WorldCat Identities

Reylé, Céline

Overview
Works: 20 works in 31 publications in 2 languages and 42 library holdings
Genres: Conference papers and proceedings  Observations  Catalogs 
Roles: Opponent, Editor, Other, Thesis advisor, Author
Publication Timeline
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Most widely held works by Céline Reylé
Low-mass stars and the transition stars-brown dwarfs by Evry Schatzman School (Conference)( Book )

8 editions published in 2012 in English and held by 16 WorldCat member libraries worldwide

Exploration de la ceinture de Kuiper par occultations stellaires by Camille Boissel( Book )

3 editions published between 2010 and 2019 in French and held by 3 WorldCat member libraries worldwide

Les objets de la ceinture de Kuiper (ou Objets Trans-Neptuniens, « OTNs »), sont des reliques du disque des planétésimaux. Ils contiennent de très importantes informations sur l'évolution passée du système solaire. Le nombre d'OTNs connus (un millier) et les plus gros atteignent 2000km de diamètre. Les objets de petite taille (< quelques km) sont invisibles. La seule manière de les détecter est d'utiliser les occultations stellaires. C'est aussi un bon outil pour l'étude et/ou la détection d'atmosphères, anneaux et satellites d'OTNs connus. Mon travail de thèse a porté sur : - une recherche par occultations stellaires d'anneaux et de satellites autour de Pluton; - une recherche de petits OTNs par occultations stellaires avec ULTRACAM ; - le développement d'une méthode statistique de sélection d'étoiles cibles pour la recherche de petits OTNs; - une participation à un projet instrumental : MIOSOTYS (Multi-object Instrument for Occultations in the SOlar system and TransitorY Systems), photomètre rapide multi-objet; - la préparation et l'organisation de la campagne de recherche d'OTNs avec MIOSOTYS, avec le développement de logiciels pour la recherche de champs stellaires, la réduction des données et la visualisation des courbes de lumières
A dynamically young and perturbed Milky Way disk by T Antoja( )

1 edition published in 2018 in English and held by 2 WorldCat member libraries worldwide

Low-mass stars as tracers of the milky way populations : investigating the effects of metallicity in cool atmosphere by Arvind Singh Rajpurohit( Book )

2 editions published in 2013 in English and held by 2 WorldCat member libraries worldwide

Very Low-Mass stars (M dwarfs) are an important source of information for probing the lowmass end of the main sequence, down to the hydrogen burning limit. They are the dominantstellar component of the Galaxy and make up the majority of baryonic matter in the Galaxy.Moreover, an increasing number of M dwarfs are now known to host exoplanets, includingsuper-Earth exoplanets. The determination of accurate fundamental parameters for M dwarfshas therefore relevant implications for both stellar and Galactic astronomy as well as planetology.Despite their large number in the Galaxy, M dwarfs remain elusive objects and themodelling of their photosphere has long remained a challenge (molecular opacities, dust cloudformation). The description of these stars therefore need a strong empirical basis, or validation.In particular, the effect of metallicity on the physics of cool atmospheres are still poorly known,even for early-type M-dwarfs.[...]
Etude du disque épais de la Galaxie avec le modèle de la Galaxie de Besançon by Guillaume Nasello( )

2 editions published in 2018 in French and held by 2 WorldCat member libraries worldwide

During my Phd thesis, I have used the Besançon Galaxy's Model (BGM) developed in my laboratory for many years.This model is widely use by astrophysicist around the world (the reference article is Robin, Reylé et al, 2003 and is cited more than 1250 times) and have been chose to be the reference model to prepare ESA's space mission Gaia.The BGM allow us to study our Galaxy by simulating statistically her stellar content. This stellar content is depending of hypothesis for the shape and history of the Milky Way.Here, I focus on the Milky Way's thick disc (old stars representing about 30 % of the total stellar content of the Milky Way).Thanks to the BGM, we can try to understand the shape and history of the thick disc. During this thesis, I've compared observation and simulations made by the BGM and adjusted the thick disc properties by using a Markov chain of Monte Carlo (MCMC)
Étude sur les paramétres stellaires des naines M et leur lien à la formation planétaire by Vasco Neves( )

1 edition published in 2013 in English and held by 2 WorldCat member libraries worldwide

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
First Estimate of the Thick Disc Mass Function by C Reylé( )

1 edition published in 2002 in English and held by 2 WorldCat member libraries worldwide

Formation des planètes géantes autour des étoiles de faibles masses : contraintes observationnelles en imagerie (optique adaptative) by Justine Lannier( )

1 edition published in 2016 in French and held by 2 WorldCat member libraries worldwide

Studying exoplanets, and in particular gaseous giant planets, is a new field of modern astrophysics. Understanding how the giant planets form, dynamically evolve, evolve with time, and have an impact on potential other planets within a stellar system are part of the biggest challenges of this science. The development of the most efficient observational technics and optimal analysis tools have been necessary to bring answers to these problematics. This is the context in which I realized my PhD thesis. I present in this manuscript the three projects that I led during these last three years.First, I studied the occurrence rate of the giant planets that orbit around M dwarfs. To realize this statistical study, I used NaCo data from two surveys. The first survey was composed of M dwarfs, the second was made of AF stars that were already studied by members of our team. I developed a Monte Carlo code, and used the contrapositive logic to lead a comparative analysis of these two surveys. I also associated stellar to planet mass ratios to planetary formation scenarios. My conclusions are that giant planets can more easily be formed by core accretion around AF stars than around M dwarfs, for separations between 8 and 400 astronomical units. Wide-orbit giant planets are rare whatever the stellar mass (basically <20%).Then, I developed a statistical tool that combines radial velocity and direct imaging data of specific stars, to better constrain the giant planet population at all separations. The code that I wrote is based on a Monte Carlo generation of synthetic planet populations. I applied this code on radial velocity and direct imaging data from young and nearby stars: AUMic, ßPictoris, HD113337, and HD95086. The future applications will be numerous thanks to the increase of the time baseline of radial velocity data and thanks to new high contrast and high resolution instruments able to probe shorter regions.These first two projects have allowed me to understand how to reduce and analyse data, and to develop statistical tools useful for my last project. This last project consists of observing, reducing and analyzing radial velocity and direct imaging data of a sample of K5-M5 young and nearby dwarfs. This project will bring strong constraints on the gaseous giant planet population that orbits around low mass stars, from short to wider separations
The eighth data release of the Sloan Digital Sky Survey : first data from SDSS-III by Hiroaki Aihara( Book )

1 edition published in 2011 in English and held by 1 WorldCat member library worldwide

"The Sloan Digital Sky Survey (SDSS) started a new phase in 2008 August, with new instrumentation and new surveys focused on Galactic structure and chemical evolution, measurements of the baryon oscillation feature in the clustering of galaxies and the quasar Ly[Greek letter alpha] forest, and a radial velocity search for planets around ~8000 stars. This paper describes the first data release of SDSS-III (and the eighth counting from the beginning of the SDSS). The release includes five-band imaging of roughly 5200 deg2 in the southern Galactic cap, bringing the total footprint of the SDSS imaging to 14,555 deg2, or over a third of the Celestial Sphere. All the imaging data have been reprocessed with an improved sky-subtraction algorithm and a final, self-consistent photometric recalibration and flat-field determination. This release also includes all data from the second phase of the Sloan Extension for Galactic Understanding and Exploration (SEGUE-2), consisting of spectroscopy of approximately 118,000 stars at both high and low Galactic latitudes. All the more than half a million stellar spectra obtained with the SDSS spectrograph have been reprocessed through an improved stellar parameter pipeline, which has better determinationof metallicity for high-metallicity stars."
Structure and kinematics of the milky way as seen from barred galactic model by José Fernandez Trincado( )

1 edition published in 2017 in English and held by 1 WorldCat member library worldwide

This work of thesis concerns an in detailed study of the structure, kinematics and dynamics of the Milky Way,with a particular emphasis on the bulge region and the halo. The main goal of this work is to establish dynamicalconstraints on the physical parameters of the Galactic bar in order to construct a detailed kinematic maps of the innerregions of the our Galaxy. Such map can be used as an ingredient for the Besançon stellar populations synthesismodel, allowing to provide accurate kinematic simulations in the inner regions of the disk and in the bar itself.In this thesis I present several analytic and semi-analytic potentials to approximate the 3D gravitational potentialmodel of the Milky Way, observationally and dynamically constrained, where the perturbations produced by theGalactic bar fit fairly well the global kinematic trends in the Galactic bulge. Using ~10 millions massless particles as tracers of stellar kinematics, we present a full study of the orbits in the bar, and non-stationary effects of the bar on the disks and the halo. In particular we trace the kinematic imprints of disk particles trapped/scattered in the Galactic bar. Finally, we analyse the orbits of chemically peculiar stars in the Milky Way field and its relation with globular clusterstars from the analysis of spectroscopic data. These results confirm previous claims that a small fraction of the Galactichalo is made up of light-element abundance patterns observed only in the globular clusters environments. Theyprovide a crucial observational support to the "merging" scenario of the Milky Way bulge region as well as in thehalo. We develop a method to compute the stellar kinematics and orbits inferred from the density profiles and the gravitational potential for several stellar populations. As a by product of this thesis, we provide the GravPot16 package, a software designed for Galactic dynamics, and orbit integration. Also taking advantage of high quality data produced by the first data release of the mission Gaia (TGAS) combined with accurate chemical information from the APOGEE datasets, I present preliminary results of the Chemo-orbital properties of the Milky Way
Gaia Data Release 2 observations of solar system objects by F Spoto( )

1 edition published in 2018 in English and held by 1 WorldCat member library worldwide

Context: The Gaia spacecraft of the European Space Agency (ESA) has been securing observations of solar system objects (SSOs) since the beginning of its operations. Data Release 2 (DR2) contains the observations of a selected sample of 14,099 SSOs. These asteroids have been already identified and have been numbered by the Minor Planet Center repository. Positions are provided for each Gaia observation at CCD level. As additional information, complementary to astrometry, the apparent brightness of SSOs in the unfiltered G band is also provided for selected observations. Aims: We explain the processing of SSO data, and describe the criteria we used to select the sample published in Gaia DR2. We then explore the data set to assess its quality. Methods: To exploit the main data product for the solar system in Gaia DR2, which is the epoch astrometry of asteroids, it is necessary to take into account the unusual properties of the uncertainty, as the position information is nearly one-dimensional. When this aspect is handled appropriately, an orbit fit can be obtained with post-fit residuals that are overall consistent with the a-priori error model that was used to define individual values of the astrometric uncertainty. The role of both random and systematic errors is described. The distribution of residuals allowed us to identify possible contaminants in the data set (such as stars). Photometry in the G band was compared to computed values from reference asteroid shapes and to the flux registered at the corresponding epochs by the red and blue photometers (RP and BP). Results: The overall astrometric performance is close to the expectations, with an optimal range of brightness G similar to 12 - 17. In this range, the typical transit-level accuracy is well below 1 mas. For fainter asteroids, the growing photon noise deteriorates the performance. Asteroids brighter than G similar to 12 are affected by a lower performance of the processing of their signals. The dramatic improvement brought by Gaia DR2 astrometry of SSOs is demonstrated by comparisons to the archive data and by preliminary tests on the detection of subtle non-gravitational effects
Assembling the puzzle of the Milky Way( Book )

1 edition published in 2012 in English and held by 1 WorldCat member library worldwide

La caractérisation des exoplanètes en transit par vélocimétrie radiale by Alexandre Santerne( )

1 edition published in 2012 in French and held by 1 WorldCat member library worldwide

The search and characterization of transiting extrasolar planets (i.e. that pass in front of their host star, as seen from the Earth) is an important domain of planetology since these planets constrain the formation, evolution and migration process of planetary systems. The CoRoT (CNES) and Kepler (NASA) space missions permit, these last years, to discover several thousand of transiting-planet candidates. However, these planet candidates need to be confirmed in order to exclude all false positive scenario that can mimic a planetary transit. For that, one of the method consist on performing radial velocity follow-up observations to measure the transiting object's mass and orbital parameters and thus, to determine the nature of planet candidates.During my PhD thesis, I tried to resolve the nature of transiting planet candidates from the CoRoT and Kepler space missions. For that, I performed follow-up observations with the SOPHIE (OHP) and HARPS (ESO) spectrographs that were used to discover several new transiting extrasolar planets. I also measured the Kepler false-positive rate, equal to 35% for giant close-in exoplanet candidates, contradicting previous estimations, much more optimistic.I also participate to the development of a new software, called "PASTIS", which objective is to validate statistically low-mass transiting exoplanets out of reach for current spectrographs. This new tool will, in a near future, validate tens of low-mass planets from the CoRoT and Kepler space missions
PLATO as it is: A legacy mission for Galactic archaeology( )

1 edition published in 2017 in English and held by 1 WorldCat member library worldwide

Abstract : Deciphering the assembly history of the Milky Way is a formidable task, which becomes possible only if one can produce high-resolution chrono-chemo-kinematical maps of the Galaxy. Data from large-scale astrometric and spectroscopic surveys will soon provide us with a well-defined view of the current chemo-kinematical structure of the Milky Way, but it will only enable a blurred view on the temporal sequence that led to the present-day Galaxy. As demonstrated by the (ongoing) exploitation of data from the pioneering photometric missions CoRoT, Kepler, and K2, asteroseismology provides the way forward: solar-like oscillating giants are excellent evolutionary clocks thanks to the availability of seismic constraints on their mass and to the tight age-initial mass relation they adhere to. In this paper we identify five key outstanding questions relating to the formation and evolution of the Milky Way that will need precise and accurate ages for large samples of stars to be addressed, and we identify the requirements in terms of number of targets and the precision on the stellar properties that are needed to tackle such questions. By quantifying the asteroseismic yields expected from PLATO for red giant stars, we demonstrate that these requirements are within the capabilities of the current instrument design, provided that observations are sufficiently long to identify the evolutionary state and allow robust and precise determination of acoustic-mode frequencies. This will allow us to harvest data of sufficient quality to reach a 10% precision in age. This is a fundamental prerequisite to then reach the more ambitious goal of a similar level of accuracy, which will be possible only if we have at hand a careful appraisal of systematic uncertainties on age deriving from our limited understanding of stellar physics, a goal that conveniently falls within the main aims of PLATO's core science. We therefore strongly endorse PLATO's current design and proposed observational strategy, and conclude that PLATO, as it is, will be a legacy mission for Galactic archaeology
A la recherche de quasars à grand décalage spectral dans le sondage CFHQSIR by Sarah Pipien( )

1 edition published in 2017 in French and held by 1 WorldCat member library worldwide

My PhD work is focused on the search for high-redshift quasars in the Canada France High-z Quasar Survey in the Near Infrared (CFHQSIR). The main scientific objective of this CFHT Large Program is to search for quasars at redshift z ∼ 7 with near-infrared images of the CFHTLS Wide fields acquired with the CFHT WIRCam camera. Firstly, I carried out the photometric calibration of the CFHQSIR images. I performed a detailed analysis of the CFHQSIR data by studying their quality, as well as their noise properties and their depths.Secondly, I computed the number of high-redshift quasars that could be detected with CFHQSIR and the corresponding constraints which could be put on the z ∼ 7 quasar luminosity function. Then, I proceeded to the identification of quasar candidates among the many thousands of sources in the 130 square degrees covered by CFHQSIR. Photometric follow-up observations of the candidates revealed about fifty objects, of which fifteen were chosen to be spectroscopically observed with the Very Large Telescope (VLT). Given that this spectroscopic follow-up is not yet completed, the exact nature of these sources will only be known in the coming months. To finish, I applied Bayesian model comparison to my sample in order to complete and consolidate my selection procedure. My candidates were finally classified according to their probability to be a high-redshift quasar. I verified that the majority of the most likely candidates were selected for spectroscopic observations
Cinématique et dynamique galactiques by Jérôme Leca( )

1 edition published in 2019 in French and held by 1 WorldCat member library worldwide

Les modèles galactiques auto-cohérents sont nécessaires pour analyser et interpréter les comptages d'étoiles, les distributions de densité stellaire et la cinématique stellaire, dans le but de comprendre la formation et l'évolution de notre Galaxie. Cette thèse a pour but de modifier et améliorer l'auto-cohérence dynamique du modèle galactique de Besançon (BGM) dans le cas d'un potentiel gravitationnel stationnaire et axisymétrique. Chaque orbite stellaire est modélisée en déterminant une troisième intégrale du mouvement de Stäckel. Une fonction de distribution de Shu généralisée avec trois intégrales du mouvement est utilisée pour modéliser la fonction de distribution stellaire. Cette nouvelle version du BGM est comparée avec la précédente version axisymétrique BGM2014 et nous trouvons que les deux versions ont des densités similaires pour chaque composante. L'auto-cohérence dynamique est améliorée et peut être testée en retrouvant les forces et le potentiel via les équations de Jeans appliquées à chaque fonction de distribution stellaire. Les forces sont retrouvées avec une précision meilleure que 1 % sur la plupart du volume galactique
Automatic stellar parameters determination : chemical characterization of the Galactic thick disk and preparation to the Gaia mission by Hélène Posbic( )

1 edition published in 2019 in English and held by 1 WorldCat member library worldwide

The formation of the Milky Way disk is still an open question. Many scenarios are proposed. Different formation scenarios predict different disk chemical trends. This thesis aims to chemically characterize the Milky Way disk inside and outside the solar neighbourhood, to better constrain its formation scenario. This is possible thanks to high resolution spectra of 200 disk stars observed using the Giraffe spectograph on the Very Large Telescope (VLT). They were selected to have galactic altitudes ǀZǀ that cover both the thin and tick disk (ǀZǀ up to 2 kpc). A new automatic spectra analysis software was developed to determine the stellar parameters, and most importantly, the elemental abundances of these stars. SPADES (Stellar PArameters DEtermination Software) is based on a line-by-line analysis using a reference grid of synthetic stellar spectra. One of its particularities is its ability to calculate synthetic spectra on-the-y. Once tested for internal and external errors, it was used to determine the radial velocity, effective temperature, surface gravity, metallicity and elemental abundances of the smple stars. The distances of these stars were also determined. The metallicity distribution function of the disk using this sample was calculated. It showed a large contribution of the disk stars and a smooth transition at the metallicity of the thick disk/halo interface. The vertivcal behaviour of the metallicity distribution function was also studied. A vertical metallicity grandient in the disk of 0.19 +/- 0.14 dex/kpc was marginally detected at the 1.4 sigma level. The [Ti/Fe] and [Ca/Fe] vs [Fe/H] trends for stars located at less than 1 kpc above the plane were found to be in good agreement with previous studies. This is conclusion from the comparison of this work with author's like Bensky et al. (2005), Takeda (2007), and Neves et al. (2009). The main result of the analysis is that the trends of [Ca/Fe] vs [Fe/H] and [Ti/He] vs [Fe/H] show no significant difference close (i.e. ǀZǀ < 1 kpc) and farther away (1 < ǀZǀ < 2.5 kpc) from the Galactic plane. This suggests that the thick disk gas and stars have been enriched by the same proportion of type II and type I super-novae from the galactic plane up to at least 2.5 kpc. These results support thick disk formation scenarios like collapse or gas-rich accretion and disfavour a thick disc formed of stars captured during merger event
Etude des populations stellaires de la Galaxie : travaux de recherche : pour l'obtention de l'habilitation à diriger des recherches by C Reylé( )

1 edition published in 2006 in English and held by 1 WorldCat member library worldwide

Assembling the puzzle of the Milky Way( )

1 edition published in 2012 in English and held by 0 WorldCat member libraries worldwide

 
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Alternative Names
Reylé, C.

Reylé, Céline

Reylé-Laffont, Céline

Languages
English (22)

French (9)