Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/35459
DC Field | Value | Language |
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dc.contributor.author | Bhatt, Maulik | en_US |
dc.contributor.author | Gallerani, Simona | en_US |
dc.contributor.author | Ferrara, Andrea | en_US |
dc.contributor.author | Mazzucchelli, Chiara | en_US |
dc.contributor.author | D'ODORICO, Valentina | en_US |
dc.contributor.author | VALENTINI, MILENA | en_US |
dc.contributor.author | Zana, Tommaso | en_US |
dc.contributor.author | Farina, Emanuele Paolo | en_US |
dc.contributor.author | Chakraborty, Srija | en_US |
dc.date.accessioned | 2024-12-11T17:25:38Z | - |
dc.date.available | 2024-12-11T17:25:38Z | - |
dc.date.issued | 2024 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/35459 | - |
dc.description.abstract | Context. Observations of z ∼ 6 quasars powered by supermassive black holes (SMBHs; M<SUB>BH</SUB> ∼ 10<SUP>8 − 10</SUP> M<SUB>⊙</SUB>) challenge our current understanding of early black hole (BH) formation and evolution. The advent of the James Webb Space Telescope (JWST) has enabled the study of massive BHs (MBHs; M<SUB>BH</SUB> ∼ 10<SUP>6 − 7</SUP> M<SUB>⊙</SUB>) up to z ∼ 11, thus bridging the properties of z ∼ 6 quasars to their ancestors. <BR /> Aims: The JWST spectroscopic observations of GN-z11, a well-known z = 10.6 star-forming galaxy, have been interpreted with the presence of a super-Eddington (Eddington ratio ≡ λ<SUB>Edd</SUB> ∼ 5.5) accreting MBH. To test this hypothesis, we used a zoom-in cosmological simulation of galaxy formation and BH co-evolution. <BR /> Methods: We first tested the simulation results against the observed probability distribution function (PDF) of λ<SUB>Edd</SUB> found in z ∼ 6 quasars. Then, in the simulation we selected the BHs that satisfy the following criteria: (a) 10 < z < 11, (b) M<SUB>BH</SUB> > 10<SUP>6</SUP> M<SUB>⊙</SUB>. Next, we applied the extreme value statistics to the PDF of λ<SUB>Edd</SUB> resulting from the simulation. <BR /> Results: We find that the probability of observing a z ∼ 10 − 11 MBH accreting with λ<SUB>Edd</SUB> ∼ 5.5 in the volume surveyed by JWST is very low (< 0.2%). We compared our predictions with those in the literature, and discussed the main limitations of our work. <BR /> Conclusions: Our simulation cannot explain the JWST observations of GN-z11. This might be due to: (i) poor resolution and statistics in simulations, (ii) simplistic sub-grid models (e.g. BH accretion and seeding), (iii) uncertainties in the data analysis and interpretation. | en_US |
dc.language.iso | eng | en_US |
dc.title | Is GN-z11 powered by a super-Eddington massive black hole? | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/202449321 | en_US |
dc.identifier.scopus | 2-s2.0-85195684652 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2024/06/aa49321-24/aa49321-24.html | en_US |
dc.identifier.url | http://arxiv.org/abs/2401.13733v2 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 686 | en_US |
dc.relation.firstpage | A141 | 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 | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2024A&A...686A.141B | 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.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.openairetype | Article | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.orcid | 0000-0003-3693-3091 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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bhatt_aa49321-24.pdf | PDF editoriale | 496.4 kB | Adobe PDF | View/Open |
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