Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26255
DC Field | Value | Language |
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dc.contributor.author | Bouwens, Rychard J. | en_US |
dc.contributor.author | Aravena, Manuel | en_US |
dc.contributor.author | DECARLI, ROBERTO | en_US |
dc.contributor.author | Walter, Fabian | en_US |
dc.contributor.author | Labbé, Ivo | en_US |
dc.contributor.author | Bauer, Franz E. | en_US |
dc.contributor.author | Bertoldi, Frank | en_US |
dc.contributor.author | Carilli, Chris | en_US |
dc.contributor.author | Chapman, Scott | en_US |
dc.contributor.author | Daddi, Emanuele | en_US |
dc.contributor.author | Hodge, Jacqueline | en_US |
dc.contributor.author | Ivison, Rob J. | en_US |
dc.contributor.author | Karim, Alex | en_US |
dc.contributor.author | Le Fevre, Olivier | en_US |
dc.contributor.author | Magnelli, Benjamin | en_US |
dc.contributor.author | Ota, Kazuaki | en_US |
dc.contributor.author | Riechers, Dominik | en_US |
dc.contributor.author | Smail, Ian R. | en_US |
dc.contributor.author | van der Werf, Paul | en_US |
dc.contributor.author | Weiss, Axel | en_US |
dc.contributor.author | Cox, Pierre | en_US |
dc.contributor.author | Elbaz, David | en_US |
dc.contributor.author | Gonzalez-Lopez, Jorge | en_US |
dc.contributor.author | Infante, Leopoldo | en_US |
dc.contributor.author | Oesch, Pascal | en_US |
dc.contributor.author | Wagg, Jeff | en_US |
dc.contributor.author | Wilkins, Steve | en_US |
dc.date.accessioned | 2020-06-29T09:26:53Z | - |
dc.date.available | 2020-06-29T09:26:53Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26255 | - |
dc.description.abstract | We make use of deep 1.2 mm continuum observations (12.7 μJy beam<SUP>-1</SUP> rms) of a 1 arcmin<SUP>2</SUP> region in the Hubble Ultra Deep Field to probe dust-enshrouded star formation from 330 Lyman-break galaxies spanning the redshift range z = 2-10 (to ∼2-3 M <SUB>☉</SUB> yr<SUP>-1</SUP> at 1σ over the entire range). Given the depth and area of ASPECS, we would expect to tentatively detect 35 galaxies, extrapolating the Meurer z ∼ 0 IRX-β relation to z ≥ 2 (assuming dust temperature T <SUB> d </SUB> ∼ 35 K). However, only six tentative detections are found at z ≳ 2 in ASPECS, with just three at >3σ. Subdividing our z = 2-10 galaxy samples according to stellar mass, UV luminosity, and UV-continuum slope and stacking the results, we find a significant detection only in the most massive (>10<SUP>9.75</SUP> M <SUB>☉</SUB>) subsample, with an infrared excess (IRX = L <SUB>IR</SUB>/L <SUB>UV</SUB>) consistent with previous z ∼ 2 results. However, the infrared excess we measure from our large selection of sub-L <SUP>∗</SUP> (<10<SUP>9.75</SUP> M <SUB>☉</SUB>) galaxies is {0.11}<SUB>-0.42</SUB><SUP>+0.32</SUP> ± 0.34 (bootstrap and formal uncertainties) and {0.14}<SUB>-0.14</SUB><SUP>+0.15</SUP> ± 0.18 at z = 2-3 and z = 4-10, respectively, lying below even an IRX-β relation for the Small Magellanic Cloud (95% confidence). These results demonstrate the relevance of stellar mass for predicting the IR luminosity of z ≳ 2 galaxies. We find that the evolution of the IRX-stellar mass relationship depends on the evolution of the dust temperature. If the dust temperature increases monotonically with redshift (\propto {(1+z)}<SUP>0.32</SUP>) such that T <SUB> d </SUB> ∼ 44-50 K at z ≥ 4, current results are suggestive of little evolution in this relationship to z ∼ 6. We use these results to revisit recent estimates of the z ≥ 3 star formation rate density. | en_US |
dc.language.iso | eng | en_US |
dc.title | ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: The Infrared Excess of UV-Selected z = 2-10 Galaxies as a Function of UV-Continuum Slope and Stellar Mass | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/833/1/72 | en_US |
dc.identifier.scopus | 2-s2.0-85006512000 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/833/1/72 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 833 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 72 | 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...72B | 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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J._Bouwens_2016_ApJ_833_72.pdf | Pdf editoriale | 2.71 MB | Adobe PDF | View/Open |
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