Congrès annuel de la Société Canadienne d'Astronomie
L'édition 2014 du congrès annuel de la Société Canadienne d'Astronomie, organisé par le Groupe de recherche en astrophysique de l'Université Laval, aura lieu à Québec du 8 au 12 juin 2014, à l'hôtel Château Laurier.
Cette rencontre sera l'occasion de partager avec les chercheurs du pays les toutes dernières découvertes canadiennes dans tous les domaines de l'astronomie.
Notez qu'une journée entière (le 12) sera consacrée à une discussion sur la revue de mi-parcours ("RMP") de notre Plan à long terme ("LRP") que l'on peut télécharger ICI.
L'horaire, incluant la liste des affiches, est maintenant disponible ici: HORAIRE
Des informations concernant les affiches peuvent être trouvées ici.
Dates importantes :
13 avril 2014:
Date limite, inscriptions régulières
Date limite, titre et résumé de présentation
8 mai 2014:
Date limite, réservation d'hôtel
8 juin 2014:
Atelier des étudiants gradués: 9h30 - 16h30
Réception d'accueil: 19h00 - 21h00
9 - 12 juin 2014:
Début des conférences régulières: 9 juin 2014, 8h30
Banquet: 10 juin 2014, 19h30
Journée spéciale RMP: 12 juin 2014, 8h30 - 15h30
Présentations spéciales
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Volker Bromm, University of Texas at Austin |
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| The First Stars and Galaxies: The Run-up to the JWST | |
| How and when did the cosmic dark ages end? I present simulations of the formation of the first stars and galaxies, discuss their feedback on the intergalactic medium, and describe ways to probe their signature with next generation facilities. I will identify the key processes and outline the major remaining uncertainties. | |
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Rennan Barkana, Tel-Aviv University |
| How to observe cosmic heating and reionization due to the first stars | |
| One of the exciting frontiers in astronomy is the era of the formation of the first stars. Since the Universe was filled with hydrogen atoms at that time, the most promising method for observing this epoch is via the prominent 21-cm line of hydrogen. Several international groups have begun operating new arrays of radio telescopes, hoping to open this new observational window on the early Universe. The common view has been that they can only search for cosmic reionization (in which radiation from stars broke up the intergalactic hydrogen atoms), while other cosmic events occurred too early to see. However, we recently overturned this long-held view, arguing for a late and uniform heating given the hard spectrum expected for the sources of X-ray heating (most likely some of the first black-hole binaries). Cosmic heating therefore imprints a clear, previously unexpected signature in radio waves, perhaps within reach of current arrays (and certainly the SKA). | |
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Lisa Kewley, Australian National University |
| Galaxy Evolution in 3D | |
| Throughout the history of the universe, shocks and large-scale gas flows have moulded the arms of spiral galaxies, formed the bulges of the most massive galaxies in the universe, fed supermassive black holes in the centres of galaxies, fuelled generation upon generation of new stars, and enriched the intergalactic medium with metals. I will discuss our current understanding of the relationship between galactic-scale outflows, star-formation, and active galactic nuclei. I will present the latest results from our large integral field surveys of nearby and high redshift galaxies which aim to reveal the relationship between galactic-scale outflows, star-formation, and active galactic nuclei in galaxies as a function of environment and redshift. | |
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Ronald Buta, University of Alabama |
| Comprehensive Galaxy Morphology and Classification from the Near to the Far Universe | |
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For almost a century, galaxy morphology and classification have been
considered an essential step in understanding how galaxies formed and
have evolved over time. Galaxy morphology is rich in details that are
clues to the internal and external physical processes that have molded
their shapes. It is non-trivial to determine exactly what a given
morphology actually implies about the history of a galaxy, because we
only see what is basically a snapshot of any galaxy. Only by examining
the collective morphology of galaxies, the full range of types both
near and far, in conjunction with physical data can we hope to piece
together the general evolutionary paths of different classes of
galaxies. The large amount of high quality imaging available at this time makes it possible to take galaxy morphology to realms it has not been taken before. In my presentation, I want to describe how galaxy classification and morphology are being used today to learn about galactic star formation history, the development and evolution of structures such as bars, rings, and lenses, and how a comprehensive approach to classification can be used to try and bridge the gap between nearby and extremely distant galaxies. |
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Christian Iliadis, University of North Carolina at Chapel Hill |
| Nuclear Astrophysics Experiments with High-Intensity Ion and Photon Beams | |
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Nuclear astrophysics constitutes a multidisciplinary crucible of knowledge addressing key questions in fundamental
research, ranging from the age of the Universe to the origin of cosmic rays, from supernova explosion mechanisms to the origin of the solar system.
This talk will present recent results of nuclear astrophysics measurements performed at the Triangle Universities Nuclear Laboratory using high-intensity proton beams (at the LENA facility) and mono-energetic gamma-ray beams (at the HIgS facility). Astrophysical implications for our understanding of AGB stars, classical novae, and the s-process will be discussed. |
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Kim Venn, University of Victoria |
| Archaeology of the Stars | |
| The most metal-poor star yet found was announced in Feb 2014, with a metallicity that is 100 times lower than previously known,
and 10 million times lower than in the Sun. These jewels are thought to be related to the earliest stages of the
formation and evolution of the Universe, and therefore studies of their properties complement analyses of the high
redshift Universe. However, these stars are rare and require large spectroscopic surveys to find, confirm, and determine their characteristics. Stellar spectroscopic surveys can also address questions such as:
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Conférence publique, 9 juin, 19h30, Amphithéâtre Hydro-Québec, Université Laval René Doyon, Université de Montréal |
| À la recherche de la vie à l'extérieur du système solaire | |
| Les progrès fulgurants de l'astrophysique des vingt dernières années confirment sans équivoque qu'une fraction importante des étoiles dans le voisinage du soleil sont entourées de planètes semblables à celles de notre système solaire. Nous avons même identifié des petites planètes rocheuses potentiellement habitables, c'est-à-dire des planètes où la température de surface y est suffisamment élevée pour maintenir l'eau
sous forme liquide.
Dans un horizon de moins d'une décennie, le développement des grands observatoires terrestres et spatiaux permettra non seulement d'identifier les planètes habitables les plus rapprochées du soleil mais aussi de détecter et mesurer la composition chimique de la fine atmosphère de ces planètes, à la recherche de vapeur d¿eau et autres molécules comme l'oxygène et le méthane qui indiquent la présence d'activité biologique. La réalité dépasse maintenant la science-fiction : l'humanité atteindra bientôt la maturité technologique lui permettant de répondre à cette grande question qui nous tenaille depuis des siècles : Sommes-nous seuls dans l'Univers? | |
