Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26189
DC Field | Value | Language |
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dc.contributor.author | Pezzulli, EDWIGE | en_US |
dc.contributor.author | VALIANTE, ROSA | en_US |
dc.contributor.author | SCHNEIDER, RAFFAELLA | en_US |
dc.date.accessioned | 2020-06-23T07:55:24Z | - |
dc.date.available | 2020-06-23T07:55:24Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26189 | - |
dc.description.abstract | The assembly of the first super massive black holes (SMBHs) at z ≳ 6 is still a subject of intense debate. If black holes (BHs) grow at their Eddington rate, they must start from ≳10<SUP>4</SUP> M<SUB>☉</SUB> seeds formed by the direct collapse of gas. Here, we explore the alternative scenario where ∼100 M<SUB>☉</SUB> BH remnants of the first stars grow at super-Eddington rate via radiatively inefficient slim accretion discs. We use an improved version of the cosmological, data-constrained semi-analytic model GAMETE/QSODUST, where we follow the evolution of nuclear BHs and gas cooling, disc and bulge formation of their host galaxies. Adopting SDSS J1148+5251 (J1148) at z = 6.4 as a prototype of luminous z ≳ 6 quasars, we find that ∼80 per cent of its SMBH mass is grown by super-Eddington accretion, which can be sustained down to z ∼ 10 in dense, gas-rich environments. The average BH mass at z ∼ 20 is M<SUB>BH</SUB> ≳ 10<SUP>4</SUP> M<SUB>☉</SUB>, comparable to that of direct collapse BHs. At z = 6.4 the AGN-driven mass outflow rate is consistent with the observations and the BH-to-bulge mass ratio is compatible with the local scaling relation. However, the stellar mass in the central 2.5 kpc is closer to the value inferred from CO observations. Finally, ∼20 per cent of J1148 progenitors at z = 7.1 have BH luminosities and masses comparable to ULAS J1120+0641, suggesting that this quasar may be one of the progenitors of J1148. | en_US |
dc.language.iso | eng | en_US |
dc.title | Super-Eddington growth of the first black holes | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stw505 | en_US |
dc.identifier.scopus | 2-s2.0-84964727170 | en_US |
dc.identifier.isi | 000375799000056 | en_US |
dc.identifier.url | http://arxiv.org/abs/1603.00475v1 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/458/3/3047/2589331 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 458 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3047 | en_US |
dc.relation.lastpage | 3059 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 3 | 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.458.3047P | 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 | 0000-0003-3050-1765 | - |
crisitem.author.orcid | 0000-0001-9317-2888 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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Pezzulli16.pdf | Pdf editoriale | 2.91 MB | Adobe PDF | View/Open |
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