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GJ 436b is a prime target for understanding warm Neptune exoplanet atmospheres and a target for multiple James Webb Space Telescope (JWST) Guaranteed Time Observation programs. Here, we report the first space-based optical transmission spectrum of the planet using two Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) transit observations from 0.53 to 1.03 mu m. We find no evidence for alkali absorption features, nor evidence of a scattering slope longward of 0.53 mu m. The spectrum is indicative of moderate to high metallicity (similar to 100-1000x solar), while moderate-metallicity scenarios (similar to 100x. solar) require aerosol opacity. The optical spectrum also rules out some highly scattering haze models. We find an increase in transit depth around 0.8 mu m in the transmission spectra of three different sub-Jovian exoplanets (GJ 436b, HAT-P-26b, and GJ 1214b). While most of the data come from STIS, data from three other instruments may indicate this is not an instrumental effect. Only the transit spectrum of GJ 1214b is well fit by a model with stellar plages on the photosphere of the host star. Our photometric monitoring of the host star reveals a stellar rotation rate of 44.1 days and an activity cycle of 7.4 years. Intriguingly, GJ 436 does not become redder as it gets dimmer, which is expected if star spots were dominating the variability. These insights into the nature of the GJ 436 system help refine our expectations for future observations in the era of JWST, whose higher precision and broader wavelength coverage will shed light on the composition and structure of GJ 436b's atmosphere.

GJ. 1214b is the most studied sub-Neptune exoplanet to date. Recent measurements have shown its near-infrared transmission spectrum to be flat, pointing to a high-altitude opacity source in the exoplanet 's atmosphere, either equilibrium condensate clouds or photochemical hazes. Many photometric observations have been reported in the optical by different groups, though simultaneous measurements spanning the entire optical regime are lacking. We present an optical transmission spectrum (4500-9260 angstrom) of GJ. 1214b in 14 bins, measured with Magellan/IMACS repeatedly over three transits. We measure a mean planet-to-star radius ratio of Rp R-s = 0.1146. 2 x 10(-4) and mean uncertainty of sigma(R-p/R-s) = 8.7 x 10(-4) in the spectral bins. The optical transit depths are shallower on average than observed in the near-infrared. We present a model for jointly incorporating the effects of a composite photosphere and atmospheric transmission through the exoplanet's limb (the CPAT model), and use it to examine the cases of absorber and temperature heterogeneities in the stellar photosphere. We find the optical and near-infrared measurements are best explained by the combination of (1) photochemical haze in the exoplanetary atmosphere with a mode particle size r = 0.1 mu m and haze-forming efficiency f(haze) = 10% and (2) faculae in the unocculted stellar disk with a temperature contrast Delta T= 354(-46)(+46) K, assuming 3.2% surface coverage. The CPAT model can be used to assess potential contributions of heterogeneous stellar photospheres to observations of exoplanet transmission spectra, which will be important for searches for spectral features in the optical.

Seminario de Título entregado a la Universidad de Chile en cumplimiento parcial de los requisitos para optar al Título de Ingeniera en Biotecnología Molecular. / El desarrollo de una respuesta inmune anti-tumoral requiere de la comunicación entre diferentes células del sistema inmune, así como del reconocimiento de la célula tumoral. Una vez que los Linfocitos T Citotóxicos (CTL) y las células Natural Killers (NK) reconocen la célula tumoral, forman la Sinapsis Inmunológica Citotóxica (SIC), una estructura supramolecular altamente especializada que resulta fundamental para la liberación localizada de los gránulos citotóxicos y la eliminación específica de la célula tumoral. Recientemente, se ha descrito la participación de canales Gap Junction (GJ) formados por la isoforma Cx43 (GJ-Cx43) en la actividad citotóxica de las células NK durante la SIC. A pesar de las similitudes funcionales y estructurales presentadas por la SIC mediada por las células NK y por CTL, la participación de los canales GJ-Cx43 en la sinapsis mediada por CTL aún no ha sido determinada. En este trabajo se estudió el rol de los canales GJ-Cx43 en la actividad de la SIC entre CTL obtenidos desde ratones pMEL-1 y células de melanoma murino B16F10. Primero, se evaluó la polarización de Cx43 hacia la zona de contacto entre CTL pMEL-1 y células B16F10, durante la SIC. Se determinó que Cx43 se acumula en el sitio de contacto entre estas células de manera antígeno específica y que esta polarización es dependiente de la activación de los CTL. Luego, se disminuyó la expresión de Cx43 en células B16F10 utilizando un RNA interferente contra Cx43 y luego se evaluó la participación de Cx43 en la formación de canales GJ mediante ensayos de transferencia de calceína y en la actividad citotóxica de los CTL, mediante ensayos de actividad de Granzima B (GrzB). Se observó que los CTL transfieren calceína a las células B16F10 formando canales GJ funcionales, al contrario de cuando se utilizan LT CD8+ vírgenes como células efectoras. Además, cuando se utilizaron las células B16F10 que expresan bajos niveles de Cx43 como células blanco, se observó una disminución en la transferencia de calceína y en la actividad de GrzB en comparación al control. Nuestros resultados demuestran que durante el reconocimiento citotóxico se forman canales GJ-Cx43 entre CTL y células B16F10 y que la formación de estos canales durante la SIC son importantes para la eliminación de células tumorales mediada por CTL. / Development of antitumor immune responses requires communication between different immune cells, and specific immune recognition of tumor cells. Upon tumor cell recognition, CD8+ cytotoxic T lymphocytes (CTL) and natural killer (NK) cells form the “Cytotoxic Immunological Synapse (SIC)”, a specialized molecular structure fundamental for the polarized delivery of cytotoxic granules and the specific tumor cell killing. Recently, it has been described the participation of Gap Junction Intercellular Communications formed by Connexin 43 (GJIC-Cx43) in the NK cell SIC activity. Despite that CTL and NK cells present functional and structural similarities in SIC formation, the participation of GJIC-Cx43 in CTL-mediated SIC remains unclear. In this work we studied the role of GJIC-Cx43 in the activity of SIC formed between CTL from pMEL-1 mice and B16F10 murine melanoma cells. First, we evaluated by immunofluorescence the polarization of Cx43 to contact site between CTL and B16F10 during SIC. We found that this protein localizes at the contact site of SIC and this polarization dependent on activation of CTL and is an antigenic-specific process. Then, we decrease Cx43 expression in B16F10 cells using interference RNA against Cx43 and we evaluated the participation of Cx43 in the formation of functional GJ channels by calcein transfer assay and in the cytotoxic activity of CTL by Granzyme B (GrzB) activity assay. We found that CTL transfer calcein to B16F10 forming functional GJ in contrast with when we used a naïve CD8+ T cells as an effector cells. In addition, when we used a B16F10 that express low levels of Cx43 as target cells, we observed a decrease in calcein transfer and GrzB activity in comparison to the control. Our results demonstrate that GJIC-Cx43 are formed between CTL and B16F10 during SIC, and suggest that their formation is important for tumor cells-killing by CTL

This dissertation investigates two stellar systems known to contain extrasolar planets. It is comprised of five chapters that are readily divided into three independent but related analyses. Chapter 1 reports on the analysis of low signal-to-noise secondary-eclipse observations of the Neptune-sized exoplanet GJ 436b using the Spitzer Space Telescope in multiple infrared channels. The measured wavelength-dependent eclipse depths provide constraints on the planet’s dayside atmospheric composition and thermal profile. The analysis indicates that GJ 436b’s atmosphere is abundant in carbon monoxide and deficient in methane relative to thermochemical equilibrium models for the predicted hydrogen-dominated atmosphere. Chapter 2 discusses the techniques used to analyze GJ 436b, introduces the Least Asymmetry centering method and compares its effectiveness to two existing techniques, and describes the functions used to model Spitzer’s position- and time-dependent systematics. Additionally, it includes best-fit parameters with uncertainties, histograms of the free parameters, and correlation plots between free parameters. Chapter 3 reports on the analysis of eleven HD 149026b secondary-eclipse observations at five Spitzer wavelengths plus three primary-transit observations at 8.0 µm. Chemical-equilibrium models find no indication of a temperature inversion in the dayside atmosphere of HD 149026b. The best-fit model favors large amounts of CO and CO2 , moderate heat redistribution (f = 0.5), and a strongly eniii hanced metallicity. These analyses use BiLinearly-Interpolated Subpixel Sensitivity (BLISS) mapping and parameter orthogonalization. The former is a new technique to model two position-dependent systematics, intrapixel variability and pixelation. The latter is a technique that accelerates the convergence of Markov chains that employ the Metropolis random walk sampler. Chapter 4 reports on the detection of GJ 436c, a 0.65 ± 0.04 R⊕ exoplanet transiting a nearby M-dwarf star with a period of 1.365862 ± 8×10−6 days. It also presents evidence for a similarly sized exoplanet candidate (currently labeled UCF-1.02) orbiting the same star with an undetermined period. Assuming an Earth-like density of 5.515 g/cm3 , GJ 436c has a predicted mass of 0.28 Earth-masses (M⊕, 2.6 Mars-masses) and a surface gravity of 0.65 g (where g is the gravity on Earth). Its weak gravitational field and close proximity to its host star imply that GJ 436c is unlikely to have retained its original atmosphere; however, a transient atmosphere is possible if recent impacts or tidal heating were to supply volatiles to the surface. Chapter 5 presents numerical simulations of the GJ 436 system using the Mercury N-body integrator and detailed calculations used to constrain the atmospheric composition of the sub-Earth-sized planet GJ 436c. The simulations find a ∼35-year periodic trend in the osculating elements wherein GJ 436c’s eccentricity varies between 0 and 0.21, its peak-to-trough inclination amplitude is 3.2◦ , and transit-timing variations range from ±200 to ±3 minutes.

Estudo das ressonâncias de três corpos na zona habitável (ZH), da estrela GJ 581 (Gliese 581), envolvendo dois planetas conhecidos e um terceiro planeta dentro da ZH. Séries de Lie são usadas para obter o Hamiltoniano médio (de segunda ordem nas massas) e teoria de Chirikov é usada para gerar um novo sistema de varáveis canônicas em que os momentos se orientam ao longo e através da ressonância. Um mapa de Hadjidemetriou é construido e permite o cálculo rápido da difusão das órbitas em uma extensa grade de condições iniciais. / Study of three-body resonances in the habitable zone (ZH), the star GJ 581 (Gliese 581), involving two known planets, and a third planet in the ZH. Lie series are used to obtain the average Hamiltonian (the second-order mass) and Chirikov theory is used to generate a new canonical variables system in which the moments are oriented along and across the resonance. A map of Hadjidemetriou is constructed and allows rapid calculation of the diffusion of orbits in an extensive grid of initial conditions.

Estudo das ressonâncias de três corpos na zona habitável (ZH), da estrela GJ 581 (Gliese 581), envolvendo dois planetas conhecidos e um terceiro planeta dentro da ZH. Séries de Lie são usadas para obter o Hamiltoniano médio (de segunda ordem nas massas) e teoria de Chirikov é usada para gerar um novo sistema de varáveis canônicas em que os momentos se orientam ao longo e através da ressonância. Um mapa de Hadjidemetriou é construido e permite o cálculo rápido da difusão das órbitas em uma extensa grade de condições iniciais. / Study of three-body resonances in the habitable zone (ZH), the star GJ 581 (Gliese 581), involving two known planets, and a third planet in the ZH. Lie series are used to obtain the average Hamiltonian (the second-order mass) and Chirikov theory is used to generate a new canonical variables system in which the moments are oriented along and across the resonance. A map of Hadjidemetriou is constructed and allows rapid calculation of the diffusion of orbits in an extensive grid of initial conditions.

Žmogaus natūralus elgesys puikiai parodo sinchronizuotus akių ir rankos judesius. Akių-rankos koordinacija naudinga tiriant alternatyvius kompensacinius įtaisus, kurie gelbsti žmogaus ir kompiuterio sąveikai, kai reabilituojami žmonės su negale. Tiriamieji buvo paprašyti pravesti ranka kursorių labirinto trajektorija (pakankamai dideliu greičiu). Eksperimento metu akių judesiai buvo fiksuojami "EyeGaze" sistema sukurta "LC technologies LTd.". Rezultatuose nustatytos akių-rankos judesių koordinacijos strategijos: GJ - šuolinė ir GMS - sekimo strategija. / Human behavior in manual control coordinated by vision illustrates perfect synchronization between the gaze and position of the target, which is controlled by hand. Investigation of eye-hand coordination is useful for alternative control of computer cursor and for an assessment and rehabilitation of a sensorimotor system of patients. Subjects were asked to move the target along the labyrinth’s path quickly enough. During all experiments, movements of both eyes were recorded with eye tracker “EyeGaze System” produced by “LC Technologies Ltd.” Gaze tracking instrumentation was setup so, that to 1 deg eye angle corresponds to 46 pixels on computer screen. The results showed two eye-hand coordination strategies Gaze Jumps (GJ) and Gaze Moves Smoothly (GMS) during guiding self-moved target along Labyrinth path can be defined. During GJ strategy gaze elicit eye jumps in the direction of the future path. Average amplitude of the jumps is around 1.5 deg and frequency is in the 2-3 Hz range. During GMS strategy gaze is concentrated on the self-moved target and leads it only by small average distance (0.1-0.2 deg).

Au moment d'écrire ma Thèse plus de 900 exoplanètes été annoncées et plus de 2700 planètes détectées par le télescope spatial Kepler sont en attente d'être confirmées. La haute précision des spectres et des courbes de lumière obtenue dans les relevés Doppler et transit, permet l'étude détaillée des paramètres des étoiles hôtes, et ouvre la possibilité d'enquêter sur les corrélations étoile planètes. En outre, la détermination des paramètres stellaires avec précision est un besoin critique pour déterminer les paramètres planétaires, à savoir, la masse, le rayon et la densité.Dans le cas des naines FGK, la détermination des paramètres stellaires est bien établie et peut être utilisée avec confiance pour étudier la relation planète-étoile ainsi que pour obtenir les paramètres planétaires avec une grande precision. Cependant, ce n'est pas le cas pour les naines M, les étoiles les plus communes de la Galaxie. Par rapport à leurs cousines plus chaudes, les naines M sont plus petites, plus froides, et plus faiblement lumineuses, et donc plus difficile à étudier. Le plus grand défi qui concerne les naines M est lié à la présence de milliards de lignes moléculaires qui gomme le continuum et rend l'analyse spectrale classique presque impossible. Trouver des fac ̧ons nouvelles et novatrices pour surmonter cet obstacle et obtenir une mesure des paramètres stellaires est l'objectif principal de cette Thèse .Pour l'atteindre, j'ai concentré mes recherches sur deux approches méthodologiques, photométrique et spectroscopiques. Mon premier travail avait pour objectif d'établir l'étalonnage de métallicité pho- tométrique précis. Par manque de binaires FGK+M avec de bonnes données photométriques je ne pouvais pas atteindre cet objectif. Il m'a cependant était possible, avec les données disponibles, de comparer les étalonnages photométriques déjà établies et légèrement améliorer le meilleur d'entre eux, comme décrit au Chapitre 3.Puis, je me suis concentré sur les approches spectroscopiques pour obtenir des paramètres stel- laires plus précis pour les naines M. À cette fin, j'ai utilisé des spectres HARPS de haute résolution et développé une méthode pour mesurer les lignes spectrales sans tenir compte du continuum . En utilisant cette méthode, je créé un nouvel étalonnage visible avec une précision de 0.08 dex pour [Fe/H] et 80 K pourTeff .Ce travail est détaillé dans le Chapitre 4.Finalement , j'ai également participé à l'amélioration des paramètres de l'étoile GJ3470 et de sa planète, où mon expertise dans les paramètres stellaires de naines M avait un rôle important. Les détails concernant cette enquête sont présentés dans le Chapitre 5 / At the time of writing of this Thesis more than 900 planets have been announced and about 2700 planets from the Kepler space telescope are waiting to be confirmed. The very precise spectra and light curves obtained in Doppler and transit surveys, allows the in-depth study of the parameters of the host stars, and opens the possibility to investigate the star-plant correlations. Also, determining the stellar parameters with precision is critical for more precise determinations of the planetary parameters, namely, mass, radius, and density.In the case of the FGK dwarfs, the determination of stellar parameters is well established and can be used with confidence to study the star-planet relation as well as to obtain precise planetary parameters. However, this is not the case for M dwarfs, the most common stars in the Galaxy. Compared to their hotter cousins, M dwarfs are smaller, colder, and fainter, and therefore harder to study. The biggest challenge regarding M dwarfs is related to the presence of billions of molecular lines that depress the continuum making a classical spectral analysis almost impossible. Finding new and innovative ways to overcome this obstacle in order to obtain precise stellar parameters is the goal of this Thesis.To achieve this goal I focused my research into two main avenues: photometric and spectroscopic methods. My initial work had the objective of establishing a precise photometric metallicity calibration, but I could not reach this goal, as I did not have enough FGK+M binaries with good photometric data. However, it was possible, with the available data, to compare the already established photometric calibrations and slightly improve the best one, as described in Chapter 3.Then, I focused on spectroscopic approaches with the aim of obtaining precise M dwarf parame- ters. To this end I used HARPS high-resolution spectra and developed a method to measure the spectral lines disregarding the continuum completely. Using this method I established a new visible calibration with a precision of 0.08 dex for [Fe/H] and 80 K for Te f f . This work is detailed in Chapter 4.Finally, I also participated in the refinement of the parameters of the star GJ3470 and its planet, where my expertise in stellar parameters of M dwarfs had an important role. The details regarding this investigation are shown in Chapter 5. / No momento em que escrevo esta Tese, o número de planetas anunciados já ultrapassou os 900 e os cerca de 2700 candidatos detectados pelo telescópio espacial Kepler esperam por confirmação. Os espectros e as curvas de luz obtidos nos programas de procura de planetas permitem, também, o estudo em profundidade dos parâmetros das estrelas com planetas e abrem a possibilidade de investigar a relação estrela-planeta. Neste contexto, a determinação com precisão dos parâmetros estelares é crítica na determinação precisa dos parâmetros planetários, nomeadamente, a massa, o raio e a densidade.No caso das anãs FGK, os métodos de determinação dos parâmetros estelares estão bem estabelecidos e podem ser usados com confiança no estudo da relação estrela-planeta, assim como na obtenção de parâmetros planetários precisos. No entanto, não é esse o caso para as anãs M, as estrelas mais comuns da nossa Galáxia. Ao contrário das suas primas, as estrelas M são mais pequenas, frias e ténues e, assim sendo, mais difíceis de estudar. O grande entrave no estudo das estrelas M está relacionado com a presença de biliões de linhas moleculares que deprimem o contínuo espectral, fazendo com que uma análise espectral clássica se torne quase impossível. A procura de métodos inovadores que possibilitem ultrapassar este obstáculo, tendo em vista a obtenção de parâmetros precisos, é o objectivo desta Tese.Tendo em conta esse objetivo, foquei os meus esforços em duas linhas principais de pesquisa, baseadas em métodos fotométricos e métodos espectroscópicos. O meu trabalho inicial tinha como objetivo o estabelecimento de uma calibração fotométrica para a metalicidade, mas não me foi possível atingir esse objetivo, pois não tinha sistemas binários FGK+M suficientes com bons dados fotométricos. No entanto, foi possível, com os dados disponíveis, comparar as calibrações fotométricas existentes e refinar ligeiramente a melhor delas, como descrito no Capítulo 3.Após este trabalho passei a concentrar-me em técnicas espectroscópicas de obtenção de parâmetros estelares em estrelas M. Tendo em mente esse objetivo, usei espectros HARPS de alta resolução para desenvolver um novo método de medição de linhas espectrais independente do contínuo espectral. Seguidamente, usei este método no desenvolvimento de uma nova calibração de metalicidade e temperatura efectiva em estrelas M na região do visível, através da qual consegui atingir uma precisão de 0.08 dex para a [Fe/H] e de 80 K para a temperatura. Este trabalho está descrito no Capítulo 4.Ao mesmo tempo colaborei na determinação com precisão dos parâmetros da estrela GJ3470 e do seu planeta, onde a minha proficiência na determinação de parâmetros estelares em anãs M teve um papel importante. Os detalhes relacionados com este trabalho de investigação estão descritos no Capítulo 5.

Halogenhaltigen atmosphärischen Spurengasen wird eine Schlüsselrolle bei lokalen, regionalen und globalen Veränderungen der Erdatmosphäre zugesprochen. Die Photolyse dieser Stoffe durch ultraviolette Strahlung der Sonne führt zum Eintrag reaktiver Atome und Radikale in die Atmosphäre. Dies betrifft vor allem den stratosphärischen Ozonabbau, der nach heutigem Kenntnisstand durch Reaktionszyklen katalysiert wird und bei dem die Photolyse halogenhaltiger Spurengase an zentraler Stelle beteiligt ist. Im Rahmen dieser Arbeit wurden primäre Photoprozesse halogenhaltiger atmosphärischer Spurengase in Laborexperimenten charakterisiert. Dabei bestand das Ziel in der Bestimmung von primären Quantenausbeuten und Verzweigungsverhältnissen konkurrierender Photolysekanäle. Hierfür wurde ein neuartiger experimenteller Ansatz genutzt, der die folgenden Komponenten beinhaltet: (a) Photolyse der Spurengase durch gepulste ultraviolette Laserstrahlung unter stoßfreien Bedingungen, (b) Ein-Photon-Ionisation der neutralen Photolyseprodukte mittels durchstimmbarer Vakuum-UV-Strahlung und (c) Identifizierung der gebildeten Photoprodukt-Ionen durch Flugzeit-Massenspektrometrie. Dieser Ansatz ermöglicht die Identifizierung aller gebildeten Photolyseprodukte, die Bestimmung des Anregungszustandes der Photoprodukte durch Ausnutzung von Autoionisationsprozessen und die Bestimmung von Verzweigungsverhältnissen und Quantenausbeuten konkurrierender Photoprozesse.Im einzelnen wurden die atmosphärischen Spurengase Chlormonoxid (ClO) und sein Dimer (Cl2O2), Nitrylchlorid (ClNO2), Brommonoxid (BrO) und Bromnitrat (BrONO2) untersucht. Die Resultate können zur Verfeinerung atmosphärischer Modelle und deren Prognosefähigkeit beitragen. Insbesondere können die Ergebnisse auch einen Beitrag zur zuverlässigen Interpretation von Ergebnissen aus Feldstudien leisten.