Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/30776
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | VANZELLA, Eros | en_US |
dc.contributor.author | CALURA, Francesco | en_US |
dc.contributor.author | MENEGHETTI, MASSIMO | en_US |
dc.contributor.author | CASTELLANO, MARCO | en_US |
dc.contributor.author | Caminha, G. B. | en_US |
dc.contributor.author | MERCURIO, AMATA | en_US |
dc.contributor.author | CUPANI, Guido | en_US |
dc.contributor.author | Rosati, P. | en_US |
dc.contributor.author | Grillo, C. | en_US |
dc.contributor.author | GILLI, Roberto | en_US |
dc.contributor.author | MIGNOLI, Marco | en_US |
dc.contributor.author | FIORENTINO, Giuliana | en_US |
dc.contributor.author | ARCIDIACONO, CARMELO | en_US |
dc.contributor.author | LOMBINI, MATTEO | en_US |
dc.contributor.author | CORTECCHIA, Fausto | en_US |
dc.date.accessioned | 2021-04-16T15:30:48Z | - |
dc.date.available | 2021-04-16T15:30:48Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30776 | - |
dc.description.abstract | We report on a superdense star-forming region with an effective radius (R<SUB>e</SUB>) smaller than 13 pc identified at z = 6.143 and showing a star formation rate density Σ<SUB>SFR</SUB> ∼ 1000 M<SUB>⊙</SUB> yr<SUP>-1</SUP> kpc<SUP>-2</SUP> (or conservatively >300 M<SUB>⊙</SUB> yr<SUP>-1</SUP> kpc<SUP>-2</SUP>). Such a dense region is detected with S/N ≳ 40 hosted by a dwarf extending over 440 pc, dubbed D1. D1 is magnified by a factor 17.4(±5.0) behind the Hubble Frontier Field galaxy cluster MACS J0416 and elongated tangentially by a factor 13.2 ± 4.0 (including the systematic errors). The lens model accurately reproduces the positions of the confirmed multiple images with a rms of 0.35 arcsec. D1 is part of an interacting star-forming complex extending over 800 pc. The SED-fitting, the very blue ultraviolet slope (β ≃ -2.5, F<SUB>λ</SUB> ∼ λ<SUP>β</SUP>), and the prominent Lyα emission of the stellar complex imply that very young (<10-100 Myr), moderately dust-attenuated (E(B - V) < 0.15) stellar populations are present and organized in dense subcomponents. We argue that D1 (with a stellar mass of 2 × 10<SUP>7</SUP> M<SUB>⊙</SUB>) might contain a young massive star cluster of M ≲ 10<SUP>6</SUP> M<SUB>⊙</SUB> and M<SUB>UV</SUB> ≃ -15.6 (or m<SUB>UV</SUB> = 31.1), confined within a region of 13 pc, and not dissimilar from some local super star clusters (SSCs). The ultraviolet appearance of D1 is also consistent with a simulated local dwarf hosting an SSC placed at z = 6 and lensed back to the observer. This compact system fits into some popular globular cluster formation scenarios. We show that future high spatial resolution imaging (e.g. E-ELT/MAORY-MICADO and VLT/MAVIS) will allow us to spatially resolve light profiles of 2-8 pc. | en_US |
dc.language.iso | eng | en_US |
dc.title | Massive star cluster formation under the microscope at z = 6 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty3311 | en_US |
dc.identifier.scopus | 2-s2.0-85067084110 | en_US |
dc.identifier.url | http://arxiv.org/abs/1809.02617v2 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/483/3/3618/5232387 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 483 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3618 | en_US |
dc.relation.lastpage | 3635 | 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 | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2019MNRAS.483.3618V | 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.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0002-5057-135X | - |
crisitem.author.orcid | 0000-0002-6175-0871 | - |
crisitem.author.orcid | 0000-0003-1225-7084 | - |
crisitem.author.orcid | 0000-0001-9875-8263 | - |
crisitem.author.orcid | 0000-0001-9261-7849 | - |
crisitem.author.orcid | 0000-0002-6830-9093 | - |
crisitem.author.orcid | 0000-0001-8121-6177 | - |
crisitem.author.orcid | 0000-0002-9087-2835 | - |
crisitem.author.orcid | 0000-0003-0376-6928 | - |
crisitem.author.orcid | 0000-0003-0142-8108 | - |
crisitem.author.orcid | 0000-0001-9818-9283 | - |
crisitem.author.orcid | 0000-0001-5072-7791 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
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