Nightly surveys of the skies detect thousands of new gravitational microlensing events every year. With the increasing number of telescopes, and advancements of the tech- nologies used, the detection rate is growing. Of these events, those that display the characteristics of a binary lens are of particular interest. They require special atten- tion with follow-up observations if possible, as such events can lead to new planetary detections. To characterise a new planetary event, high-cadence, accurate observations are optimal. However, without the ability of repeat observations, identification that any event may be planetary needs to happen before it finishes. I have developed a system that automatically retrieves all microlensing survey data and follow-up observations, models the events as single lenses, and publishes the results live to a web site. With minimal human interaction, the modelling system is able to identify and initialize binary events, and perform a thorough search of the seven dimensional parameter space of a binary lens. These results are also presented live through the web site, enabling observers an up to date view of the latest binary solutions. The real-time modelling of the system enables a prompt analysis of ongoing events, providing observers with the information, to determine if further observations are desired for the modelled events. An archive of all modelled binary lens events is maintained and accessible through the website. To date the archive contains 68 unique events’ binary lens solutions from the 2014 observing season. The system developed has been validated through model comparisons of previously published work, and is in use during the current observing season. This year it has played a role in identifying new planetary candidate events, confirming proposed solutions, and providing alternate viable solutions to previously presented solutions.

Thesis (MEng)--University of Stellenbosch, 2000. / ENGLISH ABSTRACT: In this thesis we addressed some issues concerning the automation of the detection, processing and the analysis of gravitational microlensing events, which are currently being used in the search for extra-solar planets. We were provided with a series of data images containing a microlensing event. Using these images we address several practical problems: registration, background subtraction and some PSF modelling. Registration is accomplished by using the intersection points of circular arcs drawn around stellar objects. After which the influence of the sky background is removed by using the watershedding algorithm and plane fitting. Our analysis is based on relative brightness - to counter seeing, the brightness of stars are calculated by isolating the objects from the background and summing over the area. A brightness variation curve is plotted and the trend of the lensing event and the posi tion of a blip are extracted using wavelets, calculating general trends and LOESS. The trend of the brightness variation curve can be used for both identification and classification of various events. It can also be used for the identification and classification of variable stars. Blip analysis is used to detect the presence of a planet (or dark body) in the vicinity of the source. / AFRIKAANSE OPSOMMING: Hierdie tesis beskryf tegnieke om die identifikasie, prosessering en analise van gravitasie mikro-lens gebeure te outomatiseer. Die analise van hierdie gebeure is belangrik aangesien dit gebruik word vir die opsporing van planete buite ons sonnestelsel. Om gebruik te maak van 'n reeks beelde wat een van hierdie gebeure vertoon moet ons die volgende probleme aanspreek: beeld registrasie, verwydering van die agtergrond en die modulering van die verspreiding van die lig van 'n puntbron deur die atmosfeer. Ons verkry registrasie deur die berekening van die snypunte van sirkels met middelpunte by sekere voorwerpe op die beeld. Na registrasie kan ons die invloed van die agtergrond bepaal deur gebruik te maak van die waterskeidingsalgoritme. Dit stelons in staat om die relatiewe helderheid van die voorwerpe ondersoek deur die voorwerpe te isoleer en te sommeer oor die area van 'n voorwerp. 'n Grafiese voorstelling van die helderhede dui vir ons die relatiewe variasies in die helderhede van die mikrolens objek tussen die beelde aan. Ons ondersoek die vorm van die kromme asook die moontlike voorkoms van 'n 'blip' deur middel van wavelet analiese en die LOESS metode. Die vorm van die kromme word gebruik vir die identifikasie en klassifikasie van die verskillende mikro-lens gebeure en kan uitgebrei word om ook veranderlike sterre te ondersoek. Die teenwoordighied van 'n 'blip' op die data wys op die moontlik teenwoordigheid van 'n planeet nabyaan die bron wat ons ondersoek.

Cette thèse traite de la détection d’exoplanètes et des propriétés statistiques de leurs orbites. Nous présentons d'abord de nouveaux développements dans la technique de microlentille gravitationnelle. Nous étudions les potentialités de découverte de systèmes inhabituels, comme des planètes flottantes, par des satellites en orbite autour de la Terre. Nous proposons ensuite deux nouvelles approches à la reconstruction d’images, ce qui pourrait mener à un gain de temps important dans l’interprétation des données d’observation. Nous redécouvrons d’abord le résultat peu connu de Asada (2002), en démontrant que l’équation bidimensionnelle des lentilles peut être réécrite en termes de systèmes triangulaires grâce au théorème de Labatie. Cela permet de résoudre une seule équation polynomiale réelle, au lieu de l’équation complexe habituelle. Nous proposons ensuite une nouvelle technique de reconstruction d’images basée sur la résolution d’un système d’équations différentielles ordinaires. Dans la deuxième partie de la thèse, nous faisons un premier pas vers une théorie statistique des architectures planétaires. Nous montrons que l’ensemble microcanonique de la dynamique séculaire dans le système solaire permet d’estimer assez précisément la densité de probabilité des paramètres orbitaux des planètes. Comme la dynamique future de nos planètes ne diffère pas essentiellement de l’excitation gravitationnelle à la quelle sont sujettes les exoplanètes dans la dernière phase de leur formation, un tel résultat constitue un indice préliminaire mais précieux de l’efficacité d’une approche statistique aux architectures planétaires. / This thesis deals with exoplanet detection and the statistical properties of planetary systems. In the first part of the dissertation, we present new developments in the technique of gravitational microlensing. We explore the potentialities of geosynchronous and low Earth orbit satellites to discover unusual systems, such as rogue planets and miniature planetary systems around low-mass brown dwarfs. We then propose two new approaches to image reconstruction, which could result in a precious speed-up when interpreting observational data. We first rediscover the not-well-known result of Asada (2002), demonstrating that the two-dimensional lens equation can be rewritten in terms of triangular systems via Labatie’s theorem. That allows to solve basically a single real polynomial equation, instead of the usual complex one. We then propose a technique of image reconstruction based on the resolution of a system of ordinary differential equations. This turns out to have a number of advantages, among them a straightforward application to the general case of N point-mass lenses. In the second part of the thesis, we take a first step towards a statistical theory of planetary architectures. We show that the microcanonical ensemble of secular dynamics in the solar system provides a very good guess of the probability density of the planet orbital elements over Gyr timescales. Since the future dynamics of our planets is essentially analogue to the gravitational excitation undergone by exoplanets during the final, gas-free phase of their formation, such a result constitutes a preliminary but valuable hint of the effectiveness of a statistical approach to planetary architectures.

In recent years, it has been shown that microlensing is a powerful tool for examining the atmospheres of stars in the Galactic bulge and Magellanic Clouds. The high gradient of magnification across the source during both small impact parameter events and caustic crossings offers a unique opportunity for determining the surface brightness profile of the source. Furthermore, models indicate that these events can also provide an appreciable polarization signal: arising from differential magnification across the otherwise symmetric source. Earlier work has addressed the signal from a scattering photosphere for both point mass lenses and caustic crossings. In a previous paper, polarimetric variations from point lensing of a circumstellar envelope were considered, as would be suitable for an extended envelope around a red giant. In this work, we examine the polarization in the context of caustic crossing events, the scenario that represents the most easily accessible situation for actually observing a polarization signal in Galactic microlensing. Furthermore, we present an analysis of the effectiveness of using the polarimetric data to determine the envelope properties, illustrating the potential of employing polarimetry in addition to photometry and spectroscopy with microlensing follow-up campaigns.

This paper examines line profile evolution due to the linear expansion of circumstellar material obsverved during a microlensing event. This work extends our previous papers on emission line profile evolution from radial and azimuthal flow during point mass lens events and fold caustic crossings. Both “flavours” of microlensing were shown to provide effective diagnostics of bulk motion in circumstellar envelopes. In this work a different genre of flow is studied, namely linear homologous expansion, for both point mass lenses and fold caustic crossings. Linear expansion is of particular relevance to the effects of microlensing on supernovae at cosmological distances. We derive line profiles and equivalent widths for the illustrative cases of pure resonance and pure recombination lines, modelled under the Sobolev approximation. The efficacy of microlensing as a diagnostic probe of the stellar environs is demonstrated and discussed

No description available.

Questo lavoro di tesi è dedicato al problema della ricerca e<br />della caratterizzazione della \emph(materia oscura). A livello<br />osservativo, su diverse scale, da quelle galattiche (in<br />particolare nella Via Lattea) fino all'intero universo, esiste<br />disaccordo tra le stime \emph(dinamiche) della massa di oggetti<br />astrofisici (come galassie o ammassi di galassie) rispetto alla<br />stima della loro massa \emph(luminosa). Si tratta, in un certo<br />modo, di un problema di massa \emph(mancante). Si rende così<br />necessaria, nell'ambito del quadro teorico del modello<br />cosmologico standard, l'introduzione di una componente di materia<br />``oscura'', nel senso che non emette radiazione elettromagnetica,<br />la cui presenza può essere rilevata attraverso effetti<br />gravitazionali. Nonostante la convergenza di prove osservative ed<br />esigenze teoriche a sostegno dell'ipotesi della sua esistenza, un<br />interrogativo a cui non è ancora stata data una risposta<br />basata su solide evidenze sperimentali è quello della stessa<br />natura di tale componente di massa.<br /><br />Affrontiamo in particolare il problema della materia oscura negli<br />aloni galattici, dove le evidenze osservative (curve di rotazione)<br />risultano più stringenti. Per questo analizziamo un insieme<br />originale di dati sperimentali (i dati ``MDM'', frutto di una<br />apposita campagna osservativa tuttora in corso di svolgimento<br />presso l'osservatorio Michigan-Dartmouth-MIT, USA) acquisiti per<br />lo studio della componente oscura sotto forma di oggetti massivi<br />compatti (MACHOs, \emph(Massive Astrophysical Compact Halo<br />Objects)) nell'alone della Galassia (la nostra Via Lattea) e<br />della galassia vicina di Andromeda, M31 (ovvero NGC224). Questa<br />ricerca si basa su di un effetto di natura gravitazionale, il<br />\emph(microlensing), ovvero la deflessione della luce generata da<br />un oggetto oscuro massivo in moto che attraversa la linea di vista<br />tra l'osservatore e una sorgente luminosa che si manifesta con un<br />incremento della luminosità della sorgente. Dallo studio di<br />queste variazioni di luminosità nel tempo è possibile<br />risalire, per via indiretta, alla distribuzione della materia<br />sotto forma di MACHOs nell'alone. L'analisi è stata condotta<br />con la tecnica detta del \emph(pixel lensing) (proposta e<br />implementata dalla collaborazione AGAPE, \emph(Andromeda Galaxy<br />Amplified Pixel Experiment)), che permette il rilevamento di<br />variazioni di luminosità di stelle \emph(non) risolte (in<br />particolare questo consente di considerare le possibili sorgenti<br />in una galassia distante come M31).<br /><br />Nel capitolo 1, introdotti gli elementi del modello cosmologico<br />standard e quindi il problema della materia oscura<br />nell'appropriato contesto cosmologico e astrofisico, delineamo i<br />principi del \emph(microlensing) gravitazionale e il metodo del<br />\emph(pixel lensing). Nel capitolo 2 descriviamo l'apparato<br />sperimentale e l'acquisizione dei dati (a cui chi scrive ha avuto<br />modo di partecipare direttamente). Quindi analizziamo in<br />dettaglio il trattamento preliminare delle immagini necessario<br />per rendere significativo il successivo studio dei segnali<br />astrofisici interessanti. In particolare vengono discussi alcuni<br />aspetti quali la composizione di più immagini e le operazioni<br />di ``normalizzazione'' del flusso. Nel capitolo 3 affrontiamo le<br />tematiche connesse all'analisi del segnale rispetto al problema<br />della selezione di eventi di \emph(microlensing). Il ``rumore''<br />di fondo che ne contamina la ricerca è costituito da sorgenti<br />intrensicamente variabili. Per questo consideriamo in dettaglio<br />il modo di sfruttare la caratteristica \emph(acromaticità)<br />del segnale che ci interessa. Basandoci su di una opportuna<br />simulazione consideriamo inoltre il problema dell'efficacia dei<br />criteri di selezione adottati. Discutiamo infine i risultati<br />delle simulazioni Monte Carlo dell'esperienza. Vengono quindi<br />approfonditi, nel capitolo 4, diversi aspetti legati all'analisi<br />effettuata. Rivolgiamo particolare attenzione allo studio degli<br />effetti cromatici delle variazioni di luminosità rilevate e<br />discutiamo in questa prospettiva segnali di sorgenti variabili e<br />in particolare alcuni attribuibili a delle \emph(novæ).<br />Esponiamo quindi un primo risultato dell'analisi, lo studio del<br />prolungamento sui nostri dati di candidati eventi<br />\emph(microlensing) rilevati da altre collaborazioni. Infine<br />discutiamo i risultati della selezione, 5 \emph(curve di luce)<br />(la variazione di flusso nel tempo in un elemento<br />dell'im\-ma\-gi\-ne) compatibili con un segnale di<br />\emph(microlensing), e, alla luce delle simulazioni Monte Carlo,<br />le conclusioni fisiche riguardo al problema posto.<br /><br />La nostra analisi tende a confermare (in accordo con i risultati<br />di analoghe esperienze svolte nell'ambito della Galassia) che solo<br />una piccola frazione degli aloni galattici è costituita da<br />MACHOs, e in particolare a escludere come componente importante<br />quella di oggetti di massa substellare.

L'effet de microlentille gravitationnelle est devenu un outil unique pour détecter des exoplanètes. Il se produit lorsqu'une étoile de premier plan (la microlentille) et une étoile d'arrière plan (la source) sont alignées avec la Terre. La lumière provenant de l'étoile la plus lointaine, souvent dans le bulbe galactique, est alors déviée par la microlentille située dans le disque. Au cours de ce phénomène, des images multiples de la source sont créées par la microlentille, plus grandes que la source, qui apparaît alors amplifiée. Si l'une de ces images multiples se forme au voisinage d'une planète, un pic d'amplification de la source survient, révélant sa présence. Après un tour d'horizon de l'état des connaissances dans le domaine des exoplanètes, nous décrivons les spécificités de la méthode des microlentilles dans ce domaine. Ensuite, nous présentons en détail la modélisation des microlentilles, de ses racines théoriques à la modélisation pratique des courbes de lumières expérimentales. Dans une troisième partie, nous présentons la détection de la première naine brune en orbite autour d'une étoile de type solaire par la méthode des microlentilles, et nous montrons en quoi cette technique ouvre des perspectives nouvelles et originales pour mieux connaître les mécanismes de formation de ces objets dont l'origine reste à identifier. Nous étudions enfin le potentiel de l'observation de microlentilles par interférométrie, en introduisant un nouveau formalisme adapté à l'étude conjointe des événements en photométrie et en interférométrie. Le manuscrit se termine par l'évaluation du nombre moyen d'événements de microlentille observables par interférométrie chaque année. / Gravitational microlensing effect has become a unique tool to detect and characterise exoplanets. A microlensing effect occurs when a foreground star (the microlens) and a background star (the source) are aligned with the Earth on the same line of sight. The light from the furthest star, usually in the Galactic bulge, is deflected by the microlens located on the disk. During this phenomenon, multiple images of the source are created by the lens, bigger than the source that consequently seems amplified. When one of these images are located in the vicinity of an exoplanet, a short amplification jump occurs revealing its presence. After a quick overview of the exoplanets field of research, I highlight the specificities of microlensing comparing to the other planets detection techniques. Then, I describe in details the modelling of microlensing effects, from a theoretical to a numerical point of view. In a third part, I describe the detection of the first brown dwarf orbiting a solar-type star using microlensing, strengthening the recent idea that microlensing will lead to a better understanding of the mechanisms involved in the brown dwarfs formation, still not fully understood. Finally, I investigate the potential of interferometric observations of microlensing events that will give, in the future, new original constrains on the microlens physical properties. First we introduce a new formalism that closely combines interferometric and microlensing observable quantities. Secondly, we determine an average number of events that are at reach of long baseline interferometers every year.

No description available.

The last twenty-five years have seen our understanding of the formation and abundance of planets revolutionised, thanks to the first detections of debris discs, and, a decade later, of the first extrasolar planets. Hardly a week now goes by without a planet discovery, and the range of methods used to search for planets has expanded to include techniques that are efficient at detecting different types of planets. By combining the discoveries of the various methods, we therefore have the opportunity to build a picture of planet populations across the Galaxy. In this thesis, I am presenting work done as a basis towards such an effort: first I present work carried out to improve modelling methods for gravitational microlensing events. Since the first microlensing observing campaigns, the amount of data of anomalous events has been increasing ever faster, meaning that the time required to model all observed anomalous events is putting a strain on available human and computational resources. I present work to develop a method to fit anomalous microlensing events automatically and show that it is possible to conduct a thorough and unbiased search of the parameter space, illustrating this by analysing an event from the 2007 observing season. I then discuss the possible models found with this method for this event, and their implication (Kains et al. 2009), and find that this algorithm locates good-fit models in regions of parameters that would have been very unlikely to be found using standard modelling methods. Results indicate that it is necessary to use a full Bayesian approach, in order to include prior information on the parameters. I discuss the analytical priors calculated by Cassan et al. (2009) and suggest a possible form of an automatic fitting algorithm by incorporating these priors in the algorithm used by Kains et al. (2009). Another topic with which this thesis is concerned is the evolution of debris discs around solar-type stars. Late-type stars are expected to be the most numerous host stars of planets detected with the microlensing technique. Understanding how their debris discs evolve equates to understanding the earliest stages of planet formation around these stars, allowing us to truly put our Solar System in perspective. Using the analytical model of Wyatt et al. (2007a), I modelled the evolution of infrared excess flux at 24 and 70 microns using published data of debris discs around solar-type (spectral types F, G and K) stars from the Spitzer Space Telescope. By comparing the results of this study to an analogous study carried out by for A stars by Wyatt et al. (2007b), I find that although best-fit parameters are significantly different for solar-type stars, this may be due to the varying number of inefficient emitters around stars of different spectral types. I suggest that although effective properties are different by an order of magnitude or more, intrinsic properties, while still different, are so by a much smaller factor. These differences may be due to the longer timescales over which solar-type stars evolve, which allow for the formation of larger and stronger planetesimals.