(13 février 2012) Quatre conférences

Ci-dessous une liste de conférences qui pourraient vous intéresser :

 "Structure of galaxy disks shaped by secular evolution and environmental processes", Rome, 2 juillet 2012

 "Stellar Populations 55 years after the Vatican Conference", Rome, 2-4 Juillet 2012

 "A new reduction of old observations in the Gaia era", Paris Observatory, June 20-22, 2012

 42nd Saas-Fee Winter Course on “Dynamics of Young Star Clusters and Associations”, Villars-sur-Ollon, Suisse, 25-31 Mars 2012
Date limite pour les inscriptions *15 fevrier*

Amitiés,

Misha


EWASS, Special Session, "Structure of galaxy disks shaped by secular evolution and environmental processes", Rome, 2 juillet 2012

http://wwwhip.obspm.fr/EWASS2012-SPS4/Home.html

Early registration 15th february-11th May
In a typical spiral galaxy, a disk shows details whose origin and dynamics are not yet well-understood. These include, a thin disk and a thick disk component with vastly different kinematical properties ; an extended radial structure with a fall-off at large radii that is not well-understood ; misalignment in the outer parts as resulting in a warp ; non-axisymmetric features like bars and spiral arms that are expected to lead to radial migration.Understanding the role secular evolution processes and environmental effects have in shaping galaxy disks requires to look for and to quantify the characteristics of all these different components - their sizes, dependence, if any, on the galaxy Hubble type and on the environment, their evolution with look-back time, .. - and compare them with the predictions of numerical simulations and analytical models.This one-day special session aims to bring together observers, modelers and theoreticians to make the point on the study of the structure of galaxy disks : which are the main characteristics observed in their stellar and gaseous components ? How do they depend on the Hubble type or on the environment ? Which observed features can be more fruitfully compared to models in order to constrain the formation mechanisms ?


EWASS "Stellar Populations 55 years after the Vatican Conference", Rome, 2-4 Juillet 2012

http://www.oa-roma.inaf.it/step55/

Early registration 15th february-11th May

During the last half century stellar physics has been the quantitative side of modern astrophysics and our knowledge of the physical mechanisms driving stellar evolution, stellar spectroscopy and stellar pulsation have significantly improved. A significant fraction of the astrophysical problems attacked by the community in this period started with the stellar population definitions of the seminal Vatican conference in 1957 and 55 years later we plan to celebrate its impact by organizing an EWASS symposium on the same topic.

Despite the tremendous progress in our study of the mechanisms driving the evolution of stars and of whole galaxies gained in the last decades, we still lack a solid understanding of stellar populations, gas content and dynamical properties of systems in the Local Group (LG, d < 1 Mpc) and the Local Volume (LV, d < 25 Mpc). However, our knowledge concerning the star formation history (SFH), the chemical evolution and the kinematic properties of nearby systems significantly improved. This quantitative information is crucial to constrain theoretical models, and in turn explore the physical mechanisms governing the evolution of galaxies.

Moreover, in the near future new and interesting results are expected from ongoing (RAVE, OGLE, VISTA, VST, Pan-STARRS) and future surveys and instruments (Gaia, LSST, JWST, E-ELT/TMT). These are the reasons why we consider an EAS Symposium on this topic particularly timely. Moreover, a new generation of homogeneous spectroscopic and photometric data are becoming available, together with detailed cosmological simulations. Extragalactic chemical abundances based on a variety of diagnostics are also becoming available, together with deep and precise color-magnitude diagrams of a relevant fraction of the galactic body. The new data will provide the opportunity to fully exploit the observing capabilities of the next generation of telescopes in constraining the stellar population in the LV and beyond.

Together with photometric and spectroscopic survey evolutionary and pulsation models made a significant improvement concerning the treatment of both micro (opacity, equation of state, nuclear cross sections) and macro (gravitational settling, mixing, mass loss). Homogenenous sets of evolutionary models (isochrones luminosity functions) covering a broad range of chemical compositions became available for main sequence and advanced evolutionary phases. Moreover, detailed synthetic color-magnitude diagrams provided a unique opportunity to constrain the stellar content of both simple and complex stellar systems.

The meeting that we propose is the stepping stone to cope with future challenges in the field of stellar populations (evolution, pulsation, kinematics, abundances). It is also worth mentioning that during the last few editions of the EWASS meeting there was no meeting focussed on stellar populations.


"A new reduction of old observations in the Gaia era", Paris Observatory, June 20-22, 2012

Date limite pour les inscriptions : 15 mai, nombre de participants limité à 50.
http://www.imcce.fr/hosted_sites/naroo/

The arrival of the Gaia astrometric star catalogue will change completely the astrometric accuracy of new observations. More, it will also allow to re-reduce old observations with the Gaia accuracy. At the present time, we have catalogues of a sufficient accuracy to start the new reductions. Our first purpose is to select old observational data of selected objects of the Solar System worth to be reanalyzed. Preliminary works have shown the interest of this task. Old observations such as photographic plates contain valuable unused information concerning especially the moving objects of the Solar System. We are able to "observe in the past" these moving objects, increasing the ability to understand their dynamics.
The large amount of possible old data to be studied makes necessary to start now the selection and the digitizing criteria of old plates. This workshop is dedicated to this topic.


42nd Saas-Fee Winter Course on “Dynamics of Young Star Clusters and Associations”, March 25-31, 2012, in Villars-sur-Ollon, Switzerland.

Date limite pour les inscriptions : 15 février 2012, http://www.astro.phys.ethz.ch/sf2012/

This is the second announcement of the Saas-Fee Winter Course 2012. Please display the attached poster in your institute and distribute to interested colleagues : 42nd Saas-Fee Winter Course of the Swiss Society for Astrophysics and Astronomy (SSAA) on “Dynamics of Young Star Clusters and Associations”, March 25-31, 2012, in Villars-sur-Ollon, Switzerland.

We are pleased to announce the program for the 2012 Saas-Fee Course with a series of lectures concerning the theory and observational constraints on the dynamics of young star clusters and associations. With the proliferation of large area photometric, radial velocity, and astrometric surveys from ground-based telescopes, the launch of Gaia planned for 2013, and the explosive increase in our capacity to simulate the dynamics of these complex systems, the time is right to visit this topic. The school will attempt to address such questions as :

1) How common are star-forming events of varying richness ?

2) What are the dynamical states of these events ?

3) In what sort of star-forming event did the Sun form ?

4) How can we use answers to these questions to constrain predictive theories of star formation ?

These questions will be addressed by the following distinguished international faculty :

Prof. Cathie Clarke, Institute of Astronomy, University of Cambridge
Prof. Robert Mathieu, Dept. of Astronomy, University of Wisconsin
Dr. Neill Reid, Space Telescope Science Institute


Brèves

30 avril 2014

Gaia@SF2A2014

16 avril 2014

Ateliers PNCG et LSST

24 décembre 2013

Appel d’offre 2014

17 décembre 2013

En route vers les étoiles !

INSU CNRS Centre National de la recherche scientifique DPAC Gaia ESA