Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/26349
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Shu, X. W. | en_US |
dc.contributor.author | Elbaz, D. | en_US |
dc.contributor.author | Bourne, N. | en_US |
dc.contributor.author | Schreiber, C. | en_US |
dc.contributor.author | Wang, T. | en_US |
dc.contributor.author | Dunlop, J. S. | en_US |
dc.contributor.author | FONTANA, Adriano | en_US |
dc.contributor.author | Leiton, R. | en_US |
dc.contributor.author | Pannella, M. | en_US |
dc.contributor.author | Okumura, K. | en_US |
dc.contributor.author | Michałowski, M. J. | en_US |
dc.contributor.author | SANTINI, Paola | en_US |
dc.contributor.author | MERLIN, Emiliano | en_US |
dc.contributor.author | Buitrago, F. | en_US |
dc.contributor.author | Bruce, V. A. | en_US |
dc.contributor.author | Amorin, R. | en_US |
dc.contributor.author | CASTELLANO, MARCO | en_US |
dc.contributor.author | Derriere, S. | en_US |
dc.contributor.author | COMASTRI, Andrea | en_US |
dc.contributor.author | Cappelluti, N. | en_US |
dc.contributor.author | Wang, J. X. | en_US |
dc.contributor.author | Ferguson, H. C. | en_US |
dc.date.accessioned | 2020-07-06T18:04:51Z | - |
dc.date.available | 2020-07-06T18:04:51Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0067-0049 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26349 | - |
dc.description.abstract | We present a new method to search for candidate z ≳ 2 Herschel 500 μm sources in the Great Observatories Origins Deep Survey-North field using a S<SUB>500 μm</SUB>/S<SUB>24 μm</SUB> “color deconfusion” technique. Potential high-z sources are selected against low-redshift ones from their large 500 to 24 μm flux density ratios. By effectively reducing the contribution from low-redshift populations to the observed 500 μm emission, we are able to identify counterparts to high-z 500 μm sources whose 24 μm fluxes are relatively faint. The recovery of known z ≳ 4 starbursts confirms the efficiency of this approach in selecting high-z Herschel sources. The resulting sample consists of 34 dusty star-forming galaxies at z ≳ 2. The inferred infrared luminosities are in the range 1.5 × 10<SUP>12</SUP>-1.8 × 10<SUP>13</SUP> L<SUB>☉</SUB>, corresponding to dust-obscured star formation rates (SFRs) of ∼260-3100 M<SUB>☉</SUB> yr<SUP>-1</SUP> for a Salpeter initial mass function. Comparison with previous SCUBA 850 μ {{m}}-selected galaxy samples shows that our method is more efficient at selecting high-z dusty galaxies, with a median redshift of z=3.07+/- 0.83 and with 10 of the sources at z ≳ 4. We find that at a fixed luminosity, the dust temperature is ∼5 K cooler than that expected from the {T}<SUB>d</SUB>-{L}<SUB>{{IR</SUB>}} relation at z\quad ≲ 1, though different temperature selection effects should be taken into account. The radio-detected subsample (excluding three strong active galactic nucleus) follows the far-infrared (far-IR)/radio correlation at lower redshifts, and no evolution with redshift is observed out to z∼ 5, suggesting that the far-IR emission is star formation dominated. The contribution of the high-z Herschel 500 μm sources to the cosmic SFR density is comparable to that of (sub)millimeter galaxy populations at z∼ 2.5 and at least 40% of the extinction-corrected UV samples at z∼ 4. Further investigation into the nature of these high-z dusty galaxies will be crucial for our understanding of the star formation histories and the buildup of stellar mass at the earliest cosmic epochs. | en_US |
dc.language.iso | eng | en_US |
dc.title | Identification of z ≳ 2 Herschel 500 μM Sources Using Color Deconfusion | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/0067-0049/222/1/4 | en_US |
dc.identifier.scopus | 2-s2.0-84955451286 | en_US |
dc.identifier.isi | 000368982300004 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/0067-0049/222/1/4 | en_US |
dc.identifier.url | https://arxiv.org/abs/1512.00167 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 222 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 4 | en_US |
dc.relation.numberofpages | 29 | en_US |
dc.relation.article | 4 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 22 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | FRA | en_US |
dc.contributor.country | DEU | en_US |
dc.contributor.country | CHL | en_US |
dc.contributor.country | TWN | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2016ApJS..222....4S | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering | 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 | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0003-3820-2823 | - |
crisitem.author.orcid | 0000-0002-9334-8705 | - |
crisitem.author.orcid | 0000-0001-6870-8900 | - |
crisitem.author.orcid | 0000-0001-9875-8263 | - |
crisitem.author.orcid | 0000-0003-3451-9970 | - |
crisitem.journal.journalissn | 0067-0049 | - |
crisitem.journal.ance | E016254 | - |
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