Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/32390
DC Field | Value | Language |
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dc.contributor.author | Carnall, A. C. | en_US |
dc.contributor.author | Walker, S. | en_US |
dc.contributor.author | McLure, R. J. | en_US |
dc.contributor.author | Dunlop, J. S. | en_US |
dc.contributor.author | McLeod, D. J. | en_US |
dc.contributor.author | Cullen, F. | en_US |
dc.contributor.author | Wild, V. | en_US |
dc.contributor.author | Amorin, R. | en_US |
dc.contributor.author | BOLZONELLA, MICOL | en_US |
dc.contributor.author | CASTELLANO, MARCO | en_US |
dc.contributor.author | Cimatti, A. | en_US |
dc.contributor.author | CUCCIATI, Olga | en_US |
dc.contributor.author | FONTANA, Adriano | en_US |
dc.contributor.author | GARGIULO, ADRIANA | en_US |
dc.contributor.author | GARILLI, BIANCA MARIA ROSA | en_US |
dc.contributor.author | Jarvis, M. J. | en_US |
dc.contributor.author | PENTERICCI, Laura | en_US |
dc.contributor.author | POZZETTI, Lucia | en_US |
dc.contributor.author | Zamorani, G. | en_US |
dc.contributor.author | Calabro, A. | en_US |
dc.contributor.author | Hathi, N. P. | en_US |
dc.contributor.author | Koekemoer, A. M. | en_US |
dc.date.accessioned | 2022-06-17T12:58:27Z | - |
dc.date.available | 2022-06-17T12:58:27Z | - |
dc.date.issued | 2020 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32390 | - |
dc.description.abstract | We present a sample of 151 massive (M<SUB>*</SUB> > 10<SUP>10</SUP> M<SUB>⊙</SUB>) quiescent galaxies at 2 < z < 5, based on a sophisticated Bayesian spectral energy distribution fitting analysis of the CANDELS UDS and GOODS-South fields. Our sample includes a robust sub-sample of 61 objects for which we confidently exclude low-redshift and star-forming solutions. We identify 10 robust objects at z > 3, of which 2 are at z > 4. We report formation redshifts, demonstrating that the oldest objects formed at z > 6; however, individual ages from our photometric data have significant uncertainties, typically ∼0.5 Gyr. We demonstrate that the UVJ colours of the quiescent population evolve with redshift at z > 3, becoming bluer and more similar to post-starburst galaxies at lower redshift. Based upon this, we construct a model for the time evolution of quiescent galaxy UVJ colours, concluding that the oldest objects are consistent with forming the bulk of their stellar mass at z ∼ 6-7 and quenching at z ∼ 5. We report spectroscopic redshifts for two of our objects at z = 3.440 and 3.396, which exhibit extremely weak Ly α emission in ultra-deep VANDELS spectra. We calculate star formation rates based on these line fluxes, finding that these galaxies are consistent with our quiescent selection criteria, provided their Ly α escape fractions are >3 and >10 per cent, respectively. We finally report that our highest redshift robust object exhibits a continuum break at λ ∼ 7000 Å in a spectrum from VUDS, consistent with our photometric redshift of $z_\mathrm{phot}=4.72^{+0.06}_{-0.04}$ . If confirmed as quiescent, this object would be the highest redshift known quiescent galaxy. To obtain stronger constraints on the times of the earliest quenching events, high-SNR spectroscopy must be extended to z ≳ 3 quiescent objects. | en_US |
dc.language.iso | eng | en_US |
dc.title | Timing the earliest quenching events with a robust sample of massive quiescent galaxies at 2 < z < 5 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/staa1535 | en_US |
dc.identifier.scopus | 2-s2.0-85088304752 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/496/1/695/5851291 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 496 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 695 | en_US |
dc.relation.lastpage | 707 | 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 | 2020MNRAS.496..695C | 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 | O.A. Roma | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0003-3278-4607 | - |
crisitem.author.orcid | 0000-0001-9875-8263 | - |
crisitem.author.orcid | 0000-0002-9336-7551 | - |
crisitem.author.orcid | 0000-0003-3820-2823 | - |
crisitem.author.orcid | 0000-0002-3351-1216 | - |
crisitem.author.orcid | 0000-0001-7455-8750 | - |
crisitem.author.orcid | 0000-0001-8940-6768 | - |
crisitem.author.orcid | 0000-0001-7085-0412 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
---|---|---|---|---|
staa1535.pdf | Pdf editoriale | 4.72 MB | Adobe PDF | View/Open |
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