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http://hdl.handle.net/20.500.12386/29476
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | VALIANTE, ROSA | en_US |
dc.contributor.author | SCHNEIDER, RAFFAELLA | en_US |
dc.contributor.author | GRAZIANI, Luca | en_US |
dc.contributor.author | ZAPPACOSTA, Luca | en_US |
dc.date.accessioned | 2021-01-05T09:45:00Z | - |
dc.date.available | 2021-01-05T09:45:00Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29476 | - |
dc.description.abstract | Supermassive black holes (SMBHs) of 10<SUP>9</SUP>-10<SUP>10</SUP> M<SUB>☉</SUB> were already in place ∼13 Gyr ago, at z > 6. Super-Eddington growth of low-mass BH seeds (∼100 M<SUB>☉</SUB>) or less extreme accretion on to∼10<SUP>5</SUP> M<SUB>☉</SUB> seeds have been recently considered as the main viable routes to these SMBHs. Here, we study the statistics of these SMBH progenitors at z ∼ 6. The growth of low- and high-mass seeds and their host galaxies are consistently followed using the cosmological data constrained model GAMETE/QSODUST, which reproduces the observed properties of high-z quasars, like SDSS J1148+5251. We show that both seed formation channels can be in action over a similar redshift range 15 < z < 18 and are found in dark matter haloes with comparable mass, ∼5 × 10<SUP>7</SUP> M<SUB>☉</SUB>. However, as long as the systems evolve in isolation (i.e. no mergers occur), noticeable differences in their properties emerge: At z ≥ 10 galaxies hosting high-mass seeds have smaller stellar mass and metallicity, the BHs accrete gas at higher rates and star formation proceeds less efficiently than in low-mass seeds hosts. At z < 10 these differences are progressively erased, as the systems experience minor or major mergers and every trace of the BH origin gets lost. | en_US |
dc.language.iso | eng | en_US |
dc.title | Chasing the observational signatures of seed black holes at z > 7: candidate statistics | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stx3028 | en_US |
dc.identifier.scopus | 2-s2.0-85040235032 | en_US |
dc.identifier.isi | 000424347900074 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/474/3/3825/4655201 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 474 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3825 | en_US |
dc.type.referee | REF_1 | 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 | en_US |
dc.identifier.adsbibcode | 2018MNRAS.474.3825V | 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.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0003-3050-1765 | - |
crisitem.author.orcid | 0000-0001-9317-2888 | - |
crisitem.author.orcid | 0000-0002-4205-6884 | - |
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