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Search Results: 1 - 10 of 33 matches for " Busarello "
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IDENTIDADE COMO RELA O DE CONFLITO NA EDUCA O ESCOLAR INDIGENA
FLáVIA ROBERTA BUSARELLO,ERNESTO JACOB KEIM
Espa?o Ameríndio , 2011,
Abstract: This paper aims to analyze the relationship of identity, to understand how they can generate conflicts and prejudices and how education can interact as an agent to overcome these reactions that often undermine the dignity of life. This article was based on literature review and arguments in meetings for study and discussion of the Research Group EDUCOGITANS Philosophy and Education as well as meetings related to research funded by CAPES /FINEP, "Pedagogical-Didactic Planning and Intercultural Training of Teachers forthe revitalization of the language and culture in Indigenous Schools Xokleng Lakl n and howler in Santa Catarina, "linked to the Centre for Indigenous Education.
Fitting planes to early-type galaxies: MIST for the determination of the Fundamental Plane
F. La Barbera,G. Busarello,M. Capaccioli
Physics , 2000,
Abstract: The present study deals with the problem of deriving the coefficients of the fundamental plane (FP) of early-type galaxies. We introduce statistical models of the FP and relative fitting methods: the MIST (Measurement errors and Intrinsic Scatter Three dimensional) fits. The MIST fits account for the measurement errors on the variables and their correlations as well as for the intrinsic scatter. We show that the lack of a model of the intrinsic scatter of the FP is the origin of the systematic differences between the various fitting methods. We also address the problem of estimating the uncertainties of the FP coefficients and determine a simple relation between the sample size and the expected accuracy of the coefficients. The present study leads to define a `minimum sample size' for a correct estimate of the uncertainties. For N < 30, both theoretical formulae and re-sampling techniques, like the bootstrap, do not give reliable estimates. The question of the 'universality' of the FP is addressed by applying the MIST fits to ten samples of cluster galaxies. The FP slopes are actually consistent between the different samples, but, due to the large uncertainties, they could also hide significant systematic differences. The feasibility of the measurement of the possible variations of the FP slopes as a function of redshift is also proved.
UV--NIR Restframe Luminosity Functions of the Galaxy Cluster EIS0048 at z~0.64
M. Massarotti,G. Busarello,F. La Barbera,P. Merluzzi
Physics , 2002, DOI: 10.1051/0004-6361:20030473
Abstract: We derive the galaxy luminosity functions in V, R, I, and K bands of the cluster EIS 0048 at z~0.64 from data taken at the ESO Very Large Telescope. The data span the restframe wavelength range from UV, which is sensitive to even low rates of star formation, to the NIR, which maps the bulk of the stellar mass. By comparing our data and previous results with pure luminosity evolution models, we conclude that bright (M<= M^*+1) cluster galaxies are already assembled at z~1 and that star formation is almost completed at z~1.5.
Structure and Evolution of Galaxy Clusters: Internal Dynamics of ABCG 209 at z~0.21
A. Mercurio,M. Girardi,W. Boschin,P. Merluzzi,G. Busarello
Physics , 2002, DOI: 10.1051/0004-6361:20021495
Abstract: We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, sigma_v=1250-1400 Km/s, on the whole observed area (1 Mpc/h from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15 M_sun within the virial radius, assuming the dynamical equilibrium. The presence of a velocity gradient in the velocity field, the elongation in the spatial distribution of the colour-selected likely cluster members, the elongation of the X-ray contour levels in the Chandra image, and the elongation of cD galaxy show that ABCG 209 is characterised by a preferential NW-SE direction. We also find a significant deviation of the velocity distribution from a Gaussian, and relevant evidence of substructure and dynamical segregation. All these facts show that ABCG 209 is a strongly evolving cluster, possibly in an advanced phase of merging.
Extended stellar kinematics of elliptical galaxies in the Fornax cluster
Alister Graham,Matthew Colless,Giovanni Busarello,Simone Zaggia,G. Longo
Physics , 1998, DOI: 10.1051/aas:1998325
Abstract: We present extended stellar kinematics for a sample of 13 elliptical galaxies in the Fornax cluster. Major-axis velocity dispersion profiles (VDPs) and rotation curves (RCs) are given for 12 of the galaxies. A major feature of this data is the spatial extension: for 8 galaxies the data extends beyond 1 R_e, and for 5 it extends beyond 2 R_e. Compared to the previously available data, this corresponds to an increase in spatial coverage by a factor from 1 to 5. Five of the ellipticals in the sample turn out to be rotationally-supported systems, having positive rotation parameter log (V/sigma)*. One of these five, and another 3 galaxies from the remaining sample, display evidence for bar-like kinematics. The data indicate that the true number of `dynamically hot' stellar systems, is much lower than previously thought: of the Es in the present sample only 1/4 are confirmed as `pressure-supported' systems. The data reveal a host of individual peculiarities, like: wiggles, strong gradients, and asymmetries in the rotation curve and/or in the velocity dispersion profile, thus showing that the presence of kinematically distinct components and/or triaxiality is a common characteristic of this class of object.
The Colour-Magnitude Relation and the Age of Galaxies in the Cluster AC118 at z=0.31
P. Merluzzi,G. Busarello,M. Massarotti,F. La Barbera
Physics , 2001,
Abstract: We derive the Colour-Magnitude (CM) relation for the galaxy cluster AC118 at z=0.31 and use this relation to set constraints on the formation epoch and on the age spread of cluster galaxies in the framework of the passive evolution scenario. This work is based on observations at ESO NTT (OAC guaranteed time).
Optical (VRI) Photometry in the Field of the Galaxy Cluster AC 118 at z=0.31
G. Busarello,Merluzzi,F. La Barbera,M. Massarotti,M. Capaccioli
Physics , 2002, DOI: 10.1051/0004-6361:20020624
Abstract: We present new photometric V-, R- and I-band data for the rich galaxy cluster AC 118 at z=0.31. The new photometry covers an area of 8.6x8.6 arcmin$^2$, corresponding to 2.9$\times$2.9 Mpc$^2$ (H$_0=50$ km s$^{-1}$ Mpc$^{-1}$, q$_0=0.5$ and $\Lambda = 0$). The data have been collected for a project aimed at studying galaxy evolution through the color-magnitude relation and the fundamental plane. We provide a catalogue including all the sources (N = 1206) detected in the cluster field. The galaxy sample is complete to V=22.8 mag (N_gal=574), R=22.3 mag (N_gal=649) and I=20.8 mag (N_gal=419). We give aperture magnitudes within a fixed aperture of 4.4 arcsec and Kron magnitudes. We also give photometric redshifts for 459 sources for which additional U- and K-band photometry is available. We derive and discuss the V- and R-band luminosity functions. The catalogue, which is distributed in electronic form, is intended as a tool for studies in galaxy evolution.
Análise da eficácia do laser de baixa potência no tratamento da dor tendínea em ratos imunossuprimidos
Busarello, Fernanda de Oliveira;Artifon, Elisangela Lourdes;Loth, Eduardo Alexandre;Bertolini, Gladson Ricardo Flor;
Fisioterapia e Pesquisa , 2011, DOI: 10.1590/S1809-29502011000400007
Abstract: the commitment of immune system, which may be presented by individuals with chronic diseases, leading to a low immune response. one of the treatments used for acute injuries in tendons is the low-power laser, however there is a gap in relation to its use in immunosuppression. the objective of this study was to analyze if low-level laser therapy is effective for the treatment of pain in immunosuppressed rats subjected to trauma tendon. we used 23 male rats of wistar strain, divided randomly in three groups: control group, placebo and laser. the animals were immunosuppressed (by administration of cyclosporin a) and underwent right achilles tendon injury, with impact of about 0.40 j. for treatment, we used low-level laser, 670 nm, 30 mw and 2 j/cm2, during 3 days. pain assessment was performed by the functional incapacitation test and von frey filament digital. the results showed a reduction of functional pain and pressure pain on the plantar surface and the injured site (right achilles tendon) for the laser group. therefore, we concluded that the low-power laser is effective for reducing pain in immunosuppressed rats subjected to trauma tendon.
Análise do fluxo de caixa descontado: um estudo comparativo entre as proje es segundo dados históricos e dados corrigidos pela infla o
Crislaine Fávero Busarello,Deisy Cristina Corrêa Igarashi,Wagner Igarashi,Patrícia Cristina Vincenzi Lauer
ConTexto (Porto Alegre) , 2013,
Abstract: O fluxo de caixa descontado (DCF) segue uma estrutura pré-determinada e utiliza proje es e taxas a fim de auxiliar em decis es de avalia o de empresa. Apesar de o método ser indicado por especialistas, a literatura indica que a avalia o de uma empresa é considerada subjetiva, por se tratar de uma estimativa. O estudo tem por objetivo analisar se proje es do valor presente do Fluxo de Caixa Livre da Empresa (FCLE), realizadas de 2004 a 2010, via dados históricos e dados corrigidos pelo índice Nacional de Pre os ao Consumidor Amplo (IPCA), se confirmam em termos de compatibilidade com os resultados das empresas em 2010. Para isso, foram realizadas proje es considerando três momentos: a) proje o do DCF, como a literatura sugere e se procede ao realizar a avalia o das empresas, partindo do exercício de 2004; b) proje o conforme a infla o, que nesse caso foi adicionada a corre o ano a ano, segundo o IPCA; e c) cálculo do DCF utilizando os demonstrativos de 2004 a 2010. O estudo apresenta caráter descritivo e se desenvolve a partir da análise de conteúdo com abordagem qualitativa. Observou-se que as proje es realizadas ao longo de sete anos, segundo os cenários a e b, apresentam varia o quando comparados com o cenário c. Ficou evidenciado que apesar de a ferramenta se mostrar viável em termos de uso (operacionaliza o), os resultados da proje o quando comparado aos valores obtidos pela empresa ao longo dos exercícios n o se confirmam em termos de compatibilidade. Além disso, observou-se que a ado o do critério de corre o dos valores pelo IPCA n o minimizou tal varia o.
Age, Metallicity and Star Formation History of Cluster Galaxies at z~0.3 F
P. Merluzzi,F. La Barbera,M. Massarotti,G. Busarello,M. Capaccioli
Physics , 2002, DOI: 10.1086/374636
Abstract: We investigate the color-magnitude distribution in the rich cluster AC 118 at z=0.31. The sample is selected by the photometric redshift technique, allowing to study a wide range of properties of stellar populations, and is complete in the K-band, allowing to study these properties up to a given galaxy mass. We use galaxy templates based on population synthesis models to translate the physical properties of the stellar populations - formation epoch, time-scale of star formation, and metallicity - into observed magnitudes and colors. In this way we show that a sharp luminosity-metallicity relation is inferred without any assumption on the galaxy formation scenario (either monolithic or hierarchical). Our data exclude significant differences in star formation histories along the color-magnitude relation, and therefore confirm a pure metallicity interpretation for its origin, with an early (z~5) formation epoch for the bulk of stellar populations. The dispersion in the color-magnitude diagram implies that fainter galaxies in our sample (K~18) ceased to form stars as late as z~0.5, in agreement with the picture that these galaxies were recently accreted into the cluster environment. The trend with redshift of the total stellar mass shows that half of the luminous mass in AC 118 was already formed at $z~2, but also that 20% of the stars formed at z<1.
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