Sexismo: o papel da pornografia heteronormativa nas relações românticas

O estudo pretende compreender de que forma e em que aspetos o sexismo se perpetua por meio da pornografia heteronormativa nas relações românticas. A amostra é composta por 20 jovens adultos de ambos os sexos, com idades entre os 20 e os 34 anos inclusive, que tenham experienciado pelo menos uma relação romântica heterossexual no mínimo de 6 meses, tido relações sexuais, consumido conteúdos pornográficos heteronormativos e, assinarem o consentimento informado. Para a concretização do estudo foi construído um guião de entrevista. Foi seguida uma metodologia de análise fenomenológica interpretativa (IPA), sendo os dados tratados através do software Nvivo. Os resultados revelaram que o consumo de conteúdos pornográficos heteronormativos contribui para a propagação de aspetos sexistas e impacta as relações sexuais e românticas dos/as entrevistados/as. Porém, estes/as relatam um distanciamento entre este impacto nas relações em geral e as suas relações pessoais; - Sexism: The role of heteronormative pornography in romantic relationships - Abstract: The study aims to understand how and in what ways sexism is perpetuated in romantic relationships through heteronormative pornography. The sample consisted in 20 young adults of both sexes, between 20 and 35 years old, that have experienced at least one heterosexual romantic relationship for at least 6 months, have had sexual intercourse, consumed heteronormative pornography, and signed the informed consent. To carry out the study, it was developed an interview guide. An interpretative phenomenological analysis (IPA) methodology was followed, and the data was treated through Nvivo software. The results revealed that the consumption of heteronormative pornographic content contributes to the propagation of sexist aspects and impacts the sexual and romantic relationships of the interviewees. However, they report a detachment between this impact on relationships in general and their personal relationship

What is the best etching timing in a resin infiltrant used on enamel surface after remineralization with CPP-ACP?

Abstract in proceedings of the Fourth International Congress of CiiEM: Health, Well-Being and Ageing in the 21st Century, held at Egas Moniz’ University Campus in Monte de Caparica, Almada, from 3–5 June 2019.This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.info:eu-repo/semantics/publishedVersio

The low-mass content of the massive young star cluster RCW 38

KM acknowledges funding by the Joint Committee of ESO/Government of Chile, and by the Science and Technology Foundation of Portugal (FCT), grant no. IF/00194/2015. Part of the research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. [614922]. RJ acknowledges support from NSERC grants. JA acknowledges funding by the Science and Technology Foundation of Portugal (FCT), grant no. SFRH/BPD/101562/2014.RCW 38 is a deeply embedded young (∼1 Myr), massive star cluster located at a distance of 1.7 kpc. Twice as dense as the Orion nebula cluster, orders of magnitude denser than other nearby star-forming regions and rich in massive stars, RCW 38 is an ideal place to look for potential differences in brown dwarf formation efficiency as a function of environment. We present deep, high-resolution adaptive optics data of the central ∼0.5 × 0.5 pc2 obtained with NACO at the Very Large Telescope. Through comparison with evolutionary models, we determine masses and extinction for ∼480 candidate members, and derive the first initial mass function (IMF) of the cluster extending into the substellar regime. Representing the IMF as a set of power laws in the form dN/dM ∝ M−α, we derive the slope α = 1.60 ± 0.13 for the mass range 0.5–20 M⊙,which is shallower than the Salpeter slope, but in agreement with results in several other young massive clusters. At the low-mass side, we find α = 0.71 ± 0.11 for masses between 0.02 and 0.5 M⊙, or α = 0.81 ± 0.08 for masses between 0.02 and 1 M⊙. Our result is in agreement with the values found in other young star-forming regions, revealing no evidence that a combination of high stellar densities and the presence of numerous massive stars affects the formation efficiency of brown dwarfs and very-low-mass stars. We estimate that the Milky Way galaxy contains between 25 and 100 billion brown dwarfs (with masses >0.03 M⊙).Publisher PDFPeer reviewe

Novel and Modified Neutrophil Elastase Inhibitor Loaded in Topical Formulations for Psoriasis Management

© 2020 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license (http://creativecommons.org/licenses/by/4.0/).Human neutrophil elastase (HNE) is a serine protease that degrades matrix proteins. An excess of HNE may trigger several pathological conditions, such as psoriasis. In this work, we aimed to synthesize, characterize and formulate new HNE inhibitors with a 4-oxo-β-lactam scaffold with less toxicity, as well as therapeutic index in a psoriasis context. HNE inhibitors with 4-oxo-β-lactam scaffolds were synthesized and characterized by NMR, FTIR, melting point, mass spectrometry and elemental analysis. In vitro cytotoxicity and serine protease assays were performed. The compound with the highest cell viability (AAN-16) was selected to be incorporated in an emulsion (AAN-16 E) and in a microemulsion (AAN-16 ME). Formulations were characterized in terms of organoleptic properties, pH, rheology, droplet size distribution, in vitro drug release and in vivo psoriatic activity. All compounds were successfully synthesized according to analytical methodology, with good yields. Both formulations presented suitable physicochemical properties. AAN-16 E presented the most promising therapeutic effects in a murine model of psoriasis. Overall, new HNE inhibitors were synthesized with high and selective activity and incorporated into topical emulsions with potential to treat psoriasis.This work was supported by Fundação para a Ciência e a Tecnologia, Portugal (UID/DTP/04138/2019 to iMedUlisboa and and PTDC/MEC-DER/30198/2017) and Labodidática, Equipamentos de Laboratório e Didácticos L.da.info:eu-repo/semantics/publishedVersio

VISION - Vienna survey in Orion. III. Young stellar objects in Orion A

38 pages, 25 figures, Accepted for publication by A&A. Reproduced with permission from Astronomy & Astrophysics. © 2018 ESOWe extend and refine the existing young stellar object (YSO) catalogs for the Orion A molecular cloud, the closest massive star-forming region to Earth. This updated catalog is driven by the large spatial coverage (18.3 deg^2, ~950 pc^2), seeing limited resolution (~0.7''), and sensitivity (Ks<19 mag) of the ESO-VISTA near-infrared survey of the Orion A cloud (VISION). Combined with archival mid- to far-infrared data, the VISTA data allow for a refined and more robust source selection. We estimate that among previously known protostars and pre-main-sequence stars with disks, source contamination levels (false positives) are at least ∼7% and ∼2.5%, respectively, mostly due to background galaxies and nebulosities. We identify 274 new YSO candidates using VISTA/Spitzer based selections within previously analyzed regions, and VISTA/WISE based selections to add sources in the surroundings, beyond previously analyzed regions. The WISE selection method recovers about 59% of the known YSOs in Orion A's low-mass star-forming part L1641, which shows what can be achieved by the all-sky WISE survey in combination with deep near-infrared data in regions without the influence of massive stars. The new catalog contains 2978 YSOs, which were classified based on the de-reddened mid-infrared spectral index into 188 protostars, 184 flat-spectrum sources, and 2606 pre-main-sequence stars with circumstellar disks. We find a statistically significant difference in the spatial distribution of the three evolutionary classes with respect to regions of high dust column-density, confirming that flat-spectrum sources are at a younger evolutionary phase compared to Class IIs, and are not a sub-sample seen at particular viewing angles.Peer reviewedFinal Accepted Versio

3D shape of Orion A from Gaia DR2

Reproduced with permission from Astronomy & Astrophysics. © 2018 ESO.We use the Gaia DR2 distances of about 700 mid-infrared selected young stellar objects in the benchmark giant molecular cloud Orion A to infer its 3D shape and orientation. We find that Orion A is not the fairly straight filamentary cloud that we see in (2D) projection, but instead a cometary-like cloud oriented toward the Galactic plane, with two distinct components: a denser and enhanced star-forming (bent) Head, and a lower density and star-formation quieter ~75 pc long Tail. The true extent of Orion A is not the projected ~40 pc but ~90 pc, making it by far the largest molecular cloud in the local neighborhood. Its aspect ratio (~30:1) and high column-density fraction (~45%) make it similar to large-scale Milky Way filaments ("bones"), despite its distance to the galactic mid-plane being an order of magnitude larger than typically found for these structures.Peer reviewedFinal Accepted Versio

Propriedades métricas do Oxford Knee Score em pessoas com osteoartrite após artroplastia do joelho: Revisão Sistemática da Literatura

Objective: To evaluate the metric properties of the Oxford Knee Score applied in people with osteoarthritis after knee arthroplasty. Method: Systematic review of the literature. The EBSCOhost platform was used to access the MEDLINE and LILACS database and the SCiELO platform. The descriptors were validated on the DeCS and MESH platforms, except for "Oxford Knee Score" and "responsiveness". We selected articles published in the last five years, available in Portuguese, English and Spanish. Results: There were eight articles that revealed that OKS is a valid, reliable and reproducible instrument. Responsiveness was the least studied metric property. Conclusion: The Oxford Knee Scale is adequate to evaluate the functionality and the impact of pain in people with Osteoarthritis after knee arthroplasty.Objetivo: Evaluar las propiedades métricas de la Oxford Knee Score aplicada en personas con osteoartritis después de la artroplastia de la rodilla. Método: Revisión sistemática de la literatura. Se recurrió a la plataforma EBSCOhost que permitió acceder a la base de datos MEDLINE y LILACS y plataforma SCiELO. Los descriptores fueron validados en las plataformas DeCS y MESH, con excepción de "Oxford Knee Score" y "responsividad". Se seleccionaron los artículos publicados en los últimos cinco años, disponibles en Portugués, Inglés y Español. Resultados: Se han obtenido ocho artículos que revelaron que Oxford Knee Score es un instrumento válido, fiable y reproductivo. La responsividad fue la propiedad métrica menos estudiada. Conclusión: El Oxford Knee Score es adecuado para evaluar la funcionalidad y el impacto del dolor en personas con Osteoartritis después de la artroplastia de la rodilla.Objetivo: Avaliar as propriedades métricas da Oxford Knee Score aplicada em pessoas com osteoartrite após artroplastia do joelho. Método: Revisão sistemática da literatura. Recorreu-se à plataforma EBSCOhost que permitiu aceder à base de dados MEDLINE e LILACS e plataforma SCiELO. Os descritores foram validados nas plataformas DeCS e MESH, à exceção de “Oxford Knee Score” e “responsividade”. Foram selecionados artigos publicados nos últimos cinco anos, disponíveis em português, inglês e espanhol. Resultados: Obtiveram-se oito artigos que revelaram que o Oxford Knee Score é um instrumento válido, fiável e reprodutivo. A responsividade foi a propriedade métrica menos estuda. Conclusão: O Oxford Knee Score é adequado para avaliar a funcionalidade e o impato da dor em pessoas com Osteoartrite após atroplastia do joelho

VISIONS:the VISTA Star Formation Atlas I. Survey overview

VISIONS is an ESO public survey of five nearby (d &lt; 500 pc) star-forming molecular cloud complexes that are canonically associated with the constellations of Chamaeleon, Corona Australis, Lupus, Ophiuchus, and Orion. The survey was carried out with the Visible and Infrared Survey Telescope for Astronomy (VISTA), using the VISTA Infrared Camera (VIRCAM), and collected data in the near-infrared passbands J (1.25 μm), H (1.65 μm), and KS (2.15 μm). With a total on-sky exposure time of 49.4h VISIONS covers an area of 650 deg2, it is designed to build an infrared legacy archive with a structure and content similar to the Two Micron All Sky Survey (2MASS) for the screened star-forming regions. Taking place between April 2017 and March 2022, the observations yielded approximately 1.15 million images, which comprise 19 TB of raw data. The observations undertaken within the survey are grouped into three different subsurveys. First, the wide subsurvey comprises shallow, large-scale observations and it has revisited the star-forming complexes six times over the course of its execution. Second, the deep subsurvey of dedicated high-sensitivity observations has collected data on areas with the largest amounts of dust extinction. Third, the control subsurvey includes observations of areas of low-to-negligible dust extinction. Using this strategy, the VISIONS observation program offers multi-epoch position measurements, with the ability to access deeply embedded objects, and it provides a baseline for statistical comparisons and sample completeness – all at the same time. In particular, VISIONS is designed to measure the proper motions of point sources, with a precision of 1 mas yr−1 or better, when complemented with data from the VISTA Hemisphere Survey (VHS). In this way, VISIONS can provide proper motions of complete ensembles of embedded and low-mass objects, including sources inaccessible to the optical ESA Gaia mission. VISIONS will enable the community to address a variety of research topics from a more informed perspective, including the 3D distribution and motion of embedded stars and the nearby interstellar medium, the identification and characterization of young stellar objects, the formation and evolution of embedded stellar clusters and their initial mass function, as well as the characteristics of interstellar dust and the reddening law