A EVOLUÇÃO DO DIREITO INTERNACIONAL E A PROTEÇÃO DA PESSOA HUMANA: UMA ANÁLISE A PARTIR DO SISTEMA INTERAMERICANO DE DIREITOS HUMANOS

O presente apresenta o percurso transcorrido desde as primeiras relações humanas que deram início ao que hoje conhecemos por sociedade internacional e a consolidação do Direito Internacional. Primeiramente, realiza-se um breve relato histórico-jurídico do desenvolvimento do direito internacional, de embrionário jus gentium até o atual momento de evolução em que se encontra: um direito cada vez mais rígido, vinculante e sofisticado. Em um segundo momento, destaca-se a importância da teoria do monismo internacionalista, dialogando-a com o fenômeno de internacionalização dos Direitos Humanos, conferindo-se especial atenção ao Sistema Interamericano de Direitos Humanos (SIDH) e avaliando como o sistema jurídico comporta-se no complexo mundo contemporâneo. Por fim, demonstra-se que o Sistema Interamericano de Direitos Humanos têm agido como promotor dos direitos em âmbito regional e internacional, desenvolvendo, validando e efetivando os direitos do âmbito externo para o interno, bem como evidenciando a necessária problematização da cidadania e sua formatação no contexto exposto. O método empregado é o hipotético-dedutivo, tendo como técnica de pesquisa a revisão bibliográfica

Seletividade de herbicidas aplicados em pré-emergência na cultura do crambe

In Brazil, there are no herbicides registered for crambe (Crambe abyssinica Hochst), and little is known about the selectivity of herbicides over this crop. Therefore, two experiments were conducted, simultaneously, in plastic green house, with the objective of evaluating the selectivity of herbicides sprayed in pre emergency over crambe crop initial development. In the first study, it was evaluated the answer-dose of herbicides treatments trifluralin (225, 450, 675 and 900 g ha-1), alachlor (240, 480, 720 and 960 g ha-1) and pendimethalin (250, 500, 750 and 1000 g ha-1), in factorial scheme (3x4) +1, represented by herbicides (three) and doses (four) factors and a check. In the second experiment, four herbicides tank mixtures were analyzed: trifluralin + alachlor (450+480 g ha-1), trifluralin + pendimethalin (450+500 g ha-1) and alachlor + pendimethalin (480+500 g ha-1) and a check. In both studies, vases containing 4 dm3 of soil were used in randomized entirely design with eight replications. Crambe crop was extremely sensitive to pre emergency herbicides evaluated. Only trifluralin, in doses inferior to 450 g ha-1 , demonstrated selective to crambe crop. Thus, it was evident the need for more comprehensive studies aimed to assessing the selectivity of herbicides to crambe crop.No Brasil não existem herbicidas registrados para o crambe (Crambe abyssinica Hochst), e pouco se sabe sobre a seletividade de herbicidas sobre essa cultura. Portanto, dois ensaios foram conduzidos simultaneamente em estufa plástica, com objetivo de avaliar a seletividade de herbicidas aplicados em pré-emergência no desenvolvimento inicial da cultura do crambe. No primeiro ensaio avaliou-se a dose-resposta dos tratamentos herbicidas trifluralin (225, 450, 675 e 900 g ha-1), alachlor (240, 480, 720 e 960 g ha-1) e pendimethalin (250, 500, 750 e 1000 g ha-1), em esquema fatorial (3x4)+1, representado pelos fatores herbicidas (três) e doses (quatro), e uma testemunha. No segundo ensaio foram avaliadas quatro misturas em tanque de herbicidas: trifluralin+alachlor (450+480 g ha-1), trifluralin+pendimethalin (450+500 g ha-1) e alachlor+pendimethalin (480+500 g ha-1) e uma testemunha. Em ambos ensaios utilizou-se vasos com capacidade de 4 dm3 de solo, em delineamento inteiramente casualizado, com oito repetições. A cultura do crambe mostrou-se extremamente sensível aos herbicidas pré-emergentes avaliados. Apenas o trifluralin, em doses inferiores a 450 g ha-1, demonstrou-se seletivo a cultura do crambe. Assim, ficou evidente a necessidade de estudos mais abrangentes que visem avaliar a seletividade de herbicidas à cultura do crambe

DIGESTIBILIDADE DA CANA-DE-ACÚCAR HIDROLISADA, IN NATURA E ENSILADA PARA BOVINOS

O objetivo deste trabalho foi determinar a digestibilidade ruminal in vitro da matéria seca (DIVMS), da fibra em detergente neutro (DIVFDN), da fibra em detergente ácido (DIVFDA) e da lignina (DIVL) de duas variedades (IAC 862480 e RB 835453) de cana-de-açúcar hidrolisadas com zero %, 0,5% e 1,0% de cal, durante três horas, in natura e ensiladas durante sessenta dias. Utilizou-se o delineamento inteiramente casualizado em esquema fatorial 3 x 2 x 2 com três repetições. Não houve influência dos níveis de cal na DIVFDA e da DIVL da cana-de-açúcar. As DIVMS, DIVFDA e da DIVL foram aumentadas em função dos níveis crescentes de cal, todavia, as médias de digestibilidade nos níveis de 0,5% e 1,0% assemelharam-se estatisticamente (P>0,05). A variedade IAC 862480 apresentou maior DIVMS, DIVFDN e da DIVFDA, considerando-se os níveis de cal utilizados, entretanto a DIVFDN foi maior apenas para a silagem de cana (

Chemodynamical Properties and Ages of Metal-Poor Stars in S-PLUS

Metal-poor stars are key to our understanding of the early stages of chemical evolution in the Universe. New multi-filter surveys, such as the Southern Photometric Local Universe Survey (S-PLUS), are greatly advancing our ability to select low-metallicity stars. In this work, we analyse the chemodynamical properties and ages of 522 metal-poor candidates selected from the S-PLUS data release 3. About 92% of these stars were confirmed to be metal-poor ([Fe/H] $\leq -1$) based on previous medium-resolution spectroscopy. We calculated the dynamical properties of a subsample containing 241 stars, using the astrometry from Gaia Data Release 3. Stellar ages are estimated by a Bayesian isochronal method formalized in this work. We analyse the metallicity distribution of these metal-poor candidates separated into different subgroups of total velocity, dynamical properties, and ages. Our results are used to propose further restrictions to optimize the selection of metal-poor candidates in S-PLUS. The proposed astrometric selection ($\mathrm{parallax}>0.85$ mas) is the one that returns the highest fraction of extremely metal-poor stars (16.3% have [Fe/H] $\leq -3$); the combined selection provides the highest fraction of very metal-poor stars (91.0% have [Fe/H] $\leq -2$), whereas the dynamical selection (eccentricity > 0.35 and diskness < 0.75) is better for targetting metal-poor (99.5% have [Fe/H] $\leq -1$). Using only S-PLUS photometric selections, it is possible to achieve selection fractions of 15.6%, 88.5% and 98.3% for metallicities below $-$3, $-$2 and $-$1, respectively. We also show that it is possible to use S-PLUS to target metal-poor stars in halo substructures such as Gaia-Sausage/Enceladus, Sequoia, Thamnos and the Helmi stream.Comment: 18 pages, 13 figures. To be published in MNRAS main journal (accepted 15-may-2023

S-PLUS : exploring wide field properties of multiple populations in galactic globular clusters at different metallicities

Multiple stellar populations (MSPs) are a ubiquitous phenomenon in Galactic globular clusters (GCs). By probing different spectral ranges affected by different absorption lines using the multiband photometric survey S-PLUS, we study four GCs – NGC 104, NGC 288, NGC 3201, and NGC 7089 – that span a wide range of metallicities. With the combination of broad and narrow-band photometry in 12 different filters from 3485A (u) to 9114A (z), we identified MSPs along the rectified red-giant branch in colour–magnitude diagrams and separated them using a K-means clustering algorithm. Additionally, we take advantage of the large Field of View of the S-PLUS detector to investigate radial trends in our sample. We report on six colour combinations that can be used to successfully identify two stellar populations in all studied clusters and show that they can be characterized as Na-rich and Na-poor. For both NGC 288 and NGC 7089, their radial profiles show a clear concentration of 2P population. This directly supports the formation theories that propose an enrichment of the intra-cluster medium and subsequent star formation in the more dense central regions. However, in the case of NGC 3201, the trend is reversed. The 1P is more centrally concentrated, in direct contradiction with previous literature studies. NGC 104 shows a well-mixed population. We also constructed radial profiles up to 1 half-light radius of the clusters with HST data to highlight that radial differences are lost in the inner regions of the GCs and that wide-field studies are essential when studying this

Ages and metallicities of stellar clusters using S-PLUS narrow-band integrated photometry: the Small Magellanic Cloud

The Magellanic Clouds are the most massive and closest satellite galaxies of the Milky Way, with stars covering ages from a few Myr up to 13 Gyr. This makes them important for validating integrated light methods to study stellar populations and star-formation processes, which can be applied to more distant galaxies. We characterized a set of stellar clusters in the Small Magellanic Cloud (SMC), using the $\textit{Southern Photometric Local Universe Survey}$. This is the first age (metallicity) determination for 11 (65) clusters of this sample. Through its 7 narrow bands, centered on important spectral features, and 5 broad bands, we can retrieve detailed information about stellar populations. We obtained ages and metallicities for all stellar clusters using the Bayesian spectral energy distribution fitting code $\texttt{BAGPIPES}$. With a sample of clusters in the color range $-0.20 < r-z < +0.35$, for which our determined parameters are most reliable, we modeled the age-metallicity relation of SMC. At any given age, the metallicities of SMC clusters are lower than those of both the Gaia Sausage-Enceladus disrupted dwarf galaxy and the Milky Way. In comparison with literature values, differences are $\Delta$log(age)$\approx0.31$ and $\Delta$[Fe/H]$\approx0.41$, which is comparable to low-resolution spectroscopy of individual stars. Finally, we confirm a previously known gradient, with younger clusters in the center and older ones preferentially located in the outermost regions. On the other hand, we found no evidence of a significant metallicity gradient.Comment: 12 pages, 11 figure

Galaxy evolution in compact groups I: Revealing a transitional galaxy population through a multiwavelength approach

Compact groups of galaxies (CGs) show members with morphological disturbances, mainly products of galaxy-galaxy interactions, thus making them ideal systems to study galaxy evolution, in high-density environment. To understand how this environment affects the properties of galaxies, we select a sample of 340 CGs in the Stripe 82 region, for a total of 1083 galaxies, and a sample of 2281 field galaxies as a control sample. By performing a multi-wavelength morphological fitting process using S-PLUS data, we divide our sample into early-type (ETG), late-type (LTG), and transition galaxies using the r-band S\'ersic index and the colour (u-r). We find a bimodal distribution in the plane of the effective radius-S\'ersic index, where a secondary "peculiar" galaxy population of smaller and more compact galaxies is found in CGs, which is not observed in the control sample. This indicates that galaxies are undergoing a morphological transformation in CGs. In addition, we find significant statistical differences in the distribution of specific Star Formation Rate (sSFR) when we compare both environments for LTGs and ETGs. We also find a higher fraction of quenched galaxies and a lower median sSFR in CGs than in the control sample, suggesting the existence of environmental effects favoring the cessation of star formation, regardless of galaxy type. Our results support the notion that CGs promote morphological and physical transformations, highlighting their potential as ideal systems for galaxy pre-processing.Comment: 17 pages, 15 figures. Accepted for publication in MNRA

Identification of strain-specific B-cell epitopes in Trypanosoma cruzi using genome-scale epitope prediction and high-throughput immunoscreening with peptide arrays

BACKGROUND: The factors influencing variation in the clinical forms of Chagas disease have not been elucidated; however, it is likely that the genetics of both the host and the parasite are involved. Several studies have attempted to correlate the T. cruzi strains involved in infection with the clinical forms of the disease by using hemoculture and/or PCR-based genotyping of parasites from infected human tissues. However, both techniques have limitations that hamper the analysis of large numbers of samples. The goal of this work was to identify conserved and polymorphic linear B-cell epitopes of T. cruzi that could be used for serodiagnosis and serotyping of Chagas disease using ELISA. METHODOLOGY: By performing B-cell epitope prediction on proteins derived from pair of alleles of the hybrid CL Brener genome, we have identified conserved and polymorphic epitopes in the two CL Brener haplotypes. The rationale underlying this strategy is that, because CL Brener is a recent hybrid between the TcII and TcIII DTUs (discrete typing units), it is likely that polymorphic epitopes in pairs of alleles could also be polymorphic in the parental genotypes. We excluded sequences that are also present in the Leishmania major, L. infantum, L. braziliensis and T. brucei genomes to minimize the chance of cross-reactivity. A peptide array containing 150 peptides was covalently linked to a cellulose membrane, and the reactivity of the peptides was tested using sera from C57BL/6 mice chronically infected with the Colombiana (TcI) and CL Brener (TcVI) clones and Y (TcII) strain. FINDINGS AND CONCLUSIONS: A total of 36 peptides were considered reactive, and the cross-reactivity among the strains is in agreement with the evolutionary origin of the different T. cruzi DTUs. Four peptides were tested against a panel of chagasic patients using ELISA. A conserved peptide showed 95.8% sensitivity, 88.5% specificity, and 92.7% accuracy for the identification of T. cruzi in patients infected with different strains of the parasite. Therefore, this peptide, in association with other T. cruzi antigens, may improve Chagas disease serodiagnosis. Together, three polymorphic epitopes were able to discriminate between the three parasite strains used in this study and are thus potential targets for Chagas disease serotyping

J-PLUS: A wide-field multi-band study of the M15 globular cluster. Evidence of multiple stellar populations in the RGB

The Javalambre Photometric Local Universe Survey (J-PLUS) provides wide field-of-view images in 12 narrow, intermediate and broad-band filters optimized for stellar photometry. Here we have applied J-PLUS data for the first time for the study of Galactic GCs using science verification data obtained for the very metal-poor GC M\,15. Our J-PLUS data provide low-resolution spectral energy distributions covering the near-UV to the near-IR, allowing us to search for MPs based on pseudo-spectral fitting diagnostics. J-PLUS CMDs are found to be particularly useful to search for splits in the sequences formed by the upper red giant branch (RGB) and asymptotic giant branch (AGB) stars. We interpret these split sequences as evidence for the presence of MPs. This demonstrates that the J-PLUS survey will have sufficient spatial coverage and spectral resolution to perform a large statistical study of GCs through multi-band photometry in the coming years.Comment: 11 pages, 11 figures. Accepted for publication @ A&

Galaxy evolution in compact groups II. Witnessing the influence of major structures in their evolution

Fil: Parado Montaguth, Gissel Dayana. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Antonela, Monachesi. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Sergio, Torres-Flores. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Gomez, Facundo Ariel. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Ciria, Lima-Dias. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Ciria, Lima-Dias. Universidad de La Serena. Instituto Multidisciplinario de Investigación y Postgrado; Chile.Fil: O’Mill, Ana Laura. Consejo Nacional de Investigaciones Científicas y Técnicas. Instituto de Astronomía Teórica y Experimental; Argentina.Fil: O’Mill, Ana Laura. Universidad Nacional Córdoba. Observatorio Astronómico de Córdoba; Argentina.Fil: Olave-Rojas, Daniela E. Universidad de Talca. Facultad de Ingeniería. Departamento de Tecnologías Industriales; Chile.Fil: Ricardo, Demarco. Universidad Andrés Bello. Facultad de Ciencias Exactas. Instituto de Astrofísica; Chile.Fil: Antonio, Kanaan. Universidade Federal de Santa Catarina. Departamento de Física ; Brazil.Fil: Tiago, Ribeiro. National Optical Astronomy Observatory; Estados Unidos.Fil: William, Schoenell. GMTO Corporation; Estados Unidos.Fil: Cortesi, Arianna. Universidade Federal do Rio de Janeiro. Observatório do Valongo; Brazil.Fil: Claudia, Mendes de Oliveira. Universidade de São Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brazil.Fil: Eduardo, Telles. Ministério da Ciência, Tecnologia e Inovação. Observatório Nacional; Brazil.Fil: Swayamtrupta, Panda . Ministério da Ciência, Tecnologia e Inovação. Laboratório Nacional de Astrofísica; Brazil.Fil: Marco, Grossi. Universidade Federal do Rio de Janeiro. Observatório do Valongo; Brazil.Fil: Augusto Lopes, Paulo Afrânio. Universidade Federal do Rio de Janeiro. Observatório do Valongo; Brazil.Fil: Hernandez-Jimenez, Jose A. Universidade do Vale do Paraíba; Brazil.Compact groups (CGs) of galaxies are an extreme environment for the morphological transformations and the cessation of star formation in galaxies. However, despite initially being conceived as isolated systems, it is now widely recognised that many of them are not as isolated as expected. Our objective is to understand the dynamics of CGs, as well as how the environment surrounding CGs impacts their morphological and physical properties. To achieve this, we selected a sample of 340 CGs in the Stripe 82 region, with a total of 1083 galaxies, and a sample of 2281 field galaxies as a control sample. We find that at least 27% of our sample of CGs are part of major structures, i.e. non-isolated CGs. We find a bimodality in the effective radius (Re)-Sérsic index (n) plane for all transition galaxies (those with (u − r) > 2.3 and n < 2.5) in CGs. Additionally, transition galaxies in isolated CGs populate more densely the Re − n plane for n < 1.75. In contrast, transition galaxies in non-isolated CGs have smoothly increasing n values, suggesting these galaxies have already suffered morphological transformation, and primarily contribute to the distribution of more compact galaxies in the Re−n plane for all transition galaxies in CGs. We also find significant differences in the specific star-formation rate (sSFR) distribution between the late-type galaxies (LTGs) (those with (u − r) < 2.3 and n < 2.5) in non-isolated CGs and the same type of galaxies in the control sample, suggesting that the evolution of LTGs differs in non-isolated CGs. Moreover, Early-type galaxies (those with (u − r) > 2.3 and n > 2.5) and transition galaxies in non-isolated CGs have lower sSFR values and a higher fraction of quenched galaxies, compared to those in isolated CGs. Based on our results, we propose an evolutionary scenario where the major structures in which the CGs are embedded accelerate the morphological transformations of their galaxy members, and also facilitates preprocessing. Our findings highlight the importance of considering the larger structures in which CGs may be located, when analysing the properties of their galaxy members, as this can significantly affect the evolution of CGs and their galaxies.info:eu-repo/semantics/acceptedVersionFil: Parado Montaguth, Gissel Dayana. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Antonela, Monachesi. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Sergio, Torres-Flores. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Gomez, Facundo Ariel. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Ciria, Lima-Dias. Universidad de La Serena. Departamento de Astronomía; Chile.Fil: Ciria, Lima-Dias. Universidad de La Serena. Instituto Multidisciplinario de Investigación y Postgrado; Chile.Fil: O’Mill, Ana Laura. Consejo Nacional de Investigaciones Científicas y Técnicas. Instituto de Astronomía Teórica y Experimental; Argentina.Fil: O’Mill, Ana Laura. Universidad Nacional Córdoba. Observatorio Astronómico de Córdoba; Argentina.Fil: Olave-Rojas, Daniela E. Universidad de Talca. Facultad de Ingeniería. Departamento de Tecnologías Industriales; Chile.Fil: Ricardo, Demarco. Universidad Andrés Bello. Facultad de Ciencias Exactas. Instituto de Astrofísica; Chile.Fil: Antonio, Kanaan. Universidade Federal de Santa Catarina. Departamento de Física ; Brazil.Fil: Tiago, Ribeiro. National Optical Astronomy Observatory; Estados Unidos.Fil: William, Schoenell. GMTO Corporation; Estados Unidos.Fil: Cortesi, Arianna. Universidade Federal do Rio de Janeiro. Observatório do Valongo; Brazil.Fil: Claudia, Mendes de Oliveira. Universidade de São Paulo. Instituto de Astronomia, Geofísica e Ciências Atmosféricas; Brazil.Fil: Eduardo, Telles. Ministério da Ciência, Tecnologia e Inovação. Observatório Nacional; Brazil.Fil: Swayamtrupta, Panda . Ministério da Ciência, Tecnologia e Inovação. Laboratório Nacional de Astrofísica; Brazil.Fil: Marco, Grossi. Universidade Federal do Rio de Janeiro. Observatório do Valongo; Brazil.Fil: Augusto Lopes, Paulo Afrânio. Universidade Federal do Rio de Janeiro. Observatório do Valongo; Brazil.Fil: Hernandez-Jimenez, Jose A. Universidade do Vale do Paraíba; Brazil