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<p>Globular clusters have linear sizes (tidal radii) which are theoretically de- termined by their mass and by the gravitational potential of their host galaxy. However observationally, cluster sizes are simply a determination of where the cluster’s surface brightness profile becomes zero. This distance is also known as the limiting radius. While it is commonly assumed that the tidal radius and the limiting radius of a globular cluster are the same thing, it has yet to be validated. The purpose of this thesis is to explore the assumption that cluster tidal radii and limiting radii are equal by comparing the tidal radii of an observed and simulated globular cluster population.</p> <p>An established link between cluster tidal radii and limiting radii will yield new methods of utilizing globular clusters as tools for studying galaxies. If cluster sizes are truly imposed by the tidal field of the host galaxy, then tidal radii measurements can be used to trace the mass distribution within a galaxy, including the dark matter halo. Additionally, as we will demonstrate in this thesis, cluster sizes can also be used a tracer for the orbital anisotropy profile of a galaxy.</p> <p>To explore the assumption that tidal radii and limiting radii are equal, we utilize the globular cluster population of the Virgo giant M87. Unusually deep, high signal-to-noise images of M87 are used to determine the radius for approximately 2000 globular clusters. To compare with these observations, we simulate a globular cluster population that has the same characteristics to the observed M87 cluster population. These characteristics include cluster radial distribution, mass distribution, central concentration distribution and line of sight velocity dispersion. Placing these simulated clusters in the well-studied tidal field of M87, the orbit of each cluster is solved and the theoretical tidal radius of each cluster is determined. We compare the predicted relationship between cluster size and projected galactocentric distance found in our sim- ulation to observations in order to test whether a cluster’s tidal radius and limiting radius are equal. We find that for an isotropic distribution of cluster velocities, theoretical tidal radii are approximately equal to observed limiting radii. The simulation predicts the observed increase in cluster size with galac- tocentric distance, which is expected if tidal radii are dependent on the tidal field. Additionally, simulated cluster sizes are of the same order of magnitude as observed cluster sizes. However the simulation does underestimate cluster sizes in the inner regions of M87. To minimize the discrepancy between theory and observations, we further explore the effects of orbital anisotropy on cluster sizes, and suggest a possible orbital anisotropy profile for M87 which yields the best fit between theory and observations. Finally, we suggest multiple future studies which will aid in our understanding of tidal theory and in establishing a stronger link between tidal radii and limiting radii.</p> / Master of Science (MSc)

DNA similarity studies were used to determine the species of thirty-one strains of bacteria isolated from the hemolymph of infected larvae from Mexico and throughout Central and South America. Twenty-one of the strains were determined to be <I>Paenibacillus popilliae</I> and ten were found to be more closely related to <I>Paenibacillus lentimorbus</I>. Only one of the <I>P. popilliae</I> strains, an isolate from Mexico, was resistant to the antibiotic vancomycin, a trait characteristic of <I>P. popilliae</I> strains from other geographic areas. As expected, all <I>P. lentimorbus</I> strains were sensitive to vancomycin. The polymerase chain reaction (PCR) was used to amplify a portion of a ligase gene necessary for vancomycin resistance in the Mexican strain. Sequencing of the amplicon revealed a sequence identical to that obtained from a North American strain of <I>P. popilliae</I> previously described. The ability of <I>P. popilliae</I> and the inability of <I>P. lentimorbus</I> to grow on medium supplemented with 2% sodium chloride has been used as a phenotypic trait for differentiating between the two species. Approximately 86% of the <I>P. popilliae</I> strains were capable of growth on medium supplemented with 2% sodium chloride and 60% of the <I>P. lentimorbus</I> strains were not capable of growth on this medium. Microscopic examination revealed that all of the Mexican and Central and South American strains of <I>P. popilliae</I> and <I>P. lentimorbus</I> produced a parasporal body. PCR was used to amplify two different regions of the <I>cry18Aa1</I> gene encoding the paraspore in all of the isolates. One primer pair, CryBP2, detected the <I>cry18Aa1</I> gene in 17 of the 21 <I>P. popilliae</I> strains and in all ten of the <I>P. lentimorbus</I> strains. The second primer pair, CryBP4, detected the parasporal gene in 20 of the 21 <I>P. popilliae</I> strains and in all ten of the <I>P. lentimorbus</I> strains. Thirty of the thirty-one <I>P. popilliae</I> and <I>P. lentimorbus</I> strains produced amplicons of approximately 616 bp with the CryBP4 primers. The CryBP4 primers did not detect the paraspore gene in one of the <I>P. popilliae</I> strains. The CryBP2 primer pair produced amplicons of three different sizes, indicating possible variability in the parasporal proteins of <I>P. popilliae</I> and <I>P. lentimorbus</I>. Eleven of the <I>P. popilliae</I> strains produced CryBP2 amplicons approximately 660 bp in size and six of the <I>P. popilliae</I> strains produced CryBP2 amplicons approximately 1100 bp in size. The <I>cry</I> gene was not detected in four of the <I>P. popilliae</I> strains with the CryBP2 primers. The <I>P. lentimorbus</I> strains produced CryBP2 amplicons approximately 750 bp in size. Three PCR products representing the variable CryBP2 amplicon sizes were sequenced and compared to the published <I>cry18Aa1</I> gene sequence. Sequencing data revealed that the Central and South American CryBP2 amplicons are similar to the published <I>cry18Aa1</I> sequence, however, the 1100 bp amplicon has a 453 bp insert that is not found in the published <I>cry18Aa1</I> gene sequence. Paraspores are produced by <I>P. popilliae</I> and <I>P. lentimorbus</I> and is not a reliable phenotypic trait for differentiation between the two species. The ability of Mexican and Central and South American strains of <I>P. lentimorbus</I> to produce paraspores supports the previous findings of a North American group of <I>P. lentimorbus</I> strains that were also capable of producing paraspores. Except for one Mexican strain of <I>P. popilliae</I>, the Central and South American strains of <I>P. popilliae</I> are sensitive to vancomycin. This was unexpected since all North American strains of <I>P. popilliae</I> are vancomycin resistant. Vancomycin resistance could be useful in identifying strains of <I>P. popilliae</I> from North America but not for identifying strains of <I>P. popilliae</I> from Central and South America. So far, no vancomycin resistant strains of <I>P. lentimorbus</I> have been identified. There was variability in the ability of these organisms to grow on medium supplemented with 2% sodium chloride so the usefulness of this trait is debatable. However, the majority of <I>P. popilliae</I> strains from Mexico and Central and South America will grow on medium supplemented with 2% sodium chloride and the majority of the <I>P. lentimorbus</I> strains from these same areas will not grow on this medium. North American strains of <I>P. popilliae</I> and <I>P. lentimorbus</I> also showed variability of growth on medium supplemented with 2% sodium chloride. / Master of Science

O presente trabalho propõe uma abordagem abrangente para descrever a evolução da região central da Via Láctea, compreendendo-se aí o bojo, a barra e as interfaces dos mesmos com o limite interno do disco e com a região central do halo. Pretende-se investigar as propriedades químicas e cinemáticas destas estruturas, que são interconectadas, com o objetivo de separá-las e aplicar os resultados daí obtidos a um modelo de formação e evolução do bojo e da região interna do disco que descreva simultaneamente distintos aspectos da evolução da região central da Galáxia. Na primeira parte do trabalho, uma amostra de nebulosas planetárias (NPs) localizadas no disco interno e no bojo da Galáxia é utilizada para encontrar a distância galactocêntrica que melhor separa estas duas populações, do ponto de vista das abundâncias. Foram utilizadas escalas de distâncias estatísticas para o estudo da distribuição das abundâncias na interface bojo-disco. A aplicação do teste Kolmogorov-Smirnov mostrou que, em média, a população interna não segue o gradiente radial de abundâncias do disco na direção do centro galáctico. Baseado neste estudo, propõe-se uma distância galactocêntrica de 1.5 kpc para definir a interface bojo-disco. Na segunda parte do trabalho, foram realizadas observações espectrofotométricas de 21 NPs localizadas na direção do centro da Galáxia com o telescópio SOAR. Estes objetos estão localizados bem próximos ao plano galáctico na direção central da Via Láctea, onde não existem dados de NPs na literatura. Os resultados mostram que as NPs localizadas nesta região apresentam baixas abundâncias de oxigênio comparadas com as NPs do disco interno e de outras regiões do bojo. Os resultados indicam que o bojo apresenta uma complexa composição de populações estelares. Por um lado, a presença de nebulosas com baixas abundâncias mostra que o bojo pode ter se formado a partir de um disco galáctico antigo através de uma evolução secular. Por outro lado, existem alguns objetos do bojo para os quais as abundâncias coincidem com o limite do gradiente radial do disco nesta região. Esta é uma evidência para um bojo composto por duas ou mais populações: uma originada do disco fino, e outra originada do disco espesso. Na última parte do trabalho propõe-se a inclusão de fluxos radiais de gás em um modelo de evolução química para simular os efeitos de uma barra localizada no centro da Galáxia nas distribuições de abundâncias, densidade de gás e taxa de formação estelar (SFR). Os resultados das simulações indicam que os modelos com fluxos de gás apresentam uma SFR mais alta no bojo e que os perfis da SFR e da densidade de gás na região central são melhor reproduzidos após a inclusão dos fluxos radiais no modelo. As simulações indicam ainda que o gradiente de abundâncias do disco é mais plano para o caso da inclusão da barra. Estes resultados indicam que a barra e os fluxos de gás exercem um importante papel na formação de estrelas no centro das galáxias espirais barradas. / This project proposes a comprehensive approach to describe the evolution of the central region of the Galaxy, comprising the bulge, the bar and their interfaces with the inner disk and the central region of the halo. We intend to investigate the chemical and kinematic properties of these structures, which are interconnected, aiming to separate them and apply these results to a model for the formation and evolution of the bulge and inner disk, capable to describe simultaneously distinct aspects of the evolution of the central region of the Galaxy. First, a sample of planetary nebulae (PNe) located in the inner-disk and bulge of the Galaxy is used in order to find the galactocentric distance that better separates these two populations, from the point of view of abundances. Statistical distance scales were used to study the distribution of abundances across the disk-bulge interface. A Kolmogorov-Smirnov test was used to find the distance in which the chemical properties of these regions better separates. The results of the statistical analysis indicate that, on the average, the inner population has lower abundances than the outer. Additionally, for the $\\alpha$-elements abundances, the inner population does not follow the disk radial gradient towards the galactic centre. Based on our results, we suggest a bulge-disk interface at 1.5 kpc, marking the transition between the bulge and inner-disk of the Galaxy, as defined by the intermediate mass population. Second, we present spectrophotometric observations for a sample of 21 PNe located towards the galactic centre of the Galaxy. The abundances are derived based on observations in the optical domain made at the SOAR telescope. Their location is interesting since there are no observations of PNe in this region. The data show lower oxygen abundances compared to those from PNe located in the inner disk and other bulge regions. The results show that the bulge has a complex composition of stellar populations. The presence of PNe with low abundances indicates that the bulge might be formed from an old galactic disk through secular evolution. On the other hand, other objects from our sample have abundances compared to those from inner disk PNe. This is evidence that two or more populations might compose the bulge: one originated from the thin disk, and the other from the thick disk. Last, we propose a chemical evolution model that includes radial gas flows. This is done in order to mimic the effects of the galactic bar on the chemical abundances distributions and the gas density profiles and the star formation rate (SFR). The results of the models with radial flows point to a high SFR in the bulge and, additionally, the SFR and gas density profiles in the inner Galaxy are better reproduced after the inclusion of radial gas flows in the model. After including a specific velocity pattern for the bar, the results show a flattening of the radial abundance gradient. Our results indicate that radial gas flows may play an important role in the star formation near the centre of barred spiral galaxies.

First, the baryonic content of simulated halos of virial masses between 5 x 10^{9} M_{\odot}$ to 5 x 10^{12} M_{\odot}$ in the APOSTLE project is examined in the context of the missing baryon problem. Baryonic particles in APOSTLE can be either stars or gas. Non-star-forming gas, or the circumgalactic medium (CGM) is further classified by temperature into the Cool CGM (CCGM, T < 10^{5} K), or the Warm-Hot CGM (WHCGM, T > 10^{5} K). APOSTLE halos are found to contain less than 60% of the expected mass of baryons (f_{b} = Ω{b}/Ω{m}, M_{b} = f_{b} x M_{200}) within their virial radius. The WHCGM contains 29% ± 10%, the CCGM 12% ± 5%, and the stars and star-forming gas 19% ± 5%. The metal content of the same halos is analyzed, and compared to the total metals produced by the stars within the virial radius. Over two thirds of the produced metals are retained within the halo, with 14% ± 3% in the WHCGM, 13% ± 4% in the CCGM, and 43% ± 9% in the stars and star-forming gas. Next, we focus on the overall distribution of matter within a 3Mpc radius from the Milky Way. Using the trends in APOSTLE volumes, I quantify both the ellipticity and orientation of this spatial distribution using the principal axes of the inertia tensor of the positions of these galaxies. The Zone of Avoidance has little impact on this result, and the short axis is aligned with that of the Supergalactic Plane, and is perpendicular to the vector separating the Milky Way and Andromeda galaxies. APOSTLE local group analogues are found to be similarly anisotropic, and like in the observed Local Group, the minor axis of that distribution is found to be perpendicular to the vector separating the two primaries. The angular momentum of the stellar disk shows weak alignment with the minor axis of the field galaxy distribution. In addition the simulations also suggest that the angular momenta of the two primary dark-matter halos tend to be anti-aligned. Additionally, stellar disks tend to orient themselves in the same direction as their halo. / Graduate

I present a comprehensive investigation of fast stars in the Milky Way, from brisk disc stars to stars escaping the Galaxy. My thesis is that fast stars are the smoking guns of extreme stellar collisions and explosions, and so can act as an intermediary to studying these theoretically-unconquered astrophysical processes. In Chapter 1 I give a history of fast stars, address what it means for a star to be fast, and describe the processes that accelerate stars. I concisely summarise the Gaia mission, whose recent data releases heavily influenced this thesis. Supernovae in binary systems can fling away the companion; if a runaway companion can be associated with a supernova remnant, then together they reveal the evolution that led to the supernova. However, these associations are difficult to establish. In Ch. 2, I develop a sophisticated Bayesian methodology to search the nearest ten remnants for a companion, by combining data from Gaia DR1 with a 3D dust-map and binary population synthesis. With Gaia DR2, I will identify companions of tens of supernova remnants and thus open a new window to studying late-stage stellar evolution. It is unknown why 17% of B stars are spinning near break-up; these stars are termed Be stars because of emission lines from their ejected material. Their rapid spin could be due to mass transfer, but in Ch. 3 I show this would create runaway Be stars. I demonstrate using a hierarchical Bayesian model that these exist in sufficient numbers, and thus that all Be stars may arise from mass transfer. The stars escaping the Milky Way are termed hypervelocity stars. In Ch. 4, I overturn the consensus that the hypervelocity stars originated in the Galactic centre by showing that a Large Magellanic Cloud (LMC) origin better explains their distribution on the sky. In Ch. 5 I present three ground-breaking hypervelocity results with Gaia DR2: 1) only 41 of the 524 hypervelocity star candidates are truly escaping, 2) at least one of the hypervelocity stars originates in the LMC, and 3) the discovery of three hypervelocity white dwarf runaways from thermonuclear supernovae.

<p>We are made of stardust in the sense that most atomic nuclei around us have been formed by stars. Stars synthesise new elements and expel them to the interstellar medium, from which later new generations of stars are born. We can map this chemical evolution by analysing the atmospheric contents of old Galactic halo stars. I have done two such investigations. A vigourous debate is going on whether the oxygen-to-iron ratio varies strongly with the general metal-content of halo stars. In my first study, I made an abundance analysis of 43 halo stars, and found no support for such a variation. I have also found that there probably is a cosmic spread in the abundances of oxygen, magnesium, silicon, and calcium relative to iron for halo stars. This may be an indication that the halo was built up by subsystems with differences in the star formation rate. In my second study, I performed a thorough abundance analysis of the star HE0338-3945, which is strangely overabundant in both r- and s-elements. Several other stars have been found with abundance patterns curiously similar to this star, and I define new criteria for the class r+s stars. The abundance similarities among the r+s stars suggest a common formation scenario. However, as the s-elements usually are considered to be produced in binary systems of low mass, and r-elements in supernovae of Type II, this scenario is not obvious. In the article I discuss seven hypotheses, and several of them are dismissed.</p>

We are made of stardust in the sense that most atomic nuclei around us have been formed by stars. Stars synthesise new elements and expel them to the interstellar medium, from which later new generations of stars are born. We can map this chemical evolution by analysing the atmospheric contents of old Galactic halo stars. I have done two such investigations. A vigourous debate is going on whether the oxygen-to-iron ratio varies strongly with the general metal-content of halo stars. In my first study, I made an abundance analysis of 43 halo stars, and found no support for such a variation. I have also found that there probably is a cosmic spread in the abundances of oxygen, magnesium, silicon, and calcium relative to iron for halo stars. This may be an indication that the halo was built up by subsystems with differences in the star formation rate. In my second study, I performed a thorough abundance analysis of the star HE0338-3945, which is strangely overabundant in both r- and s-elements. Several other stars have been found with abundance patterns curiously similar to this star, and I define new criteria for the class r+s stars. The abundance similarities among the r+s stars suggest a common formation scenario. However, as the s-elements usually are considered to be produced in binary systems of low mass, and r-elements in supernovae of Type II, this scenario is not obvious. In the article I discuss seven hypotheses, and several of them are dismissed.

The kinematics and white dwarf distribution have been studied for the Globular Cluster NGC 6397. The data was obtained from NASA’s Hubble Space Telescope in 2005. In particular, we used the images of a field 5’ Southeast of the core of NGC 6397 from Advanced Camera for Surveys to conduct our analyses. The first part of the study is about the kinematics of the globular cluster. Isotropy of velocity distribution and cluster rotation have been considered. As anticipated, this relaxed cluster exhibited no strong signs of anisotropy. However, there appears to be some level of rotation. The rotational motion turns out to be mu sub alpha cos(delta) = 3.88 ± 1.41 mas yr −1 and mu sub delta = −14.83 ± 0.58 mas yr −1. This result is not entirely expected and deserves further investigation in future studies. The second of the thesis is based on white dwarf populations in the globular cluster and the Galactic Bulge. As a first glance, there appears to be a lacking of white dwarfs at the age of approximately 0.6 Gyr. Further investigation reveals this to be statistically insignificant. Through this analysis, another pattern of white dwarf abundance is discovered. There appeared to be much more stars at the age between 0.9 − 2.0 Gyr. This could be a manifestation of modeling error. As the final consideration of this thesis, white dwarf candidates in the Galactic Bulge are illustrated. Approximately 10 candidates are found at the most probable location of stars in the Bulge. The analyses conducted in this thesis set stage for further development in understanding of globular clusters. In particular, the rotation analysis raises curiosity about the dynamics of NGC 6397 in the plane of the sky. Moreover, the velocity distribution analysis confirms properties and theories pertaining to globular clusters.