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Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths. It is the first mission dedicated to measuring the chemical composition and thermal structures of hundreds of transiting exoplanets, enabling planetary science far beyond the boundaries of the Solar System. The payload consists of an off-axis Cassegrain telescope (primary mirror 1100 mm x 730 mm ellipse) and two separate instruments (FGS and AIRS) covering simultaneously 0.5-7.8 micron spectral range. The satellite is best placed into an L2 orbit to maximise the thermal stability and the field of regard. The payload module is passively cooled via a series of V-Groove radiators; the detectors for the AIRS are the only items that require active cooling via an active Ne JT cooler. The Ariel payload is developed by a consortium of more than 50 institutes from 16 ESA countries, which include the UK, France, Italy, Belgium, Poland, Spain, Austria, Denmark, Ireland, Portugal, Czech Republic, Hungary, the Netherlands, Sweden, Norway, Estonia, and a NASA contribution., Comment: Ariel Definition Study Report, 147 pages. Reviewed by ESA Science Advisory Structure in November 2020. Original document available at: https://www.cosmos.esa.int/documents/1783156/3267291/Ariel_RedBook_Nov2020.pdf/

Orientador: Flavio Augusto Picchi Dissertação (mestrado) - Universidade Estadual de Campinas, Faculdade de Engenharia Civil, Arquitetura e Urbanismo Resumo: O subsetor de Edificações, da Construção Civil, é responsável por 3,3% do total de acidentes do trabalho registrados no país; números que após quatro anos apresentando quedas, mostram, em 2002, um aumento relativo de 14%, sobre os resultados de 2001, apontando para uma inconsistência, ou falta de medidas prevencionistas. Nesse trabalho, propõe-se um método visando tornar rotineira a identificação de perigos e avaliação e controle de riscos nos canteiros de obras de edificações. O método proposto consiste em planilhas direcionadas para a Identificação de Perigos e Avaliação e Controle dos Riscos, por atividade, norteadas pelas Diretrizes OHSAS 18002 e ILOOSH 2001, complementadas com Diretrizes da NR-18. Este método visa facilitar o pleno cumprimento, em micro e pequenas empresas construtoras, da NR-18, estabelecendo uma base para implantação futura de Sistema de Gestão em Saúde e Segurança no Trabalho. O método é descrito e avaliado através de estudo exploratório em obra. Espera-se como resultado imediato a redução de perigos e riscos, o que contribuirá para os demais resultados esperados, no sentido de prevenção dos acidentes graves e fatalidades na construção de edificações Abstract: Building construction is responsible for 3.3% of total registered occupational accidents in Brazil. This figure increased 14% in 2002, comparing to 2001, showing inconsistency, or lack of prevention. This research proposes a method for the identification of hazards and evaluation and control of risks in buildings job sites as a routine. The proposed method consists of spread sheets for the Identification of Hazards and Evaluation and Control of Risks, for construction activities, guided by OHSAS 18002 and ILO-OSH 2001, complemented by NR-18 Guidelines. This method aims to facilitate the fulfillment, in micro and small construction companies, of NR-18, establishing a basis for future implementation of Health and Safety Management System. The method is described and evaluated trough exploratory study in job site. Reduction of hazards and risks is an immediate expected result that will contribute for further expected results, towards prevention of major accidents and fatalities in building construction Mestrado Edificações Mestre em Engenharia Civil

Sinaliza a continuidade das principais ações desenvolvidas na proteção social básica e especial, mas destaca, em particular, o lançamento de um novo programa voltado para a primeira infância: Criança Feliz. Não obstante a complexidade do tema primeira infância, a estratégia está centrada na realização de visitas domiciliares a famílias com crianças na primeira infância em situação de vulnerabilidade social. Desde o seu lançamento, o Criança Feliz suscita incertezas nos principais atores envolvidos na Política de Assistência Social, não só pela sua forma de concepção e lançamento ser estranha à institucionalidade construída nesta política, mas também por sua eventual inadequação em relação aos objetivos protetivos consolidados da área na última década. Considerando a existência de outras ações na política direcionadas ao acompanhamento familiar (por exemplo, Proteção e Atendimento Integral à Família – Paif), incertezas se colocam sobre a novidade da estratégia e principalmente quanto à sua relação com outros serviços desenvolvidos no Suas. Por fim, é analisada a execução orçamentária do Ministério do Desenvolvimento Social (MDS), no período entre 2014 e 2016, sinalizando que a Política de Assistência Social sofreu perdas importantes, e estas poderão ser ainda maiores diante do novo teto de gastos estabelecido pela EC no 95/2016, como aponta o orçamento de 2017.

We present here the first release of the open-source python package ExoTETHyS (stable: https://zenodo.org/badge/latestdoi/169268509, development version: https://github.com/ucl-exoplanets/ExoTETHyS/), which aims to provide a stand-alone set of tools for modeling spectrophotometric observations of transiting exoplanets. In particular, we describe: (1) a new calculator of stellar limb-darkening coefficients that outperforms the existing software by one order of magnitude in terms of light-curve model accuracy, i.e., down to, The authors would like to thank Rene Gastaud and Daniel Dicken for useful discussions. G.M., M.M.-L., and P.-O.L. were supported by the LabEx P2IO, the French ANR contract 05-BLANNT09-573739 and the European Unions Horizon 2020 Research and Innovation Programme, under grant agreement No. 776403. G.M. also acknowledges the contribution from INAF through the "Progetto Premiale: A Way to Other Worlds" of the Italian Ministry of Education, University, and Research. A.C. acknowledges financial support from the Spanish MEC (AYA2015-71718-R and ESP2017-87676-C5-2-R), the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709).

Mostly multiband photometric transit observations have been used so far to retrieve broadband transmission spectra of transiting exoplanets in order to study their atmosphere. An alternative method has been proposed and has only been used once to recover transmission spectra using chromatic Rossiter-McLaughlin observations. Stellar activity has been shown to potentially imitate narrow and broadband features in the transmission spectra retrieved from multiband photometric observations; however, there has been no study regarding the influence of stellar activity on the retrieved transmission spectra through chromatic Rossiter-McLaughlin. In this study with the modified SOAP3.0 tool, we consider different types of stellar activity features (spots and plages), and we generated a large number of realistic chromatic Rossiter-McLaughlin curves for different types of planets and stars. We were then able to retrieve their transmission spectra to evaluate the impact of stellar activity on them. We find that chromatic Rossiter-McLaughlin observations are also not immune to stellar activity, which can mimic broadband features, such as Rayleigh scattering slope, in their retrieved transmission spectra. We also find that the influence is independent of the planet radius, orbital orientations, orbital period, and stellar rotation rate. However, more general simulations demonstrate that the probability of mimicking strong broadband features is lower than 25% and that can be mitigated by combining several Rossiter-McLaughlin observations obtained during several transits. © ESO 2020., M.O. acknowledges the support of the Deutsche Forschungs-gemeinschft (DFG) priority program SPP 1992 “Exploring the Diversity of Extrasolar Planets (RE 1664/17-1)”. S.B. and M.O. also acknowledge the support of the FCT/DAAD bilateral grant 2019 (DAAD ID: 57453096). M.O and N.S. were also supported by Fundação para a Ciência e a Tecnologia (FCT, Portugal) /MCTES through national funds by FEDER through COMPETE2020 by these grants: UID/FIS/04434/2019 & POCI-01-0145-FEDER-028953 and PTDC/FIS-AST/32113/2017 & PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-032113. We would like to thank the anonymous referee for insightful suggestions, which added significantly to the clarity of this paper.

This article and software are linked with research article DOI 10.3847/1538-3881/ab63dc, published in the The Astronomical Journal; International audience; ExoTETHyS is a Python2/3 package which aims to provide a stand-alone set of tools for modeling spectro-photometric observations of transiting exoplanets. The package is not a mere collection of pre-existing software, but contains algorithms with new features as well as enhancements of existing codes. The first release contains the following subpackages: 1. SAIL (Stellar Atmosphere Intensity Limb), i.e., a calculator of stellar limb-darkening coefficients that outperforms the existing software by one order of magnitude in terms of light-curve model accuracy, i.e., down to

We report the discovery of a detached double white dwarf binary with an orbital period of 20.6 minutes, PTF J053332.05+020911.6. The visible object in this binary, PTF J0533+0209B, is a 0.17 M, K.B.B. thanks the National Aeronautics and Space Administration and the Heising-Simons Foundation for supporting his research. J.F. acknowledges support from an Innovator grant from The Rose Hills Foundation and the Sloan Foundation through grant FG-2018-10515. The KPED team thanks the National Science Foundation and the National Optical Astronomical Observatory for making the Kitt Peak 2.1 m telescope available. The KPED team thanks the National Science Foundation, the National Optical Astronomical Observatory and the Murty family for support in the building and operation of KPED. In addition, they thank the CHIMERA project for use of the Electron Multiplying CCD (EMCCD). Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The research leading to these results has received funding from the European Research Council under the European Unions Horizon 2020 research and innovation program n.677706 (WD3D) This research benefited from interactions at the ZTF Theory Network Meeting that were funded by the Gordon and Betty Moore Foundation through grant GBMF5076 and support from the National Science Foundation through PHY-1748958.

We present 12,155 new differential photometric observations in the V filter made with the Undergraduate Research Studies in Astronomy and NF\Observatory WebScopes, as well as 33 radial velocities from spectroscopic observations of the detached, 4.04 day double-lined eclipsing binary star GX Gem. Absolute dimensions of the components are determined from these new, and also from previously published, data with high precision (less than 0.7% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 1.488 ? 0.011 solar masses and 2.327 ? 0.012 solar radii for the primary, and 1.467 ? 0.010 solar masses and 2.238 ? 0.012 solar radii for the secondary. The effective temperatures and interstellar reddening of the stars are accurately determined from the spectra, uvby?, and UBV photometry: 6195 ? 100 K for the primary, 6165 ? 100 K for the secondary, corresponding to spectral types of F7 and F7 V, and 0.068 mag for the color excess Eb ? y . Spectral line widths give rotational velocities that are synchronous with the mean orbital motion in a circular orbit. The components of GX Gem are relatively old main-sequence stars with an age of about 2.8 billion years according to models. Because the components are located right at the end of their main-sequence evolutionary paths, we can place good limits on the convective core overshooting parameter. The lowest value of ?ov consistent with the observations would appear to be approximately ?ov = 0.18. Two different theories of tidal synchronization and circularization agree that the components should be synchronously rotating, but disagree about whether or not the orbits should be circular.

This study seeks to determine the level of training that nurses working in the most important Spanish hospitals reached towards the year 1600 in the treatments applied to patients with STDs (sexually transmitted diseases), particularly syphilis. The nurses knew and already applied around 1600 a set of complex techniques to care for and heal the sick of syphilis and other STDs. All this demonstrates an increase in the demands of the training of Spanish nurses, who worked under ethical guidelines, and we could assume the beginnings of the professionalization of nursing in such an early age. In 16th century Spain, nurses began to raise their educational level to provide care that could respond to the new knowledge that medicine was discovering as a result of the general scientific development of the time, and that should be applied in the new hospitals that were erected in the main Spanish cities. El presente estudio tiene como objetivo principal conocer el nivel de preparación de los enfermeros que trabajaron en algunos de los más importantes hospitales españoles en torno al año 1600 en el tratamiento de las enfermedades de transmisión sexual, especialmente la sífilis. Para su tratamiento los enfermeros conocían y aplicaban ya en torno al año 1600 un conjunto de técnicas complejas y su trabajo se movía bajo unas directrices éticas. Ello podría ser indicador de los inicios de la profesionalización de la Enfermería en España, mucho antes de lo que se viene considerando en otros países, que se sitúa este proceso en el siglo XIX. Los enfermeros comenzaron ya en este período a elevar su nivel de formación para proporcionar unos cuidados que respondieran a los avances médicos del momento y se puedieran aplicar, al menos en los hospitales españoles erigidos en las grandes ciudades, como Sevilla y Madrid

The study of the variation of the curvature of non-symmetric composite laminates with temperature provides a measure of the magnitude of the thermal stresses and the mechanical behavior of the material with temperature. In the present work, an experimental method based on the pioneer use of a digital camera and image processing method is proposed to perform such measurements. Taking advantage of the method and by comparing experimental and CLT, extended-CLT and FEM simulation results, an evaluation of the residual stresses is described and an approach providing more precise determination of the residual thermal stresses in non-symmetric laminates is proposed.

We present 6907 differential photometric observations in the V filter, as well as 52 radial velocities from spectroscopic observations of the detached, eccentric 7.97 day double-lined eclipsing binary star EY Cep. Absolute dimensions of the components are determined with high precision (less than 1% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 1.523 ± 0.008 M⊙ and 1.463 ± 0.010 R⊙ for the primary and 1.498 ± 0.014 M⊙ and 1.468 ± 0.010 R⊙ for the secondary. The effective temperatures and interstellar reddening of the stars are accurately determined from the spectra, uvbyβ, and UBV photometry: 7090 ± 150 K for the primary and 6970 ± 150 K for the secondary, corresponding to spectral types of F0 and F0, and 0.036 mag for the color excess Eb-y. Spectral line widths give rotational velocities that are synchronous with the mean orbital motion in a highly eccentric orbit (e = 0.4429). The components of EY Cep are young main-sequence stars with an age of about 40 million years, according to models.

We present 3004 differential observations in the V bandpass measured by a robotic telescope, as well as 36 pairs of radial velocities from high-resolution spectroscopic observations, of the detached, eccentric, EA-type, 10.37 day period, double-lined eclipsing binary star RW Lac. Absolute dimensions of the components are determined with excellent precision (better than 0.7% in the masses and 0.5% in the radii) for the purpose of testing various aspects of theoretical modeling. We obtain 0.928 ± 0.006 M⊙ and 1.186 ± 0.004 R⊙ for the hotter, larger, more massive, and more luminous photometric primary (star A) and 0.870 ± 0.004 M⊙ and 0.964 ± 0.004 R⊙ for the cooler, smaller, less massive, and less luminous photometric secondary (star B). A faint, third component contributes 2.6% of the light in V but is not detected in our spectrograms. The effective temperatures and interstellar reddening of the stars are accurately determined from UBV and uvbyβ photometry and from analysis of the spectrograms: 5760 ± 100 K for the primary and 5560 ± 150 K for the secondary, corresponding to spectral types of G5 and G7, and 0.050 mag for interstellar reddening Eb-y. The orbits are slightly eccentric, and spectral line widths give observed rotational velocities that are not significantly different from synchronous for both components. The components of RW Lac are old, somewhat metal-deficient, low-mass, main-sequence stars with an age of about 11 Gyr, according to models.

a ICREA, Grup d’Autoecologia Humana, Area de Prehistoria, Unitat Asociada al CSIC, Universitat Rovira i Virgili. Placa Imperial Tarraco 1, 43005-Tarragona, Spain b Instituto de Astrofisica de Andalucia, CSIC. C/ Camino Bajo de Huetor, 24, 18008 Granada, Spain c University of California, Museum of Paleontology, Berkeley, CA 94720, U.S.A. d Departamento de Ecologia y Geologia (Area de Paleontologia), Facultad de Ciencias, Universidad de Malaga. Campus Universitario de Teatinos, 29071-Malaga, Spain e Centro ISCIII-UCM de Evolucion y Comportamiento Humanos. c/ Sinesio Delgado, 4. 28040-Madrid, Spain

We present 6450 differential observations in the V filter measured by a robotic telescope, as well as 28 pairs of radial velocities from high-resolution spectroscopic observations of the detached EA-type, 5.505 day period, double-lined eclipsing binary star V396 Cas. Absolute dimensions of the components are determined with good precision (better than 1% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 2.398 ± 0.022 M⊙ and 2.592 ± 0.013 R⊙ for the hotter, larger, more massive and more luminous photometric primary (star A), and 1.901 ± 0.016 M⊙ and 1.779 ± 0.010 R⊙ for the cooler, smaller, less massive and less luminous photometric secondary (star B). The effective temperatures and interstellar reddening of the stars are accurately determined from uvbyβ photometry: 9225 ± 150 K for the primary and 8550 ± 120 K for the secondary, corresponding to spectral types of A1 and A3, and 0.119 mag for Eb-y. The metallicity of the stars appears to be significantly less than solar. The stars are located at a distance of about 560 pc near the plane of the Galactic disk. The orbits of the stars are apparently circular, and spectral line widths give observed rotational velocities that are not synchronous with the orbital motion for both components. The components of V396 Cas are main-sequence stars with an age of about 420 Myr according to models.

We present 6151 differential observations in the V filter measured by a robotic telescope, as well as 29 pairs of radial velocities from high-resolution spectroscopic observations, of the detached, EA-type, 9.65 day period double-lined eclipsing binary star MU Cas. Absolute dimensions of the components are determined with good precision (better than 2% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 4.57 ? 0.09 M? and 3.67 ? 0.04 R? for the hotter, but smaller, less massive and less luminous photometric primary (star A), and 4.66 ? 0.10 M? and 4.19 ? 0.05 R? for the cooler, larger, more massive and more luminous photometric secondary (star B). The effective temperatures and interstellar reddening of the stars are accurately determined from uvby? photometry: 15,100 ? 500 K for the primary, 14,750 ? 500 K for the secondary?corresponding to spectral types of B5 and B5?and 0.356 mag for Eb-y. The stars are located at a distance of about 1.7 kpc near the plane of the Galactic disk. The orbits of the stars are eccentric, and spectral line widths give observed rotational velocities that are synchronous with the mean orbital motion for both components. The components of MU Cas are upper main-sequence stars with an age of about 65 Myr according to models.

We present 4179 differential observations in the V filter measured by a robotic telescope, as well as 25 pairs of radial velocities from high-resolution spectroscopic observations, of the detached, EB-type, 1.69 day period double-lined eclipsing binary star V885 Cyg. Absolute dimensions of the components are determined with high precision (better than 1.5% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 2.005 ± 0.029 M⊙ and 2.345 ± 0.012 R⊙ for the hotter, but smaller, less massive and less luminous photometric primary (star A), and 2.234 ± 0.026 M⊙ and 3.385 ± 0.026 R⊙ for the cooler, larger, more massive and more luminous photometric secondary (star B). The effective temperatures and interstellar reddening of the stars are accurately determined from uvbyβ photometry: 8375 ± 150 K for the primary, 8150 ± 150 K for the secondary—corresponding to spectral types of A3m and A4m—and 0.058 mag for Eb-y. The metallic-lined character of the stars is revealed by high-resolution spectroscopy and uvbyβ photometry. The orbits are circular, and spectral line widths give observed rotational velocities that are synchronous with the orbital motion for both components. The components of V885 Cyg are main-sequence stars with an age of about 500 Myr according to models. Our estimate of the age of this system would seem to favor the hydrodynamic damping formalism of Tassoul & Tassoul in this particular case, since both the components' spins are synchronous and the orbit is circular.

We present 5064 differential observations in the V filter measured by a robotic telescope, as well as 30 pairs of radial velocities from high-resolution spectroscopic observations, of the detached, EA-type, 8.46 day period double-lined eclipsing binary star V459 Cas. Absolute dimensions of the components are determined with good precision (better than 1.6% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 2.02 ± 0.03 M⊙ and 2.009 ± 0.013 R⊙ for the hotter, larger, more massive and more luminous photometric primary (star A), and 1.96 ± 0.03 M⊙ and 1.965 ± 0.013 R⊙ for the cooler, smaller, less massive and less luminous photometric secondary (star B). The effective temperatures and interstellar reddening of the stars are accurately determined from uvbyβ photometry: 9140 ± 300 K for the primary, 9100 ± 300 K for the secondary—corresponding to spectral types of A1—and 0.186 mag for Eb-y. The orbits are eccentric, and spectral line widths give observed rotational velocities that are much faster than synchronous for both components. The components of V459 Cas are main-sequence stars with an age of about 525 Myr according to models.

We have calculated theoretical isochrones for the photometric Delta a system to derive astrophysical parameters such as the age, reddening and distance modulus for open clusters. The Delta a system samples the flux depression at 520 nm which is highly efficient to detect chemically peculiar (CP) objects of the upper main sequence. The evolutionary status of CP stars is still a matter of debate and very important to test, for example, the dynamo and diffusion theories. In fact, the dynamo or fossil origin of the magnetic fields present in this kind of stars it still not clear. Using the stellar evolutionary models by Claret (1995), a grid of isochrones with different initial chemical compositions for the Delta a system was generated. The published data of 23 open clusters were used to fit these isochrones with astrophysical parameters (age, reddening and distance modulus) from the literature. As an additional test, isochrones with the same parameters for Johnson UBV data of these open clusters were also considered. The fits show a good agreement between the observations and the theoretical grid. We find that the accuracy of fitting isochrones to Delta a data without the knowledge of the cluster parameters is between 5 and 15%.

We present 5236 differential observations in the V filter measured by a robotic telescope, as well as radial velocities from spectroscopic observations, of the detached, eccentric 1.9 day double-lined eclipsing binary star BP Vul. Absolute dimensions of the components are determined with high precision (better than 1% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 1.737 ± 0.015 M⊙ and 1.852 ± 0.014 R⊙ for the primary, and 1.408 ± 0.009 M⊙ and 1.489 ± 0.014 R⊙ for the secondary. The effective temperatures and interstellar reddening of the stars are accurately determined from uvbyβ photometry: 7700 ± 150 K for the primary, 6800 ± 150 K for the secondary—corresponding to spectral types of A7m and F2m—and 0.022 mag for Eb-y. The metallic-lined character of the stars is revealed by high-resolution spectroscopy and uvbyβ photometry. Spectral line widths give rotational velocities that are synchronous with the orbital motion for the secondary component, but subsynchronous for the primary component, in a slightly eccentric orbit (e = 0.0345). Apsidal motion based on times of minimum light appears to be negative with a period of about 75 years based on recent observations of minima, but this result is not confirmed by the radial velocity measurements, and it is indeterminate when older photographic and visual data are included. The components of BP Vul are main-sequence stars with an age of about 1 Gyr according to models.

We present absolute photometric observations in uvby? and 5759 differential observations in the V filter (the most complete light curve ever obtained) measured by a robotic telescope, as well as radial velocities from spectroscopic observations of the detached, eccentric, 2.3 day, double-lined, eclipsing binary star WW Camelopardalis. Absolute dimensions of the components are determined with high precision (better than 1% in the masses and radii) for the purpose of testing various aspects of theoretical modeling. We obtain 1.920 ? 0.013 M? and 1.911 ? 0.016 R? for the primary, and 1.873 ? 0.018 M? and 1.808 ? 0.014 R? for the secondary. The effective temperatures and interstellar reddening of the stars are accurately determined from new uvby? photometry: 8350 ? 135 K for the primary and 8240 ? 135 K for the secondary, corresponding to a spectral type of A4m for both, and 0.294 mag for Eb-y. The metallic-lined character of the stars is revealed by high-resolution spectroscopy and uvby? photometry. Spectral line widths give rotational velocities that are synchronous with the orbital motion in a slightly eccentric orbit (e = 0.0098). The components of WW Cam are main-sequence stars with an age of about 490 Myr according to models.

We present photometric observations in B and V as well as spectroscopic observations of the 1.9 day¨ period, double-lined main-sequence eclipsing binary FS Mon. From the analysis of the light curves and radial velocity curves, we have determined the masses and radii of the components: 1.631 ^ 0.012 M _ and 2.051 ^ 0.012 for the primary component; 1.461 ^ 0.010 and 1.629 ^ 0.012 for the sec- R _ M _ R _ ondary component. The formal uncertainties are all less than 1%. Based on our light curves as well as on the combined-light photometry of the system, we estimate eUective temperatures of 6715 ^ 100 K for the primary and 6550 ^ 100 K for the secondary component, corresponding to spectral types of F2 and F4, respectively. Projected rotational velocities (v sin i) from the spectograms are measured as 52 ^ 2k m s~1 and 43 ^ 3k m s~1, respectively, from the spectrograms and are consistent with rotation that is synchronous with the orbital motion. Evolutionary tracks from current models are in good agreement with the observations for a system age of about 1.6 ) 109 yr with slightly nonsolar chemical composi- tion. We —nd the best match for models with a slightly lower helium abundance and a higher metal abundance than the Sun. An accurate metallicity determination for FS Mon is needed to constrain the models further.

We present photoelectric observations in B and V, as well as spectroscopic observations of the 7.3 day period double-lined eclipsing binary V364 Lacertae. From the analysis of the light curves and the radial velocity curves we have determined the absolute dimensions of the components with high precision (1%). The masses for the primary and secondary are MA = 2.333 ± 0.015 M⊙ and MB = 2.296 ± 0.025 M⊙, respectively, and the radii are RA = 3.307 ± 0.038 R⊙ and RB = 2.985 ± 0.035 R⊙. We derive also effective temperatures of T = 8250 ± 150 K and T = 8500 ± 150 K, and projected rotational velocities of vA sin i = 45 ± 1 km s-1 and vB sin i = 15 ± 1 km s-1. Evolutionary tracks from current stellar evolution models are in good agreement with the observations for a system age of log t = 8.792 (6.2 × 108 yr) and for solar metallicity. Hints of a lower metallicity from spectroscopy and photometry appear to be ruled out by these models, but a definitive comparison must await a more accurate spectroscopic abundance determination. Analysis of all available eclipse timings along with our radial velocities of this moderately eccentric system (e = 0.2873 ± 0.0014) has revealed a small but significant motion of the line of apsides of = 0.00258 ± 0.00033 deg cycle-1, corresponding to an apsidal period of U = 2810 ± 360 yr. The contribution from general relativity effects is significant (~17%). A comparison with predictions from interior structure models shows the real stars to be less concentrated in mass than expected. Our measurements of the projected rotational velocities indicate that the primary star is essentially pseudosynchronized (synchronized at periastron), while the secondary is spinning 3 times more slowly and is not yet synchronized. Both the rotational status of the stars and the nonzero eccentricity of the orbit are consistent with the predictions from tidal theory, specifically for the radiative damping mechanism.

Faunistic analyses were made to evaluate the effect of cerrado (Brazilian savannah) native vegetation on Lepidoptera associated with Eucalyptus cloeziana plantations. The insects were collected with light traps in five sampling sites for each system of Eucalyptus cultivation (i.e., with and without strips of cerrado) every 15 days during 6 months. A total of 5511 individuals of 459 species and 16,021 individuals of 300 species were collected in areas with and without strips of cerrado. In areas with the first system, a higher number of species was collected within the strips of cerrado vegetation, the four most frequent species accounting for ±20% of the individuals collected; nine species were constant (present in 50% to 100% of the samples) among the 23 most important ones, four of these were accessory (present in 25 to 50% of the samples) and ten accidental (present in 0 to 25% of the samples). The diversity was higher in the intersection of the habitats and smaller within the eucalypt plantation. In the system without strips of native vegetation, a higher number of species was collected in the native vegetation; the intersection between native vegetation and eucalypt plantation was similar in terms of species composition with a smaller number of species being collected within the eucalypt plantation. The three most frequent species in this habitat accounted for ±31% of the individuals collected; nine species were constant, nine were accessory and eight were accidental. The diversity indexes were higher in the plantation with cerrado strips than in the plantation without cerrado strips. These results suggest that the establishment of strips of native vegetation within Eucalyptus plantation may be a beneficial tactic in the management of defoliator Lepidoptera pests in Eucalyptus forests.

We determine the absolute dimensions of the eclipsing binary V578 Mon, a detached system of two early B-type stars (B0V + B1V, P$=$2.40848 d) in the star-forming region NGC 2244 of the Rosette Nebula. From the light curve analysis of 40 yr of photometry and the analysis of HERMES spectra, we find radii of $5.41\pm0.04$ Rsun and $4.29\pm 0.05$ Rsun, and temperatures of $ 30000\pm 500$~K and $ 25750\pm 435$ K respectively. We find that our disentangled component spectra for V578 Mon agree well previous spectral disentangling from the literature. We also reconfirm the previous spectroscopic orbit of V578 Mon finding that masses of $ 14.54\pm 0.08$ Msun and $ 10.29\pm 0.06$ Msun are fully compatible with the new analysis. We compare the absolute dimensions to the rotating models of the Geneva and Utrecht groups and the models of Granada group. We find all three sets of models marginally reproduce the absolute dimensions of both stars with a common age within uncertainty for gravity-effective temperature isochrones. However - there are some apparent age discrepancies for the corresponding mass-radius isochrones. Models with larger convective overshoot $>0.35$ worked best. Combined with our previously determined apsidal motion of $0.07089^{+0.00021}_{-0.00013}$ deg cycle$^{-1}$, we compute the internal structure constants (tidal Love number) for the newtonian and general relativistic contribution to the apsidal motion, $\log{k_2}=-1.975\pm0.017$ and $\log{k_2}=-3.412\pm0.018$ respectively. We find the relativistic contribution to the apsidal motion of be small $, accepted for publication in AJ 05/02/2014

We report differential photometric observations and radial-velocity measurements of the detached, 1.69-day period, double-lined eclipsing binary AQ Ser. Accurate masses and radii for the components are determined to better than 1.8% and 1.1%, respectively, and are M1 = 1.417 +/- 0.021 MSun, M2 = 1.346 +/- 0.024 MSun, R1 = 2.451 +/- 0.027 RSun, and R2 = 2.281 +/- 0.014 RSun. The temperatures are 6340 +/- 100 K (spectral type F6) and 6430 +/- 100 K (F5), respectively. Both stars are considerably evolved, such that predictions from stellar evolution theory are particularly sensitive to the degree of extra mixing above the convective core (overshoot). The component masses are different enough to exclude a location in the H-R diagram past the point of central hydrogen exhaustion, which implies the need for extra mixing. Moreover, we find that current main-sequence models are unable to match the observed properties at a single age even when allowing the unknown metallicity, mixing length parameter, and convective overshooting parameter to vary freely and independently for the two components. The age of the more massive star appears systematically younger. AQ Ser and other similarly evolved eclipsing binaries showing the same discrepancy highlight an outstanding and largely overlooked problem with the description of overshooting in current stellar theory., Comment: 12 pages in emulateapj format, including all tables and figures. To appear in The Astronomical Journal (accepted)

Context. Convective core overshooting extends the main-sequence lifetime of a star. Evolutionary tracks computed with overshooting are very different from those that use the classical Schwarzschild criterion, which leads to rather different predictions for the stellar properties. Attempts over the last two decades to calibrate the degree of overshooting with stellar mass using detached double-lined eclipsing binaries have been largely inconclusive, mainly because of a lack of suitable observational data. Aims. We revisit the question of a possible mass dependence of overshooting with a more complete sample of binaries, and examine any additional relation there might be with evolutionary state or metal abundance Z. Methods. We used a carefully selected sample of 33 double-lined eclipsing binaries strategically positioned in the H-R diagram with accurate absolute dimensions and component masses ranging from 1.2 to 4.4 M. We compared their measured properties with stellar evolution calculations to infer semi-empirical values of the overshooting parameter α for each star. Our models use the common prescription for the overshoot distance d = αH, where H is the pressure scale height at the edge of the convective core as given by the Schwarzschild criterion, and α is a free parameter. Results. We find a relation between α and mass, which is defined much more clearly than in previous work, and indicates a significant rise up to about 2 M followed by little or no change beyond this mass. No appreciable dependence is seen with evolutionary state at a given mass, or with metallicity at a given mass although the stars in our sample span a range of a factor of ten in [Fe/H], from -1.01 to + 0.01., The Spanish MEC (AYA2015-71718-R) is gratefully acknowledged for its support during the development of this work. G.T. acknowledges partial support from the NSF through grant AST-1509375

CARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Echelle Spectrographs) is a next-generation instrument for the 3.5m telescope at the Calar Alto Observatory, built by a consortium of eleven Spanish and German institutions. The CARMENES instrument consists of two separate echelle spectrographs covering the wavelength range from 0.55 μm to 1.7 μm at a spectral resolution of R = 82, 000, fed by fibers from the Cassegrain focus of the telescope. Both spectrographs are housed in temperature-stabilized vacuum tanks, to enable a long-term 1 m/s radial velocity precision employing a simultaneous calibration with Th-Ne and U-Ne emission line lamps. CARMENES has been optimized for a search for terrestrial planets in the habitable zones (HZs) of low-mass stars, which may well provide our first chance to study environments capable of supporting the development of life outside the Solar System. With its unique combination of optical and near-infrared ´echelle spectrographs, CARMENES will provide better sensitivity for the detection of low-mass planets than any comparable instrument, and a powerful tool for discriminating between genuine planet detections and false positives caused by stellar activity. The CARMENES survey will target 300 M dwarfs in the 2014 to 2018 time frame.

The NanosatC-BR – Space Weather Mission consists of a INPE-UFSM Capacity Building Integrated Program on space science, engineering and computing sciences for the development of space technologies through a CubeSat satellite, the first Brazilian Scientific Nanosatellite. The Capacity Building Program was conceived at the Southern Regional Space Research Center, (CRS), from the Brazilian National Institute for Space Research – INPE/MCT, by Dr. Nelson Jorge Schuch, who is the Mission’s General Manager and PI, having technical collaboration and management from Dr. Eng. Otavio Santos Cupertino Durao, the Mission’s local Manager at INPE’s Headquarter (HQ), in Sao Jose dos Campos, Sao Paulo, with the involvement of undergraduate students from the Federal University of Santa Maria – UFSM. The NanosatC-BR was specified to monitor in real time the Geospace, the particle precipitation and the disturbances observed at Earth’s magnetosphere over the Brazilian Territory, for the determination of their effects on regions such as the South Atlantic Magnetic Anomaly (SAMA) and the Brazilian sector of the Ionosphere Equatorial Electrojet.

We observed the Saturn-mass and Jupiter-sized exoplanet HAT-P-19b to refine its transit parameters and ephemeris as well as to shed first light on its transmission spectrum. We monitored the host star over one year to quantify its flux variability and to correct the transmission spectrum for a slope caused by starspots. A transit of HAT-P-19b was observed spectroscopically with OSIRIS at the Gran Telescopio Canarias in January 2012. The spectra of the target and the comparison star covered the wavelength range from 5600 to 7600 AA. One high-precision differential light curve was created by integrating the entire spectral flux. This white-light curve was used to derive absolute transit parameters. Furthermore, a set of light curves over wavelength was formed by a flux integration in 41 wavelength channels of 50 AA width. We analyzed these spectral light curves for chromatic variations of transit depth. The transit fit of the combined white-light curve yields a refined value of the planet-to-star radius ratio of 0.1390 pm 0.0012 and an inclination of 88.89 pm 0.32 degrees. After a re-analysis of published data, we refine the orbital period to 4.0087844 pm 0.0000015 days. We obtain a flat transmission spectrum without significant additional absorption at any wavelength or any slope. However, our accuracy is not sufficient to significantly rule out the presence of a pressure-broadened sodium feature. Our photometric monitoring campaign allowed for an estimate of the stellar rotation period of 35.5 pm 2.5 days and an improved age estimate of 5.5^+1.8_-1.3 Gyr by gyrochronology., 14 pages, 9 figures, Accepted for publication in A&A

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We continue our survey for magnetic chemically peculiar (CP2) stars in galactic open clusters to shed more light on their origin and evolution. To study the group of CP2 stars, it is essential to find these objects in different galactic environments and at a wide range of evolutionary stages. The knowledge of open clusters ages and metallicities can help to find a correlation of these parameters with the (non-)presence of peculiarities which has to be taken into account in stellar evolution models. The intermediate band Delta a photometric system samples the depth of the 5200A flux depression by comparing the flux at the center with the adjacent regions with bandwidths of 110A to 230A. It is capable to detect magnetic CP2 and CP4 stars with high efficiency, but also the groups of (metal-weak) lambda Bootis, as well as classical Be/shell stars can be successfully investigated. In addition, it allows to determine the age, reddening and distance modulus with an appropriate accuracy by fitting isochrones. From the 1677 observed members of the eight open clusters, twenty five CP2 and one Ae stars were identified. Further nineteen deviating stars are designated as questionable due to several reasons. The estimated age, reddening and distance for the programme clusters were compared with published vales of the literature and discussed in this context. The current paper shows that CP2 stars are present continuously in very young (7Myr) to intermediate age (500Myr) open clusters at distances larger than 2kpc from the Sun., Comment: 10 pages, 3 figures, A&A accepted

By pursuing the goal to find new variables in the COROT field-of-view we characterised a sample of stars located in the lower part of the instability strip. Our sample is composed of stars belonging to the disk population in the solar neighbourhood. We found that 23% of the stars display multiperiodic light variability up to few mmag of amplitude. uvbyBeta photometry fixed most of the variables in the middle of the instability strip and high-resolution spectroscopy established that they have vsin i>100 km/s. The comparison with delta Sct stars in the whole Galaxy shows slightly different features, i.e., most delta Sct stars have a 0.05-mag redder (b-y)_0 index and lower vsin i values. Additional investigation in the open cluster NGC 6633 confirms the same incidence of variability, i.e., around 20%. The wide variety of pulsational behaviours of delta Sct stars (including unusual objects such as a variable beyond the blue edge or a rapidly rotating high-amplitude pulsator) makes them very powerful asteroseismic tools to be used by COROT. Being quite common among bright stars, delta Sct stars are suitable targets for optical observations from space., 9 pages, 9 figures Accepted for publication in Astronomy & Astrophysics, Main Journal

We review briefly some basic aspects of the structure and evolution of a star distorted by tides and rotation. Proximity effects like, for example gravity-darkening, are discussed using the properties of stellar internal structure. On the other hand, the differential equations of the dynamics of close binary systems are discussed with particular attention to apsidal motion. The tidal evolution equations for late and earlytype stars are also included and theoretical predictions are compared, when possible, with observations. Concerning stellar atmospheres, limb-darkening laws are revised using recent models. Furthermore, the influence of an external radiation field on the distribution of the intensities and on the irradiated spectrum is also investigated.

We have redetermined the absolute dimensions of the mid B-type eclipsing binary U Oph from new light and radial-velocity curves, accounting for both the apsidal motion and the light-time orbit around the third star. The stars in U Oph have masses of 5.27 and 4.74 M⊙(±1.5%) and are located in the middle of the main-sequence band for an an age of ∼50 Myr. U Oph and three other systems (V760 Sco, MU, Cas and DI Her) all have components within 10% of 5M⊙ and ages below 100 Myr; we find significant heavy-element abundance differences between these young nearby stars.

O experimento teve como objetivo avaliar a tolerância de mudas de pinhao-manso a diferentes herbicidas, com a finalidade de se conhecer principios ativos passiveis de serem recomendados quando do cultivo a campo. Em condicoes de estufa, produziram-se mudas de pinhao-manso, conduzidas ate os 60 dias, quando receberam, conforme o tratamento, aplicacao pos-emergente de herbicida. Conduzido inteiramente ao acaso e repetido cinco vezes, os tratamentos foram: Controle (ausencia de aplicacao em pos-emergencia de qualquer herbicida); Chlorimuron-ethyl, 10 g i.a.ha -1 (40 g pc ha -1 ); Trifloxusulfuron-sodium, 7,5 g i.a.ha -1 (10 g pc ha -1 ); Lactofen, 120 g i.a.ha -1 (500 mL pc ha -1 ); Carfentrazone-ethyl, 10 g i.a.ha -1 (25 mL pc ha -1 ); Mesotrione, 144 g i.a.ha -1 (300 mL pc ha -1 ); Bentazon, de 0,72 kg i.a.ha -1 (1,2 L pc ha -1 ); Flazasulfuron, de 50 g i.a.ha -1 (200 g pc ha -1 ); Clethodim+fenoxaprop-p-ethyl, de 50 + 50 g i.a.ha -1 (1,0 L pc ha -1 ); Haloxyfop-methyl, de 60 g i.a.ha -1 (500 mL pc ha -1 ). Avaliou-se a fitotoxidez causada pela aplicacao do herbicida e peso de materia seca de parte aerea. Conclui-se, preliminarmente, que a cultura do pinhao-manso nao e tolerante a aplicacao em pos-emergencia dos herbicidas flazasulfuron e mesotrione, apresentando elevados niveis de fitotoxidez a aplicacao em pos-emergencia dos herbicidas carfentrazone-ethyl e lactofen, e tolerante a aplicacao do herbicida haloxyfop-methyl.

CF Tau is now known to be an eclipsing triple star with relatively deep total and annular eclipses. New light and radial velocity curves as well as new times of minima were obtained and used for further modeling of the system. Very accurate (better than 0.9%) masses and radii of the eclipsing pair are determined from analysis of the two new light curves, the radial velocity curve, and the times of minimum light. The mass and luminosity of the distant third component is accurately determined as well. Theoretical models of the detached, evolved eclipsing pair match the observed absolute properties of the stars at an age of about 4.3 Gy and [Fe/H] = -0.14.

V335 Ser is now known to be an eccentric double-lined A1+A3 binary star with fairly deep (0.5 mag) partial eclipses. Previous studies of the system are improved with 7456 differential photometric observations from the URSA WebScope and 5666 from the NFO WebScope, and 67 high-resolution spectroscopic observations from the Tennessee State University 2 m automatic spectroscopic telescope. From dates of minima, the apsidal period is about 880 years. Accurate (better than 2%) masses and radii are determined from analysis of the two new light curves and the radial velocity curve. Theoretical models match the absolute properties of the stars at an age of about 380 Myr, though the age agreement for the two components is poor. Tidal theory correctly confirms that the orbit should still be eccentric, but we find that standard tidal theory is unable to match the observed asynchronous rotation rates of the components' surface layers.

BF?Dra is now known to be an eccentric double-lined F6+F6 binary star with relatively deep (0.7?mag) partial eclipses. Previous studies of the system are improved with 7494 differential photometric observations from the URSA WebScope and 9700 from the NFO WebScope, 106 high-resolution spectroscopic observations from the Tennessee State University 2?m automatic spectroscopic telescope and the 1?m coud?-feed spectrometer at Kitt Peak National Observatory, and 31 accurate radial velocities from the CfA. Very accurate (better than 0.6%) masses and radii are determined from analysis of the two new light curves and four radial velocity curves. Theoretical models match the absolute properties of the stars at an age of about 2.72?Gyr and [Fe/H] = ?0.17, and tidal theory correctly confirms that the orbit should still be eccentric. Our observations of BF?Dra constrain the convective core overshooting parameter to be larger than about 0.13 Hp . We find, however, that standard tidal theory is unable to match the observed slow rotation rates of the components' surface layers.

Recent studies have shown that stellar chromospheric activity, and its effect on convective energy transport in the envelope, is most likely the cause of significant radius and temperature discrepancies between theoretical evolution models and observations. We aim to determine absolute dimensions and abundances for the solar-type detached eclipsing binary EF Aqr, and to perform a detailed comparison with results from recent stellar evolutionary models. uvby-beta standard photometry was obtained with the Stromgren Automatic Telescope. The broadening function formalism was applied on spectra observed with HERMES at the Mercator telescope in La Palma, to obtain radial velocity curves. Masses and radii with a precision of 0.6% and 1.0% respectively have been established for both components of EF Aqr. The active 0.956 M_sol secondary shows star spots and strong Ca II H and K emission lines. The 1.224 M_sol primary shows signs of activity as well, but at a lower level. An [Fe/H] abundance of 0.00+-0.10 is derived with similar abundances for Si, Ca, Sc, Ti, V, Cr, Co, and Ni. Solar calibrated evolutionary models such as Yonsei-Yale, Victoria-Regina and BaSTI isochrones and evolutionary tracks are unable to reproduce EF Aqr, especially for the secondary, which is 9% larger and 400 K cooler than predicted. Models adopting significantly lower mixing length parameters l/H_p remove these discrepancies, as seen in other solar type binaries. For the observed metallicity, Granada models with a mixing length of l/H_p=1.30 (primary) and 1.05 (secondary) reproduce both components at a common age of 1.5+-0.6 Gyr. Observations of EF Aqr suggests that magnetic activity, and its effect on envelope convection, is likely to be the cause of discrepancies in both radius and temperature, which can be removed by adjusting the mixing length parameter of the models downwards., 11 pages, 8 figures, accepted for publication by A&A

CONTEXT: Accurate physical properties of eclipsing stars provide important constraints on models of stellar structure and evolution, especially when combined with spectroscopic information on their chemical composition. Empirical calibrations of the data also lead to accurate mass and radius estimates for exoplanet host stars. Finally, accurate data for unusual stellar subtypes, such as Am stars, also help to unravel the cause(s) of their peculiarities. AIMS: We aim to determine the masses, radii, effective temperatures, detailed chemical composition and rotational speeds for the Am-type eclipsing binaries SW CMa (A4-5m) and HW CMa (A6m) and compare them with similar normal stars. METHODS: Accurate radial velocities from the Digital Speedometers of the Harvard-Smithsonian Center for Astrophysics were combined with previously published uvby photometry to determine precise physical parameters for the four stars. A detailed abundance analysis was performed from high-resolution spectra obtained with the Nordic Optical Telescope (La Palma). RESULTS: We find the masses of the (relatively evolved) stars in SW CMa to be 2.10 and 2.24 solar masses, with radii of 2.50 and 3.01 solar radii, while the (essentially zero-age) stars in HW CMa have masses of 1.72 and 1.78 solar masses, radii of 1.64 and 1.66 solar radii -- all with errors well below 2%. Detailed atmospheric abundances for one or both components were determined for 14 elements in SW CMa ([Fe/H] = +0.49/+0.61 dex) and 16 in HW CMa ([Fe/H] = +0.33/+0.32 dex); both abundance patterns are characteristic of metallic-line stars. Both systems are well fit by current stellar evolution models for assumed bulk abundances of [Fe/H] = +0.05 and +0.23, respectively ([alpha/Fe] = 0.0), and ages of about 700 Myr and 160 Myr., 26 pages including figures, tables, and appendices. To appear in Astronomy & Astrophysics

WOS: 000290518500022, Accurate absolute properties are determined for the first time for the 3.15 day period eccentric eclipsing binary star FT Ori based on new absolute photometry, five differential light curves, and a radial velocity curve. The stars appear to be normal for their spectral types, A0 + A2. The orbit is highly eccentric (e = 0.409) and shows apsidal motion with a period of 536 years. The absolute properties and the degree of central mass concentration of the stars are consistent with current theoretical models at an age of 190 Myr.