A global analysis of Spitzer and new HARPS data confirms the loneliness and metal-richness of GJ 436 b

Context. GJ 436b is one of the few transiting warm Neptunes for which a detailed characterisation of the atmosphere is possible, whereas its non-negligible orbital eccentricity calls for further investigation. Independent analyses of several individual datasets obtained with Spitzer have led to contradicting results attributed to the different techniques used to treat the instrumental effects. Aims. We aim at investigating these previous controversial results and developing our knowledge of the system based on the full Spitzer photometry dataset combined with new Doppler measurements obtained with the HARPS spectrograph. We also want to search for additional planets. Methods. We optimise aperture photometry techniques and the photometric deconvolution algorithm DECPHOT to improve the data reduction of the Spitzer photometry spanning wavelengths from 3-24 {\mu}m. Adding the high precision HARPS radial velocity data, we undertake a Bayesian global analysis of the system considering both instrumental and stellar effects on the flux variation. Results. We present a refined radius estimate of RP=4.10 +/- 0.16 R_Earth, mass MP=25.4 +/- 2.1 M_Earth and eccentricity e= 0.162 +/- 0.004 for GJ 436b. Our measured transit depths remain constant in time and wavelength, in disagreement with the results of previous studies. In addition, we find that the post-occultation flare-like structure at 3.6 {\mu}m that led to divergent results on the occultation depth measurement is spurious. We obtain occultation depths at 3.6, 5.8, and 8.0 {\mu}m that are shallower than in previous works, in particular at 3.6 {\mu}m. However, these depths still appear consistent with a metal-rich atmosphere depleted in methane and enhanced in CO/CO2, although perhaps less than previously thought. We find no evidence for a potential planetary companion, stellar activity, nor for a stellar spin-orbit misalignment. [ABRIDGED]Comment: 25 pages, 26 figures, 8 tables, accepted for publication in A&

Understanding stellar activity-induced radial velocity jitter using simultaneous K2 photometry and HARPS RV measurements

One of the best ways to improve our understanding of the stellar activity-induced signal in radial velocity (RV) measurements is through simultaneous high-precision photometric and RV observations. This is of prime importance to mitigate the RV signal induced by stellar activity and therefore unveil the presence of low-mass exoplanets. The K2 Campaign 7 and 8 field-of-views were located in the southern hemisphere, and provided a unique opportunity to gather unprecedented simultaneous high precision photometric observation with K2 and high-precision RV measurements with the HARPS spectrograph to study the relationship between photometric variability and RV jitter. We observed nine stars with different levels of activity; from quiet to very active. We probe the presence of any meaningful relation between measured RV jitter and the simultaneous photometric variation, and also other activity indicators (e.g. BIS, FWHM, $logR'_{HK}$, and F8), by evaluating the strength and significance of the correlation between RVs and each indicator. We found that for the case of very active stars, strong and significant correlations exist between almost all the observables and measured RVs; however, for lower activity levels the correlations become random. Except for the F8 which its strong correlation with RV jitter persists over a wide range of stellar activity level, and thus our result suggests that F8 might be a powerful proxy for activity induced RV jitter. Moreover, we examine the capability of two state-of-the-art modeling techniques, namely the FF' method and SOAP2.0, in accurately predicting the RV jitter amplitude using the simultaneous photometric observation. We found that for the very active stars both techniques can reasonably well predict the amplitude of the RV jitter, however, at lower activity levels the FF' method underpredicts the RV jitter amplitude.Comment: 13 pages, 7 figures, 2 tables, accepted for publication in A&

Reprodução no macho caprino: análise básica e aplicada.

A reprodução de pequenos ruminantes é dependente de diversos eventos fisiológicos e ambientais, assim como da harmonia dos manejos nutricionais e sanitários dos rebanhos. O conhecimento consorciado da reprodução do macho caprino, unindo avaliações básicas já existentes às práticas aplicadas a campo, torna-se de fundamental relevância para que profissionais, produtores e acadêmicos das ciências agrárias possam visualizar esta área da Medicina Veterinária de uma forma mais ampla e completa. O conhecimento de eventos fisiológicos e sua aplicação prática na utilização de exames diagnósticos, que visem à seleção de reprodutores caprinos para centrais de inseminação artificial ou mesmo que visem ? seleção de reprodutores para a utilização em programas de melhoramento genético, dar· subsídios para a escolha de animais superiores e perfeitamente confiáveis para a formão de bancos de germoplasma, por exemplo. Essa série documentos tem como objetivo esclarecer de forma conjunta a produtores, técnicos e acadêmicos, quanto ? importância de se conhecer uma avaliação andrológica e seminal com base na fisiologia dos machos caprinos e desta forma, proporcionar aos profissionais uma visão mais completa da reprodução em caprinos.bitstream/CNPC-2010/21843/1/doc79.pd

Proteínas do plasma seminal de ovinos da raça Morada Nova presentes no período de transição chuvoso-seco na região Norte do Estado do Ceará.

A identificação das proteínas é uma das principais alternativas para compreendermos as interações do plasma seminal com os espermatozóides. Em relação à espécie ovina e, mais precisamente a raça Morada Nova poucos trabalhos são encontrados na literatura relacionados a esses animais. Foram utilizados quatro animais em idade reprodutiva onde foi coletado o sêmen semanalmente, no período de transição chuvoso-seco, na região Norte do Estado do Ceará, referentes aos meses de julho e agosto/2009. Observou-se a presença de 20 e 19 bandas protéicas nos meses de julho e agosto/2009, com pesos moleculares variando de 22 a 115kDa e 20 a 98kDa, respectivamente. Foram identificadas as proteínas de peso 97, 79, 66, 55, 42, 29 e 22 kDa em todo o período estudado. Objetivou-se avaliar a variação protéica do plasma seminal presentes no período de transição chuvoso-seco em ovinos da raça Morada Nova. Abstract: The protein identification is an alternative in order to understand the seminal plasma and spermatozoid interaction. Concerning to ovine specie and specially the Morada Nova breed, are rare the works found in literature related to these animals. It were utilized four adults animals at reproductive aging where it was collected semen weekly during the transition rainy/dry period related to months of Juky and August, in the North region of Ceará State. It was observed the presence of 20 and 19 proteins bands on July and August with molecular weight varying from 22 to 115 and from 20 to 98 kDa, respectively. It were identified proteins with molecular weight of 97, 79, 66, 55, 42, 29 and 22 kDa along the period studied. Aimed to evaluate the variation of seminal plasma protein present in the transition period wetdry sheep Morada Nova

Comparison between two mobile absolute gravimeters: optical versus atomic interferometers

We report a comparison between two absolute gravimeters: the LNE-SYRTE cold atoms gravimeter and FG5#220 of Leibniz Universit\"at of Hannover. They rely on different principles of operation: atomic and optical interferometry. Both are movable which enabled them to participated to the last International Comparison of Absolute Gravimeters (ICAG'09) at BIPM. Immediately after, their bilateral comparison took place in the LNE watt balance laboratory and showed an agreement of 4.3 +/- 6.4 {\mu}Gal

Giant magnon spin conductivity approaching the two-dimensional transport regime in ultrathin yttrium iron garnet films

Conductivities are key material parameters that govern various types of transport (electronic charge, spin, heat etc.) driven by thermodynamic forces. Magnons, the elementary excitations of the magnetic order, flow under the gradient of a magnon chemical potential in proportion to a magnon (spin) conductivity $\sigma_{m}$. The magnetic insulator yttrium iron garnet (YIG) is the material of choice for efficient magnon spin transport. Here we report an unexpected giant $\sigma_{m}$ in record-thin YIG films with thicknesses down to 3.7 nm when the number of occupied two-dimensional (2D) subbands is reduced from a large number to a few, which corresponds to a transition from 3D to 2D magnon transport. We extract a 2D spin conductivity ($\approx1$ S) at room temperature, comparable to the (electronic) spin conductivity of the high-mobility two-dimensional electron gas in GaAs quantum wells at millikelvin temperatures. Such high conductivities offer unique opportunities to develop low-dissipation magnon-based spintronic devices

The SOPHIE search for northern extrasolar planets: VI. Three new hot Jupiters in multi-planet extrasolar systems

We present high-precision radial-velocity measurements of three solar-type stars: HD 13908, HD 159243, and HIP 91258. The observations were made with the SOPHIE spectrograph at the 1.93-m telescope of Observatoire de Haute-Provence (France). They show that these three bright stars host exoplanetary systems composed of at least two companions. HD 13908 b is a planet with a minimum mass of 0.865+-0.035 Mjup, on a circular orbit with a period of 19.382+-0.006 days. There is an outer massive companion in the system with a period of 931+-17 days, e = 0.12+-0.02, and a minimum mass of 5.13+-0.25 Mjup. The star HD 159243, also has two detected companions with respective masses, periods, and eccentricities of Mp = 1.13+-0.05 and 1.9+-0.13 Mjup, $P$ = 12.620+-0.004 and 248.4+-4.9 days, and e = 0.02+-0.02 and 0.075+-0.05. Finally, the star HIP 91258 has a planetary companion with a minimum mass of 1.068+-0.038 Mjup, an orbital period of 5.0505+-0.0015 days, and a quadratic trend indicating an outer planetary or stellar companion that is as yet uncharacterized. The planet-hosting stars HD 13908, HD 159243, and HIP 91258 are main-sequence stars of spectral types F8V, G0V, and G5V, respectively, with moderate activity levels. HIP 91258 is slightly over-metallic, while the two other stars have solar-like metallicity. The three systems are discussed in the frame of formation and dynamical evolution models of systems composed of several giant planets.Comment: accepted in A&

Demandas tecnológicas para o sistema produtivo da mandioca nas microrregiões de Altamira e Santarém, no estado do Pará.

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