Comparação de duas soluções extratoras na resolução de cinco sistemas enzimáticos em folhas jovens de cupuaçuzeiro (Theobroma grandiflorum Schum.).

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Protocolo de eletroforese de isoenzimas de cupuaçu em gel de poliacrilamida.

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Caracterização de acessos de pimenta-do-reino com base em sistemas enzimáticos.

Setenta e oito acessos de pimenta-do-reino, incluindo algumas espécies silvestres foram submetidos à análise eletroforética de isoenzimas em gel de poliacrilamida, visando distinguir diferenças fenotípicas que auxiliem na discriminação e seleção dos acessos. Foram utilizados os sistemas enzimáticos SKDH, GOT, ACP, ACO, PGI, FUM, 6PGDH e G6PDH. O polimorfismo de isoenzimas foi avaliado pelo número de alozimas com diferentes mobilidades por sistema enzimático, pelas freqüências de alozimas dentro de cada sistema enzimático em relação ao total de bandas do sistema e pela análise da similaridade genética, com base na ausência e presença de bandas. Todos os sistemas enzimáticos utilizados tiveram boa resolução e definição de bandas, com ênfase para SKDH, 6PGDH, PGI e ACP. Em sua totalidade, os sistemas apresentaram polimorfismo capaz de caracterizar e identificar acessos ou grupos de pequeno número de acessos, sendo que o sistema GOT foi o que apresentou maior variabilidade de alozimas e de perfis; e o que apresentou menor variabilidade foi o sistema FUM, com três alozimas e quatro perfis. Cinqüenta e sete por cento das alozimas podem ser usadas para caracterizar e identificar clones ou grupos de clones. Cerca de 64% dos acessos analisados podem ser identificados por um a seis fenótipos individuais de sistemas enzimáticos. A análise da similaridade indicou os grupos G1, G2 e G3 como os mais divergentes da coleção, os quais são indicados para cruzamentos intraespecíficos e interespecíficos visando a obtenção de clones superiores.Título em inglês: Characterization of black pepper accessions using isozymes. Publicado também on-line

Kinetic energy of solid neon by Monte Carlo with improved Trotter- and finite-size extrapolation

The kinetic energy of solid neon is calculated by a path-integral Monte Carlo approach with a refined Trotter- and finite-size extrapolation. These accurate data present significant quantum effects up to temperature T=20 K. They confirm previous simulations and are consistent with recent experiments.Comment: Text and figures revised for minor corrections (4 pages, 3 figures included by psfig

On the progenitor system of V392 Persei

A discussion regarding the progenitor system of the nova and dwarf nova system V392 Persei using archival data from 2MASS and WISE. We find that the system is unlikely to contain a luminous red giant donor (i.e. a symbiotic system), but cannot exclude the presence of a lower luminosity red giant or a sub-giant donor. The similarity of the SED of the quiescent V392 Per to that of GK Persei is noted

Definição de protocolos de eletroforese para análise de isoenzimas em pimenta-do-reino (piper nigrum L.).

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Understanding Society Innovation Panel Wave 8: results from methodological experiments

This paper presents some preliminary findings from Wave 8 of the Innovation Panel (IP8) of Understanding Society: The UK Household Longitudinal Study. Understanding Society is a major panel survey in the UK. May 2015, the eighth wave of the Innovation Panel went into the field. IP8 used a mixed-mode design, using on-line interviews and face-to-face interviews. This paper describes the design of IP8, the experiments carried and the preliminary findings from early analysis of the data

Understanding Society Innovation Panel Wave 9: Results from Methodological Experiments. Understanding Society Working Paper Series

This paper presents some preliminary findings from Wave 9 of the Innovation Panel (IP9) of Understanding Society: The UK Household Longitudinal Study. Understanding Society is a major panel survey in the UK. IP9 included experiments on the use mixed mode data collection, the value of respondent incentives, targeted timing of email invitations, measurement of household finances, subjective expectations about returns to schooling, people’s assessment of what constitutes “successful ageing”, format of response options, use of multiple measurements to improve measurement of attitudes, and measurement of sensitive topics. This paper describes the design of IP9, the experiments carried and the preliminary findings from early analysis of the data

VIRAC: The VVV Infrared Astrometric Catalogue

© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.We present VIRAC version 1, a near-infrared proper motion and parallax catalogue of the VISTA Variables in the Via Lactea (VVV) survey for 312 587 642 unique sources averaged across all overlapping pawprint and tile images covering 560 deg 2 of the bulge of the MilkyWay and southern disc. The catalogue includes 119 million high-quality proper motion measurements, of which 47 million have statistical uncertainties below 1 mas yr -1. In the 11 < K s < 14 magnitude range, the high-quality motions have a median uncertainty of 0.67 mas yr -1. The catalogue also includes 6935 sources with quality-controlled 5s parallaxes with a median uncertainty of 1.1 mas. The parallaxes show reasonable agreement with the Tycho- Gaia Astrometric Solution, though caution is advised for data with modest significance. The SQL data base housing the data is made available via the web. We give example applications for studies of Galactic structure, nearby objects (low-mass stars and brown dwarfs, subdwarfs, white dwarfs) and kinematic distance measurements of young stellar objects. Nearby objects discovered include LTT 7251 B, an L7 benchmark companion to a G dwarf with over 20 published elemental abundances, a bright L subdwarf, VVV 1256-6202, with extremely blue colours and nine new members of the 25 pc sample. We also demonstrate why this catalogue remains useful in the era of Gaia. Future versions will be based on profile fitting photometry, use the Gaia absolute reference frame and incorporate the longer time baseline of the VVV extended survey.Peer reviewedFinal Published versio

Gaia Early Data Release 3: The astrometric solution

[Context] Gaia Early Data Release 3 (Gaia EDR3) contains results for 1.812 billion sources in the magnitude range G = 3-21 based on observations collected by the European Space Agency Gaia satellite during the first 34 months of its operational phase. [Aims] We describe the input data, the models, and the processing used for the astrometric content of Gaia EDR3, as well as the validation of these results performed within the astrometry task. [Methods] The processing broadly followed the same procedures as for Gaia DR2, but with significant improvements to the modelling of observations. For the first time in the Gaia data processing, colour-dependent calibrations of the line- and point-spread functions have been used for sources with well-determined colours from DR2. In the astrometric processing these sources obtained five-parameter solutions, whereas other sources were processed using a special calibration that allowed a pseudocolour to be estimated as the sixth astrometric parameter. Compared with DR2, the astrometric calibration models have been extended, and the spin-related distortion model includes a self-consistent determination of basic-angle variations, improving the global parallax zero point. [Results] Gaia EDR3 gives full astrometric data (positions at epoch J2016.0, parallaxes, and proper motions) for 1.468 billion sources (585 millionwith five-parameter solutions, 882 million with six parameters), and mean positions at J2016.0 for an additional 344 million.Solutions with five parameters are generally more accurate than six-parameter solutions, and are available for 93% of the sources brighter than the 17th magnitude. The median uncertainty in parallax and annual proper motion is 0.02-0.03 mas at magnitude G = 9-14, and around 0.5 mas at G = 20. Extensive characterisation of the statistical properties of the solutions is provided, including the estimated angular power spectrum of parallax bias from the quasars.This work was financially supported by the European Space Agency (ESA) in the framework of the Gaia project; the German Aerospace Agency (Deutsches Zentrum für Luft- und Raumfahrt e.V., DLR) through grants 50QG0501, 50QG0601, 50QG0901, 50QG1401 and 50QG1402; the Spanish Ministry of Economy (MINECO/FEDER, UE) through grants ESP2016-80079-C2-1-R, RTI2018-095076-B-C21 and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia “María de Maeztu”) through grants MDM-2014-0369 and CEX2019-000918-M; the Swedish National Space Agency (SNSA/Rymdstyrelsen); and the United Kingdom Particle Physics and Astronomy Research Council (PPARC), the United Kingdom Science and Technology Facilities Council (STFC), and the United Kingdom Space Agency (UKSA) through the following grants to the University of Bristol, the University of Cambridge, the University of Edinburgh, the University of Leicester, the Mullard Space Sciences Laboratory of University College London, and the United Kingdom Rutherford Appleton Laboratory (RAL): PP/D006511/1, PP/D006546/1, PP/D006570/1, ST/I000852/1, ST/J005045/1, ST/K00056X/1, ST/K000209/1, ST/K000756/1, ST/L006561/1, ST/N000595/1, ST/N000641/1, ST/N000978/1, ST/N001117/1, ST/S000089/1, ST/S000976/1, ST/S001123/1, ST/S001948/1, ST/S002103/1, and ST/V000969/1