CHEMICALSUBSTRUCTURE

Elemental abundance analysis of substructures in the Galaxy disk. Implications for disk formation

Coordinatore	LUNDS UNIVERSITET    more  Organization address address: Paradisgatan 5c city: LUND postcode: 22100 contact info Titolo: Dr. Nome: Sofia Cognome: Feltzing Email: send email Telefono: -2227294 Fax: -2224614
Nazionalità Coordinatore	Sweden [SE]
Totale costo	0 €
EC contributo	173˙893 €
Programma	FP7-PEOPLE Specific programme "People" implementing the Seventh Framework Programme of the European Community for research, technological development and demonstration activities (2007 to 2013)
Code Call	FP7-PEOPLE-IIF-2008
Funding Scheme	MC-IIF
Anno di inizio	2009
Periodo (anno-mese-giorno)	2009-11-25   -   2011-11-24

 Partecipanti

#	participant	country	role	EC contrib. [€]
1	LUNDS UNIVERSITET  Organization address address: Paradisgatan 5c city: LUND postcode: 22100 contact info Titolo: Dr. Nome: Sofia Cognome: Feltzing Email: send email Telefono: -2227294 Fax: -2224614	SE (LUND)	coordinator	173˙893.90

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 Obiettivo del progetto (Objective)

'Elemental abundances in stars have proved to be an important tool in the study of the formation and evolution of the Milky Way. Combining the elemental abundances with the motions of the stars provide even stronger evidence for past and present evolution. Much recent work has focused on the identification of stellar streams in the Milky Way halo. Some of these streams have been identified as ruptured dwarf galaxies that are currently being engulfed by our Galaxy. However, it is the thin disk that dynamically and morphologically is the defining part of a disk galaxy. Several studies utilizing the Hipparcos data have unveiled a multitude of substructure within the thin disk. The origin of these substructures is not clear. Stars form in clusters and depending on their mass they may lose all or some of the cluster stars to the general field. As the cluster orbits around the Galaxy, it will disperse into a tube-like structure around the galactic plane. After several orbits it dissolves into the general background. The stars from the original cluster will be spread over the sky, but can be identified as a group through their common space motion. Hence, dissolving cluster can be one explanation for the substructures. Dynamical evolution within the disk and interaction with the bar can be another explanation. By obtaining elemental abundances of dispersing clusters and their associated superclusters and/or moving groups we can find out if they all come from the same original cluster (i.e. they have the same elemental abundance pattern) or if the structure is simply due to stirring of the general disk population (the stars do not share the same abundance pattern). We propose a comprehensive study of open clusters and associated groups as well as a truly differential study between these substructures and the Milky Way field population in order to shed light on how much of the disk population comes from dispersing clusters and how common the dynamical substructures are.'