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http://hdl.handle.net/20.500.12386/29476
Title: | Chasing the observational signatures of seed black holes at z > 7: candidate statistics | Authors: | VALIANTE, ROSA SCHNEIDER, RAFFAELLA GRAZIANI, Luca ZAPPACOSTA, Luca |
Issue Date: | 2018 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Number: | 474 | Issue: | 3 | First Page: | 3825 | 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. | URI: | http://hdl.handle.net/20.500.12386/29476 | URL: | https://academic.oup.com/mnras/article/474/3/3825/4655201 | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stx3028 | Bibcode ADS: | 2018MNRAS.474.3825V | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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stx3028.pdf | pdf editoriale | 724.49 kB | Adobe PDF | View/Open |
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