Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/29914
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Pilo, S. | en_US |
dc.contributor.author | CASTELLANO, MARCO | en_US |
dc.contributor.author | FONTANA, Adriano | en_US |
dc.contributor.author | GRAZIAN, Andrea | en_US |
dc.contributor.author | Boutsia, K. | en_US |
dc.contributor.author | PENTERICCI, Laura | en_US |
dc.contributor.author | GIALLONGO, Emanuele | en_US |
dc.contributor.author | MERLIN, Emiliano | en_US |
dc.contributor.author | PARIS, Diego | en_US |
dc.contributor.author | SANTINI, Paola | en_US |
dc.date.accessioned | 2021-01-21T11:31:29Z | - |
dc.date.available | 2021-01-21T11:31:29Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29914 | - |
dc.description.abstract | Context. The analysis of the UV slope β of Lyman-break galaxies (LBG) at different luminosities and redshifts is fundamental for understanding their physical properties, and in particular, their dust extinction. <BR /> Aims: We analyse a unique sample of 517 bright (L > L<SUP>*</SUP>) LBGs at redshift z ∼ 3 in order to characterise the distribution of their UV slopes β and infer their dust extinction under standard assumptions. <BR /> Methods: We exploited multi-band observations over 750 arcmin<SUP>2</SUP> of the COSMOS field that were acquired with three different ground-based facilities: the Large Binocular Camera (LBC) on the Large Binocular Telescope (LBT), the Suprime-Cam on the SUBARU telescope, and the VIRCAM on the VISTA telescope (ULTRAVISTA DR2). Our multi-band photometric catalogue is based on a new method that is designed to maximise the signal-to-noise ratio in the estimate of accurate galaxy colours from images with different point spread functions (PSF). We adopted an improved selection criterion based on deep Y-band data to isolate a sample of galaxies at z ∼ 3 to minimise selection biases. We measured the UV slopes (β) of the objects in our sample and then recovered the intrinsic probability density function of β values (PDF(β)), taking into account the effect of observational uncertainties through detailed simulations. <BR /> Results: The galaxies in our sample are characterised by mildly red UV slopes with ⟨β⟩≃ - 1.70 throughout the enitre luminosity range that is probed by our data (-24 ≲ M<SUB>1600</SUB> ≲ -21). The resulting dust-corrected star formation rate density (SFRD) is log(SFRD)≃ - 1.6 M<SUB>☉</SUB> yr<SUP>-1</SUP> Mpc<SUP>-3</SUP>, corresponding to a contribution of about 25% to the total SFRD at z ∼ 3 under standard assumptions. Conclusions: Ultra-bright LBGs at z ∼ 3 match the known trends, with UV slopes being redder at decreasing redshifts, and brighter galaxies being more highly dust extinct and more frequently star-forming than fainter galaxies. | en_US |
dc.language.iso | eng | en_US |
dc.title | UV slope of z ∼ 3 bright (L > L*) Lyman-break galaxies in the COSMOS field | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201834442 | en_US |
dc.identifier.isi | 000470957700004 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2019/06/aa34442-18/aa34442-18.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 626 | en_US |
dc.relation.firstpage | A45 | 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 | 2019A&A...626A..45P | 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. Padova | - |
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 | O.A. Roma | - |
crisitem.author.orcid | 0000-0001-9875-8263 | - |
crisitem.author.orcid | 0000-0003-3820-2823 | - |
crisitem.author.orcid | 0000-0002-5688-0663 | - |
crisitem.author.orcid | 0000-0001-8940-6768 | - |
crisitem.author.orcid | 0000-0003-0734-1273 | - |
crisitem.author.orcid | 0000-0001-6870-8900 | - |
crisitem.author.orcid | 0000-0002-7409-8114 | - |
crisitem.author.orcid | 0000-0002-9334-8705 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
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1901.11302.pdf | postprint | 2.39 MB | Adobe PDF | Visualizza/apri |
aa34442-18.pdf | Pdf editoriale | 3.9 MB | Adobe PDF | Visualizza/apri |
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