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http://hdl.handle.net/20.500.12386/29219
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | MASSARI, DAVIDE | en_US |
dc.contributor.author | H. H. Koppelman | en_US |
dc.contributor.author | A. Helmi | en_US |
dc.date.accessioned | 2020-12-28T15:22:52Z | - |
dc.date.available | 2020-12-28T15:22:52Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29219 | - |
dc.description.abstract | $Context$. The assembly history experienced by the Milky Way is currently being unveiled thanks to the data provided by the $Gaia$ mission. It is likely that the globular cluster system of our Galaxy has followed a similarly intricate formation path. $Aims$. To constrain this formation path, we explore the link between the globular clusters and the known merging events that the Milky Way has experienced. $Methods$. To this end, we combined the kinematic information provided by $Gaia$ for almost all Galactic clusters, with the largest sample of cluster ages available after carefully correcting for systematic errors. To identify clusters with a common origin we analysed their dynamical properties, particularly in the space of integrals of motion. $Results$. We find that about 40% of the clusters likely formed in situ. A similarly large fraction, 35%, appear to be possibly associated to known merger events, in particular to $Gaia$-Enceladus (19%), the Sagittarius dwarf galaxy (5%), the progenitor of the Helmi streams (6%), and to the Sequoia galaxy (5%), although some uncertainty remains due to the degree of overlap in their dynamical characteristics. Of the remaining clusters, 16% are tentatively associated to a group with high binding energy, while the rest are all on loosely bound orbits and likely have a more heterogeneous origin. The resulting age-metallicity relations are remarkably tight and differ in their detailed properties depending on the progenitor, providing further confidence on the associations made. $Conclusions$. We provide a table listing the likely associations. Improved kinematic data by future Gaia data releases and especially a larger, systematic error-free sample of cluster ages would help to further solidify our conclusions. | en_US |
dc.language.iso | eng | en_US |
dc.title | Origin of the system of globular clusters in the Milky Way | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201936135 | en_US |
dc.identifier.scopus | 2-s2.0-85086072364 | en_US |
dc.identifier.isi | 000487184400004 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2019/10/aa36135-19/aa36135-19.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 630 | en_US |
dc.relation.firstpage | L4 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.grantfulltext | open | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0001-8892-4301 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
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1804.09381.pdf | pdf editoriale | 9.43 MB | Adobe PDF | Visualizza/apri |
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