For a sample of collisional ring galaxies, archival Hubble Space Telescope images were used to compare individual star clusters and kpc-sized clumps of star formation to each other in a variety of ways. For each galaxy, instrument, and filter, the magnitude of the brightest cluster in a clump was compared to the magnitude of the entire clump, and the fraction of the flux of the clusters in a clump over the flux of the entire clump was calculated and compared to star formation rates. In addition, a cluster luminosity function for each galaxy was derived. Comparing the brightest cluster in a clump to the magnitude of the entire clump and the flux ratio to the star formation rate did not show any significant patterns. However, the α found for the galaxies tended to be much flatter than what had been found in previous research. The α found seemed to be affected by the size of the bin used in the luminosity function. Using this information, α could be calculated for other incredibly luminous galaxies to see if the trend of flatter α continues.

Cette thèse explore la question ouverte des mécanismes selon lesquels les galaxies lointaines évoluent au cours du temps. Elle se concentre sur l’étude des galaxies irrégulières et sur la cause de l’évolution en taille des galaxies passives et compactes. Bien que des régions de formation stellaire très lumineuses (clumps) soient observées dans les galaxies irrégulières depuis longtemps, leur nature et évolution sont encore débattues. Les instabilités gravitationnelles des disques ont été proposées comme la cause principale pour la formation in-situ des clumps, même si certains d’entre eux pourraient avoir une origine ex-situ. De plus, il n’est pas encore clair s’ils peuvent vivre longtemps ou si les vents stellaires les détruisent rapidement. À partir de l’étude détaillée d’un clump très jeune que nous avons découvert dans le disque d’une galaxie à redshift z~2 et de l’analyse d’un échantillon statistique, j’ai conclu que les clumps peuvent se former in-situ et qu’ils vivent typiquement 500 Myr. Ce résultat conforte les simulations numériques qui indiquent que les clumps ont un rôle important pour la croissance de leur noyau. Cela pourrait stabiliser le disque et y avoir un lien avec la formation des galaxies compactes et passives qui ont été decouvertes à haut redshift. Elles ont des tailles significativement plus petites, à masse égale, que celles de leurs homologues locales. Cette découverte a déclenché un débat concernant les possibles mécanismes qui peuvent augmenter leur taille sans altérer leur masse. J’ai analysé un échantillon de 32 galaxies et j’ai conclu que des multiples fusions mineures pourraient être les responsables principaux de leur evolution temporelle / This thesis explores the still unanswered question of how distant galaxies evolve through cosmic time: on one side it focuses on star-forming clumpy galaxies, on the other it investigates the size evolution of passive compact ones. Despite star forming clumps have been observed in high-redshift irregular galaxies since a while, their nature and fate are still highly debated. Violent gravitational disk instability in gas-rich, turbulent galaxies has been proposed as the main cause for in-situ clumps formation, although a fraction of them might have an ex-situ origin. Furthermore, clumps contribution to galaxy evolution is highly debated: it is not clear yet if they are long-lived or if stellar feedback rapidly disrupts them. From both the in-depth study of an extremely young clump that we discovered in the disk of a galaxy at redshift z ~ 2, and the analysis of a full statistical sample, I concluded that at least some clumps form in-situ due to violent disk instability and that they typically live ~ 500 Myr. This supports numerical simulations indicating that clumps are longlived and could play an important role in bulge growth. This might stabilize the disk, quench star formation and have therefore a link with the formation of the compact and passive galaxies that have been observed at high redshift. They have significant smaller sizes, at fixed stellar mass, than local counterparts. This discovery has ignited an important debate concerning the possible mechanisms that could inflate the galaxy sizes without altering much their mass. I analyzed a sample of 32 galaxies and I concluded that multiple minor mergers could be the main drivers of their observed time evolution

Since high-mass stars form deeply embedded within dense molecular clumps, the evolution of young stars and of dense clumps is inextricably linked. Previous datasets, however, lack the information necessary to test the prevailing theories. Definitive tests require a sufficiently large sample of molecular clumps and maps of their gas temperatures, column densities, velocity dispersions, and velocities at a spatial resolution comparable to, or smaller than, the clump scale (~1 pc). The Radio Ammonia Mid-Plane Survey (RAMPS), a new molecular line survey of thermal NH3 and H2O masers, provides the necessary data. In this dissertation, I used RAMPS data and archival datasets to test several theories of high-mass star formation and to investigate the co-evolution of molecular clumps and high-mass stars. All theories of high-mass star formation make testable predictions regarding clump kinematics and gravitational stability. Analyses of RAMPS kinematic data revealed that the majority of molecular clumps, particularly those in early evolutionary stages, are unstable to gravitational collapse. Further, they display infall motions, a key prediction of the theory of competitive accretion. I also investigated the kinematics of molecular filaments by comparing their measured velocity gradients to those predicted by hydrodynamical simulations. The measured spatial distributions of velocity gradients are inconsistent with existing models. Feedback from protostars and stars is predicted to alter the properties of surrounding clumps. I investigated feedback size scales and found that high-mass protostellar and stellar feedback significantly changes the temperatures, chemical abundances, and velocity dispersions of clumps on scales of ~0.3 to 3 pc. Finally, I observed a massive molecular cloud filament undergoing an interaction with a supernova shock, which is accelerating, heating, and injecting turbulence into the filament's gas. Although the molecular cores hosted by the filament may remain gravitationally bound, the filament is gravitationally unbound and likely being dispersed. Given that the shock is removing a reservoir of gas that could have been accreted by the cores, these data suggest that the supernova is inhibiting star formation.

<p>Haematology instruments using optical and fluorescence techniques have improved the platelet count in domestic animals. There are still some difficulties present, especially when counting cat thrombocytes due to their ability to aggregate and the occurrence of large platelets.</p><p>The objective of this study was to evaluate and compare the platelet count, mean platelet volume and platelet crit in dogs, horses and cats on Advia 2120 and Sysmex XT-2000iV.</p><p>Fresh blood samples from 64 dogs, 40 horses and 39 cats with various medical conditions were analysed on both instruments. Manual blood smears of all feline samples were scrutiniously analysed to evaluate the aggregation warning flag from Advia.</p><p>There was good agreement between the instruments for the optical platelet count in dogs and cats. Slightly higher values were reported from Advia. Samples from horses presented poor correlations for all studied parameters. Platelet clumps appeared in 70% of the 37 scrutinized feline blood smears, while 46% of the samples generated aggregation warning flags from the Advia instrument.</p><p>Advia and Sysmex showed good agreement for platelet counts in blood from dogs and cats. Mean platelet volume and platelet crit need further evaluation before conclusions can be made concerning their clinical relevance. The sensitivity of the platelet aggregation warning flag from the Advia instument needs further elevation.</p>

Haematology instruments using optical and fluorescence techniques have improved the platelet count in domestic animals. There are still some difficulties present, especially when counting cat thrombocytes due to their ability to aggregate and the occurrence of large platelets. The objective of this study was to evaluate and compare the platelet count, mean platelet volume and platelet crit in dogs, horses and cats on Advia 2120 and Sysmex XT-2000iV. Fresh blood samples from 64 dogs, 40 horses and 39 cats with various medical conditions were analysed on both instruments. Manual blood smears of all feline samples were scrutiniously analysed to evaluate the aggregation warning flag from Advia. There was good agreement between the instruments for the optical platelet count in dogs and cats. Slightly higher values were reported from Advia. Samples from horses presented poor correlations for all studied parameters. Platelet clumps appeared in 70% of the 37 scrutinized feline blood smears, while 46% of the samples generated aggregation warning flags from the Advia instrument. Advia and Sysmex showed good agreement for platelet counts in blood from dogs and cats. Mean platelet volume and platelet crit need further evaluation before conclusions can be made concerning their clinical relevance. The sensitivity of the platelet aggregation warning flag from the Advia instument needs further elevation.

Active Galactic Nuclei (AGN) are compact regions in the centers of some galaxies. They emit significantly in the whole range of the electromagnetic spectrum and show variability at different timescales. Observational evidence suggests the presence of a dusty torus obscuring the central radiation source of AGN. According to the Unified Model the observed general properties of AGN emission can be understood on the basis of orientation of this torus toward an observer. Two main types of AGN are distinguished: Type 1, with detected emission from the inner torus cavity viewed pole-on, and Type 2, viewed through the obscuring torus. There are numerous attempts in the past decade to model the emission from the torus, considering a homogeneous distribution of dust. However, important problems in explaining the observations still remain unsolved: it is hard to suppress the 10 m emission feature of silicate dust for a pole-on view and at the same time produce an absorption feature for an edge-on viewed torus; despite the huge optical depths inferred from X-ray observations of Type 2 sources, the observed absorption feature is shallow. Unlike observations, models of homogeneous tori with large optical depths always produce deep absorption feature. While it is realized that dust contained in clumps would resolve these issues, modeling of a clumpy medium poses a serious computational challenge. We are the first to incorporate clumps in our model of a dusty torus and to successfully explain the infrared emission from AGN. We model two types of clouds: directly illuminated by the AGN and diffusely heated by other clouds. We calculate the emission of the first type as angle-averaged emission from a dusty slab. The second type of clouds is modeled as dusty spheres embedded in the radiation field of the directly heated clouds. The radiative transfer problem for a dusty slab and externally heated sphere is solved exactly with our code DUSTY. The overall emission of the torus is found by integration over the spatial distribution of clouds. We find a very good agreement of our model results with observations. Comparison with them can constrain the physical conditions in the AGN dusty tori.

We calculated the fraction of ‘clumpy’ galaxies (fclumpy) for three samples of nearby galaxies. These samples include interacting galaxies with strong tidal features, collisional ring galaxies, and normal spiral galaxies. We define a ‘clumpy’ galaxy as a galaxy that has luminous star-forming regions contributing more than 8% of the total flux for the galaxy. We calculate fclumpy for 16 different wavelengths. We find that fclumpy is highest in the ultraviolet, Hα, and 24μm, while fclumpy is the lowest in optical and near-infrared wavelengths. We also see a significant increase in fclumpy for the interacting samples compared to the normal spirals.

At higher redshift galaxies exhibit increasingly irregular and clumpy morphologies, withstar-forming clumps dominating the FUV output of their host galaxies thus being inti-mately related to star formation and the formation and evolution of galaxies. This workexamines star-forming clumps in a remarkable, young spiral galaxy at Cosmic Noon witha redshift ofz= 2.584, lensed by the galaxy cluster Abell 2744. To this aim, NIRCamobservations in 7 filter bands are utilized to determine photometry of clumps and performbroadband SED fitting to determine characteristic sizes, ages and masses and infer theirdynamical ages and mass surface densities. The clump within this galaxy spans a widerange of properties with sizes between 20 to 200 pc and masses between 105M⊙and109M⊙. While clumps are not resolved down to scales of individual star clusters, small,dense clumps may host star clusters. A number of clumps exhibits agestage&gt;100 Myr,thus being able to survive feedback up to these timescales. This population of clumpsalso appears to be dynamically evolved and gravitationally bound as well as the denseststructures within the investigated sample, with roughly∼20% of clumps exhibiting masssurface densities comparable to bound stellar clusters in the local Universe.

The polarimetric and photometric variability of Wolf-Rayet (WR) stars as caused by clumps in the winds, is revisited. In the model which is improved from Li et al. 2000, the radial expansion of the thickness is accounted for, but we retain the dependence on the beta velocity law, stellar occultation effects. We again search for parameters that can yield results consistent with observations in regards to the mean polarization, the ratio of polarimetric to photometric variability, and the volume filling factor. Clump generation and spatial distribution are randomized by the Monte Carlo method so as to produce clumps which are, in the mean, distributed uniformly in space and have time intervals with a Gaussian distribution. The generated clumps move radially outward with a velocity law determined by a beta index, and the angular size of the clumps is assumed to keep fixed. By fitting the observational results and the volume filling factor, the clump velocity law index beta and clump ejection rate are inferred, and are found to be well constrained. In addition, the subpeak features on broad emission lines seem to support the clump ejection rate. Meanwhile, the fraction of the total mass loss rate that is contained in the clumps is obtained by fitting the observed polarization. We conclude that this picture for the clump properties produces a valuable diagnostic of WR wind structure.

The hot star wind momentum problem eta = M-upsiloninfinity/(L/c) much greater than 1 is revisited, and it is shown that the conventional belief, that it can be solved by a combination of clumping of the wind and multiple scattering of photons, is not self-consistent for optically thick clumps. Clumping does reduce the mass loss rate. M, and hence the momentum supply, required to generate a specified radio emission measure epsilon, while multiple scattering increases the delivery of momentum from a specified stellar luminosity L. However, in the case of thick clumps, when combined the two effects act in opposition rather than in unison since clumping reduces multiple scattering. From basic geometric considerations, it is shown that this reduction in momentum delivery by clumping more than offsets the reduction in momentum required, for a specified epsilon. Thus the ratio of momentum deliverable to momentum required is maximal for a smooth wind and the momentum problem remains for the thick clump case. In the case of thin clumps, all of the benefit of clumping in reducing lies in eta reducing. M for a given epsilon so that extremely small filling factors f approximate to 10(-4) are needed. It is also shown that clumping affects the inference of M from radio epsilon not only by changing the emission measure per unit mass but also by changing the radio optical depth unity radius R-rad, and hence the observed wind volume, at radio wavelengths. In fact, for free-free opacity proportional to n(2), contrary to intuition, R-rad increases with increasing clumpiness.