78 research outputs found
Évolution chimique du Grand Nuage de Magellan
No full textDespite decades of intensive observational and theoretical work, we are still far from a complete and clear understanding of the nearby universe, the Milky Way (MW) and its neighbours. Among the satellites of the MW, the Small and Large Magellanic Cloud (LMC) are of particular interest since they form the closest example of galaxies in gravitational and hydrodynamical interaction, and therefore constitute a unique laboratory to study the effect of tides and matter exchange on the chemical evolution and star formation history of a galaxy. The LMC is a low-mass barred disc galaxy, prototypical of gas-rich galaxies that are thought to play an important role in the build-up of large galaxies in the ΛCDM framework. Furthermore, with its present day metallicity of only third of solar, the chemical enrichment path followed by the LMC gives a heavy weight to the yields of metal-poor stellar generations, which makes the LMC an ideal environment to study nucleosynthesis at low metallicities. This thesis work aims at: 1) chemically characterizing the LMC bar population, 2) comparing the elemental trends of the MW and the LMC and interpreting the differences or similarities in terms of chemical evolution and/or nucleosynthesis processes (constraints on the nucleosynthetic sites and processes), 3) comparing the chemical evolution of the LMC bar and inner disc and interpreting the differences or similarities between the LMC bar and inner disc in the context of the bar formation. Our results show that the chemical history of the LMC experienced a strong contribution from type Ia supernovae as well as a strong s-process enrichment from metal-poor AGB winds. Massive stars made a smaller contribution to the chemical enrichment compared to the MW. The observed differences between the bar and the disc speak in favour of an episode of enhanced star formation a few Gyr ago, occurring in the central parts of the LMC and leading to the formation of the bar. This is in agreement with recently derived star formation histories.Malgré des années de travaux théoriques et observationnels intensifs, nous sommes toujours loin d’une complète compréhension de l’univers proche, la Voie Lactée (MW) et ses galaxies voisines. Parmi les satellites de la MW, le Petit et le Grand Nuage de Magellan (LMC) sont particulièrement intéressants puisqu’ils forment le plus proche exemple de galaxies en interaction gravitationnelle et hydrodynamique, et partant, constituent un laboratoire unique pour étudier les effets des marées et l’échange de matière sur l’évolution chimique et l’histoire de la formation stellaire d’une galaxie. Le LMC est une galaxie de petite masse barrée à disque, prototype des galaxies riches en gaz que l’on pense jouer un rôle important dans la construction des grandes galaxies dans le cadre du ΛCDM. De plus, avec sa métallicité actuelle d’environ le tiers de la métallicité solaire, le chemin d’enrichissement chimique suivi par le LMC donne un grand poids aux yields des générations stellaires pauvres en métaux, ce qui fait du LMC un environnement idéal pour étudier la nucléosynthèse aux basses métallicités. Ce travail de doctorat vise à: 1) caractériser chimiquement la population de la barre du LMC, 2) comparer les tendances des éléments de la MW et du LMC et interpréter les différences ou ressemblance en termes d’évolution chimique et/ou de processus nucléosynthétiques (contraintes sur les sites et les processus nucléosynthétiques), 3) comparer l’évolution chimique de la barre et du disque interne du LMC et interpréter les différence ou ressemblance dans le contexte de la formation de la barre. Nos résultats montrent que l’histoire chimique du LMC a connu un forte contribution des supernovae de type I ainsi qu’un fort enrichissement en éléments s par les vents d’étoiles AGB pauvres en métaux. Par rapport à la MW, les étoiles massives ont eu une contribution plus petite à l’enrichissement chimique du LMC. Les différences observées entre la barre et le disque parlent en faveur d’un épisode de formation stellaire accrue il y a quelques Gyr, ayant lieu dans les zones centrales du LMC et conduisant à la formation de la barre. Ceci est en accord avec les histoires de la formation stellaire récemment dérivées
Chemical abundances across the first kpc of the LMC
No full textThe chemical evolution of the Large Magellanic Cloud (LMC) yields information on many different aspects of low-mass disc galaxy evolution, and the evolution of an interacting system. It is a complementary approach to that of understanding the star formation history of this galaxy, and over the last two decades, the amount of stars with high-quality radial velocities and chemical abundances has kept increasing, going from few luminous supergiants to hundreds or thousands of fainter giant stars. Using medium-resolution (R~20000) spectra from FLAMES at the VLT, we obtained the detailed chemical abundances of more than 250 LMC RGB stars, spread in three fields within the first 2 kpc of the LMC. I will discuss our results in the context of the chemical evolution of the LMC. In particular, our alpha abundances exhibit the canonical alpha-pattern with a knee likely located below [Fe/H] ~ -1. Our results seem at odds with recent APOGEE trends
Chemical evolution of the Large Magellanic Cloud
No full textMalgré des années de travaux théoriques et observationnels intensifs, nous sommes toujours loin d’une complète compréhension de l’univers proche, la Voie Lactée (MW) et ses galaxies voisines. Parmi les satellites de la MW, le Petit et le Grand Nuage de Magellan (LMC) sont particulièrement intéressants puisqu’ils forment le plus proche exemple de galaxies en interaction gravitationnelle et hydrodynamique, et partant, constituent un laboratoire unique pour étudier les effets des marées et l’échange de matière sur l’évolution chimique et l’histoire de la formation stellaire d’une galaxie. Le LMC est une galaxie de petite masse barrée à disque, prototype des galaxies riches en gaz que l’on pense jouer un rôle important dans la construction des grandes galaxies dans le cadre du ΛCDM. De plus, avec sa métallicité actuelle d’environ le tiers de la métallicité solaire, le chemin d’enrichissement chimique suivi par le LMC donne un grand poids aux yields des générations stellaires pauvres en métaux, ce qui fait du LMC un environnement idéal pour étudier la nucléosynthèse aux basses métallicités. Ce travail de doctorat vise à: 1) caractériser chimiquement la population de la barre du LMC, 2) comparer les tendances des éléments de la MW et du LMC et interpréter les différences ou ressemblance en termes d’évolution chimique et/ou de processus nucléosynthétiques (contraintes sur les sites et les processus nucléosynthétiques), 3) comparer l’évolution chimique de la barre et du disque interne du LMC et interpréter les différence ou ressemblance dans le contexte de la formation de la barre. Nos résultats montrent que l’histoire chimique du LMC a connu un forte contribution des supernovae de type I ainsi qu’un fort enrichissement en éléments s par les vents d’étoiles AGB pauvres en métaux. Par rapport à la MW, les étoiles massives ont eu une contribution plus petite à l’enrichissement chimique du LMC. Les différences observées entre la barre et le disque parlent en faveur d’un épisode de formation stellaire accrue il y a quelques Gyr, ayant lieu dans les zones centrales du LMC et conduisant à la formation de la barre. Ceci est en accord avec les histoires de la formation stellaire récemment dérivées.Despite decades of intensive observational and theoretical work, we are still far from a complete and clear understanding of the nearby universe, the Milky Way (MW) and its neighbours. Among the satellites of the MW, the Small and Large Magellanic Cloud (LMC) are of particular interest since they form the closest example of galaxies in gravitational and hydrodynamical interaction, and therefore constitute a unique laboratory to study the effect of tides and matter exchange on the chemical evolution and star formation history of a galaxy. The LMC is a low-mass barred disc galaxy, prototypical of gas-rich galaxies that are thought to play an important role in the build-up of large galaxies in the ΛCDM framework. Furthermore, with its present day metallicity of only third of solar, the chemical enrichment path followed by the LMC gives a heavy weight to the yields of metal-poor stellar generations, which makes the LMC an ideal environment to study nucleosynthesis at low metallicities. This thesis work aims at: 1) chemically characterizing the LMC bar population, 2) comparing the elemental trends of the MW and the LMC and interpreting the differences or similarities in terms of chemical evolution and/or nucleosynthesis processes (constraints on the nucleosynthetic sites and processes), 3) comparing the chemical evolution of the LMC bar and inner disc and interpreting the differences or similarities between the LMC bar and inner disc in the context of the bar formation. Our results show that the chemical history of the LMC experienced a strong contribution from type Ia supernovae as well as a strong s-process enrichment from metal-poor AGB winds. Massive stars made a smaller contribution to the chemical enrichment compared to the MW. The observed differences between the bar and the disc speak in favour of an episode of enhanced star formation a few Gyr ago, occurring in the central parts of the LMC and leading to the formation of the bar. This is in agreement with recently derived star formation histories
Évolution chimique du Grand Nuage de Magellan
No full textDespite decades of intensive observational and theoretical work, we are still far from a complete and clear understanding of the nearby universe, the Milky Way (MW) and its neighbours. Among the satellites of the MW, the Small and Large Magellanic Cloud (LMC) are of particular interest since they form the closest example of galaxies in gravitational and hydrodynamical interaction, and therefore constitute a unique laboratory to study the effect of tides and matter exchange on the chemical evolution and star formation history of a galaxy. The LMC is a low-mass barred disc galaxy, prototypical of gas-rich galaxies that are thought to play an important role in the build-up of large galaxies in the ΛCDM framework. Furthermore, with its present day metallicity of only third of solar, the chemical enrichment path followed by the LMC gives a heavy weight to the yields of metal-poor stellar generations, which makes the LMC an ideal environment to study nucleosynthesis at low metallicities. This thesis work aims at: 1) chemically characterizing the LMC bar population, 2) comparing the elemental trends of the MW and the LMC and interpreting the differences or similarities in terms of chemical evolution and/or nucleosynthesis processes (constraints on the nucleosynthetic sites and processes), 3) comparing the chemical evolution of the LMC bar and inner disc and interpreting the differences or similarities between the LMC bar and inner disc in the context of the bar formation. Our results show that the chemical history of the LMC experienced a strong contribution from type Ia supernovae as well as a strong s-process enrichment from metal-poor AGB winds. Massive stars made a smaller contribution to the chemical enrichment compared to the MW. The observed differences between the bar and the disc speak in favour of an episode of enhanced star formation a few Gyr ago, occurring in the central parts of the LMC and leading to the formation of the bar. This is in agreement with recently derived star formation histories.Malgré des années de travaux théoriques et observationnels intensifs, nous sommes toujours loin d’une complète compréhension de l’univers proche, la Voie Lactée (MW) et ses galaxies voisines. Parmi les satellites de la MW, le Petit et le Grand Nuage de Magellan (LMC) sont particulièrement intéressants puisqu’ils forment le plus proche exemple de galaxies en interaction gravitationnelle et hydrodynamique, et partant, constituent un laboratoire unique pour étudier les effets des marées et l’échange de matière sur l’évolution chimique et l’histoire de la formation stellaire d’une galaxie. Le LMC est une galaxie de petite masse barrée à disque, prototype des galaxies riches en gaz que l’on pense jouer un rôle important dans la construction des grandes galaxies dans le cadre du ΛCDM. De plus, avec sa métallicité actuelle d’environ le tiers de la métallicité solaire, le chemin d’enrichissement chimique suivi par le LMC donne un grand poids aux yields des générations stellaires pauvres en métaux, ce qui fait du LMC un environnement idéal pour étudier la nucléosynthèse aux basses métallicités. Ce travail de doctorat vise à: 1) caractériser chimiquement la population de la barre du LMC, 2) comparer les tendances des éléments de la MW et du LMC et interpréter les différences ou ressemblance en termes d’évolution chimique et/ou de processus nucléosynthétiques (contraintes sur les sites et les processus nucléosynthétiques), 3) comparer l’évolution chimique de la barre et du disque interne du LMC et interpréter les différence ou ressemblance dans le contexte de la formation de la barre. Nos résultats montrent que l’histoire chimique du LMC a connu un forte contribution des supernovae de type I ainsi qu’un fort enrichissement en éléments s par les vents d’étoiles AGB pauvres en métaux. Par rapport à la MW, les étoiles massives ont eu une contribution plus petite à l’enrichissement chimique du LMC. Les différences observées entre la barre et le disque parlent en faveur d’un épisode de formation stellaire accrue il y a quelques Gyr, ayant lieu dans les zones centrales du LMC et conduisant à la formation de la barre. Ceci est en accord avec les histoires de la formation stellaire récemment dérivées
Chemical evolution of the Large Magellanic Cloud
No full textMalgré des années de travaux théoriques et observationnels intensifs, nous sommes toujours loin d une complète compréhension de l univers proche, la Voie Lactée (MW) et ses galaxies voisines. Parmi les satellites de la MW, le Petit et le Grand Nuage de Magellan (LMC) sont particulièrement intéressants puisqu ils forment le plus proche exemple de galaxies en interaction gravitationnelle et hydrodynamique, et partant, constituent un laboratoire unique pour étudier les effets des marées et l échange de matière sur l évolution chimique et l histoire de la formation stellaire d une galaxie. Le LMC est une galaxie de petite masse barrée à disque, prototype des galaxies riches en gaz que l on pense jouer un rôle important dans la construction des grandes galaxies dans le cadre du CDM. De plus, avec sa métallicité actuelle d environ le tiers de la métallicité solaire, le chemin d enrichissement chimique suivi par le LMC donne un grand poids aux yields des générations stellaires pauvres en métaux, ce qui fait du LMC un environnement idéal pour étudier la nucléosynthèse aux basses métallicités. Ce travail de doctorat vise à: 1) caractériser chimiquement la population de la barre du LMC, 2) comparer les tendances des éléments de la MW et du LMC et interpréter les différences ou ressemblance en termes d évolution chimique et/ou de processus nucléosynthétiques (contraintes sur les sites et les processus nucléosynthétiques), 3) comparer l évolution chimique de la barre et du disque interne du LMC et interpréter les différence ou ressemblance dans le contexte de la formation de la barre. Nos résultats montrent que l histoire chimique du LMC a connu un forte contribution des supernovae de type I ainsi qu un fort enrichissement en éléments s par les vents d étoiles AGB pauvres en métaux. Par rapport à la MW, les étoiles massives ont eu une contribution plus petite à l enrichissement chimique du LMC. Les différences observées entre la barre et le disque parlent en faveur d un épisode de formation stellaire accrue il y a quelques Gyr, ayant lieu dans les zones centrales du LMC et conduisant à la formation de la barre. Ceci est en accord avec les histoires de la formation stellaire récemment dérivées.Despite decades of intensive observational and theoretical work, we are still far from a complete and clear understanding of the nearby universe, the Milky Way (MW) and its neighbours. Among the satellites of the MW, the Small and Large Magellanic Cloud (LMC) are of particular interest since they form the closest example of galaxies in gravitational and hydrodynamical interaction, and therefore constitute a unique laboratory to study the effect of tides and matter exchange on the chemical evolution and star formation history of a galaxy. The LMC is a low-mass barred disc galaxy, prototypical of gas-rich galaxies that are thought to play an important role in the build-up of large galaxies in the CDM framework. Furthermore, with its present day metallicity of only third of solar, the chemical enrichment path followed by the LMC gives a heavy weight to the yields of metal-poor stellar generations, which makes the LMC an ideal environment to study nucleosynthesis at low metallicities. This thesis work aims at: 1) chemically characterizing the LMC bar population, 2) comparing the elemental trends of the MW and the LMC and interpreting the differences or similarities in terms of chemical evolution and/or nucleosynthesis processes (constraints on the nucleosynthetic sites and processes), 3) comparing the chemical evolution of the LMC bar and inner disc and interpreting the differences or similarities between the LMC bar and inner disc in the context of the bar formation. Our results show that the chemical history of the LMC experienced a strong contribution from type Ia supernovae as well as a strong s-process enrichment from metal-poor AGB winds. Massive stars made a smaller contribution to the chemical enrichment compared to the MW. The observed differences between the bar and the disc speak in favour of an episode of enhanced star formation a few Gyr ago, occurring in the central parts of the LMC and leading to the formation of the bar. This is in agreement with recently derived star formation histories.NICE-Bibliotheque electronique (060889901) / SudocSudocFranceF
Stellar spectroscopic surveys: overview, expectations and achievements
No full textInternational audienceMulti-fibre spectrographs have made possible the run of large spectroscopic surveys targeting 10^5 to millions of Milky Way (MW) stars. The targeted stars belong to the main stellar structures of our Galaxy and mostly sample stellar evolutionary stages from the (pre-)main-sequence to the red giant branch. Their primary aim is to harvest a vast amount of data (radial velocities, stellar parameters, abundances) in order to constrain the formation and evolution of the MW. We will focus on two spectroscopic surveys France is involved in. First, we will briefly introduce the WEAVE spectroscopic survey, that will soon start to observe at the William Herschel Telescope, and show from simulations what can be expected in terms of chemical abundances. Second, we will highlight the relevance and usefulness of such large project by reminding some of the results obtained within the Gaia-ESO survey
Detection of spectroscopic binaries: lessons from the Gaia-ESO survey
No full textinfo:eu-repo/semantics/publishe
The Gaia–ESO Survey: Carbon Abundance in the Galactic Thin and Thick Disks
No full textThis paper focuses on carbon, which is one of the most abundant elements in the universe and is of high importance in the field of nucleosynthesis and galactic and stellar evolution. The origin of carbon and the relative importance of massive and low- to intermediate-mass stars in producing it is still a matter of debate. We aim at better understanding the origin of carbon by studying the trends of [C/H], [C/Fe], and [C/Mg] versus [Fe/H] and [Mg/H] for 2133 FGK dwarf stars from the fifth Gaia─ESO Survey internal data release (GES iDR5). The availability of accurate parallaxes and proper motions from Gaia DR2 and radial velocities from GES iDR5 allows us to compute Galactic velocities, orbits, absolute magnitudes, and, for 1751 stars, Bayesian-derived ages. Three different selection methodologies have been adopted to discriminate between thin- and thick-disk stars. In all the cases, the two stellar groups show different [C/H], [C/Fe], and [C/Mg] and span different age intervals, with the thick-disk stars being, on average, older than the thin-disk ones. The behaviors of [C/H], [C/Fe], and [C/Mg] versus [Fe/H], [Mg/H], and age all suggest that C is primarily produced in massive stars. The increase of [C/Mg] for young thin-disk stars indicates a contribution from low-mass stars or the increased C production from massive stars at high metallicities due to the enhanced mass loss. The analysis of the orbital parameters R med and | {Z}max | supports an “inside─out” and “upside─down” formation scenario for the disks of the Milky Way
Heavy elements Ba, La, Ce, Nd, and Eu in 56 Galactic bulge red giants
No full textAims: The aim of this work is the study of abundances of the heavy elements Ba, La, Ce, Nd, and Eu in 56 bulge giants (red giant branch and red clump) with metallicities ranging from -1.3 dex to 0.5 dex.
Methods: We obtained high-resolution spectra of our giant stars using the FLAMES-UVES spectrograph on the Very Large Telescope. We inspected four bulge fields along the minor axis.
Results: We measure the chemical evolution of heavy elements, as a function of metallicity, in the Galactic bulge.
Conclusions: The [Ba,La,Ce,Nd/Fe] vs. [Fe/H] ratios decrease with increasing metallicity, in which aspect they differ from disc stars. In our metal-poor bulge stars, La and Ba are enhanced relative to their thick disc counterpart, while in our metal-rich bulge stars La and Ba are underabundant relative to their disc counterpart. Therefore, this contrast between bulge and discs trends indicates that bulge and (solar neighbourhood) thick disc stars could behave differently. An increase in [La,Nd/Eu] with increasing metallicity, for metal-rich stars with [Fe/H] > 0 dex, may indicate that the s-process from AGB stars starts to operate at a metallicity around solar. Finally, [Eu/Fe] follows the [α/ Fe] behaviour, as expected, since these elements are produced by SNe type II
The mass-ratio and eccentricity distributions of barium and S stars, and red giants in open clusters
No full textContext. A complete set of orbital parameters for barium stars, including the longest orbits, has recently been obtained thanks to a radial-velocity monitoring with the HERMES spectrograph installed on the Flemish Mercator telescope. Barium stars are supposed to belong to post-mass-transfer systems. Aims. In order to identify diagnostics distinguishing between pre- and post-mass-transfer systems, the properties of barium stars (more precisely their mass-function distribution and their period-eccentricity (P-e) diagram) are compared to those of binary red giants in open clusters. As a side product, we aim to identify possible post-mass-transfer systems among the cluster giants from the presence of s-process overabundances. We investigate the relation between the s-process enrichment, the location in the (P-e) diagram, and the cluster metallicity and turn-off mass. Methods. To invert the mass-function distribution and derive the mass-ratio distribution, we used the method pioneered by Boffin et al. (1992) that relies on a Richardson-Lucy deconvolution algorithm. The derivation of s-process abundances in the open-cluster giants was performed through spectral synthesis with MARCS model atmospheres. Results. A fraction of 22% of post-mass-transfer systems is found among the cluster binary giants (with companion masses between 0.58 and 0.87 M⊙, typical for white dwarfs), and these systems occupy a wider area than barium stars in the (P-e) diagram. Barium stars have on average lower eccentricities at a given orbital period. When the sample of binary giant stars in clusters is restricted to the subsample of systems occupying the same locus as the barium stars in the (P-e) diagram, and with a mass function compatible with a WD companion, 33% (=4/12) show a chemical signature of mass transfer in the form of s-process overabundances (from rather moderate - about 0.3 dex - to more extreme - about 1 dex). The only strong barium star in our sample is found in the cluster with the lowest metallicity in the sample (i.e. star 173 in NGC 2420, with [Fe/H] = -0.26), whereas the barium stars with mild s-process abundance anomalies (from 0.25 to 0.6 dex) are found in the clusters with slightly subsolar metallicities. Our finding confirms the classical prediction that the s-process nucleosynthesis is more efficient at low metallicities, since the s-process overabundance is not clearly correlated with the cluster turn-off (TO) mass; such a correlation would instead hint at the importance of the dilution factor. We also find a mild barium star in NGC 2335, a cluster with a large TO mass of 4.3 M⊙, which implies that asymptotic giant branch stars that massive still operate the s-process and the third dredge-up.SCOPUS: ar.jinfo:eu-repo/semantics/publishe
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