Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26559
DC Field | Value | Language |
---|---|---|
dc.contributor.author | VANZELLA, Eros | en_US |
dc.contributor.author | CALURA, Francesco | en_US |
dc.contributor.author | MENEGHETTI, MASSIMO | en_US |
dc.contributor.author | MERCURIO, AMATA | en_US |
dc.contributor.author | CASTELLANO, MARCO | en_US |
dc.contributor.author | Caminha, G. B. | en_US |
dc.contributor.author | Balestra, I. | en_US |
dc.contributor.author | Rosati, P. | en_US |
dc.contributor.author | TOZZI, Paolo | en_US |
dc.contributor.author | De Barros, S. | en_US |
dc.contributor.author | GRAZIAN, Andrea | en_US |
dc.contributor.author | D'Ercole, A. | en_US |
dc.contributor.author | Ciotti, L. | en_US |
dc.contributor.author | Caputi, K. | en_US |
dc.contributor.author | Grillo, C. | en_US |
dc.contributor.author | MERLIN, Emiliano | en_US |
dc.contributor.author | PENTERICCI, Laura | en_US |
dc.contributor.author | FONTANA, Adriano | en_US |
dc.contributor.author | CRISTIANI, Stefano | en_US |
dc.contributor.author | Coe, D. | en_US |
dc.date.accessioned | 2020-07-22T05:46:17Z | - |
dc.date.available | 2020-07-22T05:46:17Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26559 | - |
dc.description.abstract | We report on five compact, extremely young (<10 Myr) and blue (β<SUB>UV</SUB> < -2.5, F<SUB>λ</SUB> = λ<SUP>β</SUP>) objects observed with VLT/Multi Unit Spectroscopic Explorer at redshifts 3.1169 and 3.235, in addition to three objects at z = 6.145. These sources are strongly magnified (3-40 times) by the Hubble Frontier Field galaxy clusters MACS J0416 and AS1063. Their delensed half-light radii (R<SUB>e</SUB>) are between 16 and 140 pc, the stellar masses are ≃1-20 × 10<SUP>6</SUP> M<SUB>☉</SUB>, the magnitudes are m<SUB>UV</SUB> = 28.8-31.4 (-17 < M<SUB>UV</SUB> < -15) and specific star formation rates can be as large as ∼800 Gyr<SUP>-1</SUP>. Remarkably, the inferred physical properties of two objects are similar to those expected in some globular cluster formation scenarios, representing the best candidate proto-GCs discovered so far. Rest-frame optical high-dispersion spectroscopy of one of them at z = 3.1169 yields a velocity dispersion σ<SUB>v</SUB> ≃ 20 km s<SUP>-1</SUP>, implying a dynamical mass dominated by the stellar mass. Another object at z = 6.145, with delensed M<SUB>UV</SUB> ≃ -15.3 (m<SUB>UV</SUB> ≃ 31.4), shows a stellar mass and a star formation rate surface density consistent with the values expected from popular GC formation scenarios. An additional star-forming region at z = 6.145, with delensed m<SUB>UV</SUB> ≃ 32, a stellar mass of 0.5 × 10<SUP>6</SUP> M<SUB>☉</SUB> and a star formation rate of 0.06 M<SUB>☉</SUB> yr<SUP>-1</SUP> is also identified. These objects currently represent the faintest spectroscopically confirmed star-forming systems at z > 3, elusive even in the deepest blank fields. We discuss how proto-GCs might contribute to the ionization budget of the Universe and augment Lyα visibility during reionization. This work underlines the crucial role of JWST in characterizing the rest-frame optical and near-infrared properties of such low-luminosity high-z objects. | en_US |
dc.language.iso | eng | en_US |
dc.title | Paving the way for the JWST: witnessing globular cluster formation at z > 3 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stx351 | en_US |
dc.identifier.scopus | 2-s2.0-85040217837 | en_US |
dc.identifier.isi | 000398421100040 | en_US |
dc.identifier.url | http://arxiv.org/abs/1612.01526v2 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 467 | en_US |
dc.relation.issue | 4 | en_US |
dc.relation.firstpage | 4304 | en_US |
dc.relation.lastpage | 4321 | 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 | 2017MNRAS.467.4304V | 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.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.orcid | 0000-0002-5057-135X | - |
crisitem.author.orcid | 0000-0002-6175-0871 | - |
crisitem.author.orcid | 0000-0003-1225-7084 | - |
crisitem.author.orcid | 0000-0001-9261-7849 | - |
crisitem.author.orcid | 0000-0001-9875-8263 | - |
crisitem.author.orcid | 0000-0003-3096-9966 | - |
crisitem.author.orcid | 0000-0002-5688-0663 | - |
crisitem.author.orcid | 0000-0001-6870-8900 | - |
crisitem.author.orcid | 0000-0001-8940-6768 | - |
crisitem.author.orcid | 0000-0003-3820-2823 | - |
crisitem.author.orcid | 0000-0002-2115-5234 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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stx351.pdf | Pdf editoriale | 4.68 MB | Adobe PDF | View/Open |
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