Empirical relations defining the growth of supermassive black holes: Implications for the origins of black hole seeds. Aggarwal, Y. arXiv:2112.06338 [astro-ph], December, 2021. arXiv: 2112.06338![Empirical relations defining the growth of supermassive black holes: Implications for the origins of black hole seeds [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We compiled available mass and redshift z data for supermassive black holes (SMBHs) at z \textgreater7.5, ranging in mass over 2 orders of magnitude and in age by nearly 300 million years. The data reveal that a large subset covering the entire age spectrum has markedly similar masses. The most likely implication is that SMBHs within the subset had seeds with similar masses and formed essentially concurrently. Based on this inference, the data of the subset are used derive quantitative empirical relations that provide insights into the origins of black hole seeds and constraints for models of seed formation. The relationships are tested and applied to thousands of SMBHs at nearly all redshifts. The results show that the masses of SMBHs \textgreater a million solar masses are accounted for with seeds formed at or near z=30 and ranging from Sun's mass to about 50-thousand solar masses. Apparently, the seeds grew at an exponentially increasing accretion rate that reached a maximum near z=7 and decreased thereafter. From z=30 to 15, the average accretion rate either exceeded the Eddington limit by a factor of 2 or less, or the radiative efficiency was less than its canonical value of 0.1 and increased thereafter. About half of the growth apparently occurs from z=30 to 3.5 at an average rate of about 614 solar masses per million years per unit solar seed mass, and the rest in the succeeding 12-billion years. The maximum mass that a black hole can accrete is about 2.35-million times the seed mass, and the largest observable black hole should not exceed about 100-billion solar masses. The seed of Sagittarius A* is inferred to have had a mass a few times Sun's mass and may have stopped accreting recently having achieved its maximum growth potential.
@article{aggarwal_empirical_2021,
title = {Empirical relations defining the growth of supermassive black holes: {Implications} for the origins of black hole seeds},
shorttitle = {Empirical relations defining the growth of supermassive black holes},
url = {http://arxiv.org/abs/2112.06338},
abstract = {We compiled available mass and redshift z data for supermassive black holes (SMBHs) at z {\textgreater}7.5, ranging in mass over 2 orders of magnitude and in age by nearly 300 million years. The data reveal that a large subset covering the entire age spectrum has markedly similar masses. The most likely implication is that SMBHs within the subset had seeds with similar masses and formed essentially concurrently. Based on this inference, the data of the subset are used derive quantitative empirical relations that provide insights into the origins of black hole seeds and constraints for models of seed formation. The relationships are tested and applied to thousands of SMBHs at nearly all redshifts. The results show that the masses of SMBHs {\textgreater} a million solar masses are accounted for with seeds formed at or near z=30 and ranging from Sun's mass to about 50-thousand solar masses. Apparently, the seeds grew at an exponentially increasing accretion rate that reached a maximum near z=7 and decreased thereafter. From z=30 to 15, the average accretion rate either exceeded the Eddington limit by a factor of 2 or less, or the radiative efficiency was less than its canonical value of 0.1 and increased thereafter. About half of the growth apparently occurs from z=30 to 3.5 at an average rate of about 614 solar masses per million years per unit solar seed mass, and the rest in the succeeding 12-billion years. The maximum mass that a black hole can accrete is about 2.35-million times the seed mass, and the largest observable black hole should not exceed about 100-billion solar masses. The seed of Sagittarius A* is inferred to have had a mass a few times Sun's mass and may have stopped accreting recently having achieved its maximum growth potential.},
urldate = {2021-12-20},
journal = {arXiv:2112.06338 [astro-ph]},
author = {Aggarwal, Yash},
month = dec,
year = {2021},
note = {arXiv: 2112.06338},
keywords = {Astrophysics - Astrophysics of Galaxies},
}
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Based on this inference, the data of the subset are used derive quantitative empirical relations that provide insights into the origins of black hole seeds and constraints for models of seed formation. The relationships are tested and applied to thousands of SMBHs at nearly all redshifts. The results show that the masses of SMBHs \\textgreater a million solar masses are accounted for with seeds formed at or near z=30 and ranging from Sun's mass to about 50-thousand solar masses. Apparently, the seeds grew at an exponentially increasing accretion rate that reached a maximum near z=7 and decreased thereafter. From z=30 to 15, the average accretion rate either exceeded the Eddington limit by a factor of 2 or less, or the radiative efficiency was less than its canonical value of 0.1 and increased thereafter. About half of the growth apparently occurs from z=30 to 3.5 at an average rate of about 614 solar masses per million years per unit solar seed mass, and the rest in the succeeding 12-billion years. The maximum mass that a black hole can accrete is about 2.35-million times the seed mass, and the largest observable black hole should not exceed about 100-billion solar masses. 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From z=30 to 15, the average accretion rate either exceeded the Eddington limit by a factor of 2 or less, or the radiative efficiency was less than its canonical value of 0.1 and increased thereafter. About half of the growth apparently occurs from z=30 to 3.5 at an average rate of about 614 solar masses per million years per unit solar seed mass, and the rest in the succeeding 12-billion years. The maximum mass that a black hole can accrete is about 2.35-million times the seed mass, and the largest observable black hole should not exceed about 100-billion solar masses. 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