The Gemini NICI planet-finding campaign: the frequency of giant planets around young B and A stars

We have carried out high contrast imaging of 70 young, nearby B and A stars to search for brown dwarf and planetary companions as part of the Gemini NICI Planet-Finding Campaign. Our survey represents the largest, deepest survey for planets around high-mass stars (≈1.5-2.5 M ☉) conducted to date and includes the planet hosts β Pic and Fomalhaut. We obtained follow-up astrometry of all candidate companions within 400 AU projected separation for stars in uncrowded fields and identified new low-mass companions to HD 1160 and HIP 79797. We have found that the previously known young brown dwarf companion to HIP 79797 is itself a tight (3 AU) binary, composed of brown dwarfs with masses 58$^{+21}_{-20}$ M Jup and 55$^{+20}_{-19}$ M Jup, making this system one of the rare substellar binaries in orbit around a star. Considering the contrast limits of our NICI data and the fact that we did not detect any planets, we use high-fidelity Monte Carlo simulations to show that fewer than 20% of 2 M ☉ stars can have giant planets greater than 4 M Jup between 59 and 460 AU at 95% confidence, and fewer than 10% of these stars can have a planet more massive than 10 M Jup between 38 and 650 AU. Overall, we find that large-separation giant planets are not common around B and A stars: fewer than 10% of B and A stars can have an analog to the HR 8799 b (7 M Jup, 68 AU) planet at 95% confidence. We also describe a new Bayesian technique for determining the ages of field B and A stars from photometry and theoretical isochrones. Our method produces more plausible ages for high-mass stars than previous age-dating techniques, which tend to underestimate stellar ages and their uncertainties.

Prevalência de hipertensão arterial em Adventistas do Sétimo Dia da capital e do interior paulista

FUNDAMENTO: Sabe-se que hábitos de vida inadequados favorecem a hipertensão, e os adventistas preconizam hábitos saudáveis. OBJETIVO: Avaliar a prevalência da hipertensão nos adventistas do sétimo dia na capital e no interior paulistas. MÉTODOS: Foram estudados 264 adventistas (41,17 ± 15,27 anos, 59,8% mulheres, com alto nível de religiosidade avaliada pela escala Duke-DUREL). A medida da pressão arterial foi realizada com aparelho automático validado. Nível de significância adotado foi p < 0,05. Resultados: A prevalência total de hipertensão foi 22,7%, (27,4% no interior e 15% na capital). Os adventistas da capital diferiram dos do interior (p < 0,05), respectivamente, quanto: escolaridade superior (62% vs 36,6%); ter vínculo empregatício (44%) vs autônomos (40,9%); renda familiar (8,39 ± 6,20 vs 4,59 ± 4,75 salários mínimos) e renda individual (4,54 ± 5,34 vs 6,35 ± 48 salários mínimos); casal responsável pela renda familiar (35% vs 39,6%); vegetarianismo (11% vs 3%); pressão arterial (115,38 ± 16,52/68,74 ± 8,94 vs 123,66 ± 19,62/74,88 ± 11,85 mmHg); etnia branca (65% vs 81,1%); casados (53% vs 68,9%); menor apoio social no domínio material (15,7 ± 5,41 vs 16,9 ± 4,32) e lembrar da última vez que mediu a pressão arterial (65% vs 48,8%). A análise multivariada associou hipertensão com: 1) vegetarianismo (OR 0,051, IC95% 0,004-0,681), 2) escolaridade (OR 5,317, IC95% 1,674-16,893), 3) lembrar quando mediu a pressão (OR 2,725, IC95% 1,275-5,821), 4) aposentado (OR 8,846, IC95% 1,406-55,668), 5) responsável pela renda familiar (OR 0,422, IC95% 0,189-0,942). CONCLUSÃO: A prevalência de hipertensão dos adventistas foi menor se comparada com estudos nacionais, sendo menor na capital em relação ao interior possivelmente por melhores condições socioeconômicas e hábitos de vida.

Effects of high-energy astrophysical events on habitable planets

With the possible exception of meteor impacts, high-energy astrophysical events such as supernovae, gamma-ray bursts (GRB) and flares are usually not taken into account for biological and evolutionary studies due to their low rates of occurrence. We show that a class of these events may occur at distances and time scales in which their biological effects are non-negligible, maybe more frequent than the impacts of large asteroids. We review the effects of four transient astrophysical sources of ionizing radiation on biospheres - stellar flares, giant flares from soft gamma repeaters (SGR), supernovae and GRB. The main damaging features of them are briefly discussed and illustrated. We point out some open problems and ongoing work. Received 28 February 2012, accepted 6 July 2012, first published online 10 August 2012

Predicting epidemic outbreak from individual features of the spreaders

Knowing which individuals can be more efficient in spreading a pathogen throughout a determinate environment is a fundamental question in disease control. Indeed, over recent years the spread of epidemic diseases and its relationship with the topology of the involved system have been a recurrent topic in complex network theory, taking into account both network models and real-world data. In this paper we explore possible correlations between the heterogeneous spread of an epidemic disease governed by the susceptible-infected-recovered (SIR) model, and several attributes of the originating vertices, considering Erdos-Renyi (ER), Barabasi-Albert (BA) and random geometric graphs (RGG), as well as a real case study, the US air transportation network, which comprises the 500 busiest airports in the US along with inter-connections. Initially, the heterogeneity of the spreading is achieved by considering the RGG networks, in which we analytically derive an expression for the distribution of the spreading rates among the established contacts, by assuming that such rates decay exponentially with the distance that separates the individuals. Such a distribution is also considered for the ER and BA models, where we observe topological effects on the correlations. In the case of the airport network, the spreading rates are empirically defined, assumed to be directly proportional to the seat availability. Among both the theoretical and real networks considered, we observe a high correlation between the total epidemic prevalence and the degree, as well as the strength and the accessibility of the epidemic sources. For attributes such as the betweenness centrality and the k-shell index, however, the correlation depends on the topology considered.

VVV DR1: The first data release of the Milky Way bulge and southern plane from the near-infrared ESO public survey VISTA variables in the Via Lactea

Context. The ESO public survey VISTA variables in the Via Lactea (VVV) started in 2010. VVV targets 562 sq. deg in the Galactic bulge and an adjacent plane region and is expected to run for about five years. Aims. We describe the progress of the survey observations in the first observing season, the observing strategy, and quality of the data obtained. Methods. The observations are carried out on the 4-m VISTA telescope in the ZYJHK(s) filters. In addition to the multi-band imaging the variability monitoring campaign in the K-s filter has started. Data reduction is carried out using the pipeline at the Cambridge Astronomical Survey Unit. The photometric and astrometric calibration is performed via the numerous 2MASS sources observed in each pointing. Results. The first data release contains the aperture photometry and astrometric catalogues for 348 individual pointings in the ZYJHK(s) filters taken in the 2010 observing season. The typical image quality is similar to 0 ''.9-1 ''.0. The stringent photometric and image quality requirements of the survey are satisfied in 100% of the JHK(s) images in the disk area and 90% of the JHK(s) images in the bulge area. The completeness in the Z and Y images is 84% in the disk, and 40% in the bulge. The first season catalogues contain 1.28 x 10(8) stellar sources in the bulge and 1.68 x 10(8) in the disk area detected in at least one of the photometric bands. The combined, multi-band catalogues contain more than 1.63 x 10(8) stellar sources. About 10% of these are double detections because of overlapping adjacent pointings. These overlapping multiple detections are used to characterise the quality of the data. The images in the JHK(s) bands extend typically similar to 4 mag deeper than 2MASS. The magnitude limit and photometric quality depend strongly on crowding in the inner Galactic regions. The astrometry for K-s = 15-18 mag has rms similar to 35-175 mas. Conclusions. The VVV Survey data products offer a unique dataset to map the stellar populations in the Galactic bulge and the adjacent plane and provide an exciting new tool for the study of the structure, content, and star-formation history of our Galaxy, as well as for investigations of the newly discovered star clusters, star-forming regions in the disk, high proper motion stars, asteroids, planetary nebulae, and other interesting objects.

Is income area level associated with blood pressure in adults regardless of individual-level characteristics? A multilevel approach

This population-based health survey was carried out in Florianopolis, Brazil, to assess the association between adult systolic blood pressure (SBP) and contextual income level, after controlling for potential individual-level confounders. A statistically significant negative association between SBP levels and contextual income was identified after adjusting for individual-level characteristics. SBP levels in the highest and in the intermediate tertiles of contextual income were 5.78 and 2.82 mmHg lower, respectively, than that observed in the bottom tertile. The findings suggest an association between income area level and blood pressure, regardless of well-known individual-level hypertension risk factors. (C) 2012 Elsevier Ltd. All rights reserved.

Differences between female and male adolescents regarding individual vulnerability to HIV

The objective of this study was to comparatively analyze male and female adolescents' vulnerability to HIV/AIDS, based on their knowledge, values and practices. This is an exploratory-descriptive study, performed using a quantitative approach. The students answered a questionnaire from which relevant questions were selected for the analysis. The participants were 207 adolescents, 43.5% male and 56.5% female. Most adolescents report having initiated sexual activities. It was observed that the participants have knowledge deficits regarding HIV transmission and safe sexual practices. Although they report knowing about condom use as a method of protection against HIV, they do not always use them. It was observed that there are values connected to the representations of gender, but it is noticed there is an evolution regarding the autonomy and power of the girls' negotiation regarding condom use.

Stochastic gravito-inertial modes discovered by CoRoT in the hot Be star HD51452

Context. Be stars are rapidly rotating stars with a circumstellar decretion disk. They usually undergo pressure and/or gravity pulsation modes excited by the kappa-mechanism, i.e. an effect of the opacity of iron-peak elements in the envelope of the star. In the Milky Way, p-modes are observed in stars that are hotter than or equal to the B3 spectral type, while g-modes are observed at the B2 spectral type and cooler. Aims. We observed a B0IVe star, HD51452, with the high-precision, high-cadence photometric CoRoT satellite and high-resolution, ground-based HARPS and SOPHIE spectrographs to study its pulsations in great detail. We also used the lower resolution spectra available in the BeSS database. Methods. We analyzed the CoRoT and spectroscopic data with several methods: CLEAN-NG, FREQFIND, and a sliding window method. We also analyzed spectral quantities, such as the violet over red (V/R) emission variations, to obtain information about the variation in the circumstellar environment. We calculated a stellar structure model with the ESTER code to test the various interpretation of the results. Results. We detect 189 frequencies of variations in the CoRoT light curve in the range between 0 and 4.5 c d(-1). The main frequencies are also recovered in the spectroscopic data. In particular we find that HD51452 undergoes gravito-inertial modes that are not in the domain of those excited by the kappa-mechanism. We propose that these are stochastic modes excited in the convective zones and that at least some of them are a multiplet of r-modes (i.e. subinertial modes mainly driven by the Coriolis acceleration). Stochastically excited gravito-inertial modes had never been observed in any star, and theory predicted that their very low amplitudes would be undetectable even with CoRoT. We suggest that the amplitudes are enhanced in HD51452 because of the very rapid stellar rotation. In addition, we find that the amplitude variations of these modes are related to the occurrence of minor outbursts. Conclusions. Thanks to CoRoT data, we have detected a new kind of pulsations in HD51452, which are stochastically excited gravito-inertial modes, probably due to its very rapid rotation. These modes are probably also present in other rapidly rotating hot Be stars.

Contextual and individual assessment of dental pain period prevalence in adolescents: a multilevel approach

Abstract Background Despite evidence that health and disease occur in social contexts, the vast majority of studies addressing dental pain exclusively assessed information gathered at individual level. Objectives To assess the association between dental pain and contextual and individual characteristics in Brazilian adolescents. In addition, we aimed to test whether contextual Human Development Index is independently associated with dental pain after adjusting for individual level variables of socio-demographics and dental characteristics. Methods The study used data from an oral health survey carried out in São Paulo, Brazil, which included dental pain, dental exams, individual socioeconomic and demographic conditions, and Human Development Index at area level of 4,249 12-year-old and 1,566 15-year-old schoolchildren. The Poisson multilevel analysis was performed. Results Dental pain was found among 25.6% (95%CI = 24.5-26.7) of the adolescents and was 33% less prevalent among those living in more developed areas of the city than among those living in less developed areas. Girls, blacks, those whose parents earn low income and have low schooling, those studying at public schools, and those with dental treatment needs presented higher dental-pain prevalence than their counterparts. Area HDI remained associated with dental pain after adjusting for individual level variables of socio demographic and dental characteristics. Conclusions Girls, students whose parents have low schooling, those with low per capita income, those classified as having black skin color and those with dental treatment needs had higher dental pain prevalence than their counterparts. Students from areas with low Human Development Index had higher prevalence of dental pain than those from the more developed areas regardless of individual characteristics.

Avaliação do benefício do uso de aparelhos de amplificação sonora individual em crianças

INTRODUÇÃO: No Brasil, são raros estudos com crianças surdas usuárias de aparelho auditivo acima de sete anos. OBJETIVO: Investigar o benefício fornecido pela amplificação em crianças surdas de sete a 11 anos usuárias de aparelho auditivo, sob a perspectiva da própria criança e dos adultos com quem ela mais convive, e verificar se o tempo de convívio dos adultos com a criança interfere em suas respostas. MÉTODO: Trata-se de um estudo clínico e experimental. Participaram do estudo 48 sujeitos, divididos em 4 grupos distintos: G1- 12 crianças surdas; G2- 12 adultos com convivência média de 40 horas semanais com a criança surda; G3- 12 adultos com convivência média de 20 horas semanais com a criança surda; G4- 12 adultos com convivência média de 10 horas semanais com a criança surda. Todas as crianças eram usuárias de aparelho bilateralmente e apresentavam perda auditiva de grau severo ou profundo. RESULTDOS: Os resultados indicam um prejuízo nas habilidades auditivas das crianças avaliadas devido às dificuldades enfrentadas por elas para escutar elementos presentes em situações de seu cotidiano. Não houve diferenças nos resultados entre os diferentes grupos conforme o tempo de convivência com a criança. CONCLUSÃO: Constatou-se clinicamente a viabilidade da avaliação do benefício proporcionado pelo aparelho auditivo em crianças com base nas informações da família. O aparelho de amplificação sonora individual exerceu influência nas habilidades auditivas das crianças avaliadas, apesar do benefício proporcionado pelo seu uso ser menor do que o esperado.

Telessaúde: avaliação da eficácia da teleconsulta na programação e adaptação de aparelho de amplificação sonora individual

OBJETIVO: Avaliar a eficácia da teleconsulta para a programação, verificação e adaptação do aparelho de amplificação sonora individual (AASI). MÉTODOS: Cinquenta participantes com deficiência auditiva (idades entre 39 e 88 anos), com média dos limiares audiométricos entre 30 e 68,75 dBNA, foram alocados em dois grupos (randomização estratificada), controle (n=25) e experimental (n=25), submetidos respectivamente à consulta face a face e teleconsulta síncrona com video interativo e controle remoto de aplicativos. Foram realizadas a programação e verificação do AASI (medidas com microfone sonda) e orientação dos participantes quanto ao uso e cuidados com o dispositivo. O tempo para os procedimentos foi cronometrado. Após as consultas um avaliador, cego quanto aos grupos, aplicou o teste de percepção da fala Hearing in Noise Test (HINT) Brasil. Aproximadamente um mês após as consultas, foi verificado o tempo diário de uso do AASI e administrado o questionário International Outcome Inventory for Hearing Aids (IOI-HA). RESULTADOS: Maior tempo para a programação e verificação e menor tempo para orientação foi observado para o grupo experimental. Não houve diferença entre grupos no tempo total do atendimento. A equiparação das medidas com microfone sonda aos respectivos targets de amplificação foi similar para os dois grupos. Não houve diferença entre os grupos quanto aos resultados do HINT-Brasil (silêncio e ruído), o tempo médio de uso diário do AASI e resultados do IOI-HA. CONCLUSÃO: A teleconsulta é um procedimento eficaz para a programação, verificação do AASI e orientação de usuários quando serviços face a face não estiverem disponíveis.

The Gemini planet-finding campaign: the frequency of giant planets aroud debris disk stars

We have completed a high-contrast direct imaging survey for giant planets around 57 debris disk stars as part of the Gemini NICI Planet-Finding Campaign. We achieved median H-band contrasts of 12.4 mag at 0.''5 and 14.1 mag at 1'' separation. Follow-up observations of the 66 candidates with projected separation <500 AU show that all of them are background objects. To establish statistical constraints on the underlying giant planet population based on our imaging data, we have developed a new Bayesian formalism that incorporates (1) non-detections, (2) single-epoch candidates, (3) astrometric and (4) photometric information, and (5) the possibility of multiple planets per star to constrain the planet population. Our formalism allows us to include in our analysis the previously known β Pictoris and the HR 8799 planets. Our results show at 95% confidence that <13% of debris disk stars have a ≥5 M Jup planet beyond 80 AU, and <21% of debris disk stars have a ≥3 M Jup planet outside of 40 AU, based on hot-start evolutionary models. We model the population of directly imaged planets as d 2 N/dMdavpropm α a β, where m is planet mass and a is orbital semi-major axis (with a maximum value of a max). We find that β < –0.8 and/or α > 1.7. Likewise, we find that β < –0.8 and/or a max < 200 AU. For the case where the planet frequency rises sharply with mass (α > 1.7), this occurs because all the planets detected to date have masses above 5 M Jup, but planets of lower mass could easily have been detected by our search. If we ignore the β Pic and HR 8799 planets (should they belong to a rare and distinct group), we find that <20% of debris disk stars have a ≥3 M Jup planet beyond 10 AU, and β < –0.8 and/or α < –1.5. Likewise, β < –0.8 and/or a max < 125 AU. Our Bayesian constraints are not strong enough to reveal any dependence of the planet frequency on stellar host mass. Studies of transition disks have suggested that about 20% of stars are undergoing planet formation; our non-detections at large separations show that planets with orbital separation >40 AU and planet masses >3 M Jup do not carve the central holes in these disks.

Stochastic gravito-inertial modes discovered by CoRoT in the hot Be star HD51452

Context. Be stars are rapidly rotating stars with a circumstellar decretion disk. They usually undergo pressure and/or gravity pulsation modes excited by the κ-mechanism, i.e. an effect of the opacity of iron-peak elements in the envelope of the star. In the Milky Way, p-modes are observed in stars that are hotter than or equal to the B3 spectral type, while g-modes are observed at the B2 spectral type and cooler. Aims. We observed a B0IVe star, HD51452, with the high-precision, high-cadence photometric CoRoT satellite and high-resolution, ground-based HARPS and SOPHIE spectrographs to study its pulsations in great detail. We also used the lower resolution spectra available in the BeSS database. Methods. We analyzed the CoRoT and spectroscopic data with several methods: Clean-NG, FreqFind, and a sliding window method. We also analyzed spectral quantities, such as the violet over red (V/R) emission variations, to obtain information about the variation in the circumstellar environment. We calculated a stellar structure model with the ESTER code to test the various interpretation of the results. Results. We detect 189 frequencies of variations in the CoRoT light curve in the range between 0 and 4.5 c d−1. The main frequencies are also recovered in the spectroscopic data. In particular we find that HD51452 undergoes gravito-inertial modes that are not in the domain of those excited by the κ-mechanism. We propose that these are stochastic modes excited in the convective zones and that at least some of them are a multiplet of r-modes (i.e. subinertial modes mainly driven by the Coriolis acceleration). Stochastically excited gravito-inertial modes had never been observed in any star, and theory predicted that their very low amplitudes would be undetectable even with CoRoT. We suggest that the amplitudes are enhanced in HD51452 because of the very rapid stellar rotation. In addition, we find that the amplitude variations of these modes are related to the occurrence of minor outbursts. Conclusions. Thanks to CoRoT data, we have detected a new kind of pulsations in HD51452, which are stochastically excited gravito-inertial modes, probably due to its very rapid rotation. These modes are probably also present in other rapidly rotating hot Be stars.