Détection et caractérisation de naines brunes et exoplanètes avec un filtre accordable pour applications dans l'espace

Cette thèse porte sur la capacité à détecter des compagnons de faible intensité en présence de bruit de tavelures dans le contexte de l’imagerie à haute gamme dynamique pour l’astronomie spatiale. On s’intéressera plus particulièrement à l’imagerie spectrale différentielle (ISD) obtenue en utilisant un étalon Fabry-Pérot comme filtre accordable. Les performances d’un tel filtre accordable sont présentées dans le cadre du Tunable Filter Imager (TFI), instrument conçu pour le télescope spatial James Webb (JWST). La capacité de l’étalon à supprimer les tavelures avec ISD est démontrée expérimentalement grâce à un prototype de l’étalon installé sur un banc de laboratoire. Les améliorations de contraste varient en fonction de la séparation, s’étendant d’un facteur 10 pour les séparations supérieures à 11 lambda/D jusqu’à un facteur 60 à 5 lambda/D. Ces résultats sont cohérents avec une étude théorique qui utilise un modèle basé sur la propagation de Fresnel pour montrer que les performances de suppression de tavelures sont limitées par le banc optique et non pas par l’étalon. De plus, il est démontré qu’un filtre accordable est une option séduisante pour l’imagerie à haute gamme dynamique combinée à la technique ISD. Une seconde étude basée sur la propagation de Fresnel de l’instrument TFI et du télescope, a permis de définir les performances de la technique ISD combinée avec un étalon pour l’astronomie spatiale. Les résultats prévoient une amélioration de contraste de l’ordre de 7 jusqu’à 100, selon la configuration de l’instrument. Une comparaison entre ISD et la soustraction par rotation a également été simulée. Enfin, la dernière partie de ce chapitre porte sur les performances de la technique ISD dans le cadre de l’instrument Near-Infrared Imager and Slitless Spectrograph (NIRISS), conçu pour remplacer TFI comme module scientifique à bord du Fine Guidance Sensor du JWST. Cent quatre objets localisés vers la région centrale de la nébuleuse d’Orion ont été caractérisés grâce à un spectrographe multi-objet, de basse résolution et multi-bande (0.85-2.4 um). Cette étude a relevé 7 nouvelles naines brunes et 4 nouveaux candidats de masse planétaire. Ces objets sont utiles pour déterminer la fonction de masse initiale sous-stellaire et pour évaluer les modèles atmosphériques et évolutifs futurs des jeunes objets stellaires et sous-stellaires. Combinant les magnitudes en bande H mesurées et les valeurs d’extinction, les objets classifiés sont utilisés pour créer un diagramme de Hertzsprung-Russell de cet amas stellaire. En accord avec des études antérieures, nos résultats montrent qu’il existe une seule époque de formation d’étoiles qui a débuté il y a environ 1 million d’années. La fonction de masse initiale qui en dérive est en accord avec des études antérieures portant sur d’autres amas jeunes et sur le disque galactique.

Imagerie à haut contraste et caractérisation d'exoplanètes par la spectroscopie intégrale de champ

Cette thèse porte sur l’amélioration des techniques d’imagerie à haut-contraste permettant la détection directe de compagnons à de faibles séparations de leur étoile hôte. Plus précisément, elle s’inscrit dans le développement du Gemini Planet Imager (GPI) qui est un instrument de deuxième génération pour les télescopes Gemini. Cette caméra utilisera un spectromètre à champ intégral (SCI) pour caractériser les compagnons détectés et pour réduire le bruit de tavelure limitant leur détection et corrigera la turbulence atmosphérique à un niveau encore jamais atteint en utilisant deux miroirs déformables dans son système d’optique adaptative (OA) : le woofer et le tweeter. Le woofer corrigera les aberrations de basses fréquences spatiales et de grandes amplitudes alors que le tweeter compensera les aberrations de plus hautes fréquences ayant une plus faible amplitude. Dans un premier temps, les performances pouvant être atteintes à l’aide des SCIs présentement en fonction sur les télescopes de 8-10 m sont investiguées en observant le compagnon de l’étoile GQ Lup à l’aide du SCI NIFS et du système OA ALTAIR installés sur le télescope Gemini Nord. La technique de l’imagerie différentielle angulaire (IDA) est utilisée pour atténuer le bruit de tavelure d’un facteur 2 à 6. Les spectres obtenus en bandes JHK ont été utilisés pour contraindre la masse du compagnon par comparaison avec les prédictions des modèles atmosphériques et évolutifs à 8−60 MJup, où MJup représente la masse de Jupiter. Ainsi, il est déterminé qu’il s’agit plus probablement d’une naine brune que d’une planète. Comme les SCIs présentement en fonction sont des caméras polyvalentes pouvant être utilisées pour plusieurs domaines de l’astrophysique, leur conception n’a pas été optimisée pour l’imagerie à haut-contraste. Ainsi, la deuxième étape de cette thèse a consisté à concevoir et tester en laboratoire un prototype de SCI optimisé pour cette tâche. Quatre algorithmes de suppression du bruit de tavelure ont été testés sur les données obtenues : la simple différence, la double différence, la déconvolution spectrale ainsi qu’un nouvel algorithme développé au sein de cette thèse baptisé l’algorithme des spectres jumeaux. Nous trouvons que l’algorithme des spectres jumeaux est le plus performant pour les deux types de compagnons testés : les compagnons méthaniques et non-méthaniques. Le rapport signal-sur-bruit de la détection a été amélioré d’un facteur allant jusqu’à 14 pour un compagnon méthanique et d’un facteur 2 pour un compagnon non-méthanique. Dernièrement, nous nous intéressons à certains problèmes liés à la séparation de la commande entre deux miroirs déformables dans le système OA de GPI. Nous présentons tout d’abord une méthode utilisant des calculs analytiques et des simulations Monte Carlo pour déterminer les paramètres clés du woofer tels que son diamètre, son nombre d’éléments actifs et leur course qui ont ensuite eu des répercussions sur le design général de l’instrument. Ensuite, le système étudié utilisant un reconstructeur de Fourier, nous proposons de séparer la commande entre les deux miroirs dans l’espace de Fourier et de limiter les modes transférés au woofer à ceux qu’il peut précisément reproduire. Dans le contexte de GPI, ceci permet de remplacer deux matrices de 1600×69 éléments nécessaires pour une séparation “classique” de la commande par une seule de 45×69 composantes et ainsi d’utiliser un processeur prêt à être utilisé plutôt qu’une architecture informatique plus complexe.

Stress analysis of carotid atheroma in transient ischemic attack patients: Evidence for extreme stress-induced plaque rupture

Plaque rupture has been considered to be the result of its structural failure. The aim of this study is to suggest a possible link between higher stresses and rupture sites observed from in vivo magnetic resonance imaging (MRI) of transient ischemic attack (TIA) patients, by using stress analysis methods. Three patients, who had recently suffered a TIA, underwent in vivo multi-spectral MR imaging. Based on plaque geometries reconstructed from the post-rupture status, six pre-rupture plaque models were generated for each patient dataset with different reconstructions of rupture sites to bridge the gap of fibrous cap from original MRI images. Stress analysis by fluid structure interaction simulation was performed on the models, followed by analysis of local stress concentration distribution and plaque rupture sites. Furthermore, the sensitivity of stress analysis to the pre-rupture plaque geometry reconstruction was examined. Local stress concentrations were found to be located at the plaque rupture sites for the three subjects studied. In the total of 18 models created, the locations of the stress concentration regions were similar in 17 models in which rupture sites were always associated with high stresses. The local stress concentration region moved from circumferential center to the shoulder region (slightly away from the rupture site) for a case with a thick fibrous cap. Plaque wall stress level in the rupture locations was found to be much higher than the value in non-rupture locations. The good correlation between local stress concentrations and plaque rupture sites, and generally higher plaque wall stress level in rupture locations in the subjects studied could provide indirect evidence for the extreme stress-induced plaque rupture hypothesis. Local stress concentration in the plaque region could be one of the factors contributing to plaque rupture.

Infrared non-detection of fomalhaut b: Implications for the planet interpretation

The nearby A4-type star Fomalhaut hosts a debris belt in the form of an eccentric ring, which is thought to be caused by dynamical influence from a giant planet companion. In 2008, a detection of a point source inside the inner edge of the ring was reported and was interpreted as a direct image of the planet, named Fomalhaut b. The detection was made at 600-800nm, but no corresponding signatures were found in the near-infrared range, where the bulk emission of such a planet should be expected. Here, we present deep observations of Fomalhaut with Spitzer/IRAC at 4.5 µm, using a novel point-spread function subtraction technique based on angular differential imaging and Locally Optimized Combination of Images, in order to substantially improve the Spitzer contrast at small separations. The results provide more than an order ofmagnitude improvement in the upper flux limit of Fomalhaut b and exclude the possibility that any flux from a giant planet surface contributes to the observed flux at visible wavelengths. This renders any direct connection between the observed light source and the dynamically inferred giant planet highly unlikely. We discuss several possible interpretations of the total body of observations of the Fomalhaut system and find that the interpretation that best matches the available data for the observed source is scattered light from a transient or semi-transient dust cloud. © 2012 The American Astronomical Society. All rights reserved.

GEMINI near-infrared spectroscopic observations of young massive stars embedded in molecular clouds

K-band spectra of young stellar candidates in four Southern hemisphere clusters have been obtained with the Gemini Near-Infrared Spectrograph in Gemini South. The clusters are associated with IRAS sources that have colours characteristic of ultracompact H II regions. Spectral types were obtained by comparison of the observed spectra with those of a near-infrared (NIR) library; the results include the spectral classification of nine massive stars and seven objects confirmed as background late-type stars. Two of the studied sources have K-band spectra compatible with those characteristic of very hot stars, as inferred from the presence of C IV, N III and N V emission lines at 2.078, 2.116 and 2.100 mu m, respectively. One of them, I16177_IRS1, has a K-band spectrum similar to that of Cyg OB2 7, an O3If* supergiant star. The nebular K-band spectrum of the associated Ultra-Compact (UC) H II region shows the s-process [Kr III] and [Se IV] high excitation emission lines, previously identified only in planetary nebula. One young stellar object was found in each cluster, associated with either the main IRAS source or a nearby resolved Midecourse Space eXperiment (MSX) component, confirming the results obtained from previous NIR photometric surveys. The distances to the stars were derived from their spectral types and previously determined JHK magnitudes; they agree well with the values obtained from the kinematic method, except in the case of IRAS 15408-5356, for which the spectroscopic distance is about a factor of 2 smaller than the kinematic value.

Avaliação com Doppler colorido e espectral da veia porta de cães

A perfusão total do fígado e suas contribuições relativas, pelo sistema portal e pela artéria hepática, podem estar alteradas por vários processos hepáticos, como doença hepato-celular difusa, neoplasia e shunts intra-hepáticos. O estudo do comportamento do fluxo sangüíneo nos vasos do fígado por meio da ultra-sonografia Doppler tem demonstrado que este é um método viável não-invasivo e de grande auxílio, principalmente na avaliação da hemodinâmica portal. São duas as modalidades de ultra-sonografia Doppler com maior aplicação na rotina para avaliação de fluxo nos vasos abdominais, o Doppler espectral e o Doppler colorido. Na doença hepática crônica, ocorre alteração da complacência hepática devido à fibrose ou à cirrose, as quais acarretam alterações vasculares, levando ao aumento da pressão venosa portal. As principais indicações desse exame são os casos em que há suspeita de hipertensão portal. A hemodinâmica portal é avaliada pela mensuração de sua área, da velocidade média, do volume de fluxo no vaso e do índice de congestão portal. Esta revisão de literatura tem como objetivo descrever os princípios físicos básicos da ultra-sonografia Doppler e sua aplicação na avaliação da hemodinâmica portal nos cães.

La PCA per la riduzione dei dati di SPHERE IFS

Nel primo capitolo di questa tesi viene presentata una panoramica dei principali metodi di rivelazione degli esopianeti: il metodo della Velocità Radiale, il metodo Astrometrico, il metodo del Pulsar Timing, il metodo del Transito, il metodo del Microlensing ed infine il metodo del Direct Imaging che verrà approfondito nei capitoli successivi. Nel secondo capitolo vengono presentati i principi della diffrazione, viene mostrato come attenuare la luce stellare con l'uso del coronografo; vengono descritti i fenomeni di aberrazione della luce provocati dalla strumentazione e dagli effetti distorsivi dell'atmosfera che originano le cosiddette speckle; vengono poi presentate le moderne soluzioni tecniche come l'ottica attiva e adattiva, che hanno permesso un considerevole miglioramento della qualità delle osservazioni. Nel terzo capitolo sono illustrate le tecniche di Differential Imaging che permettono di rimuovere efficacemente le speckle e di migliorare il contrasto delle immagini. Nel quarto viene presentata una descrizione matematica della Principal Component Analysis (Analisi delle Componenti Principali), il metodo statistico utilizzato per la riduzione dei dati astronomici. Il quinto capitolo è dedicato a SPHERE, lo strumento progettato per il Very Large Telescope (VLT), in particolare viene descritto il suo spettrografo IFS con il quale sono stati ottenuti, nella fase di test, i dati analizzati nel lavoro di tesi. Nel sesto capitolo vengono mostrate le procedure di riduzione dati e l'applicazione dell'algoritmo di IDL LA_SVD che applica la Principal Component Analysis e ha permesso, analogamente ai metodi di Differenzial Imaging visti in precedenza, di rimuovere le speckle e migliorare il contrasto delle immagini. Nella parte conclusiva, vengono discussi i risultati.

Orthogonal polarization spectroscopy to detect mesenteric hypoperfusion

OBJECTIVE: Orthogonal polarization spectral (OPS) imaging is used to assess mucosal microcirculation. We tested sensitivity and variability of OPS in the assessment of mesenteric blood flow (Q (sma)) reduction. SETTING: University Animal Laboratory. INTERVENTIONS: In eight pigs, Q (sma) was reduced in steps of 15% from baseline; five animals served as controls. Jejunal mucosal microcirculatory blood flow was recorded with OPS and laser Doppler flowmetry at each step. OPS data from each period were collected and randomly ordered. Samples from each period were individually chosen by two blinded investigators and quantified [capillary density (number of vessels crossing predefined lines), number of perfused villi] after agreement on the methodology. MEASUREMENT AND RESULTS: Interobserver coefficient of variation (CV) for capillary density from samples representing the same flow condition was 0.34 (0.04-1.41) and intraobserver CV was 0.10 (0.02-0.61). Only one investigator observed a decrease in capillary density [to 62% (48-82%) of baseline values at 45% Q (sma) reduction; P = 0.011], but comparisons with controls never revealed significant differences. In contrast, reduction in perfused villi was detected by both investigators at 75% of mesenteric blood flow reduction. Laser Doppler flow revealed heterogeneous microcirculatory perfusion. CONCLUSIONS: Assessment of capillary density did not reveal differences between animals with and without Q (sma) reduction, and evaluation of perfused villi revealed blood flow reduction only when Q (sma) was very low. Potential explanations are blood flow redistribution and heterogeneity, and suboptimal contrast of OPS images. Despite agreement on the method of analysis, interobserver differences in the quantification of vessel density on gut mucosa using OPS are high.

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits II. Survey description, results, and performances

Context. Young, nearby stars are ideal targets for direct imaging searches for giant planets and brown dwarf companions. After the first-imaged planet discoveries, vast efforts have been devoted to the statistical analysis of the occurence and orbital distributions of giant planets and brown dwarf companions at wide (>= 5-6 AU) orbits. Aims. In anticipation of the VLT/SPHERE planet-imager, guaranteed-time programs, we have conducted a preparatory survey of 86 stars between 2009 and 2013 to identify new faint comoving companions to ultimately analyze the occurence of giant planets and brown dwarf companions at wide (10-2000 AU) orbits around young, solar-type stars. Methods. We used NaCo at VLT to explore the occurrence rate of giant planets and brown dwarfs between typically 0.1 and 8 ''. Diffraction-limited observations in H-band combined with angular differential imaging enabled us to reach primary star-companion brightness ratios as small as 10(-6) at 1.5 ''. Repeated observations at several epochs enabled us to discriminate comoving companions from background objects. Results. During our survey, twelve systems were resolved as new binaries, including the discovery of a new white dwarf companion to the star HD8049. Around 34 stars, at least one companion candidate was detected in the observed field of view. More than 400 faint sources were detected; 90% of them were in four crowded fields. With the exception of HD8049 B, we did not identify any new comoving companions. The survey also led to spatially resolved images of the thin debris disk around HD61005 that have been published earlier. Finally, considering the survey detection limits, we derive a preliminary upper limit on the frequency of giant planets for the semi-major axes of [10, 2000] AU: typically less than 15% between 100 and 500 AU and less than 10% between 50 and 500 AU for exoplanets that are more massive than 5 M-Jup and 10 M-Jup respectively, if we consider a uniform input distribution and a confidence level of 95%. Conclusions. The results from this survey agree with earlier programs emphasizing that massive, gas giant companions on wide orbits around solar-type stars are rare. These results will be part of a broader analysis of a total of similar to 210 young, solar-type stars to bring further statistical constraints for theoretical models of planetary formation and evolution.

Temporal Coding of Volumetric Imagery

'Image volumes' refer to realizations of images in other dimensions such as time, spectrum, and focus. Recent advances in scientific, medical, and consumer applications demand improvements in image volume capture. Though image volume acquisition continues to advance, it maintains the same sampling mechanisms that have been used for decades; every voxel must be scanned and is presumed independent of its neighbors. Under these conditions, improving performance comes at the cost of increased system complexity, data rates, and power consumption.

This dissertation explores systems and methods capable of efficiently improving sensitivity and performance for image volume cameras, and specifically proposes several sampling strategies that utilize temporal coding to improve imaging system performance and enhance our awareness for a variety of dynamic applications.

Video cameras and camcorders sample the video volume (x,y,t) at fixed intervals to gain understanding of the volume's temporal evolution. Conventionally, one must reduce the spatial resolution to increase the framerate of such cameras. Using temporal coding via physical translation of an optical element known as a coded aperture, the compressive temporal imaging (CACTI) camera emonstrates a method which which to embed the temporal dimension of the video volume into spatial (x,y) measurements, thereby greatly improving temporal resolution with minimal loss of spatial resolution. This technique, which is among a family of compressive sampling strategies developed at Duke University, temporally codes the exposure readout functions at the pixel level.

Since video cameras nominally integrate the remaining image volume dimensions (e.g. spectrum and focus) at capture time, spectral (x,y,t,\lambda) and focal (x,y,t,z) image volumes are traditionally captured via sequential changes to the spectral and focal state of the system, respectively. The CACTI camera's ability to embed video volumes into images leads to exploration of other information within that video; namely, focal and spectral information. The next part of the thesis demonstrates derivative works of CACTI: compressive extended depth of field and compressive spectral-temporal imaging. These works successfully show the technique's extension of temporal coding to improve sensing performance in these other dimensions.

Geometrical optics-related tradeoffs, such as the classic challenges of wide-field-of-view and high resolution photography, have motivated the development of mulitscale camera arrays. The advent of such designs less than a decade ago heralds a new era of research- and engineering-related challenges. One significant challenge is that of managing the focal volume (x,y,z) over wide fields of view and resolutions. The fourth chapter shows advances on focus and image quality assessment for a class of multiscale gigapixel cameras developed at Duke.

Along the same line of work, we have explored methods for dynamic and adaptive addressing of focus via point spread function engineering. We demonstrate another form of temporal coding in the form of physical translation of the image plane from its nominal focal position. We demonstrate this technique's capability to generate arbitrary point spread functions.

Multiscale photoacoustic tomography using reversibly switchable bacterial phytochrome as a near-infrared photochromic probe.

Photoacoustic tomography (PAT) of genetically encoded probes allows for imaging of targeted biological processes deep in tissues with high spatial resolution; however, high background signals from blood can limit the achievable detection sensitivity. Here we describe a reversibly switchable nonfluorescent bacterial phytochrome for use in multiscale photoacoustic imaging, BphP1, with the most red-shifted absorption among genetically encoded probes. BphP1 binds a heme-derived biliverdin chromophore and is reversibly photoconvertible between red and near-infrared light-absorption states. We combined single-wavelength PAT with efficient BphP1 photoswitching, which enabled differential imaging with substantially decreased background signals, enhanced detection sensitivity, increased penetration depth and improved spatial resolution. We monitored tumor growth and metastasis with ∼ 100-μm resolution at depths approaching 10 mm using photoacoustic computed tomography, and we imaged individual cancer cells with a suboptical-diffraction resolution of ∼ 140 nm using photoacoustic microscopy. This technology is promising for biomedical studies at several scales.

Spectral Invariance of SG Pseudo-Differential Operators on L-P(R-n)

We prove the spectral invariance of SG pseudo-differential operators on L-P(R-n), 1 < p < infinity, by using the equivalence of ellipticity and Fredholmness of SG pseudo-differential operators on L-p(R-n), 1 < p < infinity. A key ingredient in the proof is the spectral invariance of SC pseudo-differential operators on L-2(R-n).

Differential binding of ppGpp and pppGpp to E-coli RNA polymerase: photo-labeling and mass spectral studies

(p) ppGpp, a secondary messenger, is induced under stress and shows pleiotropic response. It binds to RNA polymerase and regulates transcription in Escherichia coli. More than 25 years have passed since the first discovery was made on the direct interaction of ppGpp with E. coli RNA polymerase. Several lines of evidence suggest different modes of ppGpp binding to the enzyme. Earlier cross-linking experiments suggested that the beta-subunit of RNA polymerase is the preferred site for ppGpp, whereas recent crystallographic studies pinpoint the interface of beta'/omega-subunits as the site of action. With an aim to validate the binding domain and to follow whether tetra-and pentaphosphate guanosines have different location on RNA polymerase, this work was initiated. RNA polymerase was photo-labeled with 8-azido-ppGpp/8-azido-pppGpp, and the product was digested with trypsin and subjected to mass spectrometry analysis. We observed three new peptides in the trypsin digest of the RNA polymerase labeled with 8-azido-ppGpp, of which two peptides correspond to the same pocket on beta'-subunit as predicted by X-ray structural analysis, whereas the third peptide was mapped on the beta-subunit. In the case of 8-azido-pppGpp-labeled RNA polymerase, we have found only one cross-linked peptide from the beta'-subunit. However, we were unable to identify any binding site of pppGpp on the beta-subunit. Interestingly, we observed that pppGpp at high concentration competes out ppGpp bound to RNA polymerase more efficiently, whereas ppGpp cannot titrate out pppGpp. The competition between tetraphosphate guanosine and pentaphosphate guanosine for E. coli RNA polymerase was followed by gel-based assay as well as by a new method known as DRaCALA assay.