This thesis presents deep photometry of the globular cluster system of the massive elliptical galaxy, M49. Using the C and T1 Washington filters from the MOSAIC camera on the Cerro Tololo Inter-American Observatory 4m telescope, we studied the color, metallicity and luminosity distributions of the globular cluster system. We find a strong bimodality in the color and metallicity distributions of the globular cluster system down to a magnitude of R <24, with 1718 clusters belonging to the blue population and 698 to the red population. In agreement with previous studies, the blue sequence does not exhibit a strong mass-metallicity relation. No difference is found in the mass-metallicity relation between the inner and outer clusters of M49. These results suggest that the mechanism responsible for the mass-metallicity re- lation is not local and may be affected by the galaxy’s individual dynamic history, location in the galaxy cluster and the formation of the globular cluster system itself. We suggest a mechanism based on accretion of gas by proto-clusters as they orbit within their parent dwarf galaxies. The latter would fit the observed behavior of the MMR. / Thesis / Master of Science (MSc)

No description available.

Recent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this "iron-complex" cluster class, and we provide here a chemical and kinematic analysis of > 300 red giant branch and asymptotic giant branch member stars using high-resolution spectra obtained with the Magellan-M2FS and VLT-FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that ranges from about [Fe/H] = -2 to -1 dex, and may include at least three populations with different [Fe/H] values. The three populations identified here contain separate first (Na/Al-poor) and second (Na/Al-rich) generation stars, but a Mg-Al anti-correlation may only be present in stars with [Fe/H] greater than or similar to -1.65. The strong correlation between [La/Eu] and [Fe/H] suggests that the sprocess must have dominated the heavy element enrichment at higher metallicities. A small group of stars with low [alpha/Fe] is identified and may have been accreted from a former surrounding field star population. The cluster's large abundance variations are coupled with a complex, extended, and multimodal blue horizontal branch (HB). The HB morphology and chemical abundances suggest that NGC 6273 may have an origin that is similar to omega Cen and M54.

O objetivo do presente trabalho, consistiu na obtenção de ferro fundidos nodulares, a serem utilizados na fabricação de eixos, com as seguintes características mecânicas após os tratamentos térmicos adequados: limites de resistência à tração e escoamento mínimos de 700 N/mm2 e 450 N/mm2 respectivamente, alongamento mínimo de 5% e dureza entre 235 à 285 HB. A microestrutura mais adequada à obtenção das características mecânicas desejadas deveria consistir de cementita esferoidizada numa matriz ferrítica, a ser obtida com o tratamento de recozimento ou revenimento de microestruturas previamente perlíticas ou martensíticas, respectivamente. No caso do tratamento de recozimento, as estruturas iniciais consistiram de perlita grossa mais ferrita, presentes no material no estado bruto de fusão, ou, de perlita fina mais ferrita, do material normalizado. Todos os tratamentos térmicos utilizados, dependendo do tempo de tratamento, permitiram a obtenção de cementita esferoidizada. O material normalizado e recozido durante 2 horas a 700ºC, possibilitou a obtenção das propriedades mecânicas desejadas: limites de resistência à tração e de escoamento de 827 N/mm2 e 547 N/mm2 respectivamente, alongamento de 7% e dureza de 277 HB, valores estes, dentro dos limites desejados no presente trabalho. No caso do material temperado e revenido a 700ºC durante 0,5 hora, obteve-se limites de escoamento de 542 N/mm2, alongamento de 6% e dureza de 246 HB. O tratamento de recozimento realizado durante 48 horas, produziu microestrutura quase totalmente ferrítica, com pequenas áreas de agregados de carbonetos. O restante do carbono migrou para os nódulos de grafita secundária ao redor dos mesmos. / The purpose of the present work, consisted in obtaining ductile casting iron, that will be used in the shaft production, with de following mechanical properties after the appropriated heat treatments: ultimate tensile strength and yield strength values of 700 N/mm2 and 450 N/mm2 minimum respectively, elongation of 5% minimum and hardness value from 235 to 285 HB. The microstructure more adequated to obtaining the desired mechanical characteristics should consist of spheroidized cementite in a ferritic matrix, to be obtained with the annealing or tempering treatments of microstructures previously pearlitic or martensitic respectively. In the case of the annealing treatment, the initial structures consisted of thick pearlite plus ferrite, wich were in the material in the ascast state, or fine pearlite plus ferrite, of the normalized material. All the used heat treatment, depending on the time of treatment, allowed the obtainment of spheroidized cementite. The material normalized and annealed for 2 hours at 700°C made possible the obtaining of the desired mechanical properties: ultimate tensile strength and yield strength value of 827 N/mm2 and 547 N/mm2 respectively, elongation of 7% and hardness values of 277 HB, values these, in acordance with the aims initially proposed in the present work. In the case of the material quenched and tempered at 700°C for 0,5 hour, it was obtained yield strength values of 542 N/mm2, elongation of 6% and hardness value of 246 HB. The annealing treatment made during 48 hours, produced a microstructure almost totally ferritic, with small areas of aggregated carbides. The remaining of the carbon migrated to the graphite nodules producing secondary graphite around them.

Neste trabalho, estudamos dois aglomerados globulares, o NGC 6397 com módulo de distância (m- M) = 12,03 ± 0,06 mag e o NGC288 com módulo de distância (m- M) = 14,57 ± 0,08 mag. Para o NGC6397, realizamos um estudo fotométrico em UBV com dados do ESO-VLT, obtendo a função de luminosidade corrigida por completeza. Observamos que próximo à região cent ral do aglomerado, a função de luminosidade apresenta uma maior densidade de estrelas brilhantes do que a região mais externa. Calculamos os modelos projetado e deprojetado cobrindo todo o aglomerado. As formas dos perfis de brilho de superfície e densidade de número mostraram redução de luminosidade, demonstrando assim a segregação de massa. Assumindo a massa média total, estimamos o número de estrelas deste aglomerado. Para as séries temporais obtidas com o ESO-VLT, com rv 11 h de imagens fotométricas ut ilizando o imageador FORS2 distríbuidas ao longo de duas noites consecut ivas, realizamos uma inspeção no aglomerado globular NGC 6397 para determinar a fração de estrelas variáveis. Analisando 9 868 curvas de luz de estrelas mais brilhantes do que magtútude 23 no filtro 465-nm, identificamos 412 novas estrelas variáveis com escala de tempos entre 0,004 e 2 dias. Além disso, realizamos uma análise da. já conhecida binária eclipsante V4 no NGC6397, obtendo massas Mp = 0,76 ± 0,02 M0 e Ms = 0,73 ± 0,02 M0 para as componentes primária e secundária e raios de Rp = 1,01± 0,10 R0 and Rp = 0,99 ± 0,10 R0. Analisando curvas de luz de 12 438 estrelas do NGC 288, descobrimos duas novas estrelas variáveis. Pela posição no Diagrama Cor-Magtútude, pelas características de variabilidade, classificamos as novas estrelas como SX Phe. Utilizamos os períodos de seis SX Phe já conhecidas anteriormente e das duas novas descobertas para. estudar a relação período-luminosidade. / In t his work, we studied two globular clusters, NGC 6397 with distance modulus (m-M) = 12.03 ± 0.06 mag and the NGC 288 with distance modulus (m-M) = 14.57 ± 0.08 mag. For NGC6397, we conducted a UBV photometric study with ESO-VLT data, obtaining the luminosity function corrected for completeness. We observe that near the central region of the cluster, the luminosity function has a greater density than the bright stars in the externai region. We estimate the models projected and deprojected covering ali cluster. T he shapes of surface brightness profiles and number density showed reduced luminosity, thus demonstrating the mass segregation. Assuming the average total mass, we estimate the number of stars of this cluster. For the t ime series obtained with the ESO-VLT, with rv 11 h photometric images using imaging FORS2 distributed over two consecut ive nights, we detennined the fraction of variable stars with mass. Analyzing 9 868 light cmves of stars brighter than magnitude 23 in the filter 465-nm, we identified 412 new variable stars with scale t imes between 0.004 and 2days. In addit ion, we analysed of aJready known eclipsing binary V4 in NGC6397, obtaining masses Mp = 0.76 ± 0.02 M0 and Ms = 0.73 ± 0.02!\,10 for the primary and secondary components and radii R,= 1.01± 0. 10~ and R,= 0.99 ± 0. 1 0~. AnaJyzing 12438 light cmves of NGC 288 stru·s , we discovered two new vru·iable stars. The position in the CMD and the chru·acteristics variabilit ies, we classified the new stru·s as SX Phe. We use the redetermined periods of six SX Phe already known and two new discoveries to study the period-lmn inosity relation.

Detailed chemical abundances of globular clusters in the Milky Way and M31 (the Andromeda Galaxy) are presented based on analyses of high resolution spectra. The unusual Milky Way cluster Palomar 1 (Pal 1) is studied through spectra of individual red giant branch stars; these abundances show that Pal 1 is not a classical globular cluster, and may have been accreted from a dwarf satellite of the Milky Way. The Milky Way globular clusters 47 Tuc, M3, M13, NGC 7006, and M15 are studied through their integrated light (i.e. a single spectrum is obtained for each cluster) in order to test high resolution integrated light analyses. The integrated abundances from these clusters reproduce the average abundances from individual stellar analyses for elements that do not vary within a cluster (e.g. Fe, Ca, and Ni). For elements that do vary within the clusters (e.g. Na and Mg) the integrated abundances fall within the observed ranges from individual stars. Certain abundance ratios are found to be extremely sensitive to uncertainties in the underlying stellar populations, such as input models, empirical relations to determine atmospheric parameters, interloping field stars, etc., while others (such as [Ca I/Fe I]) are largely insensitive to these effects. With these constraints on the accuracy and precision of high resolution integrated light analyses, detailed abundances are obtained for seven clusters in the outer halo of M31 that were recently discovered in the Pan-Andromeda Archaeological Survey (PAndAS) and are likely to have originated in dwarf galaxy satellites. Three clusters are relatively metal rich ([Fe/H] > −1.5) for their locations in the outer halo; their chemical abundances suggest that they likely originated in one or more fairly massive dwarf satellities. The other four are more metal-poor, and may have originated in less massive dwarf satellites. These results indicate that the Milky Way and M31 have both experienced some amount of accretion from dwarf satellites, though M31 may have had a more active accretion history. / Graduate

Neste trabalho, estudamos dois aglomerados globulares, o NGC 6397 com módulo de distância (m- M) = 12,03 ± 0,06 mag e o NGC288 com módulo de distância (m- M) = 14,57 ± 0,08 mag. Para o NGC6397, realizamos um estudo fotométrico em UBV com dados do ESO-VLT, obtendo a função de luminosidade corrigida por completeza. Observamos que próximo à região cent ral do aglomerado, a função de luminosidade apresenta uma maior densidade de estrelas brilhantes do que a região mais externa. Calculamos os modelos projetado e deprojetado cobrindo todo o aglomerado. As formas dos perfis de brilho de superfície e densidade de número mostraram redução de luminosidade, demonstrando assim a segregação de massa. Assumindo a massa média total, estimamos o número de estrelas deste aglomerado. Para as séries temporais obtidas com o ESO-VLT, com rv 11 h de imagens fotométricas ut ilizando o imageador FORS2 distríbuidas ao longo de duas noites consecut ivas, realizamos uma inspeção no aglomerado globular NGC 6397 para determinar a fração de estrelas variáveis. Analisando 9 868 curvas de luz de estrelas mais brilhantes do que magtútude 23 no filtro 465-nm, identificamos 412 novas estrelas variáveis com escala de tempos entre 0,004 e 2 dias. Além disso, realizamos uma análise da. já conhecida binária eclipsante V4 no NGC6397, obtendo massas Mp = 0,76 ± 0,02 M0 e Ms = 0,73 ± 0,02 M0 para as componentes primária e secundária e raios de Rp = 1,01± 0,10 R0 and Rp = 0,99 ± 0,10 R0. Analisando curvas de luz de 12 438 estrelas do NGC 288, descobrimos duas novas estrelas variáveis. Pela posição no Diagrama Cor-Magtútude, pelas características de variabilidade, classificamos as novas estrelas como SX Phe. Utilizamos os períodos de seis SX Phe já conhecidas anteriormente e das duas novas descobertas para. estudar a relação período-luminosidade. / In t his work, we studied two globular clusters, NGC 6397 with distance modulus (m-M) = 12.03 ± 0.06 mag and the NGC 288 with distance modulus (m-M) = 14.57 ± 0.08 mag. For NGC6397, we conducted a UBV photometric study with ESO-VLT data, obtaining the luminosity function corrected for completeness. We observe that near the central region of the cluster, the luminosity function has a greater density than the bright stars in the externai region. We estimate the models projected and deprojected covering ali cluster. T he shapes of surface brightness profiles and number density showed reduced luminosity, thus demonstrating the mass segregation. Assuming the average total mass, we estimate the number of stars of this cluster. For the t ime series obtained with the ESO-VLT, with rv 11 h photometric images using imaging FORS2 distributed over two consecut ive nights, we detennined the fraction of variable stars with mass. Analyzing 9 868 light cmves of stars brighter than magnitude 23 in the filter 465-nm, we identified 412 new variable stars with scale t imes between 0.004 and 2days. In addit ion, we analysed of aJready known eclipsing binary V4 in NGC6397, obtaining masses Mp = 0.76 ± 0.02 M0 and Ms = 0.73 ± 0.02!\,10 for the primary and secondary components and radii R,= 1.01± 0. 10~ and R,= 0.99 ± 0. 1 0~. AnaJyzing 12438 light cmves of NGC 288 stru·s , we discovered two new vru·iable stars. The position in the CMD and the chru·acteristics variabilit ies, we classified the new stru·s as SX Phe. We use the redetermined periods of six SX Phe already known and two new discoveries to study the period-lmn inosity relation.

Neste trabalho, estudamos dois aglomerados globulares, o NGC 6397 com módulo de distância (m- M) = 12,03 ± 0,06 mag e o NGC288 com módulo de distância (m- M) = 14,57 ± 0,08 mag. Para o NGC6397, realizamos um estudo fotométrico em UBV com dados do ESO-VLT, obtendo a função de luminosidade corrigida por completeza. Observamos que próximo à região cent ral do aglomerado, a função de luminosidade apresenta uma maior densidade de estrelas brilhantes do que a região mais externa. Calculamos os modelos projetado e deprojetado cobrindo todo o aglomerado. As formas dos perfis de brilho de superfície e densidade de número mostraram redução de luminosidade, demonstrando assim a segregação de massa. Assumindo a massa média total, estimamos o número de estrelas deste aglomerado. Para as séries temporais obtidas com o ESO-VLT, com rv 11 h de imagens fotométricas ut ilizando o imageador FORS2 distríbuidas ao longo de duas noites consecut ivas, realizamos uma inspeção no aglomerado globular NGC 6397 para determinar a fração de estrelas variáveis. Analisando 9 868 curvas de luz de estrelas mais brilhantes do que magtútude 23 no filtro 465-nm, identificamos 412 novas estrelas variáveis com escala de tempos entre 0,004 e 2 dias. Além disso, realizamos uma análise da. já conhecida binária eclipsante V4 no NGC6397, obtendo massas Mp = 0,76 ± 0,02 M0 e Ms = 0,73 ± 0,02 M0 para as componentes primária e secundária e raios de Rp = 1,01± 0,10 R0 and Rp = 0,99 ± 0,10 R0. Analisando curvas de luz de 12 438 estrelas do NGC 288, descobrimos duas novas estrelas variáveis. Pela posição no Diagrama Cor-Magtútude, pelas características de variabilidade, classificamos as novas estrelas como SX Phe. Utilizamos os períodos de seis SX Phe já conhecidas anteriormente e das duas novas descobertas para. estudar a relação período-luminosidade. / In t his work, we studied two globular clusters, NGC 6397 with distance modulus (m-M) = 12.03 ± 0.06 mag and the NGC 288 with distance modulus (m-M) = 14.57 ± 0.08 mag. For NGC6397, we conducted a UBV photometric study with ESO-VLT data, obtaining the luminosity function corrected for completeness. We observe that near the central region of the cluster, the luminosity function has a greater density than the bright stars in the externai region. We estimate the models projected and deprojected covering ali cluster. T he shapes of surface brightness profiles and number density showed reduced luminosity, thus demonstrating the mass segregation. Assuming the average total mass, we estimate the number of stars of this cluster. For the t ime series obtained with the ESO-VLT, with rv 11 h photometric images using imaging FORS2 distributed over two consecut ive nights, we detennined the fraction of variable stars with mass. Analyzing 9 868 light cmves of stars brighter than magnitude 23 in the filter 465-nm, we identified 412 new variable stars with scale t imes between 0.004 and 2days. In addit ion, we analysed of aJready known eclipsing binary V4 in NGC6397, obtaining masses Mp = 0.76 ± 0.02 M0 and Ms = 0.73 ± 0.02!\,10 for the primary and secondary components and radii R,= 1.01± 0. 10~ and R,= 0.99 ± 0. 1 0~. AnaJyzing 12438 light cmves of NGC 288 stru·s , we discovered two new vru·iable stars. The position in the CMD and the chru·acteristics variabilit ies, we classified the new stru·s as SX Phe. We use the redetermined periods of six SX Phe already known and two new discoveries to study the period-lmn inosity relation.

O objetivo do presente trabalho, consistiu na obtenção de ferro fundidos nodulares, a serem utilizados na fabricação de eixos, com as seguintes características mecânicas após os tratamentos térmicos adequados: limites de resistência à tração e escoamento mínimos de 700 N/mm2 e 450 N/mm2 respectivamente, alongamento mínimo de 5% e dureza entre 235 à 285 HB. A microestrutura mais adequada à obtenção das características mecânicas desejadas deveria consistir de cementita esferoidizada numa matriz ferrítica, a ser obtida com o tratamento de recozimento ou revenimento de microestruturas previamente perlíticas ou martensíticas, respectivamente. No caso do tratamento de recozimento, as estruturas iniciais consistiram de perlita grossa mais ferrita, presentes no material no estado bruto de fusão, ou, de perlita fina mais ferrita, do material normalizado. Todos os tratamentos térmicos utilizados, dependendo do tempo de tratamento, permitiram a obtenção de cementita esferoidizada. O material normalizado e recozido durante 2 horas a 700ºC, possibilitou a obtenção das propriedades mecânicas desejadas: limites de resistência à tração e de escoamento de 827 N/mm2 e 547 N/mm2 respectivamente, alongamento de 7% e dureza de 277 HB, valores estes, dentro dos limites desejados no presente trabalho. No caso do material temperado e revenido a 700ºC durante 0,5 hora, obteve-se limites de escoamento de 542 N/mm2, alongamento de 6% e dureza de 246 HB. O tratamento de recozimento realizado durante 48 horas, produziu microestrutura quase totalmente ferrítica, com pequenas áreas de agregados de carbonetos. O restante do carbono migrou para os nódulos de grafita secundária ao redor dos mesmos. / The purpose of the present work, consisted in obtaining ductile casting iron, that will be used in the shaft production, with de following mechanical properties after the appropriated heat treatments: ultimate tensile strength and yield strength values of 700 N/mm2 and 450 N/mm2 minimum respectively, elongation of 5% minimum and hardness value from 235 to 285 HB. The microstructure more adequated to obtaining the desired mechanical characteristics should consist of spheroidized cementite in a ferritic matrix, to be obtained with the annealing or tempering treatments of microstructures previously pearlitic or martensitic respectively. In the case of the annealing treatment, the initial structures consisted of thick pearlite plus ferrite, wich were in the material in the ascast state, or fine pearlite plus ferrite, of the normalized material. All the used heat treatment, depending on the time of treatment, allowed the obtainment of spheroidized cementite. The material normalized and annealed for 2 hours at 700°C made possible the obtaining of the desired mechanical properties: ultimate tensile strength and yield strength value of 827 N/mm2 and 547 N/mm2 respectively, elongation of 7% and hardness values of 277 HB, values these, in acordance with the aims initially proposed in the present work. In the case of the material quenched and tempered at 700°C for 0,5 hour, it was obtained yield strength values of 542 N/mm2, elongation of 6% and hardness value of 246 HB. The annealing treatment made during 48 hours, produced a microstructure almost totally ferritic, with small areas of aggregated carbides. The remaining of the carbon migrated to the graphite nodules producing secondary graphite around them.

We analyze the resolved stellar populations of the faint stellar system, Crater, based on deep optical imaging taken with the Advanced Camera for Surveys on the Hubble Space Telescope. Crater's color-magnitude diagram (CMD) extends similar to 4 mag below the oldest main-sequence (MS) turnoff. Structurally, we find that Crater has a half-light radius of similar to 20 pc and no evidence for tidal distortions. We model. Crater's CMD as a simple stellar population (SSP) and alternatively by solving for its full star formation history. In both cases, Crater is well. described by an SSP with an age of similar to 7.5 Gyr, a metallicity of [ M / H] similar to 1.65, a total stellar mass of M-star similar to 1e4 M-circle dot, and. a luminosity of M-V similar to - 5.3, located at a distance of d similar to 145 kpc, with modest uncertainties due to differences in the underlying stellar evolution models. We argue that the sparse sampling of stars above the turnoff and subgiant branch are likely to be 1.0-1.4 M-circle dot blue stragglers and their evolved descendants, as opposed to intermediate- age MS stars. We find that. Crater is an unusually young cluster given its location in the Galaxy's outer halo. We discuss scenarios for Crater's origin, including the possibility of being stripped from the SMC or the accretion from lower- mass dwarfs such as Leo I or Carina. Despite uncertainty over its progenitor system, Crater appears to have been incorporated into the Galaxy more recently than z similar to 1 (8 Gyr ago), providing an important new constraint on the accretion history of the Galaxy.