Efeito dos ácidos graxos ômega-3, ômega-6 e ômega-9 sobre o risco cardiovascular de indivíduos adultos: estudo clínico de prevenção primária.

INTRODUÇÃO: As doenças cardiovasculares (DCV) são a principal causa de morte no mundo, sendo muitos dos fatores de risco passíveis de prevenção e controle. Embora as DCV sejam complexas em sua etiologia e desenvolvimento, a concentração elevada de LDL-c e baixa de HDL-c constituem os fatores de risco modificáveis mais monitorados na prática clínica, embora não sejam capazes de explicar todos os eventos cardiovasculares. Portanto, investigar como intervenções farmacológicas e nutricionais podem modular parâmetros oxidativos, físicos e estruturais das lipoproteínas pode fornecer estimativa adicional ao risco cardiovascular. Dentre os diversos nutrientes e compostos bioativos relacionados às DCV, os lipídeos representam os mais investigados e descritos na literatura. Nesse contexto, os ácidos graxos insaturados (ômega-3, ômega-6 e ômega-9) têm sido foco de inúmeros estudos. OBJETIVOS: Avaliar o efeito da suplementação com ômega-3, ômega-6 e ômega-9 sobre os parâmetros cardiometabólicos em indivíduos adultos com múltiplos fatores de risco e sem evento cardiovascular prévio. MATERIAL E MÉTODOS: Estudo clínico, randomizado, duplo-cego, baseado em intervenção nutricional (3,0 g/dia de ácidos graxos) sob a fórmula de cápsulas contendo: ômega-3 (37 por cento de EPA e 23 por cento de DHA) ou ômega-6 (65 por cento de ácido linoleico) ou ômega-9 (72 por cento de ácido oleico). A amostra foi composta por indivíduos de ambos os sexos, com idade entre 30 e 74 anos, apresentando pelo menos um dos seguintes fatores de risco: Dislipidemia, Diabetes Mellitus, Obesidade e Hipertensão Arterial Sistêmica. Após aprovação do Comitê de Ética, os indivíduos foram distribuídos nos três grupos de intervenção. No momento basal, os indivíduos foram caracterizados quanto aos aspectos demográficos (sexo, idade e etnia) e clínicos (medicamentos, doenças atuais e antecedentes familiares). Nos momentos basal e após 8 semanas de intervenção, amostras de sangue foram coletadas após 12h de jejum. A partir do plasma foram analisados: perfil lipídico (CT, LDL-c, HDL-c, TG), apolipoproteínas AI e B, ácidos graxos não esterificados, atividade da PON1, LDL(-) e auto-anticorpos, ácidos graxos, glicose, insulina, tamanho e distribuição percentual da LDL (7 subfrações e fenótipo A e não-A) e HDL (10 subfrações). O efeito do tempo, da intervenção e associações entre os ácidos graxos e aspectos qualitativos das lipoproteínas foram testados (SPSS versão 20.0, p <0,05). RESULTADOS: Uma primeira análise dos resultados baseada em um corte transversal demonstrou, por meio da análise de tendência linear ajustada pelo nível de risco cardiovascular, que o maior tercil plasmático de DHA se associou positivamente com HDL-c, HDLGRANDE e tamanho de LDL e negativamente com HDLPEQUENA e TG. Observou-se também que o maior tercil plasmático de ácido linoleico se associou positivamente com HDLGRANDE e tamanho de LDL e negativamente com HDLPEQUENA e TG. Esse perfil de associação não foi observado quando foram avaliados os parâmetros dietéticos. Avaliando uma subamostra que incluiu indivíduos tabagistas suplementados com ômega-6 e ômega-3, observou-se que ômega-3 modificou positivamente o perfil lipídico e as subfrações da HDL. Nos modelos de regressão linear ajustados pela idade, sexo e hipertensão, o DHA plasmático apresentou associações negativas com a HDLPEQUENA. Quando se avaliou exclusivamente o efeito do ômega-3 em indivíduos tabagistas e não tabagistas, observou-se que fumantes, do sexo masculino, acima de 60 anos de idade, apresentando baixo percentual plasmático de EPA e DHA (<8 por cento ), com excesso de peso e gordura corporal elevada, apresentam maior probabilidade de ter um perfil de subfrações de HDL mais aterogênicas. Tendo por base os resultados acima, foi comparado o efeito do ômega-3, ômega-6 e ômega-9 sobre os parâmetros cardiometabólicos. O ômega-3 promoveu redução no TG, aumento do percentual de HDLGRANDE e redução de HDLPEQUENA. O papel cardioprotetor do ômega-3 foi reforçado pelo aumento na incorporação de EPA e DHA, no qual indivíduos com EPA e DHA acima de 8 por cento apresentaram maior probabilidade de ter HDLGRANDE e menor de ter HDLPEQUENA. Em adição, observou-se também que o elevado percentual plasmático de ômega-9 se associou com partículas de LDL menos aterogênicas (fenótipo A). CONCLUSÃO: Ácidos graxos plasmáticos, mas não dietéticos, se correlacionam com parâmetros cardiometabólicos. A suplementação com ômega-3, presente no óleo de peixe, promoveu redução no TG e melhoria nos parâmetros qualitativos da HDL (mais HDLGRANDE e menos HDLPEQUENA). Os benefícios do ômega-3 foram particularmente relevantes nos indivíduos tabagistas e naqueles com menor conteúdo basal de EPA e DHA plasmáticos. Observou-se ainda que o ômega-9 plasmático, presente no azeite de oliva, exerceu impacto positivo no tamanho e subfrações da LDL.

Variabilidade intratípica de HPV 16 em relação à origem étnica e HLA de uma população de alto risco para o câncer do colo do útero

A infecção por papilomavirus é a principal causa de desenvolvimento de neoplasias intraepiteliais cervicais (NIC) e câncer do colo do útero (CCU). Estudos epidemiológicos têm demonstrado que a persistência do genoma viral encontra-se associado a variantes moleculares específicas de papilomavirus humano (HPV) de alto risco. As moléculas HLA de classe II têm um importante papel na resposta imune. Associações entre HLA e CCU ou infecção por HPV tem sido demonstrado em diferentes populações. O nosso objetivo foi verificar se a variabilidade de HLA-DRB1 e DQB1 estavam associada ao CCU e NIC III em mulheres de Belém, uma população formada pelos 3 principais grupos étnicos humanos e uma área de alto risco para o CCU no Norte do Brasil. Foi investigada a existência de diferenças na distribuição de alelos HLA entre mulheres com CCU e NIC III portadoras de diferentes variantes de HPV-16 e mulheres citologicamente normais. Os genes HLA DQB1 e DRB1 foram tipados pelo método de PCR-SSO em 95 casos e 287 controles de mulheres com citologia normal atendidas em um centro de prevenção do colo do útero na mesma cidade. As variantes de HPV-16 foram tipadas por sequenciamento de um fragmento da região controladora do genoma viral (LCR). O polimorfismo na posição 350 do gene E6 foi tipado baseado em um protocolo de hibridização em pontos, para identificar a alteração na posição 350T→G. A magnitude das associações foi estimada por odds ratio (OR) e os respectivos intervalos de confiança (IC), ajustados para potenciais fatores de confusão. Uma associação positiva foi observada entre CCU e os haplótipos DRB1* 150 l-DQB1*0602, DRB1*04-DQB1*0301 e DRB1*1602-DQB1*0301. Ao contrário, DRB1*01-DQB1*0501 mostrou um efeito protetor. Os alelos DRB1*0804, DQB1*0402 apresentaram efeito protetor contra positividade por HPV. O alelo DQB1*0502 e o grupo DRB1*15 foram positivamente associados. Os nossos resultados mostram que as associações positivas de DRB1*1501 e DRB1*1602 podem ser atribuídas a variantes asiático-americanas quando comparado a variantes européias. O risco conferido a DRB1*1501 foi encontrado associado tanto a variantes E6350G quanto a variantes E6350T, entretanto, o maior efeito foi devido às variantes E6250T. A associação positiva de DRB1*1602 foi significativa somente no grupo de mulheres positivas para E6350G. Estes resultados estão de acordo com a composição étnica da população estudada bem como um maior potencial oncogênico de certas variantes. Nossos dados sugerem que a contribuição dos alelos HLA na susceptibilidade genética ao CCU difere de acordo com a distribuição das variantes de HPV em uma dada região geográfica ou grupo étnico.

Identifying sociodemographic differences in Intimate Partner Violence among immigrant and native women in Spain: a cross-sectional study

Objectives: To analyze whether sociodemographics and social support have a different or similar effect on the likelihood of Intimate Partner Violence in immigrants and natives, and to estimate prevalences and associations between different types of IPV depending on women's birthplace. Methods: Cross-sectional study of 10,048 women (18–70 years) attending primary healthcare in Spain (2006–2007). Outcome: Current Intimate Partner Violence (psychological, physical and both). Sociodemographics and social support were considered first as explicative and later as control variables. Results: Similar Intimate Partner Violence sociodemographic and social support factors were observed among immigrants and natives. However, these associations were stronger among immigrants, except in the case of poor social support (adjusted odds ratio natives 4.36 and adjusted odds ratio immigrants 4.09). When these two groups were compared, immigrants showed a higher likelihood of IPV than natives (adjusted odds ratios 1.58). Conclusion: Immigrant women are in a disadvantaged Intimate Partner Violence situation. It is necessary that interventions take these inequalities into account.

A third cluster of red supergiants in the vicinity of the massive cluster RSGC3

Context. Recent studies have shown that the area around the massive, obscured cluster RSGC3 may harbour several clusters of red supergiants. Aims. We analyse a clump of photometrically selected red supergiant candidates 20′ south of RSGC3 in order to confirm the existence of another of these clusters. Methods. Using medium-resolution infrared spectroscopy around 2.27 μm, we derived spectral types and velocities along the line of sight for the selected candidates, confirming their nature and possible association. Results. We find a compact clump of eight red supergiants and four other candidates at some distance, all of them spectroscopically confirmed red supergiants. The majority of these objects must form an open cluster, which we name Alicante 10. Because of the high reddening and strong field contamination, the cluster sequence is not clearly seen in 2MASS or GPS-UKIDSS. From the observed sources, we derive E(J − KS) = 2.6 and d ≈ 6 kpc. Conclusions. Although the cluster is smaller than RSGC3, it has an initial mass in excess of 10 000 M⊙, and it seems to be part of the RSGC3 complex. With the new members this association already has 35 spectroscopically confirmed red supergiants, confirming its place as one of the most active sites of recent stellar formation in the Galaxy.

Red supergiants around the obscured open cluster Stephenson 2

Context. Several clusters of red supergiants have been discovered in a small region of the Milky Way close to the base of the Scutum-Crux Arm and the tip of the Long Bar. Population synthesis models indicate that they must be very massive to harbour so many supergiants. Amongst these clusters, Stephenson 2, with a core grouping of 26 red supergiants, is a strong candidate to be the most massive young cluster in the Galaxy. Aims. Stephenson 2 is located close to a region where a strong over-density of red supergiants had been found. We explore the actual cluster size and its possible connection to this over-density. Methods. Taking advantage of Virtual Observatory tools, we have performed a cross-match between the DENIS, USNO-B1 and 2MASS catalogues to identify candidate obscured luminous red stars around Stephenson 2, and in a control nearby region. More than 600 infrared bright stars fulfill our colour criteria, with the vast majority having a counterpart in the I band and >400 being sufficiently bright in I to allow observation with a 4-m class telescope. We observed a subsample of ~250 stars, using the multi-object, wide-field, fibre spectrograph AF2 on the WHT telescope in La Palma, obtaining intermediate-resolution spectroscopy in the 7500–9000 Å range. We derived spectral types and luminosity classes for all these objects and measured their radial velocities. Results. Our targets turned out to be G and K supergiants, late (≥ M4) M giants, and M-type bright giants (luminosity class II) and supergiants. We found ~35 red supergiants with radial velocities similar to Stephenson 2 members, spread over the two areas surveyed. In addition, we found ~40 red supergiants with radial velocities incompatible in principle with a physical association. Conclusions. Our results show that Stephenson 2 is not an isolated cluster, but part of a huge structure likely containing hundreds of red supergiants, with radial velocities compatible with the terminal velocity at this Galactic longitude (and a distance ~6 kpc). In addition, we found evidence of several populations of massive stars at different distances along this line of sight.

The circumstellar environment and evolutionary status of the supergiant B[e] star Wd1-9

Context. Historically, supergiant (sg)B[e] stars have been difficult to include in theoretical schemes for the evolution of massive OB stars. Aims. The location of Wd1-9 within the coeval starburst cluster Westerlund 1 means that it may be placed into a proper evolutionary context and we therefore aim to utilise a comprehensive multiwavelength dataset to determine its physical properties and consequently its relation to other sgB[e] stars and the global population of massive evolved stars within Wd1. Methods. Multi-epoch R- and I-band VLT/UVES and VLT/FORS2 spectra are used to constrain the properties of the circumstellar gas, while an ISO-SWS spectrum covering 2.45−45μm is used to investigate the distribution, geometry and composition of the dust via a semi-analytic irradiated disk model. Radio emission enables a long term mass-loss history to be determined, while X-ray observations reveal the physical nature of high energy processes within the system. Results. Wd1-9 exhibits the rich optical emission line spectrum that is characteristic of sgB[e] stars. Likewise its mid-IR spectrum resembles those of the LMC sgB[e] stars R66 and 126, revealing the presence of equatorially concentrated silicate dust, with a mass of ~10−4M⊙. Extreme historical and ongoing mass loss (≳ 10−4M⊙yr−1) is inferred from the radio observations. The X-ray properties of Wd1-9 imply the presence of high temperature plasma within the system and are directly comparable to a number of confirmed short-period colliding wind binaries within Wd1. Conclusions. The most complete explanation for the observational properties of Wd1-9 is that it is a massive interacting binary currently undergoing, or recently exited from, rapid Roche-lobe overflow, supporting the hypothesis that binarity mediates the formation of (a subset of) sgB[e] stars. The mass loss rate of Wd1-9 is consistent with such an assertion, while viable progenitor and descendent systems are present within Wd1 and comparable sgB[e] binaries have been identified in the Galaxy. Moreover, the rarity of sgB[e] stars - only two examples are identified from a census of ~ 68 young massive Galactic clusters and associations containing ~ 600 post-Main Sequence stars - is explicable given the rapidity (~ 104yr) expected for this phase of massive binary evolution.

New galactic star clusters discovered in the VVV survey. Candidates projected on the inner disk and bulge

Context. VISTA Variables in the Vía Láctea (VVV) is one of six ESO Public Surveys using the 4 meter Visible and Infrared Survey Telescope for Astronomy (VISTA). The VVV survey covers the Milky Way bulge and an adjacent section of the disk, and one of the principal objectives is to search for new star clusters within previously unreachable obscured parts of the Galaxy. Aims. The primary motivation behind this work is to discover and analyze obscured star clusters in the direction of the inner Galactic disk and bulge. Methods. Regions of the inner disk and bulge covered by the VVV survey were visually inspected using composite JHKS color images to select new cluster candidates on the basis of apparent overdensities. DR1, DR2, CASU, and point spread function photometry of 10 × 10 arcmin fields centered on each candidate cluster were used to construct color–magnitude and color–color diagrams. Follow-up spectroscopy of the brightest members of several cluster candidates was obtained in order to clarify their nature. Results. We report the discovery of 58 new infrared cluster candidates. Fundamental parameters such as age, distance, and metallicity were determined for 20 of the most populous clusters.

Orbital and Physical Properties of the σ Ori Aa, Ab, B Triple System

We provide a complete characterization of the astrophysical properties of the σ Ori Aa, Ab, B hierarchical triple system and an improved set of orbital parameters for the highly eccentric σ Ori Aa, Ab spectroscopic binary. We compiled a spectroscopic data set comprising 90 high-resolution spectra covering a total time span of 1963 days. We applied the Lehman-Filhés method for a detailed orbital analysis of the radial velocity curves and performed a combined quantitative spectroscopic analysis of the σ Ori Aa, Ab, B system by means of the stellar atmosphere code FASTWIND. We used our own plus other available information on photometry and distance to the system for measuring the radii, luminosities, and spectroscopic masses of the three components. We also inferred evolutionary masses and stellar ages using the Bayesian code BONNSAI. The orbital analysis of the new radial velocity curves led to a very accurate orbital solution of the σ Ori Aa, Ab pair. We provided indirect arguments indicating that σ Ori B is a fast-rotating early B dwarf. The FASTWIND+BONNSAI analysis showed that the Aa, Ab pair contains the hottest and most massive components of the triple system while σ Ori B is a bit cooler and less massive. The derived stellar ages of the inner pair are intriguingly younger than the one widely accepted for the σ Orionis cluster, at 3 ± 1 Ma. The outcome of this study will be of key importance for a precise determination of the distance to the σ Orionis cluster, the interpretation of the strong X-ray emission detected for σ Ori Aa, Ab, B, and the investigation of the formation and evolution of multiple massive stellar systems and substellar objects.

The little-studied cluster Berkeley 90 I. LS III +46 11: a very massive O3.5 If* + O3.5 If* binary

Context. It appears that most (if not all) massive stars are born in multiple systems. At the same time, the most massive binaries are hard to find owing to their low numbers throughout the Galaxy and the implied large distances and extinctions. Aims. We want to study LS III +46 11, identified in this paper as a very massive binary; another nearby massive system, LS III +46 12; and the surrounding stellar cluster, Berkeley 90. Methods. Most of the data used in this paper are multi-epoch high S/N optical spectra, although we also use Lucky Imaging and archival photometry. The spectra are reduced with dedicated pipelines and processed with our own software, such as a spectroscopic-orbit code, CHORIZOS, and MGB. Results. LS III +46 11 is identified as a new very early O-type spectroscopic binary [O3.5 If* + O3.5 If*] and LS III +46 12 as another early O-type system [O4.5 V((f))]. We measure a 97.2-day period for LS III +46 11 and derive minimum masses of 38.80 ± 0.83 M⊙ and 35.60 ± 0.77 M⊙ for its two stars. We measure the extinction to both stars, estimate the distance, search for optical companions, and study the surrounding cluster. In doing so, a variable extinction is found as well as discrepant results for the distance. We discuss possible explanations and suggest that LS III +46 12 may be a hidden binary system where the companion is currently undetected.

The Gaia-ESO Survey: Empirical determination of the precision of stellar radial velocities and projected rotation velocities

Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey at the European Southern Observatory Very Large Telescope. Aims. A key aim is to provide precise radial velocities (RVs) and projected equatorial velocities (vsini) for representative samples of Galactic stars, which will complement information obtained by the Gaia astrometry satellite. Methods. We present an analysis to empirically quantify the size and distribution of uncertainties in RV and vsini using spectra from repeated exposures of the same stars. Results. We show that the uncertainties vary as simple scaling functions of signal-to-noise ratio (S/N) and vsini, that the uncertainties become larger with increasing photospheric temperature, but that the dependence on stellar gravity, metallicity and age is weak. The underlying uncertainty distributions have extended tails that are better represented by Student’s t-distributions than by normal distributions. Conclusions. Parametrised results are provided, which enable estimates of the RV precision for almost all GES measurements, and estimates of the vsini precision for stars in young clusters, as a function of S/N, vsini and stellar temperature. The precision of individual high S/N GES RV measurements is 0.22–0.26 km s-1, dependent on instrumental configuration.

Open cluster Dolidze 25: Stellar parameters and the metallicity in the Galactic anticentre

Context. The young open cluster Dolidze 25, in the direction of the Galactic anticentre, has been attributed a very low metallicity, with typical abundances between −0.5 and −0.7 dex below solar. Aims. We intend to derive accurate cluster parameters and accurate stellar abundances for some of its members. Methods. We have obtained a large sample of intermediate- and high-resolution spectra for stars in and around Dolidze 25. We used the fastwind code to generate stellar atmosphere models to fit the observed spectra. We derive stellar parameters for a large number of OB stars in the area, and abundances of oxygen and silicon for a number of stars with spectral types around B0. Results. We measure low abundances in stars of Dolidze 25. For the three stars with spectral types around B0, we find 0.3 dex (Si) and 0.5 dex (O) below the values typical in the solar neighbourhood. These values, even though not as low as those given previously, confirm Dolidze 25 and the surrounding H ii region Sh2-284 as the most metal-poor star-forming environment known in the Milky Way. We derive a distance 4.5 ± 0.3 kpc to the cluster (rG ≈ 12.3 kpc). The cluster cannot be older than ~3 Myr, and likely is not much younger. One star in its immediate vicinity, sharing the same distance, has Si and O abundances at most 0.15 dex below solar. Conclusions. The low abundances measured in Dolidze 25 are compatible with currently accepted values for the slope of the Galactic metallicity gradient, if we take into account that variations of at least ±0.15 dex are observed at a given radius. The area traditionally identified as Dolidze 25 is only a small part of a much larger star-forming region that comprises the whole dust shell associated with Sh2-284 and very likely several other smaller H ii regions in its vicinity.

Stabilizing and Modulating Color by Copigmentation: Insights from Theory and Experiment

Natural anthocyanin pigments/dyes and phenolic copigments/co-dyes form noncovalent complexes, which stabilize and modulate (in particular blue, violet, and red) colors in flowers, berries, and food products derived from them (including wines, jams, purees, and syrups). This noncovalent association and their electronic and optical implications constitute the copigmentation phenomenon. Over the past decade, experimental and theoretical studies have enabled a molecular understanding of copigmentation. This review revisits this phenomenon to provide a comprehensive description of the nature of binding (the dispersion and electrostatic components of π–π stacking, the hydrophobic effect, and possible hydrogen-bonding between pigment and copigment) and of spectral modifications occurring in copigmentation complexes, in which charge transfer plays an important role. Particular attention is paid to applications of copigmentation in food chemistry.

When “Where” is More Important Than “When”: Birthplace and Birthdate Effects On The Achievement Of Sporting Expertise

In this study, we assessed whether contextual factors related to where or when an athlete is born influence their likelihood of playing professional sport. The birthplace and birth month of all American players in the National Hockey League, National Basketball Association, Major League Baseball, and Professional Golfer's Association, and all Canadian players in the National Hockey League were collected from official websites. Monte Carlo simulations were used to verify if the birthplace of these professional athletes deviated in any systematic way from the official census population distribution, and chi-square analyses were conducted to determine whether the players' birth months were evenly distributed throughout the year. Results showed a birthplace bias towards smaller cities, with professional athletes being over-represented in cities of less than 500,000 and under-represented in cities of 500,000 and over. A birth month/relative age effect (in the form of a distinct bias towards elite athletes being relatively older than their peers) was found for hockey and baseball but not for basketball and golf. Comparative analyses suggested that contextual factors associated with place of birth contribute more influentially to the achievement of an elite level of sport performance than does relative age and that these factors are essentially independent in their influences on expertise development.

Yearbook.

List of members in each volume except 1929/30-1931/32.

Report of the proceedings of the second pre-conference workshop for librarians and rural sociologists, 1948.

Mode of access: Internet.