Avaliação de modelos de estimativa de radiação solar global para o Estado de Goiás.

O objetivo deste estudo foi calibrar e avaliar o desempenho, de forma diária, de cinco modelos empíricos de estimativa de radiação solar. Foram utilizados dados de 10 municípios do estado de Goiás. A calibração e validação dos modelos BC, CD, DB e DCBB foram feitas utilizando a minimização do erro do quadrado médio. Já o modelo HG foi utilizado o método de iteração. O desempenho da calibração e validação dos modelos foi avaliado pelo coeficiente de determinação, erro do quadrado médio, erro relativo do quadrado médio, erro médio absoluto, eficiência do modelo pelo método de Nash-Sutcliff e pelos índices de concordância de Willmott e de confiança de Camargo. Os resultados permitiram observar que os modelos que mais subestimam ou superestimam os valores de radiação solar foram o modular DCBB e o HG, nessa ordem, com o erro médio absoluto variando em média de 2,60 a 3,02 M.J.m-2.dia-1 tanto na calibração quanto na validação. Conclui-se que os modelos CD e DB tiveram os melhores desempenhos em estimar os valores de radiação solar para o estado de Goiás

Sistema de suporte a decisões agronômicas via Web para o Estado de Goiás.

O objetivo desse trabalho é ilustrar o desenvolvimento de um SSD, via web, no qual disponibilizará a cada hora, as variáveis meteorológicas precipitação, temperatura máxima e mínima do ar, umidade relativa do ar, velocidade média e direção do vento para diferentes localidades de Goiás com a finalidade de dar suporte a decisões relacionadas as práticas de manejo agrícolas

The spatially resolved star formation history of CALIFA galaxies: Cosmic time scales

This paper presents the mass assembly time scales of nearby galaxies observed by CALIFA at the 3.5m telescope in Calar Alto. We apply the fossil record method of the stellar populations to the complete sample of the 3rd CALIFA data release, with a total of 661 galaxies, covering stellar masses from 10$^{8.4}$ to 10$^{12}$ M$_{\odot}$ and a wide range of Hubble types. We apply spectral synthesis techniques to the datacubes and process the results to produce the mass growth time scales and mass weighted ages, from which we obtain temporal and spatially resolved information in seven bins of galaxy morphology and six bins of stellar mass (M$_{\star}$) and stellar mass surface density ($\Sigma_{\star}$). We use three different tracers of the spatially resolved star formation history (mass assembly curves, ratio of half mass to half light radii, and mass-weighted age gradients) to test if galaxies grow inside-out, and its dependence with galaxy stellar mass, $\Sigma_{\star}$, and morphology. Our main results are as follows: (a) The innermost regions of galaxies assemble their mass at an earlier time than regions located in the outer parts; this happens at any given M$_{\star}$, $\Sigma_{\star}$, or Hubble type, including the lowest mass systems. (b) Galaxies present a significant diversity in their characteristic formation epochs for lower-mass systems. This diversity shows a strong dependence of the mass assembly time scales on $\Sigma_{\star}$ and Hubble type in the lower-mass range (10$^{8.4}$ to 10$^{10.4}$), but a very mild dependence in higher-mass bins. (c) All galaxies show negative $\langle$log age$\rangle_{M}$ gradients in the inner 1 HLR. The profile flattens with increasing values of $\Sigma_{\star}$. There is no significant dependence on M$_{\star}$ within a particular $\Sigma_{\star}$ bin, except for the lowest bin, where the gradients becomes steeper.Comment: 15 pages, 13 figures, 3 tables, accepted for publication in Astronomy & Astrophysics. *Abridged abstract

Retinal response of low myopes during orthokeratology treatment

The aim of this study was to evaluate the changes in retinal activity during orthokeratology (OK) treatment in 20 myopic eyes. Pattern electroretinography (PERG) and visual evoked potential (VEP) were assessed with the RETI-port/scan21 (Roland Consult, Wiesbaden, Germany). Measurements were taken at baseline (BL) and 1 night (1N), 15 nights (15N), 30 nights (30N), and 60 nights (60N) of OK lens wear. Repeated measures analysis of variance (ANOVA) and the Friedman test were used. Twenty eyes (23.20 ± 3.46 years, 70% female) with visual acuity ≤ 0.00 logMAR in post-treatment showed that despite a slight increase in retinal and cortical response amplitude, observed with both PERG and VEP, respectively, immediately after the initial treatment, these differences found were not statistically significant during the 60 days of OK treatment, despite a statistically significant increase in N95 response with PERG. This shows that retinal and cortical visual-related electrical activity is maintained or slightly increased during OK treatment.This research was supported by the Portuguese Foundation for Science and Technology (FCT) PTDC/FIS-OPT/0677/2014, the Strategic Funding UID/FIS/04650/2013 at Center of Physics, UMinho, and predoctoral grant SFRH/BD/136684/2018 to A.A.

Spatially resolved mass-to-light from the CALIFA survey. Mass-to-light ratio vs. color relations

We investigated the mass-to-light versus color relations (MLCRs) derived from the spatially resolved star formation history of a sample of 452 galaxies observed with integral field spectroscopy in the CALIFA survey. We derived the stellar mass ($M_\star$) and the stellar mass surface density from the combination of full spectral fitting (using different sets of stellar population models) with observed and synthetic colors in optical broad bands. This method allows obtaining the radial structure of the mass-to-light ratio ($M/L$) at several wavelengths and studying the spatially resolved MLCRs. Our sample covers a wide range of Hubble types from Sc to E, with stellar masses ranging from $M_\star \sim 10^{8.4}$ to $10^{12}$ M$_\odot$. The scatter in the MLCRs was studied as a function of morphology, stellar extinction, and emission line contribution to the colors. The effects of the initial mass function (IMF) and stellar population models in the MLCRs were also explored. Our main results are that (a) the $M/L$ ratio has a negative radial gradient that is steeper within the central 1 half-light-radius (HLR). It is steeper in Sb-Sbc than in early-type galaxies. (b) The MLCRs between $M/L$ and optical colors were derived with a scatter of $\sim$ 0.1 dex. Extinction and emission line contributions do not affect the scatter of these relations. Morphology does not produce a significant effect, except if the general relation is used for galaxies redder than $(u-i) > 4$ or bluer than $(u-i) < 0$. (c) The IMF has a large effect on MLCRs, as expected. The change from a Chabrier to a Salpeter IMF produces a median shift of $\sim$ \oimf\ dex when mass loss from stellar evolution is also taken into account. (d) These MLCRs are in agreement with previous results, in particular for relations with $g$ and $r$ bands and the $B$ and $V$ Johnson systems. FITS tables available at http://pycasso.iaa.es/MLComment: 13 pages, 10 figures, 12 tables, accepted for publication in Astronomy & Astrophysics. Abridged abstract. All tables are available in electronic format at http://pycasso.iaa.es/M