Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26530
DC Field | Value | Language |
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dc.contributor.author | SOLLIMA, ANTONIO LUIGI | en_US |
dc.contributor.author | Baumgardt, H. | en_US |
dc.date.accessioned | 2020-07-20T15:11:32Z | - |
dc.date.available | 2020-07-20T15:11:32Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26530 | - |
dc.description.abstract | We have derived the global mass functions of a sample of 35 Galactic globular clusters (GCs) by comparing deep Hubble Space Telescope photometry from the globular clusters treasury project (Sarajedini et al. 2007) with suitable multimass dynamical models. For a subset of 29 clusters with available radial velocity information, we were also able to determine dynamical parameters, mass-to-light ratios and the mass fraction of dark remnants. The derived global mass functions are well described by single power laws in the mass range 0.2 < m/ M<SUB>☉</SUB> < 0.8 with mass function slopes α > -1. Less-evolved clusters show deviations from a single-power law, indicating that the original shape of their mass distribution was not a power law. We find a tight anticorrelation between the present-day mass function slopes and the half-mass relaxation times, which can be understood if clusters started from the same universal initial mass function (IMF) and internal dynamical evolution is the main driver in shaping the present-day mass functions. Alternatively, IMF differences correlated with the present-day half-mass relaxation time are needed to explain the observed correlation. The large range of mass function slopes seen for our clusters implies that most GCs are dynamically highly evolved, a fact that seems difficult to reconcile with standard estimates for the dynamical evolution of clusters. The mass function slopes also correlate with the dark remnant fractions indicating a preferential retention of massive remnants in clusters subject to high mass-loss rates. | en_US |
dc.language.iso | eng | en_US |
dc.title | The global mass functions of 35 Galactic globular clusters: I. Observational data and correlations with cluster parameters | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stx1856 | en_US |
dc.identifier.scopus | 2-s2.0-85043525929 | en_US |
dc.identifier.isi | 000409035700083 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/471/3/3668/4002693 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 471 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3668 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 2 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | AUS | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | en_US |
dc.identifier.adsbibcode | 2017MNRAS.471.3668S | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_6 Stars and stellar systems | en_US |
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.cerifentitytype | Publications | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0001-7484-8467 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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stx1856.pdf | PDF editoriale | 1.45 MB | Adobe PDF | View/Open |
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