Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/29738
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Novak, M. | en_US |
dc.contributor.author | Smolčić, V. | en_US |
dc.contributor.author | Delhaize, J. | en_US |
dc.contributor.author | DELVECCHIO, IVAN | en_US |
dc.contributor.author | Zamorani, G. | en_US |
dc.contributor.author | Baran, N. | en_US |
dc.contributor.author | BONDI, MARCO | en_US |
dc.contributor.author | Capak, P. | en_US |
dc.contributor.author | Carilli, C. L. | en_US |
dc.contributor.author | CILIEGI, Paolo | en_US |
dc.contributor.author | Civano, F. | en_US |
dc.contributor.author | Ilbert, O. | en_US |
dc.contributor.author | Karim, A. | en_US |
dc.contributor.author | Laigle, C. | en_US |
dc.contributor.author | Le Fèvre, O. | en_US |
dc.contributor.author | MARCHESI, STEFANO | en_US |
dc.contributor.author | McCracken, H. | en_US |
dc.contributor.author | Miettinen, O. | en_US |
dc.contributor.author | Salvato, M. | en_US |
dc.contributor.author | Sargent, M. | en_US |
dc.contributor.author | Schinnerer, E. | en_US |
dc.contributor.author | Tasca, L. | en_US |
dc.date.accessioned | 2021-01-13T14:48:32Z | - |
dc.date.available | 2021-01-13T14:48:32Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29738 | - |
dc.description.abstract | We make use of the deep Karl G. Jansky Very Large Array (VLA) COSMOS radio observations at 3 GHz to infer radio luminosity functions of star-forming galaxies up to redshifts of z 5 based on approximately 6000 detections with reliable optical counterparts. This is currently the largest radio-selected sample available out to z 5 across an area of 2 square degrees with a sensitivity of rms ≈ 2.3 μJy beam<SUP>-1</SUP>. By fixing the faint and bright end shape of the radio luminosity function to the local values, we find a strong redshift trend that can be fitted with a pure luminosity evolution L<SUB>1.4 GHz</SUB> ∝ (1 + z)<SUP>(3.16 ± 0.2)-(0.32 ± 0.07)z</SUP>. We estimate star formation rates (SFRs) from our radio luminosities using an infrared (IR)-radio correlation that is redshift dependent. By integrating the parametric fits of the evolved luminosity function we calculate the cosmic SFR density (SFRD) history since z 5. Our data suggest that the SFRD history peaks between 2 < z < 3 and that the ultraluminous infrared galaxies (100 M<SUB>☉</SUB> yr<SUP>-1</SUP> < SFR < 1000 M<SUB>☉</SUB> yr<SUP>-1</SUP>) contribute up to 25% to the total SFRD in the same redshift range. Hyperluminous infrared galaxies (SFR > 1000 M<SUB>☉</SUB> yr<SUP>-1</SUP>) contribute an additional ≲2% in the entire observed redshift range. We find evidence of a potential underestimation of SFRD based on ultraviolet (UV) rest-frame observations of Lyman break galaxies at high redshifts (z ≳ 4) on the order of 15-20%, owing to appreciable star formation in highly dust-obscured galaxies, which might remain undetected in such UV observations. | en_US |
dc.language.iso | eng | en_US |
dc.title | The VLA-COSMOS 3 GHz Large Project: Cosmic star formation history since z 5 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201629436 | en_US |
dc.identifier.scopus | 2-s2.0-85020720103 | en_US |
dc.identifier.isi | 000404648300024 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2017/06/aa29436-16/aa29436-16.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 602 | en_US |
dc.relation.firstpage | A5 | 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 | 2017A&A...602A...5N | en_US |
dc.description.apc | sì | 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 | O.A. Brera | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0001-8706-2252 | - |
crisitem.author.orcid | 0000-0002-9553-7999 | - |
crisitem.author.orcid | 0000-0002-0447-4620 | - |
crisitem.author.orcid | 0000-0001-5544-0749 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
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