Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26259
DC Field | Value | Language |
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dc.contributor.author | Aravena, M. | en_US |
dc.contributor.author | DECARLI, ROBERTO | en_US |
dc.contributor.author | Walter, F. | en_US |
dc.contributor.author | Bouwens, R. | en_US |
dc.contributor.author | Oesch, P. A. | en_US |
dc.contributor.author | Carilli, C. L. | en_US |
dc.contributor.author | Bauer, F. E. | en_US |
dc.contributor.author | Da Cunha, E. | en_US |
dc.contributor.author | Daddi, E. | en_US |
dc.contributor.author | Gónzalez-López, J. | en_US |
dc.contributor.author | Ivison, R. J. | en_US |
dc.contributor.author | Riechers, D. A. | en_US |
dc.contributor.author | Smail, I. | en_US |
dc.contributor.author | Swinbank, A. M. | en_US |
dc.contributor.author | Weiss, A. | en_US |
dc.contributor.author | Anguita, T. | en_US |
dc.contributor.author | Bacon, R. | en_US |
dc.contributor.author | Bell, E. | en_US |
dc.contributor.author | Bertoldi, F. | en_US |
dc.contributor.author | Cortes, P. | en_US |
dc.contributor.author | Cox, P. | en_US |
dc.contributor.author | Hodge, J. | en_US |
dc.contributor.author | Ibar, E. | en_US |
dc.contributor.author | Inami, H. | en_US |
dc.contributor.author | Infante, L. | en_US |
dc.contributor.author | Karim, A. | en_US |
dc.contributor.author | Magnelli, B. | en_US |
dc.contributor.author | Ota, K. | en_US |
dc.contributor.author | Popping, G. | en_US |
dc.contributor.author | van der Werf, P. | en_US |
dc.contributor.author | Wagg, J. | en_US |
dc.contributor.author | Fudamoto, Y. | en_US |
dc.date.accessioned | 2020-06-29T09:52:23Z | - |
dc.date.available | 2020-06-29T09:52:23Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26259 | - |
dc.description.abstract | We present a search for [C II] line and dust continuum emission from optical dropout galaxies at z > 6 using ASPECS, our Atacama Large Millimeter submillimeter Array Spectroscopic Survey in the Hubble Ultra-deep Field (UDF). Our observations, which cover the frequency range of 212-272 GHz, encompass approximately the range of 6 < z < 8 for [C II] line emission and reach a limiting luminosity of L <SUB>[C II]</SUB> ∼ (1.6-2.5) × 10<SUP>8</SUP> L <SUB>☉</SUB>. We identify 14 [C II] line emitting candidates in this redshift range with significances >4.5σ, two of which correspond to blind detections with no optical counterparts. At this significance level, our statistical analysis shows that about 60% of our candidates are expected to be spurious. For one of our blindly selected [C II] line candidates, we tentatively detect the CO(6-5) line in our parallel 3 mm line scan. None of the line candidates are individually detected in the 1.2 mm continuum. A stack of all [C II] candidates results in a tentative detection with S <SUB>1.2 mm</SUB> = 14 ± 5 μJy. This implies a dust-obscured star-formation rate (SFR) of (3 ± 1) M <SUB>☉</SUB> yr<SUP>-1</SUP>. We find that the two highest-SFR objects have candidate [C II] lines with luminosities that are consistent with the low-redshift L <SUB>[C II]</SUB> versus SFR relation. The other candidates have significantly higher [C II] luminosities than expected from their UV-based SFR. At the current sensitivity, it is unclear whether the majority of these sources are intrinsically bright [C II] emitters, or spurious sources. If only one of our line candidates was real (a scenario greatly favored by our statistical analysis), we find a source density for [C II] emitters at 6 < z < 8 that is significantly higher than predicted by current models and some extrapolations from galaxies in the local universe. | en_US |
dc.language.iso | eng | en_US |
dc.title | The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: Search for [CII] Line and Dust Emission in 6 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/833/1/71 | en_US |
dc.identifier.scopus | 2-s2.0-85006375111 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/833/1/71 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 833 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 71 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2016ApJ...833...71A | 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.orcid | 0000-0002-2662-8803 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Aravena_2016_ApJ_833_71.pdf | Pdf editoriale | 4.42 MB | Adobe PDF | View/Open |
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