Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/30833
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Marmol-Queralto, E. | en_US |
dc.contributor.author | McLure, R. J. | en_US |
dc.contributor.author | Cullen, F. | en_US |
dc.contributor.author | Dunlop, J. S. | en_US |
dc.contributor.author | FONTANA, Adriano | en_US |
dc.contributor.author | McLeod, D. J. | en_US |
dc.date.accessioned | 2021-04-21T14:18:18Z | - |
dc.date.available | 2021-04-21T14:18:18Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30833 | - |
dc.description.abstract | We present the results of a study which uses spectral energy distribution (SED) fitting to investigate the evolution of the equivalent width (EW) of the Halpha emission line in star-forming galaxies over the redshift interval 1<z<5. After first demonstrating the ability of our SED-fitting technique to recover EW(Ha) using a sample of galaxies at z~1.3 with EW(Ha) measurements from 3D-HST grism spectroscopy, we proceed to apply our technique to samples of spectroscopically confirmed and photometric-redshift selected star-forming galaxies at z>=1 in the CANDELS UDS and GOODS-S fields. Confining our analysis to a constant stellar mass range (9.5<log(M/Msun)<10.5), we find that the median EW(Ha) evolves only modestly with redshift, reaching a rest-frame value of EW(Ha)=301+/-30 Angs by redshift z~4.5. Furthermore, using estimates of star-formation rate (SFR) based on both UV luminosity and Ha line flux, we use our galaxy samples to compare the evolution of EW(Ha) and specific star-formation rate (sSFR). Our results indicate that over the redshift range 1<z<5, the evolution displayed by EW(Ha) and sSFR is consistent, and can be adequately parameterized as: propto (1+z)^(1.0+/-0.2). As a consequence, over this redshift range we find that the sSFR and rest-frame EW(Ha) of star-forming galaxies with stellar masses M~10^(10) Msun are related by: EW(Ha)/Ang=(63+/-7)sSFR/Gyr^(-1). Given the current uncertainties in measuring the SFRs of high-redshift galaxies, we conclude that EW(Ha) provides a useful independent tracer of sSFR for star-forming galaxies out to redshifts of z=5. | en_US |
dc.language.iso | eng | en_US |
dc.title | The evolution of the equivalent width of the Ha emission line and specific star-formation rate in star-forming galaxies at 1<z<5 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stw1212 | en_US |
dc.identifier.scopus | 2-s2.0-84980322501 | en_US |
dc.identifier.url | http://arxiv.org/abs/1511.01911v2 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/460/4/3587/2609102 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 460 | en_US |
dc.relation.issue | 4 | en_US |
dc.relation.firstpage | 3587 | en_US |
dc.relation.lastpage | 3597 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | GBR | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2016MNRAS.460.3587M | 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.grantfulltext | open | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0003-3820-2823 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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stw1212.pdf | PDF editoriale | 564.65 kB | Adobe PDF | View/Open |
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