Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/34647
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Monaco, L. | en_US |
dc.contributor.author | Saviane, I. | en_US |
dc.contributor.author | PERINA, SIBILLA | en_US |
dc.contributor.author | BELLAZZINI, Michele | en_US |
dc.contributor.author | BUZZONI, Alberto | en_US |
dc.contributor.author | Federici, L. | en_US |
dc.contributor.author | Fusi Pecci, F. | en_US |
dc.contributor.author | GALLETI, SILVIA | en_US |
dc.date.accessioned | 2024-01-29T15:21:48Z | - |
dc.date.available | 2024-01-29T15:21:48Z | - |
dc.date.issued | 2009 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/34647 | - |
dc.description.abstract | Context: NGC 205 is a peculiar dwarf elliptical galaxy hosting in its center a population of young blue stars. Their origin is still matter of debate, the central fresh star formation activity possibly being related to dynamical interactions between NGC 205 and M 31. <BR />Aims: The star formation history in the central 30´´ (~120 pc) around the NGC 205 central nucleus is investigated in order to obtain clues to the origin of the young stellar population. <BR />Methods: Deep HST/ACS CCD photometry is compared with theoretical isochrones and luminosity functions to characterize the stellar content of the region under study and compute the recent SF rate. <BR />Results: Our photometry reveals a previously undetected blue plume of young stars clearly distinguishable down to I≃ 26. Our analysis suggests that 1.9 × 10<SUP>5</SUP> M_⊙ were produced between approximately 62 Myr and 335 Myr ago in the NGC 205 inner regions, with a latest minor episode occurring ~25 Myr ago. This implies a star formation rate of ~7× 10<SUP>-4</SUP> M_⊙/yr over this period. <BR />Conclusions: The excellent fit of the observed luminosity function of young main sequence stars obtained with a model having a constant star formation rate argues against a tidally triggered star formation activity over the last ~300 Myr. Rather, a constant SF may be consistent with NGC 205 being on its first interaction with M 31. | en_US |
dc.language.iso | eng | en_US |
dc.title | The young stellar population at the center of NGC 205 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/200912412 | en_US |
dc.identifier.scopus | 2-s2.0-68949187657 | en_US |
dc.identifier.url | http://arxiv.org/abs/0907.0029v1 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2009/29/aa12412-09/aa12412-09.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 502 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | L9 | en_US |
dc.relation.lastpage | L12 | en_US |
dc.type.referee | REF_1 | 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.identifier.adsbibcode | 2009A&A...502L...9M | 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.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | O.A. Torino | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0001-6189-3883 | - |
crisitem.author.orcid | 0000-0001-8200-810X | - |
crisitem.author.orcid | 0000-0002-6514-1870 | - |
crisitem.author.orcid | 0000-0003-3825-2273 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
aa12412-09.pdf | PDF editoriale | 272.96 kB | Adobe PDF | View/Open |
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