We conduct a broad investigation about stellar mass and population diagnostics in order to formulate novel constraints related to the formation and evolution of galaxies from a nearby cluster environment. Our work is powered by the use of stellar population models which transform galaxy colours and/or absorption line strengths into estimates of its stellar properties. As input to such models, we assemble an extensive compilation of age and chemical abundance information for Galactic globular clusters. This compilation allows a confident expansion of these models into new regions of parameter space that promise to refine our knowledge of galactic chemical evolution. We then draw upon a state-of-the-art spectroscopic and photometric survey of the Virgo galaxy cluster in order to constrain spatial variations of the stellar ages, metallicities, and masses within its member galaxies, and their dynamical masses. We interpret these data in the context of the histories of star formation, chemical enrichment, and stellar mass assembly to formulate a broad picture of the build-up of this cluster’s content over time. In it, the giant early-type galaxies formed through highly dissipational processes at early times that built up most of their stellar mass and drew significant amounts of dark matter within their optical radii. Conversely, dwarf early-types experienced environmental processes that quenched their star formation during either the early stages of cluster assembly or upon infall at later times. Somewhat perplexing is our finding that the internal dynamics of these galaxies are largely explained by their stellar masses. Lastly, Virgo spirals also suffer from their dense environment, through ram pressure stripping and/or tidal harrassment. In addition to quenching, these effects leave an imprint on their internal dynamical evolution too. Late-type spirals exhibit evidence of having ejected significant amounts of baryons from their inner regions, likely via energetic feedback events. Rich as our picture of the history of the Virgo cluster has become, real progress in our understanding of this system will truly benefit from future high-resolution cosmological and hydrodynamic simulations of this environment. Such simulations are still in their infancy, but the data assembled here should soon provide their most direct validation. / Thesis (Ph.D, Physics, Engineering Physics and Astronomy) -- Queen's University, 2013-09-30 23:32:48.575

We examine the evolution of globular star clusters, modelled as spherically symmetric stellar systems, using various techniques. Such clusters possess a central region of approximately uniform density which is referred to as the core. We concentrate our analysis on the evolution of the cluster after the core has undergone core collapse; a process where its radius decreases and its density increases. After this collapse, the system as a whole can expand in a self-similar fashion (homologous post-collapse evolution) which has long been thought to be due to gravitational interactions between different populations of single stars and binary stars in the core. We confirm this assumption by constructing a simple analytical model which combines much of the theoretical knowledge of previous research in the field. This model consists of two stellar populations, each defined by the mass of the individual stars, and a separate core. Our simple model is itself constructed from two simpler models – a twocomponent model without a core and a single mass model with a core – and takes into account the main gravitational interactions thought to drive the post-collapse evolution. To ensure that no important mechanisms have been neglected in our simple model, we will compare it with an N-body simulation. We compute our N-body models with NBODY6 (using a GPU version for large N). When we compare the N-body model with the simple model, we find qualitative agreement between them for most cases. Even though some mechanisms (e.g. escape of stars) are neglected in our simple model, we find that both models show homologous post-collapse evolution. We also review the homologous post-collapse Fokker-Planck model in the case of equal stellar masses derived by H´enon (1961) with the intention of extending this for the two-component case. We present our numerical solutions for H´enon’s model and find that our numerical solutions are in satisfactory agreement with the results shown in this paper. When we extend this work for a general two-component model (i.e. with no restriction on the number of heavier stars), we find that a homologous solution cannot be found with this approach. By contrast, we suggest that it would be possible to find a homologous two-component solution by extending the one-component solution published later by H´enon (1965), which differs from the earlier model by neglecting the external tidal field of the parent galaxy. Much of the work shown in this thesis would be relevant for such future study.

Formation of globular clusters (GCs), the Galactic bulge, or galaxy bulges in general is an important unsolved problem in Galactic astronomy. Homogeneous infrared observations of large samples of stars belonging to GCs and the Galactic bulge field are one of the best ways to study these problems. We report the discovery by APOGEE (Apache Point Observatory Galactic Evolution Experiment) of a population of field stars in the inner Galaxy with abundances of N, C, and Al that are typically found in GC stars. The newly discovered stars have high [N/Fe], which is correlated with [Al/Fe] and anticorrelated with [C/Fe]. They are homogeneously distributed across, and kinematically indistinguishable from, other field stars within the same volume. Their metallicity distribution is seemingly unimodal, peaking at [Fe/H] similar to -1, thus being in disagreement with that of the Galactic GC system. Our results can be understood in terms of different scenarios. N-rich stars could be former members of dissolved GCs, in which case the mass in destroyed GCs exceeds that of the surviving GC system by a factor of similar to 8. In that scenario, the total mass contained in so-called 'first-generation' stars cannot be larger than that in 'second-generation' stars by more than a factor of similar to 9 and was certainly smaller. Conversely, our results may imply the absence of a mandatory genetic link between 'second-generation' stars and GCs. Last, but not least, N-rich stars could be the oldest stars in the Galaxy, the by-products of chemical enrichment by the first stellar generations formed in the heart of the Galaxy.

La bêta lactoglobuline (βlg) est une protéine globulaire qui forme le constituant majoritaire du sérum du lait ou petit lait. Par chauffage la protéine se dénature irréversiblement, puis s’assemble pour former des agrégats ou gels présentant des structures très différentes selon les conditions environnementales, en particulier de pH et de force ionique. Des travaux récents ont montré la possibilité de créer des agrégats stables de βlg de forme sphérique, de 100 à 400 nm de diamètre dans une plage de pH bien spécifique. Ces particules sphériques que nous appelons microgels, sont potentiellement très intéressantes pour des applications dans l’agroalimentaire (blanchissement, stabilisation d’interfaces et encapsulation). L’objectif de la thèse est d’étudier le mécanisme de formation de ces microgels et leurs propriétés structurales dans différentes conditions environnementales afin de pouvoir créer de nouvelles fonctionnalités. La première partie de la thèse a consisté à étudier l’influence du pH sur la formation des microgels. Les suspensions stables de microgels sont formées par chauffage de la solution de βlg en absence de sel jusqu’à 50 g.L-1 de protéine si le pH est placé dans une gamme très étroite entre 5,75 et 6,1. La densité de ces particules sphériques est environ 150 g.L-1 et leur rayon hydrodynamique diminue de 200 nm à 75 nm en augmentant le pH. La formation de ces microgels entraine une augmentation de pH, qui est nécessaire pour obtenir une suspension stable. L’augmentation spontanée du pH pendant la formation des microgels entraine une augmentation de leur densité de charge à la surface qui a pour conséquence d'empêcher leur agrégation. Ce mécanisme d’auto-stabilisation n’est plus suffisant si le pH initial est inférieur à 5,75 et on observe alors la précipitation des microgels. Les microgels ne sont plus formés au-delà d’une valeur critique du pH initial. Dans ce cas, les agrégats fibrillaires sont formés avec un rayon hydrodynamique d’environ 15 à 20 nm. La seconde partie de ce travail traite de la formation des microgels induite par l’ajout des ions calcium. Nous avons montré que des suspensions stables de microgels peuvent être obtenues en chauffant les solutions de βlg en présence des ions calcium. Les conditions de formation des microgels ont été étudiées à différents pH entre 5.8 et 7.5 et différentes concentrations de protéine entre 5 et 100 g.L-1. Il existe un rapport molaire critique calcium/protéine (R) pour former des microgels qui est indépendant de la concentration de protéine. R diminue en diminuant le pH. Les microgels ont un rayon hydrodynamique qui varie entre 100 et 300 nm et leur densité est comprise entre 200 et 450 g.L-1. La détermination de quantité de calcium lié aux microgels indique que le paramètre crucial pour la formation des microgels est la densité des charges nettes des protéines natives. Les suspensions de microgels sont stables dans certaines gammes étroites de R mais s’agrègent et précipitent ou gélifient à des concentrations de calcium plus élevées. Dans la troisième partie, nous avons continué à étudier la formation des microgels dans les étapes initiales et observer leur croissance en présence des ions calcium. On a proposé un mécanisme de formation des microgels de βlg, qui commence par un processus de nucléation et croissance. Des nucléi de tailles bien définies sont formés à la première étape, puis ils continuent à grossir jusqu’à la taille finale des microgels. A des faibles concentrations de calcium les microgels sont stables. A des concentrations plus élevées, les microgels peuvent s’agréger pour former des agrégats plus grands et finalement un gel. La structure des gels de microgels est hétérogène à l’échelle de la microscopie confocale et similaire à celle formée en présence de NaCl 0.3M. Pourtant le processus de formation de ces gels n’est pas le même... / Beta lactoglobulin (βlg) is a major whey protein in the bovine milk. Upon heating above its denaturation temperature (which is pH-dependent), this globular protein undergoes molecular changes leading to the irreversible aggregation. Depending on the pH and ionic strength, either protein aggregates or gels exhibiting various structures and morphologies have been described. Very recently, it was found that in a narrow range of the pH close to iso-electric point, stable suspensions of rather monodisperse spherical particles with a radius of about a hundred nanometers were formed. These spherical particles which were called microgels might be of special interest for the production of liquid dispersions of β-lactoglobulin aggregates exhibiting various functionalities for food applications. The project on which I report here was a collaboration with the Nestlé Reseach Center (Lausanne, Switzerland) and its objective was to study the formation and structural properties of the microgels in different environmental conditions. The first part of the project is to study the influence of the pH on the formation of microgels. Stable suspensions of protein microgels are formed by heating salt free βlg solutions at concentrations up to about C = 50 g.L-1 if the pH is set within a narrow range between 5.75 and 6.1. The internal protein concentration of these spherical particles is about 150 g.L-1 and the average hydrodynamic radius decreases with increasing pH from 200 nm to 75 nm. The formation of the microgels leads to an increase of the pH, which is a necessary condition to obtain stable suspensions. The spontaneous increase of the pH during microgel formation leads to an increase of their surface charge density and inhibits secondary aggregation. This self-stabilization mechanism is not sufficient if the initial pH is below 5.75 in which case secondary aggregation leads to precipitation. Microgels are no longer formed above a critical initial pH, but instead short curved protein strands are obtained with a hydrodynamic radius of about 15-20 nm. The second part of the work is about the formation of microgels driven by the addition of calcium ions. We found that stable suspensions of spherical protein particles (microgels) can be formed by heating βlg solutions in the presence of calcium ions. The conditions for the calcium induced microgel formation were studied at different pH between 5.8 and 7.5 and different protein concentrations between 5 – 100 g.L-1. The results showed that a critical molar ratio of calcium to proteins (R) is needed to form microgels independent of the protein concentration. R decreases with decreasing pH. The microgels have a hydrodynamic radius ranging from 100 to 300 nm and their internal protein concentration ranges from 0.2 to 0.45 g.mL-1. The determination of calcium bound to the microgels suggests that the crucial parameter for microgel formation is the net charge density of the native proteins. The microgel suspensions are stable in a narrow range of R but aggregate at higher Ca2+ concentrations. In the third part, we continued to investigate the formation of microgels at initial step and how it is growing in the presence of calcium ions. We have proposed a mechanism of formation of blg microgels which follows a nucleation and growing process. The nucleus with define size are formed at the initial state and that is growing in size to reach final size of aggregates. At low calcium concentration it stabilizes and then we obtain a stable suspension of microgels. But at high concentrations, the microgels here can jump to form big aggregates and finally a gel. The structure of gel from microgels is heterogenous at the scale of confocal microscopy and similar to those formed in the presence of NaCl 0.3 M. However the process of formation of these gels is not the same...

We present Chandra/ACIS-S subarray observations of the quiescent neutron star (NS) low-mass X-ray binaries X7 and X5 in the globular cluster 47 Tuc. The large reduction in photon pile-up compared to previous deep exposures enables a substantial improvement in the spectroscopic determination of the NS radius and mass of these NSs. Modeling the thermal emission from the NS surface with a non-magnetized hydrogen atmosphere and accounting for numerous sources of uncertainties, we obtain for the NS in X7 a radius of R = 11.1(-0.7)(+0.8) km for an assumed stellar mass of M = 1.4 M-circle dot (68% confidence level). We argue, based on astrophysical grounds, that the presence of a He atmosphere is unlikely for this source. Due to the excision of data affected by eclipses and variable absorption, the quiescent low-mass X-ray binary X5 provides less stringent constraints, leading to a radius of R = 9.6(-1.1)(+0.9) km, assuming a hydrogen atmosphere and a mass of M. =. 1.4 Me. When combined with all existing spectroscopic radius measurements from other quiescent low-mass X-ray binaries and Type I X-ray bursts, these measurements strongly favor radii in the 9.9-11.2 km range for a similar to 1.5 M-circle dot NS and point to a dense matter equation of state that is somewhat softer than the nucleonic ones that are consistent with laboratory experiments at low densities.

Uma previsão fundamental do cenário L cold dark matter (LCDM) na formação de estruturas é que os halos galácticos de DM do tamanho da Via Láctea (MW) crescem pela acreção de subsistemas menores. Neste contexto, simulações deNcorpos prevêem um número de sub-halos de matéria escura, cujo tamanho e massa são comparáveis às galáxias anãs, que é muito maior do que as galáxias satélites conhecidas. Este é o que se convencionu chamar de problema das satélites faltantes (MSP). A interpretação mais popular do MSP é que os sub-halos de matéria escura menores são extremamente ineficientes na formação de estrelas, o que torna mais difícil detectá-los. Com a chegada dos grandes levantamentos fotométricos, nos últimos anos, a descoberta de uma nova população de galáxias satélites que orbitam a MW fornece evidências empíricas para acreditar que realmente existem várias galáxias pouco luminosas não detectadas ou que simplesmente habitam regiões no céu que ainda não foram observadas. Neste trabalho implementamos um algoritmo estatístico eficiente para detectar subestruturas ultra fracas da MW. O código, chamado SPARSEX, foi testado e otimizado usando um conjunto de objetos estelares previamente identificados nos dados do Sloan Digital Sky Survey (SDSS), conseguindo recuperar todos os objetos com sucesso. Além disso, a aplicação do algoritmo aos dados dos dois primeiro anos do Dark Energy Survey (DES) deu como resultado centenas de candidatos a sistemas estelares. Dezessete sistemas estelares detectados em comum com outras técnicas de busca por subestruturas, implementadas dentro do grupo de colaboração do DES, foram publicados em três artigos em 2015. Um dos candidatos publicados é o aglomerado estelar DES 1. DES1 foi detectado pelo código SPARSEX com uma alta significância estatística e aparece nas imagens do DES como uma concentração compacta de fontes pontuais azuis. O sistema estelar é consistente com uma população velha e pobre em metal. Assumindo dois diferentes perfis de densidade, os quais permitem estimar a probabilidade de que cada estrela realmente pertença ao sistema, determinamos uma distância heliocêntrica e uma magnitude absoluta total num intervalo de 77.6—87.1 kpc e 3.00 . MV . 2.21, respectivamente. O raio à meia-luz desse objeto, rh 9.88 pc, e a luminosidade são consistentes com um aglomerado estelar de baixa luminosidade do halo externo. DES1 também é x alongado (e 0.6), o que faz supor que este objeto está em estágio avançado de dissolução. Mais tarde, através de uma cuidadosa reanálise de nossos resultados, dois novos candidatos foram detectados, DES J01111341 e DES J0225+0304. Os candidatos estão localizados a uma distância heliocêntrica de 25 kpc e parecem também estar dominados por populações estelares velhas e pobres em metais. Suas distâncias ao plano orbital da galáxia anã de Sagitário, 1.73 kpc (DES J01111341) e 0.50 kpc (DES J0225+0304), indicam que eles estão possivelmente associados com a corrente da anã de Sagitário. O raio à meia-luz (rh ' 4.55 pc) e a luminosidade (MV ' +0.3) de DES J01111341 são consistentes com um aglomerado estelar ultra fraco, enquanto o raio à meia-luz (rh ' 18.55 pc) e a luminosidade (MV ' 1.1) de DES J0225+0304 colocam este objeto em uma região ambígua do plano tamanho-luminosidade entre aglomerados estelares e galáxias anãs. Determinações dos parâmetros característicos da corrente de Sagitário, tais como o espalhamento de metalicidade (2.18 . [Fe/H] . 0.95) e o gradiente de distância (23 kpc . D . 29 kpc), dentro da área amostrada do DES no hemisfério sul, também indicam uma possível associação com estes sistemas. Se esses objetos forem confirmados através de follow-up espectroscópico como sistemas ligados gravitacionalmente e compartilharem uma trajetoria Galáctica com a corrente de Sagitário, DES J01111341 e DES J0225+0304 seriam os primeiros sistemas estelares ultra fracos associados com tal corrente. Recentemente, nós reportamos a descoberta de um novo aglomerado estelar, DES 3. O novo sistema foi detectado como uma sobredensidade estelar nos dados do primeiro ano do DES e confirmado com follow-up fotométrico obtido com o Southerm Astrophysical Research (SOAR) Telecope. Nós determinamos que DES 3 está localizado a uma distância heliocêntrica de 76 kpc e é dominado por uma população velha (' 9.8Ganos) e pobre em metal ([Fe/H] ' 1.88). Embora os valores de idade e metalicidade de DES 3 são semelhantes aos aglomerados globulares, o seu raio à meia-luz (rh 6.5 pc) e a luminosidade (MV 1.9) são mais indicativos de um aglomerados estelar fraco. Com base no tamanho angular aparente, o DES 3, com um valor de rh 0.03, está entre os menores aglomerados estelares fracos conhecidos até à data. Estas novas detecções indicam que o censo de satélites da MW é ainda incompleto. A identificação e estudo de novos satélites em futuros surveys, como por exemplo o Large Synoptic Survey Telescope (LSST) será crucial para a nossa compreensão das subestruturas existentes no halo Galáctico e a evolução da Galáxia como um todo. / A fundamental prediction of the L cold dark matter (LCDM) scenario of structure formation is that galactic DM haloes of the size of the Milky Way (MW) grow by the accretion of smaller sub-systems. In this context, Nbody simulations predict a number of dark matter subhalos, with size and mass comparable to dwarf galaxies, but which is much larger than currently known satellite galaxies. This is what is conventionally called the missing satellites problem (MSP). The most popular interpretation of the MSP is that the smaller dark matter subhalos are extremely inefficient in star formation, making it more difficult to detect them. With the arrival of large photometric surveys, in recent years, the discovery of a new population of satellite galaxies orbiting the MW provides empirical evidence to believe that there are actually several low luminosity galaxies that were not yet detected or that simply inhabit regions in the sky that have not yet been observed. In this work we present an efficient statistical algorithm to detect ultra-faint MW substructures. The code, called SPARSEX, was tested and optimized using a set of stellar objects previously identified in the Sloan Digital Sky Survey (SDSS) data. It has detected successfully all known objects. In addition, the algorithm was applied on the first two years of Dark Energy Survey (DES) data, resulting in hundreds of stellar system candidates. Seventeen stellar systems detected in common with other substructure search techniques implemented within the DES collaboration were published in three papers in 2015. In particular, one published candidate is a star cluster, DES 1. DES 1 was detected by the SPARSEX code with high statistical significance and appears in DES images as a compact concentration of blue point sources. The stellar system is consistent with being dominated by an old and metal-poor population. Assuming two different density profiles, based on which we may evaluate a membership probability for each star, we determined a heliocentric distance and total absolute magnitude in the ranges of 77.6—87.1 kpc and 3.00 . MV . 2.21, respectively. The half-light radius of this object, rh 9.88 pc, and luminosity are consistent with a low-mass halo star cluster. DES1 is also elongated (e 0.6), which suggests that this object is in advanced stage of dissolution. Later, through a careful reanalysis of our results, two new candidates were detected, DES J01111341 e DES J0225+0304. The candidates are located at a heliocentric xii distance of 25 kpc and appear to have old and metal-poor populations as well. Their distances to the Sagittarius dwarf orbital plane, 1.73 kpc (DES J01111341) and 0.50 kpc (DES J0225+0304), indicate that they are possibly associated with the Sagittarius dwarf stream. The half-light radius (rh ' 4.55 pc) and luminosity (MV ' +0.3) of DES J01111341 are consistent with it being an ultra-faint star cluster, while the half-light radius (rh ' 18.55 pc) and luminosity (MV ' 1.1) of DES J0225+0304 place it in an ambiguous region of size-luminosity space between star clusters and dwarf galaxies. Determinations of the characteristic parameters of the Sagittarius stream, such as its metallicity spread (2.18 . [Fe/H] . 0.95) and distance gradient (23 kpc . D . 29 kpc), within the DES footprint in the Southern hemisphere, also indicate a possible association with these systems. If theses objects are confirmed through spectroscopic follow-up to be gravitationally bound systems and to share a Galactic trajectory with the Sagittarius stream, DES J01111341 and DES J0225+0304 would be the first ultra-faint stellar systems associated with the Sagittarius stream. Recently, we reported the discovery of a new star cluster, DES 3. The new system was detected as a stellar overdensity in first-year DES data, and confirmed with deeper photometry from the Southern Astrophysical Research (SOAR) telescope. We determine that DES 3 is located at a heliocentric distance of 76 kpc and it is dominated by an old (' 9.8 Gyr) and metal-poor ([Fe/H] ' 1.88) population. While the age and metallicity values of DES 3 are similar to globular clusters, its half-light radius (rh 6.5 pc) and luminosity (MV 1.9) are more indicative of faint star clusters. Based on the apparent angular size, DES 3, with a value of rh 0.03, is among the smallest faint star clusters known to date. These new detections indicate that the MW satellites census is still incomplete. The identification and study of new satellites in future surveys, such as the Large Synoptic Survey Telescope (LSST), will be crucial to our understanding of substructures in the Galactic halo and the evolution of the Galaxy as a whole.

Fornecemos uma amostra de 170 Aglomerados Globulares Galácticos (GCs) e analisamos as propriedades de sua distribuição espacial. Utilizando um vasto catálogo de nuvens escuras identificadas, listamos os GCs que estão atrás de uma ou mais delas e que podem estar submetidos a uma extinção mais complexa do que a considerada por mapas de extinção. Valores de incerteza em distância são obtidos da literatura recente e comparados com valores derivados de uma fórmula de propagação de erro. GCs são agrupados de acordo com características inusitadas, tais como idades relativamente jovens ou possível conexão com núcleos de galáxias anãs, de forma que o efeito desses grupos pode ser isolado na distribuição espacial geral. Adicionalmente, computamos o centróide da distribuição de GCs e estudamos como esse se relaciona com a distância ao centro da Galáxia. Considerando que uma formação galáctica via colapso monolítico é supostamente simétrica, investigamos assimetrias e como os valores de incerteza das distâncias as modificam. Velocidades espaciais e um potencial Galáctico são empregados para verificar se quaisquer assimetrias na distribuição espacial são devidas a objetos em movimento coerente, ou se são somente efeitos transientes. / We provide a sample of 170 Galactic Globular Clusters (GCs) and analyse its spatial distribution properties. Using a comprehensive dust cloud catalogue, we list the GCs that are behind one or more identified dust clouds and could be subjected to a more complex extinction curve than extinction catalogues consider. Distance uncertainty values are gathered from recent literature and compared to values derived from an error propagation formula. GCs are grouped according to unusual characteristics, such as relatively young age or possible connection to dwarf galaxy nuclei, so that their effect on the general distribution can be isolated. Additionally, we compute the centroid of the GC distribution and study how it relates to the distance to the centre of the Galaxy. Considering that galactic formation via monolithic collapse is expected to be symmetrical, we probe asymmetries and how distance uncertainty values modify them. Spatial velocities and a Galactic potential are used to verify if any asymmetries in the spatial distribution are due to co-moving objects, or if they are merely transient effects.

Mycobacterium tuberculosis (Mtb), one of the major pathogens of mankind, kills approximately 2 million people each year. Mtb induces inflammation at the site of infection, leading to leakage of serum proteins, which in turn, are likely to come in contact with the pathogen, thus modulate the pathogenesis of tuberculosis. We studied some of these proteins such as surfactant protein D (SP-D), complement protein C1q and fibronectin, which are either produced locally or they leak-out from serum during inflammation, for their interaction with M.smegmatis and BCG. These non-pathogenic mycobacteria were used as model for Mtb. In this study, the recombinant form of truncated human surfactant protein D (rhSP-D) and three globular heads of human C1q (ghA, ghB, and ghC) were expressed in E.coli. The interaction of each of these proteins with mycobacteria and human monocytic cell line THP-1, was examined via ELISA. We demonstrated that rhSP-D, C1q, three globular heads of C1q and fibronectin bind with both mycobacteria and THP-1 cells. Moreover, using rhSP-D and globular heads of C1q, the binding of SP-D and C1q was localised to C-terminal globular regions. The direct effect for each of these proteins on mycobacterial growth, their effect on the uptake and intracellular fate of mycobacteria inside THP-1 cells were also investigated. Direct interaction of rhSP-D and C1q inhibited mycobacterial growth, whereas fibronectin interaction with the mycobacteria increased their growth. RhSP-D inhibited the uptake and growth of mycobacteria inside THP-1 cells, whereas C1q and each individual globular heads of C1q enhanced the uptake of mycobacteria by THP-1 cells. However, C1q protein inhibited BCG growth but enhanced M.smegmatis growth inside these cells and the later activity was localised to ghA. Fibronectin increased the uptake and growth of mycobacteria inside THP-1 cells. Examining the gene expression of inducible nitric oxide synthase, pro-inflammatory and anti-inflammatory cytokines produced by THP-1 cells infected with the proteins treated and untreated mycobacteria, along with cytokine neutralization experiments, suggest that the nitric oxide components and cytokines could be responsible for mycobacterial growth control inside THP-1 cells. These novel and interesting functions of SP-D, C1q, and fibronectin on mycobacteria provide an insight into the modulatory function of these proteins on Mtb infection, and, therefore, in the pathogenesis of tuberculosis.

No description available.

Beta lactoglobulin (βlg) is a major whey protein in the bovine milk. Upon heating above its denaturation temperature (which is pH-dependent), this globular protein undergoes molecular changes leading to the irreversible aggregation. Depending on the pH and ionic strength, either protein aggregates or gels exhibiting various structures and morphologies have been described. Very recently, it was found that in a narrow range of the pH close to iso-electric point, stable suspensions of rather monodisperse spherical particles with a radius of about a hundred nanometers were formed. These spherical particles which were called microgels might be of special interest for the production of liquid dispersions of β-lactoglobulin aggregates exhibiting various functionalities for food applications. The project on which I report here was a collaboration with the Nestlé Reseach Center (Lausanne, Switzerland) and its objective was to study the formation and structural properties of the microgels in different environmental conditions. The first part of the project is to study the influence of the pH on the formation of microgels. Stable suspensions of protein microgels are formed by heating salt free βlg solutions at concentrations up to about C = 50 g.L-1 if the pH is set within a narrow range between 5.75 and 6.1. The internal protein concentration of these spherical particles is about 150 g.L-1 and the average hydrodynamic radius decreases with increasing pH from 200 nm to 75 nm. The formation of the microgels leads to an increase of the pH, which is a necessary condition to obtain stable suspensions. The spontaneous increase of the pH during microgel formation leads to an increase of their surface charge density and inhibits secondary aggregation. This self-stabilization mechanism is not sufficient if the initial pH is below 5.75 in which case secondary aggregation leads to precipitation. Microgels are no longer formed above a critical initial pH, but instead short curved protein strands are obtained with a hydrodynamic radius of about 15-20 nm. The second part of the work is about the formation of microgels driven by the addition of calcium ions. We found that stable suspensions of spherical protein particles (microgels) can be formed by heating βlg solutions in the presence of calcium ions. The conditions for the calcium induced microgel formation were studied at different pH between 5.8 and 7.5 and different protein concentrations between 5 - 100 g.L-1. The results showed that a critical molar ratio of calcium to proteins (R) is needed to form microgels independent of the protein concentration. R decreases with decreasing pH. The microgels have a hydrodynamic radius ranging from 100 to 300 nm and their internal protein concentration ranges from 0.2 to 0.45 g.mL-1. The determination of calcium bound to the microgels suggests that the crucial parameter for microgel formation is the net charge density of the native proteins. The microgel suspensions are stable in a narrow range of R but aggregate at higher Ca2+ concentrations. In the third part, we continued to investigate the formation of microgels at initial step and how it is growing in the presence of calcium ions. We have proposed a mechanism of formation of blg microgels which follows a nucleation and growing process. The nucleus with define size are formed at the initial state and that is growing in size to reach final size of aggregates. At low calcium concentration it stabilizes and then we obtain a stable suspension of microgels. But at high concentrations, the microgels here can jump to form big aggregates and finally a gel. The structure of gel from microgels is heterogenous at the scale of confocal microscopy and similar to those formed in the presence of NaCl 0.3 M. However the process of formation of these gels is not the same...