde as florestas naturais são sistematicamente cortadas para extração de madeira, ou para implantação de pastagens cultivadas. Fatores climáticos e edáficos, característicos do Pantanal, sub-região da Nhecolândia, induzem a formação de anéis anuais de crescimento. Objetivou-se, com este trabalho, determinar a idade e os incrementos radiais de Anadenanthera colubrina var. cebil e Tabebuia impetiginosa, pela análise dos anéis de crescimento. Discos de oito árvores de Anadenanthera colubrina var. cebil e seis de Tabebuia impetiginosa foram coletados em julho de 1996, na fazenda Nhumirim, de propriedade da Embrapa Pantanal, localizada na sub-região da Nhecolândia. As árvores de Anadenanthera colubrina var. cebil e Tabebuia impetiginosa apresentavam 14 a 30 e 15 a 30 anos respectivamente, com crescimento anual médio, em diâmetro a 1,3 m do solo, variando de 5,4 a 8,0 mm em Anadenanthera colubrina var. cebil e de 4,8 a 11,6 mm em Tabebuia impetiginosa. O tempo médio para Anadenanthera colubrina var. cebil e Tabebuia impetiginosa atingirem 40 cm de diâmetro foi estimado em, no mínimo, 55 anos

Limitations of model fitting methods for lensing shear estimation

Gravitational lensing shear has the potential to be the most powerful tool for constraining the nature of dark energy. However, accurate measurement of galaxy shear is crucial and has been shown to be non-trivial by the Shear TEsting Programme. Here we demonstrate a fundamental limit to the accuracy achievable by model-fitting techniques, if oversimplistic models are used. We show that even if galaxies have elliptical isophotes, model-fitting methods which assume elliptical isophotes can have significant biases if they use the wrong profile. We use noise-free simulations to show that on allowing sufficient flexibility in the profile the biases can be made negligible. This is no longer the case if elliptical isophote models are used to fit galaxies made up of a bulge plus a disk, if these two components have different ellipticities. The limiting accuracy is dependent on the galaxy shape but we find the most significant biases for simple spiral-like galaxies. The implications for a given cosmic shear survey will depend on the actual distribution of galaxy morphologies in the universe, taking into account the survey selection function and the point spread function. However our results suggest that the impact on cosmic shear results from current and near future surveys may be negligible. Meanwhile, these results should encourage the development of existing approaches which are less sensitive to morphology, as well as methods which use priors on galaxy shapes learnt from deep surveys.Comment: 10 pages, 8 figure

Does Training on Broad Band Tactile Stimulation Promote the Generalization of Perceptual Learning?

Given the clear role of sensory feedback in successful motor control, there is a growing interest in integrating substitutionary tactile feedback into robotic limb devices. To enhance the utility of such feedback, here we investigate how to best improve the limited generalization of tactile learning across body parts and stimulus properties. Specifically, we sought to understand how perceptual learning with different types of tactile stimuli may give rise to different patterns of learning generalization. To address this, we utilized vibro-tactile effectors to present patterns of stimulation in a match-to-sample paradigm. One group of participants trained on narrow-band stimulation consisting of simple sinusoidal vibrations, and the other on broad-band stimulation generated from music. We hypothesized that training on broad-band tactile stimulation would promote greater generalization of learning outcomes. We found training with broad-band stimuli generalized to underlying stimulus features of frequency discrimination but showed weaker generalization to un-trained digits. This study provides a first step towards devising perceptual learning paradigms that will generalize broadly to the untrained perceptual contexts

Gravitational Lenses in Generalized Einstein-Aether theory: the Bullet Cluster

We study the lensing properties of an asymmetric mass distribution and vector field in Generalized Einstein-Aether (GEA) theory. As vector field fluctuations are responsible in GEA for seeding baryonic structure formation, vector field concentrations can exist independently of baryonic matter. Such concentrations would not be expected to be tied to baryonic matter except gravitationally, and so, like dark matter halos, would become separated from baryonic matter in interacting systems such as the Bullet Cluster. These vector field concentrations cause metric deviations that affect weak lensing. Therefore, the distribution of weak lensing deviates from that which would be inferred from the luminous mass distribution, in a way that numerical calculations demonstrate can be consistent with observations. This suggests that MOND-inspired theories can reproduce weak lensing observations, but makes clear the price: the existence of a coherent large-scale fluctuation of a field(s) weakly tied to the baryonic matter, not completely dissimilar to a dark matter halo.Comment: 7 pages, 10 figure

Submicron Systems Architecture: Semiannual Technical Report

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Submicron Systems Architecture Project : Semiannual Technical Report

The Mosaic C is an experimental fine-grain multicomputer based on single-chip nodes. The Mosaic C chip includes 64KB of fast dynamic RAM, processor, packet interface, ROM for bootstrap and self-test, and a two-dimensional selftimed router. The chip architecture provides low-overhead and low-latency handling of message packets, and high memory and network bandwidth. Sixty-four Mosaic chips are packaged by tape-automated bonding (TAB) in an 8 x 8 array on circuit boards that can, in turn, be arrayed in two dimensions to build arbitrarily large machines. These 8 x 8 boards are now in prototype production under a subcontract with Hewlett-Packard. We are planning to construct a 16K-node Mosaic C system from 256 of these boards. The suite of Mosaic C hardware also includes host-interface boards and high-speed communication cables. The hardware developments and activities of the past eight months are described in section 2.1. The programming system that we are developing for the Mosaic C is based on the same message-passing, reactive-process, computational model that we have used with earlier multicomputers, but the model is implemented for the Mosaic in a way that supports finegrain concurrency. A process executes only in response to receiving a message, and may in execution send messages, create new processes, and modify its persistent variables before it either exits or becomes dormant in preparation for receiving another message. These computations are expressed in an object-oriented programming notation, a derivative of C++ called C+-. The computational model and the C+- programming notation are described in section 2.2. The Mosaic C runtime system, which is written in C+-, provides automatic process placement and highly distributed management of system resources. The Mosaic C runtime system is described in section 2.3

Microlensing toward crowded fields: Theory and applications to M31

We present a comprehensive treatment of the pixel-lensing theory and apply it to lensing experiments and their results toward M31. Using distribution functions for the distances, velocities, masses, and luminosities of stars, we derive lensing event rates as a function of the event observables. In contrast to the microlensing regime, in the pixel-lensing regime (crowded or unresolved sources) the observables are the maximum excess flux of the source above a background and the full width at half-maximum (FWHM) time of the event. To calculate lensing event distribution functions depending on these observables for the specific case of M31, we use data from the literature to construct a model of M31, reproducing consistently photometry, kinematics and stellar population. We predict the halo- and self-lensing event rates for bulge and disk stars in M31 and treat events with and without finite source signatures separately. We use the M31 photon noise profile and obtain the event rates as a function of position, field of view, and S/N threshold at maximum magnification. We calculate the expected rates for WeCAPP and for a potential Advanced Camera for Surveys (ACS) lensing campaign. The detection of two events with a peak signal-to-noise ratio larger than 10 and a timescale larger than 1 day in the WeCAPP 2000/2001 data is in good agreement with our theoretical calculations. We investigate the luminosity function of lensed stars for noise characteristics of WeCAPP and ACS. For the pixel-lensing regime, we derive the probability distribution for the lens masses in M31 as a function of the FWHM timescale, flux excess and color, including the errors of these observables.Comment: 45 pages, 27 figures LaTeX; corrected typos; published in the Astrophysical Journal Supplemen