This study consisted of an optical photometric and spectroscopic analysis on a 7′ 7′ field around the Southern high mass star forming region RCW 34. A previous study on RCW 34 in the NIR discov- ered many deeply embedded young stellar objects which were suspected to be T Tauri stars and which justified further investigation. The data used in this study consisted of three sets, the first two are photometric and spectroscopic data sets which were obtained during the first two weeks of February 2002. A third data set of spectroscopic observations was obtained by the author during the second week of 2011 of selected candidates using results from the NIR study and from the photometric data sets. All of the spectroscopy was conducted with the long slit spectrograph on the 1.9-m telescope and the photometry with DANDICAM on the 1.0-m telescope at the South African Astronomical Observatory (SAAO) in Sutherland. Objectives accomplished in the course of this study were to understand, ob- tain, reduce and interpret photometric and long slit spectroscopic CCD images. From the photometric results 57 stars showed excess blue emission on a colour-colour diagram which could be generated by circumstellar matter. The spectroscopic study showed 5 stars that showed H emission and 2 with strong Li absorption lines which confirm the suspicions of the NIR study about T Tauri stars in the region. All of the stars from the spectroscopic study in 2011 were identified as low-mass K or M type stars. Using colour-magnitude diagrams it was possible to see that the majority of the stars in the cluster are low-mass pre-main sequence stars. The stars matching between the optical and NIR filters were plotted on NIR colour-colour diagrams showing that the 5 stars that had H emission lines also had NIR colours characteristic to T Tauri stars. Out of the 5 stars that showed H emission, 2 were found to be classical T Tauris and three were found to be weak line T Tauris. / Thesis (MSc (Space Physics))--North-West University, Potchefstroom Campus, 2013

This study consisted of an optical photometric and spectroscopic analysis on a 7′ 7′ field around the Southern high mass star forming region RCW 34. A previous study on RCW 34 in the NIR discov- ered many deeply embedded young stellar objects which were suspected to be T Tauri stars and which justified further investigation. The data used in this study consisted of three sets, the first two are photometric and spectroscopic data sets which were obtained during the first two weeks of February 2002. A third data set of spectroscopic observations was obtained by the author during the second week of 2011 of selected candidates using results from the NIR study and from the photometric data sets. All of the spectroscopy was conducted with the long slit spectrograph on the 1.9-m telescope and the photometry with DANDICAM on the 1.0-m telescope at the South African Astronomical Observatory (SAAO) in Sutherland. Objectives accomplished in the course of this study were to understand, ob- tain, reduce and interpret photometric and long slit spectroscopic CCD images. From the photometric results 57 stars showed excess blue emission on a colour-colour diagram which could be generated by circumstellar matter. The spectroscopic study showed 5 stars that showed H emission and 2 with strong Li absorption lines which confirm the suspicions of the NIR study about T Tauri stars in the region. All of the stars from the spectroscopic study in 2011 were identified as low-mass K or M type stars. Using colour-magnitude diagrams it was possible to see that the majority of the stars in the cluster are low-mass pre-main sequence stars. The stars matching between the optical and NIR filters were plotted on NIR colour-colour diagrams showing that the 5 stars that had H emission lines also had NIR colours characteristic to T Tauri stars. Out of the 5 stars that showed H emission, 2 were found to be classical T Tauris and three were found to be weak line T Tauris. / Thesis (MSc (Space Physics))--North-West University, Potchefstroom Campus, 2013

In this work, we analyze the data from 1.5 m telescope of Tubitak National Observatory (TUG) for two objects V2275 Cyg and RW UMi. After applying aperture and PSF photometry to the CCD data, we derive the light curve of the objects. Also we apply discrete Fourier transform and Scargle time series analysis to obtain power spectrum and search for periodicities in their power spectra in which both systems show interesting properties. We discover large variations in V2275 Cyg due to irradiation effects on the secondary, with an orbital period Porb = 0.316&plusmn / 0.007 day. We also detect a very short orbital period for RW UMi Porb = 1.96&plusmn / 0.073h and also a spin period Pspin = 1.29&plusmn / 0.036h in the presence of several beat frequencies. These results (if con&amp / #64257 / rmed) lead us to say that RW UMi can be an intermediate of polar system.

Dans cette thèse, nous étudions le problème du réflecteur. Etant données une source lumineuse et une cible à éclairer avec une certaine distribution d'intensité, il s'agit de construire une surface réfléchissant la lumière issue de la source vers la cible avec la distribution d'intensité prescrite. Ce problème se pose dans de nombreux domaines tels que l'art ou l'architecture. Le domaine qui nous intéresse ici est le domaine automobile. En effet, cette thèse Cifre est réalisée en partenariat avec l'entreprise Optis qui développe des logiciels de simulation de lumière et de conception optique utilisés dans les processus de fabrication des phares de voiture. Les surfaces formant les réflecteurs des phares de voiture doivent répondre à un certain nombre de critères imposés par les fabricants ainsi que les autorités de contrôle nationales et internationales. Ces critères peuvent être objectifs comme par exemple l'encombrement du véhicule ou encore le respect des normes d'éclairage mais peuvent également être subjectifs comme l'aspect esthétique des surfaces. Notre objectif est de proposer des outils industrialisables permettant de résoudre le problème du réflecteur tout en prenant en compte ces critères. Dans un premier temps, nous nous intéresserons au cas de sources lumineuses ponctuelles. Nous reprenons les travaux d'Oliker, Glim, Cafarrelli et Wang qui montrent que le problème du réflecteur peut être formulé comme un problème de transport optimal. Cette formulation du problème est présentée et mise en œuvre dans un cas discret. Dans un second temps, nous cherchons à prendre en compte les critères imposés par les fabricants de phares de voitures. Nous nous sommes intéressés ici aux contraintes d'encombrement et d'esthétique. La solution choisie consiste à utiliser des surfaces de Bézier définies comme le graphe d'une certaine fonction paramétrée par un domaine du plan. Les surfaces de Bézier permettent d'obtenir des surfaces lisses et la paramétrisation par un domaine du plan permet de gérer l'encombrement et le style d'un réflecteur. Nous avons proposé une méthode heuristique itérative par point fixe pour obtenir ce type surface. Enfin, dans un dernier temps, nous prenons en compte des sources lumineuses non ponctuelles. L'approche proposée consiste à adapter itérativement les paramètres du réflecteur de façon à minimiser une distance entre intensité souhaitée et intensité réfléchie. Ceci nous a conduits à proposer une méthode d'évaluation rapide de l'intensité réfléchie par une surface. Les méthodes développées durant cette thèse ont fait l'objet d'une implémentation dans un cadre industriel en partenariat avec l'entreprise Optis. / The far-field reflector problem consists in building a surface that reflects light from a given source back into a target at infinity with a prescribed intensity distribution. This problem arises in many fields such as art or architecture. In this thesis, we are interested in applications to the car industry. Indeed, this thesis is conducted in partnership with the company Optis that develops lighting and optical simulation software used in the design of car headlights. Surfaces in car headlight reflectors must satisfy several constraints imposed by manufacturers as well as national and international regulatory authorities. These constraints can be objective such as space requirements or compliance with lighting legal standards but can also can be subjective such as the aesthetic aspects of surfaces. Our goal is to provide industrializable tools to solve the reflector problem while taking into account these constraints. First, we focus on the case of point light sources. We rely on the work of Oliker, Glim, Cafarrelli and Wang who show that the reflector problem can be formulated as an optimal transport problem. This formulation of the problem is presented and implemented in a discrete case. In a second step, we take into account some of the constraints imposed by car headlight manufacturers, such as the size and the style of the reflector. The chosen solution consists in using Bezier surfaces defined as the graph of a function parameterized over a planar domain. Bezier surfaces allow to obtain smooth surfaces and the parameterization over a planar domain allows to control the size and style of the reflector. To build the surface, we propose a heuristic based on a fixed-point algorithm. Finally, we take into account extended light sources. We present an approach that iteratively adapts the parameters of the reflector by minimizing the distance between the desired intensity and the reflected intensity. This led us to propose a method that efficiently evaluates the reflection of light on the surface. Methods developed in this thesis were implemented in an industrial setting at our partner company Optis.

Nous allons assister au cours de la prochaine décennie, à la première lumière des nouveaux Extremely Large Telescopes. Leur grande taille (de 25 à 39 m de diamètre) permet d’augmenter à la fois leur sensibilité et leur résolution angulaire. Cependant, la résolution angulaire d'un télescope terrestre, est toujours limitée par la turbulence atmosphérique. Pour pallier à ce problème, les grands télescopes sont désormais équipés d'instruments d’Optique Adaptative (OA). L’OA est une technique qui permet d’analyser les effets de la turbulence et de les compenser en temps réel à l’aide de miroirs déformables. En complément, la plupart des télescopes de la génération 8-10 m sont maintenant équipés de systèmes d’étoiles lasers qui permettent d’augmenter la proportion du ciel pouvant bénéficier d’une correction par OA: on parle alors d'Optique Adaptative Grand Champ (OAGC). Malgré les excellentes performances de ces systèmes, la correction apportée aux images reste partielle et des résidus de correction limitent encore leur qualité. Pour extraire les meilleurs résultats scientifiques des images issues de l'OAGC, il est donc essentiel d'optimiser les outils de réduction et d'analyse de données. La première partie de cette thèse détaille une analyse astrophysique de données OAGC ayant pour but d'étudier la formation des étoiles massives dans un environnement extra-galactique. Au delà des résultats scientifiques nouveaux, cette étude a permis de mettre en évidence les termes d'erreur limitant l'analyse scientifique de données OAGC. La seconde partie de cette thèse est dédiée au développement d'un nouvel outil de correction de la distorsion permettant de réduire ces termes d'erreurs. / The next decade will see the first light of the new Extremely Large Telescopes. Their large diameter (from 25 to 39 meters across), increases both their sensitivity and their angular resolution. However, angular resolution of all sizes ground-based telescope is always strongly limited by the atmospheric turbulence. To tackle this problem and fully exploit their capabilities, large optical telescopes are now indissociable of their Adaptive Optics (AO) instruments. AO is a technic that consists in analyzing the effects of turbulence on the wavefront and compensating for it in real time, thanks to one or several deformable mirrors in order to restore the initial angular resolution of optical telescopes. In addition, most of the 8-10 meters telescopes are supplied with laser guide stars systems in order to increase the portion of the sky that can benefit for such an AO correction. Such systems are called Wide Field AO (WFAO). However, despite the excellent performance of such systems, the correction performed is not perfect and some residuals still limit the image quality. In order to get the best science results out of the WFAO images, dedicated and optimized reduction and analyses tools are needed. The first part of this document present an astrophysics analyses of WFAO images aiming to study massive star formation in an extra-galactic environment. In addition to new science results, the study carried out on these observations has enable to highlight the critical parameters that limit the scientific analyses of Wide Field AO data. The second part of this document is dedicated to the development of a new distorsion correction tool that aims to reduce these error terms.

Orientador: Paulo Sergio Scarazzato / Dissertação (mestrado) - Universidade Estadual de Campinas, Faculdade de Engenharia Civil, Arquitetura e Urbanismo / Made available in DSpace on 2018-08-07T10:08:06Z (GMT). No. of bitstreams: 1 Ciampini_Flavia_M.pdf: 46784073 bytes, checksum: e6d43d6ef27616aa1ae3ce6f61745be3 (MD5) Previous issue date: 2005 / Resumo: A importância desta pesquisa reside na avaliação quantitativa de diferentes dispositivos de iluminação natural, disponíveis no mercado internacional, mediante a aquisição das iluminâncias obtidas através de ensaios em protótipos. Este trabalho foi realizado com objetivo de verificar se a aplicação destes sistemas, restritos a sistemas de iluminação lateral, no território nacional trariam de fato alguma vantagem para as edificações, no sentido de otimizar a iluminação natural obtida em ambientes profundos, em território brasileiro. As medições foram realizadas sob condição de céu real na cidade de Campinas, SP. A dissertação é composta por três etapas. A primeira, traz uma revisão dos princípios básicos necessários para o estudo das tecnologias utilizadas. Em seguida são apresentados alguns dispositivos de iluminação natural no cenário internacional, identificando suas características e os princípios físicos que determinam seu funcionamento. Na segunda etapa, mediante utilização de planilhas eletrônicas, determinou-se, para cada painel, a posição e o desenho mais adequados à latitude de Campinas para fachada norte. De acordo com estas especificações foram solicitados, no exterior, os painéis aos fabricantes. Na terceira fase, com um sistema de medição de iluminâncias, criado especialmente para esta tarefa, foram registradas as iluminâncias obtidas no interior de quatro protótipos, construídos na Universidade Estadual de Campinas (UNICAMP) utilizando-se os 12 diferentes painéis doados por universidades e empresas estrangeiras. Os painéis de iluminação natural foram acoplados à abertura dos protótipos, localizada na fachada norte. As iluminâncias obtidas com cada painel foram registradas de 8:00 as 18:00, de março a julho. Para que todos os painéis fossem medidos com condições de sol semelhantes foi realizado um rodízio de forma que a cada quatro dias todos os painéis foram acoplados aos protótipos e suas iluminâncias medidas ao longo do dia. Os dados são tratados de forma a obter valores médios mensais das iluminâncias, em função da profundidade do ambiente, onde foram realizadas as medições para dias claros, encobertos e parcialmente encobertos. A partir da comparação dos dados obtidos experimentalmente procurou-se estabelecer quais dos dispositivos estudados, iluminam o ambiente de forma otimizada em relação a um vidro comum de 3mm, criando uma iluminação mais homogênea ou conseguindo iluminâncias maiores no fundo do ambiente. O estudo mostrou que todos os dispositivos poderiam facilmente ser adaptados ao clima luminoso de Campinas, para fachada norte, no entanto cada um destes dispositivos tem as suas limitações e vantagens. Por fim uma solução ótima para alcançar um aproveitamento otimizado da luz natural dentro dos espaços, de acordo com os dispositivos estudados é sugerido na conclusão do trabalho / Abstract: The importance of this research relies on the quantitative evaluation of different daylighting devices, available in the international market, by means of acquiring the iIIuminance through models. This work was accomplished with objective of verifying the application of these systems, restricted to lateral iIIumination in national territory, if they would bring in fact some advantage for buildings, in the sense of optimizing the daylighting obtained in deep rooms, in Brazilian territory. The measurement has been made under real sky condition in the city of Campinas, SP. This thesis is composed of three stages. The first, brings a revision of the basic principies necessary for the study of the technologies used. Soon afterwards these daylighting devices in the international scene are presented, identifying their characteristics and the physical principies that determine its operation. In the second stage, by use of electronic spreadsheets, it was determined for each panel, the position and the most appropriate drawing for the latitude of Campinas for a North façade. In agreement with these specifications the panels were requested abroad from their manufacturers. In the third phase, with an iIIuminance measurement system, especially created for this task, the iIIuminance inside four prototypes were acquired, built in the State University of Campinas (UNICAMP), using the 12 different panels donated by universities and foreign companies. The daylinghting panels were coupled to the opening of the prototypes, located in the north façade. The illuminance obtained with each of these panels was registered from 8:00 to 18:00, from March to July. So that all of the panels were measured with the similar sun conditions so that every four days all of the panels were coupled to the prototypes and their iIIuminance measured during the day. The data are treated to get monthly average values of the illuminances, as a function of the depth of the environment, where the measurements were accomplished for clear, partially cloudy and cloudy days. From the comparison of these data we establish which of the studied devices can achieve a better performance if compared with a standard clear glass panel, and which can obtain a homogeneous iIIumination or greater iIIuminances along the deep of the room. The study showed that all the devices could easily be adapted to the luminous climate of Campinas, for the north façade, however each one of these devices has their limitations and advantages. Finally a new solution is suggested to reach an optimized exploitation of daylight in interior spaces, in agreement with the results obtained in the conclusion of this work / Mestrado / Edificações / Mestre em Engenharia Civil

Les techniques de reconstruction 3d sont devenues incontournables pour des applicationstelles que la caractérisation et l'analyse de surfaces. Les travaux réalisés au coursde cette thèse ont pour objectif d'améliorer la qualité des reconstructions 3d par stéréophotométrie.Cette méthode repose sur deux principes, l'inversion d'un modèle d'interactionlumière/matière (BRDF) et la configuration d'un système d'éclairage et de prises de vues.Pour des surfaces diffuses, la stéréo-photométrie est réalisée à partir d'un minimum detrois images acquises d'un point de vue fixe pour des directions d'éclairages différentes.Son avantage est d'extraire simultanément les propriétés géométriques et colorimétriquesdes surfaces analysées même en cas de forte rugosité. Néanmoins, son application exige laformulation de plusieurs hypothèses qui sont difficilement respectables dans un contexteréel. Ceci génère des erreurs significatives dans les reconstructions. Pour les réduire, nousproposons différentes contributions qui s'articulent autour de la prise en compte globale de lachaine d'acquisition. Les apports de nos travaux se situent aux niveaux de la caractérisationet de la modélisation du système d'éclairage, du capteur d'acquisition et de l'améliorationde la qualité des images. Nous nous sommes aussi intéressés à l'optimisation des protocolesde prises de vues dans le cas de spécularité surfacique ou d'ombrage dus à la présence derugosité. Les résultats obtenus montrent que la prise en compte de ces caractéristiques dansl'inversion d'un modèle de BRDF permet une nette amélioration des reconstructions et offrela possibilité de réduire la taille des systèmes d'acquisition. / Tridimensional reconstruction method has become essential for applications suchas the characterization and analysis of surfaces. In this thesis, aims are to increase the qualityof 3d reconstructions by photometric stereo. This method is based on two principles, reversinglight-matter interaction model and configuration of a lighting system. With diffuse surfaces,the photometric stereo use three captured images from a fixed point of view for differentillumination directions. Its main advantage is to extract the color and geometric propertiesfor the textured rough surfaces. However, its application requires to make assumptions thatare not credible in real cases. This problem generates significant errors in the reconstructions.To reduce them, we offer various solutions around the overall consideration of the acquisitionchain. Our contribution focuses on the characterization and modeling of the lighting system,the acquisition sensor and improved image quality. We are also interested to optimize acquisitionprotocol in the case of specular surface or shading due to the surface geometry. Ourresults show that the inclusion of these features in the inversion of a BRDF model allowsan improvement of 3d reconstructions as well as the possibility of reducing the size of theacquisition systems.

Magister Scientiae - MSc / We determine the stellar mass of star forming galaxies in the X-ray luminous cluster MS 0451.6-0305 at z ∼ 0.54. The stellar masses are estimated from fitting model spectral energy distributions (SEDs) to deep, optical UBRIz observations obtained from WIYN 3.5m telescope and public NIR K-band image from Palomar Observatory telescope. The model SEDs are based on the stellar population synthesis (SPS) model of Bruzual & Charlot (2003) and Conroy et al. (2009) that span a wide range of age, star formation history, Initial Mass Function (IMF), metallicity and dust content. We measure stellar masses for galaxies down to M∗∼2×10⁸M(.) We find a tight correlation between stellar masses derived from the two SPSs. We compare the derived stellar masses to the dynamical masses for a set of 25 star forming galaxies. The dynamical masses are derived from high resolution, spectroscopic observations of emission lines from the DEIMOS spectrograph on the Keck telescope. A strong correlation is seen between the dynamical and stellar mass for the galaxies; and the star forming galaxies show fairly constant ratio between stellar and dynamical mass. When comparing to the field sample of Guzm ́an et al. (2003) of luminous compact blue galaxies, we see an excess of low mass galaxies in the cluster. / South Africa

Age related macular degeneration (AMD) is one of the leading causes of blindness amongst the elderly. Macular pigment (MP) in the retina has been established to protect individuals against AMD. Improving levels of MP by diet or supplements is the constant quest of clinical practitioners and researchers, thus necessitating development of instruments capable of repeatable and reliable MP measurement. Cataract, a consequence of the rising opacity levels of the lens with age is one of the other major causes of blindness in the world. Mapcatsf, a LED-based microprocessor-controlled heterochromatic flicker photometer (HFP) using photopic vision is capable of measuring the levels of MP and the opacity of the lens in terms of optical density. Test-retest measurements conducted on 83 subjects were analyzed for repeatability in macular pigment optical density (MPOD) measurements. Reliability of the lens optical density (LOD) measurements were tested and compared with those obtained at absolute scotopic thresholds for 25 individuals. A supplement study with 32 individuals both in the young (50) age groups for 6 months further established Mapcatsf’s capacity to monitor changing levels of MP in individuals. As an overall outcome, high levels of repeatability and reliability were obtained in MPOD and LOD measurements establishing Mapcatsf as an instrument for use in clinical settings in the future.

Cette thèse présente les avancées dans l'étude des étoiles naines blanches magnétiques. L'étude des étoiles naines blanches en général, le state final d'évolution de près de 95% des étoiles de notre galaxie, permet d'obtenir de l'information cruciale sur leurs progéniteurs. Se pencher sur les propriétés des champs magnétiques des étoiles naines blanches par opposition à celles de leur progéniteur, beaucoup plus difficiles à observer en partie à cause de la faible intensité du champ, est bien plus réalisable. Plusieurs hypothèses ont été formulées afin de décrire l'origine et l'évolution de ces objets atypiques. Que les champs soient d'origine fossile suite à l'évolution d'une étoile isolée et conservation du flux magnétique, ou créés lors de la rotation rapide de la fusion de deux étoiles, il nous faut bien comprendre leur résultat, les naines blanches magnétiques, avant de pouvoir retracer leur évolution. Toutefois, les modèles de naines blanches magnétiques d'aujourd'hui reposent sur un nombre d'approximation, qui ne sont valides jusqu'à une relativement faible intensité de champ. Ceci a été la motivation derrière ce projet de doctorat. Nous avons implémenté un traitement des raies d'absorption utilisant le calcul des énergies de transition de l'atome d'hydrogène et d'hélium sous champs magnétiques arbitraires. Ces calculs, fournis par le groupe de l'université de Tübingen en Allemagne, ont utilisé une approche numérique à la résolution de l'Hamiltonien de l'atome d'hydrogène et d'hélium en présence d'un champ magnétique d'intensité arbitraire. Cet ajout aux modèles d'atmosphères permet de modéliser la position et l'intensité des raies d'absorption dans le spectre des étoiles. Une procédure de discrétisation de la surface visible de l'étoile nous permet de modéliser des champs magnétiques avec une géométrie arbitraire, tel qu'un dipôle décentré et incliné par rapport à l'observateur. Ces nouveaux outils ont été utilisés afin d'étudier en premier lieu un ensemble des naines blanches magnétiques avec une atmosphère riche en hydrogène. De ces résultats, nous avons déterminé une distribution de masse de ces étoiles, avec une masse moyenne significativement plus élevée que leurs homologues non-magnétiques, tels qu'attendu par les théories d'évolution binaires. Les informations extraites des différentes caractéristiques des distributions obtenues suite à cette analyse ne nous permettent cependant pas de favoriser une hypothèse d'évolution plutôt qu'une autre. Suite à ceci, celles avec une atmosphère riche en hélium ont été les prochaines à être analysées. Nous avons ainsi déterminé rigoureusement, pour la première fois, les paramètres magnétiques de ces étoiles riches en hélium. / This thesis presents advances in the study of magnetic white dwarf stars. The study of white dwarf stars in general, the final state of evolution of nearly 95% of the stars in our galaxy, provides crucial information about their progenitors. It is much more feasible to study the magnetic field properties of white dwarf stars as opposed to their progenitor stars, which are much more difficult to observe in part because of the weak field strength. Several hypotheses have been formulated to describe the origin and evolution of these atypical objects. Whether the fields are of fossil origin following the evolution of an isolated star and conservation of magnetic flux, or created during the rapid rotation of the merger of two stars, we need to understand their result, the magnetic white dwarfs, before we can trace their evolution. However, today's models of magnetic white dwarfs rely on a number of approximations, which are only valid up to relatively low field strengths. This was the motivation behind this doctoral thesis. We have implemented a treatment of the absorption lines using the calculation of the transition energies of the hydrogen and helium atom under arbitrary magnetic fields. These calculations, provided by the group of the University of Tubingen in Germany, used a numerical approach to the resolution of the Hamiltonian of the hydrogen and helium atom in the presence of a magnetic field of arbitrary intensity. This addition to atmospheric models allows to model the position and intensity of absorption lines in the spectrum of stars. A discretization procedure of the visible surface of the star allows us to model magnetic fields with an arbitrary geometry, such as an offset and inclined dipole. These new tools have been used to study first a set of magnetic white dwarfs with a hydrogen-rich atmosphere. From these results, we have determined a mass distribution of these stars, with an average mass significantly higher than their non-magnetic counterparts, as expected by the binary evolution theories. The information extracted from the different characteristics of the distributions obtained from this analysis does not however allow us to favor one evolutionary hypothesis over another. Following this, those with a helium rich atmosphere were the next to be analyzed. We have thus determined rigorously, for the first time, the magnetic parameters of these helium-rich stars.