Using data from the SCUBA Legacy Catalogue (850 µm) and Spitzer (3.6 - 70 µm), we explore dense cores in the Ophiuchus, Taurus, Perseus, Serpens, and Orion molecular clouds. In particular, we focus on identifying which cores host young stars while others remain starless. Understanding the nature of star formation and the influence of local environment will give us insight into several key properties, such as the origin of stellar mass. Here, we present starless and protostellar core mass functions (CMFs) for the five clouds. We develop a new method to discriminate starless from protostellar cores, using Spitzer colours and positions. We found best-fit slopes to the high-mass end of −1.26±0.20, −1.22±0.06, −0.95±0.20, and −1.85±0.53 for Ophiuchus, Taurus, Perseus, and Orion, respectively. We were unable to fit a slope to our fifth cloud, Serpens. Broadly, these slopes are consistent with the −1.35 power-law seen in the Salpeter IMF, but suggest some differences. We examined a variety of trends between these CMF shapes and their parent cloud properties, potentially finding a correlation between the high-mass slope and temperature. We also attempt to predict what future surveys with SCUBA-2 will detect in each of our clouds.

The process of particle growth in a warm cloud caused by coalescence is studied. The purely probabilistic model introduced by Gillespie [J. Atmos. Sci. 29 (1972) 1496-1510j is used and solved exactly by the aid of the Monte Carlo algorithm developed by Gillespie [J. Atmos. Sci. 32 (1975) 1977-1989]. Another approach uses the kinetic coalescence equation which is solved numerically using finite difference methods. It is known that the stochastic completeness of the kinetic coalescence equation depends on the extent of correlations between particles. Our objective is to compare these two models and analyze the suitability of the kinetic coalescence equation to simulate the coalescence process using a Brownian diffusion collision kernel. The stochastic coalescence model introduced by Gillespie is discussed in detail. A description of Gillespie's Monte Carlo simulation procedure and the numerical code that implements this algorithm in Fortran are provided. This algorithm is applied to the coalescence kernel for Brownian diffusion and initial Poisson and uniform droplet size distributions. Numerical methods which can he applied to the continuous and the discrete forms of the kinetic equation are described. The discrete form of this equation is solved by using Euler's and the fourth order Runge-Kutta methods. Solutions from the two models at early and later times are examined and the effect of the number of droplets used in simulations is investigated. It is shown that solutions agree well for early and later times using large and relatively small number of droplets initially. The problem of the growth of a large particle as it settles through a monodisperse suspension of small elemental particles is considered. It is demonstrated that the solution to the stochastic equation predicts about twice the growth rate of a large particle than the kinetic model. To validate solutions obtained by the stochastic algorithm, the convergence of the solution to Poisson distribution as time increases is studied. It is shown that the normalized average concentration obtained from the initial uniform and Pois¬son distributions in the stochastic coalescence model can be approximated by the Marshall-Palmer distribution function well known in the cloud physics community. The results of numerical simulations of the coalescence process using Brownian diffusion suggest that the kinetic equation in general produces an average size spec-trum that well matches the stochastic average spectrum. However, in the case of poorly mixed suspensions when correlations between particles are more important, these two models predict different size distributions, which is expected.

The relative importance of physical processes occurring on the various scales within molecular clouds is strongly debated, partly due to the lack of systematic cloud-wide observations available until recently. My thesis characterizes the kinematics of star formation across the entire Perseus molecular cloud as well as in a suite of simulations, providing statistical measures that successful theories of star formation will have to explain. My thesis consists of three interconnected projects described below. Dense core survey: The kinematics of the dense cores in Perseus were measured through single pointing observations of the N2H+(1–0) and C18O(2–1) transitions, tracing the dense core gas and surrounding lower density gas respectively. The internal velocity dispersion of the dense cores was observed to be small – dominated by thermal motions, and roughly the size expected for the cores to be in virial equilibrium. The dense cores also have little motion with respect to the surrounding low density gas – usually much less than the ambient sound speed of the medium. Comparison to cloud survey: The dense core observations were compared to a full spectral cube of 13CO(1–0) emission from the COMPLETE Survey, tracing the lower-density cloud material. From this analysis, it was determined that the dense cores have little motion with respect to the larger structures that they inhabit – smaller than the typical velocity dispersion or the estimated virial velocity dispersion of the region. Analysis of simulations: A suite of thin-sheet MHD simulations with varying levels of input magnetic field strengths and turbulence were analyzed in a manner to mimic the above observational surveys. While the small internal velocity dispersion of the dense cores could be reproduced by most of the simulations, the small motion between the core and its surrounding lower density gas could not be produced at the same time as the observed large-scale non-thermal motions. Future directions: The kinematic measures presented here will be straightforward to apply to future multi-cloud surveys as well as other numerical simulations. This will allow the effect of environment on star formation to be better explored in both the observational and simulated domains.

No description available.

This dissertation presents a series of work related to the representation of the Hadley circulation (HC) in atmospheric reanalyses and general circulation models (GCMs), with connections to the underlying tropical and subtropical cloud systems that comprise the mean meridional circulation. An intercomparison of eight atmospheric reanalyses showed that significant variability exists in the mean state for HC intensity, with less variability in HC width. Ensemble trends were broadly consistent with previous work and suggest a strengthening and widening of the tropical circulation over the last 30 years. Composite profiles of the apparent heat source and moisture sink were calculated for the International Satellite Cloud Climatology Project (ISCCP) cloud regimes using sounding observations from 10 field campaigns. Distinct heating profiles were determined for each ISCCP cloud regime, ranging from strong, upper-tropospheric heating for mesoscale convective systems to integrated cooling for populations associated with marine stratus and stratocumulus clouds. The derived profiles were generally similar over land and ocean with the notable exception of the fair-weather cumulus regime, which leads to some uncertainty in the mid- and upper-level reconstruction of subtropical heating. An instrument simulator indicated that low-latitude cloud properties from the NASA MERRA reanalysis qualitatively matched the distributions of cloud-top pressure and optical thickness in the ISCCP data, though the tallest and thickest clouds were missing from the reanalysis. Simulator results were sensitive to the choice of cloud overlap parameterization and the reanalysis consistently underpredicted the observed cloud fractions for all regimes. The vertical velocity, temperature, and moisture for each regime in MERRA largely matched observations from previous studies, suggesting that the dynamic and thermodynamic properties of the cloud regimes are well captured by the reanalysis. Finally, HC interannual variability was examined as a function of the observed frequency of the ISCCP cloud regimes. The strongest HC overturning events were attributed to an El Niño response in the central Pacific Ocean in addition to links between the intensity and position of the Pacific ITCZ. The ISCCP regime describing the most vigorous and organized convection contributed the most towards the total anomalous heating during HC extremes, despite an overall low frequency of occurrence. Idealized GCM simulations forced with the observed three-dimensional diabatic heating from ISCCP data produced too strong a HC with some improvement in other fields. Overall, much progress has been made regarding the links between low-latitude cloud systems and the HC, though future work will continue to address the upscale feedbacks of regional cloud variations upon the tropical circulation.

Thesis (Ph.D.)--McMaster University (Canada), 1991. / Source: Dissertation Abstracts International, Volume: 53-01, Section: B, page: 0178. Supervisor: John A. Davies.

Thesis (Ph.D.)--York University, 2005. Graduate Programme in Earth and Space Science. / Typescript. Includes bibliographical references (leaves 181-196). Also available on the Internet. MODE OF ACCESS via web browser by entering the following URL: http://wwwlib.umi.com/cr/yorku/fullcit?pNR11647

Revisiting a crime scene is a vital part of investigating a crime. When physically visiting a crime scene there is however always a risk of contaminating the scene, and when working on a cold case, chances are that the physical crime has been altered. This thesis aims to explore what tools a criminal investigator would need to investigate a crime in a virtual environment and if a virtual reconstruction of a crime scene can be used to aid investigators when solving crimes. To explore these questions, an application has been developed in Unreal Engine that uses virtual reality (VR) to investigate a scene, reconstructed from data that has been obtained through laser scanning. The result is an application where the user is located in the court of Stockholm city, which was scanned with a laser scanner by NFC in conjunction with the terror attack on Drottninggatan in April 2017. The user can choose between a set of tools, e.g. a measuring tool and to place certain objects in the scene, in order to draw conclusions of what has happened. User tests with criminal investigators show that this type of application might be of use in some way for the Swedish police. It is however not clear how or when this would be possible which can be expected since this is a new type of application that has not been used by the police before.

Les mécanismes de formation des nuages de glace arctiques durant la nuit polaire sont encore mal définis en raison de l’absence d’observations et de l’éloignement de cette région. Pourtant, leur influence sur les conditions météorologiques et sur le climat dans l’hémisphère nord est d’une importance primordiale ; et les connaissances sur la modification de leurs propriétés, liées à des processus d’interaction aérosol-nuage, doivent être améliorées. Les fortes concentrations d’aérosols en Arctique durant la nuit polaire sont associées au transport des aérosols anthropiques des latitudes moyennes jusqu’au pôle Nord. Les observations et les modèles montrent que cela peut conduire à un transport important de particules d’aérosol acidifiées. Les mesures en laboratoire et in situ montrent qu’à basse température (< -30°C), le revêtement d’acide sur les noyaux glaçogènes (IN) peut réduire leurs propriétés de nucléation de la glace. Par conséquent, leur concentration est réduite dans ces régions entraînant une plus faible concentration de plus gros cristaux de glace en raison d’une diminution de la compétition pour une humidité disponible similaire. De nombreuses mesures de terrain et par télédétection par satellite (CloudSat et CALIPSO) révèlent l’existence de deux types de nuages de glace (TIC) en Arctique durant la nuit polaire. Les nuages de glace de type 1 (TIC-1) ne sont visibles que par le lidar tandis que les nuages de glace de type 2 (TIC-2) sont perçus à la fois par le lidar et le radar. Les TIC-2 sont divisés en TIC-2A et TIC-2B. Les TIC-2A sont recouverts d’une fine couche de petits cristaux de glace non-précipitant (invisible par le radar) (TIC-1), tandis que les TIC-2B ne le sont pas. Ils sont caractérisés par une faible concentration de gros cristaux de glace. On suppose que la microstructure des TIC-2B est liée à l’acidification des aérosols. Pour vérifier cette hypothèse, des études de cas et des approches statistiques ont été combinées afin d’analyser le transport des aérosols et les propriétés des nuages de glace en Arctique. La première partie de la thèse enquête sur les propriétés microphysiques des TIC-1/2A et TIC-2B, en analysant des mesures aéroportées et satellitaires de cas spécifiques observés durant la campagne de mesures ISDAC (Alaska, Avril 2008). Pour la première fois, les microstructures des TIC-1/2A et TIC-2B en Arctique sont comparées en utilisant les observations in-situ des nuages. (...) La deuxième partie de la thèse enquête sur l’origine des masses d’air formant deux cas spécifiques de TICs ISDAC : TIC-1/2A (1 Avril 2008) et TIC-2B (15 Avril 2008), en utilisant des outils de trajectoire et des données satellitaires. / Arctic ice cloud formation during winter is poorly understood mainly due to the lack of observations and the remoteness of this region. Yet, their influence on Northern Hemisphere weather and climate is of paramount importance, and the modification of their properties, linked to aerosol-cloud interaction processes, needs to be better understood.Large concentration of aerosols in the Arctic during winter is associated to long-range transport of anthropogenic aerosols from the mid-latitudes to the Arctic. Observations and models show that this may lead to a significant transport of acidified aerosol particles. Laboratory and in-situ measurements show that at cold temperature (< -30°C), acidic coating may reduce the ice nucleating properties of ice nuclei (IN). Therefore, the IN concentration is reduced in these regions, resulting to a smaller concentration of larger ice crystals and because of the reduced competition for the same available moisture.Extensive measurements from ground-based sites and satellite remote sensing (CloudSat and CALIPSO) reveal the existence of two Types of Ice Clouds (TICs) in the Arctic during the polar night and early spring. The first Type of Ice Clouds (TIC-1) are visible only by the lidar while the second Type of Ice Clouds (TIC-2) are detected by both the lidar and radar. TIC-2 are divided into TIC-2A and TIC-2B. TIC-2A are topped by a cover of non-precipitating very small (radar-unseen) ice crystals (TIC-1), while TIC-2B are not. They are characterized by a low concentration of large ice crystals. It is hypothesized that the observed low concentration of large ice crystals, leading to precipitation (e.g. cloud regime TIC-2B), is linked to the acidification of aerosols. To check this, we are combining case studies and statistical approaches to analyse aerosol transport and cloud properties in the Arctic.The first part of the thesis investigate the microphysical properties of TIC-1/2A and TIC-2B, analysing airborne in-situ and satellite measurements of specific cases observed during the ISDAC campaign (Alaska, April 2008). For the first time, Arctic TIC-1/2A and TIC-2B microstructures are compared using in-situ cloud observations. Results show that the differences between them are confined in the upper part of the clouds where ice nucleation occurs. TIC-2B were characterized by fewer (< 10 L-1) and larger (> 110 μm) ice crystals, a larger ice supersaturation (> 15 %) and a fewer ice nuclei (IN) concentration (< 2 order of magnitude) when compared to TIC-1/2A. Ice crystal growth in TIC-2B clouds seems explosive whereas it seems more gradual in TIC-1/2A. It is hypothesized that these differences are linked to the number concentration and the chemical composition of aerosols. The second part of the thesis investigate the origin of air masses forming two specific cases ; TIC-1/2A (1 April 2008) and TIC-2B (15 April 2008), using trajectory tools and satellite data.(...)

O objetivo desta tese é analisar aspectos do sistema de satélites da Via Láctea de relevância cosmológica. Dentre estes aspectos destacam-se dois: o censo de satélites da Galáxia – onde constata-se que a quantidade destes objetos é muito inferior ao predito por modelos cosmológicos do tipo Matéria Escura Fria – e a frequência anômala de satélites luminosos, como a Pequena e Grande Nuvem de Magalhães (SMC e LMC respectivamente). Além disso, a determinação dos parâmetros estruturais da LMC pode impor vínculos a sua formação, histórico orbital e sobre a massa de nossa Galáxia. Neste trabalho é desenvolvida uma técnica de busca por satélites da Via Láctea. Esta técnica foi otimizada para utilizar dados da nova geração de grandes surveys de maneira eficiente. Este código, o FindSat, foi validado em uma amostra de galáxias anãs conhecidas e se mostrou eficiente em detectar as galáxias anãs mais tênues de que se tem registro. A aplicação desse código a uma região do Sloan Digital Sky Survey (SDSS) ainda não explorada nesse sentido revelou uma série de candidatos a novos satélites. Foram selecionados os candidatos mais promissores para observação de follow-up. Estas observações revelaram que um destes candidatos é de fato um novo satélite da Via Láctea. Este novo objeto é muito provavelmente um aglomerado globular do halo em estágio avançado de dissolução, porém, seu tamanho e magnitude integrada colocamno em um domínio limítrofe entre aglomerado e galáxia anã. Através da cuidadosa análise dos demais candidatos, constatou-se que nenhum outro é de fato um novo satélite da Galáxia. Além disso, foi realizado o estudo do perfil de densidade e geometria da LMC. Este estudo utilizou dados de verificação científica do Dark Energy Survey (DES). Constatase que o perfil de densidades para estrelas jovens (< 3 Gyr) possui um raio de escala cerca de 50% menor que o da população velha (> 3 Gyr), favorecendo o cenário de formação tipo outside-in. O estudo da extensão da componente estelar da LMC revela um raio de maré de cerca de 18 kpc, permitindo o cálculo da massa dinâmica total da LMC. O valor de massa obtido favorece a hipótese onde as Nuvens de Magalhães estariam por sua primeira passagem pelo perigaláctico. Além disso, a distância heliocêntrica e espessura do disco da LMC foram determinadas utilizando estrelas do Red Clump (RC). Notou-se que regiões no extremo norte da LMC estão sistematicamente mais próximas de nós do que o esperado, este efeito evidencia o warp no disco dessa galáxia. Observou-se que a espessura do disco aumenta na periferia da LMC, caracterizando o fenômeno de flare. O aumento na espessura juntamente com a maior extensão da população velha da LMC é interpretado como a presença de dois componentes discoidais. Esta é a primeira evidência desse tipo baseada apenas em métodos de contagem de estrelas. / The goal of this thesis is to analyse comologically relevant aspects of the Milky Way (MW) satellite system. Among these we may highlight two: the census of MW satellites – where the observed number of these objects is much less than what is expected by Cold Dark Matter (CDM) models – and the anomalous frequency of luminous satellites, such as the Small and Large Magellanic Clouds (SMC and LMC respectively). Besides the cosmological importance of the Clouds, the determination of its structural parameters may help to constraint models for their formation, orbital history, and ultimately the mass assembly in our Galaxy. In this work a technique to search newMWsatellites is developed. This technique was optimized to run efficiently on large datasets, such as the ones being generated by the new generation of surveys. The code, FindSat was validated in a sample of well known MW satellites and has proven to be well succeeded even for the most faint of these objects. The application of this code to an unexplored region of the Sloan Digital Sky Survey (SDSS) revealed a large amount of new dwarf galaxy candidates, some of which where selected for follow-up observation. These observations led to the discovery of a new MW satellite. This new object is most likely a globular cluster in an extreme stage of dissolution. However, its integrated magnitude and size makes it difficult to discern it from a dwarf galaxy. By a careful analysis of the remaining candidates, it was shown that no other new satellite was in the sample. The density profile and geometry of the LMC was also analysed. This study used the recent science verification data from the Dark Energy Survey (DES). It was found that the density profile for young stars (< 3 Gyr) has a scale radius 50% smaller when compared to the one obtained for older stars (> 3 Gyr). This result favours the outsidein galaxy formation scenario. The total extension of the LMC stellar component was measured, allowing the estimate of a truncation radius of about 18 kpc. Assuming that this truncation has tidal origins the dynamical mass of the LMC is inferred. The mass value found favours the case for the first perigalactic passage of the Clouds. Besides that, the heliocentric distance and thickness of the LMC disk was determined using Red Clump (RC) stars. Evidence for warp was found in the North edge of the LMC, in the sense that the disk is systematically more distance than expected. While the thickness of the disk increases towards the outer parts of the LMC, which is a phenomena known as flare. This effect joined with the fact that the older LMC stellar population is more extended, favours the presence of two disk components in this galaxy. This is the first evidence of this kind based only on star counts.