Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/27542
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Roy, N. | en_US |
dc.contributor.author | NAPOLITANO, NICOLA ROSARIO | en_US |
dc.contributor.author | LA BARBERA, Francesco | en_US |
dc.contributor.author | TORTORA, CRESCENZO | en_US |
dc.contributor.author | GETMAN, FEDOR | en_US |
dc.contributor.author | RADOVICH, MARIO | en_US |
dc.contributor.author | Capaccioli, M. | en_US |
dc.contributor.author | BRESCIA, Massimo | en_US |
dc.contributor.author | CAVUOTI, STEFANO | en_US |
dc.contributor.author | Longo, G. | en_US |
dc.contributor.author | RAJ, MARIA ANGELA | en_US |
dc.contributor.author | PUDDU, Emanuella Anna | en_US |
dc.contributor.author | Covone, G. | en_US |
dc.contributor.author | Amaro, V. | en_US |
dc.contributor.author | Vellucci, C. | en_US |
dc.contributor.author | GRADO, ANIELLO | en_US |
dc.contributor.author | Kuijken, K. | en_US |
dc.contributor.author | Verdoes Kleijn, G. | en_US |
dc.contributor.author | Valentijn, E. | en_US |
dc.date.accessioned | 2020-10-02T09:02:29Z | - |
dc.date.available | 2020-10-02T09:02:29Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27542 | - |
dc.description.abstract | We have obtained structural parameters of about 340 000 galaxies from the Kilo-Degree Survey (KiDS) in 153 deg<SUP>2</SUP> of data release 1, 2, and 3. We have performed a seeing convolved 2D single Sérsic fit to the galaxy images in the four photometric bands (u, g, r, i) observed by KiDS, by selecting high signal-to-noise ratio (S/N > 50) systems in every bands. We have classified galaxies as spheroids and disc-dominated by combining their spectral energy distribution properties and their Sérsic index. Using photometric redshifts derived from a machine learning technique, we have determined the evolution of the effective radius, R<SUB>e</SUB> and stellar mass, M<SUB>⋆</SUB>, versus redshift, for both mass complete samples of spheroids and disc-dominated galaxies up to z∼0.6. Our results show a significant evolution of the structural quantities at intermediate redshift for the massive spheroids (log M<SUB>*</SUB>/M<SUB>☉</SUB> > 11, Chabrier IMF), while almost no evolution has found for less massive ones (log M<SUB>*</SUB>/M<SUB>☉</SUB> < 11). On the other hand, disc dominated systems show a milder evolution in the less massive systems (log M<SUB>*</SUB>/M<SUB>☉</SUB> < 11) and possibly no evolution of the more massive systems. These trends are generally consistent with predictions from hydrodynamical simulations and independent datasets out to redshift z ∼ 0.6, although in some cases the scatter of the data is large to drive final conclusions. These results, based on 1/10 of the expected KiDS area, reinforce precedent finding based on smaller statistical samples and show the route towards more accurate results, expected with the the next survey releases. | en_US |
dc.language.iso | eng | en_US |
dc.title | Evolution of galaxy size-stellar mass relation from the Kilo-Degree Survey | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty1917 | en_US |
dc.identifier.scopus | 2-s2.0-85053454144 | en_US |
dc.identifier.isi | 000442567900072 | en_US |
dc.identifier.url | http://arxiv.org/abs/1807.06085v1 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article-abstract/480/1/1057/5056193?redirectedFrom=fulltext | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 480 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 1057 | en_US |
dc.relation.lastpage | 1080 | en_US |
dc.relation.numberofpages | 23 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 19 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | FRA | en_US |
dc.contributor.country | DEU | en_US |
dc.contributor.country | IND | en_US |
dc.contributor.country | NLD | 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 | 2018MNRAS.480.1057R | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | 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. Capodimonte | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.orcid | 0000-0003-0911-8884 | - |
crisitem.author.orcid | 0000-0003-1181-6841 | - |
crisitem.author.orcid | 0000-0001-7958-6531 | - |
crisitem.author.orcid | 0000-0003-1550-0182 | - |
crisitem.author.orcid | 0000-0002-3585-866X | - |
crisitem.author.orcid | 0000-0001-9506-5680 | - |
crisitem.author.orcid | 0000-0002-3787-4196 | - |
crisitem.author.orcid | 0000-0002-8374-0340 | - |
crisitem.author.orcid | 0000-0002-4522-6164 | - |
crisitem.author.orcid | 0000-0002-0501-8256 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
RoyEtAl-sty1917.pdf | Pdf editoriale | 11.3 MB | Adobe PDF | View/Open |
27542-RoyEtAl-sty1917_P01.pdf | Miur | 9.14 MB | Adobe PDF | |
27542-RoyEtAl-sty1917_P02.pdf | Miur | 2.23 MB | Adobe PDF |
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