Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/29068
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Zoldan, Anna | en_US |
dc.contributor.author | DE LUCIA, GABRIELLA | en_US |
dc.contributor.author | XIE, Lizhi | en_US |
dc.contributor.author | FONTANOT, Fabio | en_US |
dc.contributor.author | Hirschmann, Michaela | en_US |
dc.date.accessioned | 2020-12-22T07:10:12Z | - |
dc.date.available | 2020-12-22T07:10:12Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29068 | - |
dc.description.abstract | In this work, we study the basic statistical properties of H I-selected galaxies extracted from six different semi-analytic models, all run on the same cosmological N-body simulation. One model includes an explicit treatment for the partition of cold gas into atomic and molecular hydrogen. All models considered agree nicely with the measured H I mass function in the local Universe, with the measured scaling relations between H I and galaxy stellar mass, and with the predicted two-point correlation function for H I-rich galaxies. One exception is given by one model that predicts very little H I associated with galaxies in haloes above ∼10<SUP>12</SUP> M<SUB>☉</SUB>: we argue this is due to a too efficient radio-mode feedback for central galaxies, and to a combination of efficient stellar feedback and instantaneous stripping of hot gas for satellites. We demonstrate that treatment of satellite galaxies introduces large uncertainties at low H I masses. While models assuming non-instantaneous stripping of hot gas tend to form satellite galaxies with H I masses slightly smaller than those of centrals with the same stellar mass, instantaneous gas stripping does not translate necessarily in lower H I masses. In fact, the adopted stellar feedback and star formation affect the satellites too. We analyse the relation between H I content and spin of simulated haloes: low-spin haloes tend to host H I-poor galaxies, while high-spin haloes are populated by galaxies in a wide range of H I mass. In our simulations, this is due to a correlation between the initial gas disc size and the halo spin. | en_US |
dc.language.iso | eng | en_US |
dc.title | H I-selected galaxies in hierarchical models of galaxy formation and evolution | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stw2901 | en_US |
dc.identifier.scopus | 2-s2.0-85029071333 | en_US |
dc.identifier.isi | 000393785500071 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/465/2/2236/2454760 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 465 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 2236 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | 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 | 2017MNRAS.465.2236Z | 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. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.orcid | 0000-0002-6220-9104 | - |
crisitem.author.orcid | 0000-0003-4744-0188 | - |
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 | |
---|---|---|---|---|
stw2901.pdf | PDF editoriale | 2.71 MB | Adobe PDF | View/Open |
1610.02042(1).pdf | 1.78 MB | Adobe PDF | View/Open |
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