The high energy X-ray probe (HEX-P): constraining supermassive black hole growth with population spin measurements

J. M. Piotrowska; J. A. García; D. J. Walton; R. S. Beckmann; D. Stern; D. R. Ballantyne; D. R. Wilkins; S. Bianchi; P. G. Boorman; J. Buchner; C.-T. Chen; P. Coppi; T. Dauser; A.C. Fabian; E. Kammoun; K. Madsen; L. Mallick; G. Matt; G. Matzeu; E. Nardini; A. Pizzetti; S. Puccetti; C. Ricci; F. Tombesi; N. Torres-Albà; K.-W. Wong

doi:10.3389/fspas.2024.1324796

The high energy X-ray probe (HEX-P): constraining supermassive black hole growth with population spin measurements

J. M. Piotrowska, J. A. García, D. J. Walton, R. S. Beckmann, D. Stern, D. R. Ballantyne, D. R. Wilkins, S. Bianchi, P. G. Boorman, J. Buchner, C.-T. Chen, P. Coppi, T. Dauser, A.C. Fabian, E. Kammoun, K. Madsen, L. Mallick, G. Matt, G. Matzeu, E. NardiniA. Pizzetti, S. Puccetti, C. Ricci, F. Tombesi, N. Torres-Albà, K.-W. Wong

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Abstract

Constraining the primary growth channel of supermassive black holes (SMBHs) remains one the most actively debated questions in the context of cosmological structure formation. Owing to the expected connection between SMBH spin parameter evolution and the accretion and merger history of individual black holes, population spin measurements offer a rare observational window into the cosmic growth of SMBHs. As of today, the most common method for estimating SMBH spin relies on modeling the relativistically broaden atomic profiles in the reflection spectrum observed in X-rays. In this paper, we study the observational requirements needed to confidently distinguish between the primary SMBH growth channels based on their distinct spin-mass distributions predicted by the Horizon-AGN cosmological simulation. Indoing so, we characterize outstanding limitations associated with the existing measurements and discuss the landscape of future observational campaigns which could be planned and executed with future X-ray observatories. We focus our attention on the High-Energy X-ray Probe (HEX-P), a proposed probe-class mission designed to serve the high-energy community in the 2030s.

Original language	English
Article number	1324796
Pages (from-to)	1-23
Number of pages	23
Journal	Frontiers in Astronomy and Space Sciences
Volume	11
Early online date	28 Mar 2024
DOIs	https://doi.org/10.3389/fspas.2024.1324796
Publication status	E-pub ahead of print - 28 Mar 2024

Keywords

future X-ray observatories
black hole growth
AGN
supermassive black holes
black hole spin

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© 2024 The Author(s). This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/
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Piotrowska, J. M., García, J. A., Walton, D. J., Beckmann, R. S., Stern, D., Ballantyne, D. R., Wilkins, D. R., Bianchi, S., Boorman, P. G., Buchner, J., Chen, C.-T., Coppi, P., Dauser, T., Fabian, A. C., Kammoun, E., Madsen, K., Mallick, L., Matt, G., Matzeu, G., ... Wong, K.-W. (2024). The high energy X-ray probe (HEX-P): constraining supermassive black hole growth with population spin measurements. Frontiers in Astronomy and Space Sciences, 11, 1-23. Article 1324796. Advance online publication. https://doi.org/10.3389/fspas.2024.1324796

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title = "The high energy X-ray probe (HEX-P): constraining supermassive black hole growth with population spin measurements",

abstract = "Constraining the primary growth channel of supermassive black holes (SMBHs) remains one the most actively debated questions in the context of cosmological structure formation. Owing to the expected connection between SMBH spin parameter evolution and the accretion and merger history of individual black holes, population spin measurements offer a rare observational window into the cosmic growth of SMBHs. As of today, the most common method for estimating SMBH spin relies on modeling the relativistically broaden atomic profiles in the reflection spectrum observed in X-rays. In this paper, we study the observational requirements needed to confidently distinguish between the primary SMBH growth channels based on their distinct spin-mass distributions predicted by the Horizon-AGN cosmological simulation. Indoing so, we characterize outstanding limitations associated with the existing measurements and discuss the landscape of future observational campaigns which could be planned and executed with future X-ray observatories. We focus our attention on the High-Energy X-ray Probe (HEX-P), a proposed probe-class mission designed to serve the high-energy community in the 2030s.",

keywords = "future X-ray observatories, black hole growth, AGN, supermassive black holes, black hole spin",

author = "Piotrowska, {J. M.} and Garc{\'i}a, {J. A.} and Walton, {D. J.} and Beckmann, {R. S.} and D. Stern and Ballantyne, {D. R.} and Wilkins, {D. R.} and S. Bianchi and Boorman, {P. G.} and J. Buchner and C.-T. Chen and P. Coppi and T. Dauser and A.C. Fabian and E. Kammoun and K. Madsen and L. Mallick and G. Matt and G. Matzeu and E. Nardini and A. Pizzetti and S. Puccetti and C. Ricci and F. Tombesi and N. Torres-Alb{\`a} and K.-W. Wong",

note = "{\textcopyright} 2024 The Author(s). This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/",

year = "2024",

month = mar,

day = "28",

doi = "10.3389/fspas.2024.1324796",

language = "English",

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Piotrowska, JM, García, JA, Walton, DJ, Beckmann, RS, Stern, D, Ballantyne, DR, Wilkins, DR, Bianchi, S, Boorman, PG, Buchner, J, Chen, C-T, Coppi, P, Dauser, T, Fabian, AC, Kammoun, E, Madsen, K, Mallick, L, Matt, G, Matzeu, G, Nardini, E, Pizzetti, A, Puccetti, S, Ricci, C, Tombesi, F, Torres-Albà, N & Wong, K-W 2024, 'The high energy X-ray probe (HEX-P): constraining supermassive black hole growth with population spin measurements', Frontiers in Astronomy and Space Sciences, vol. 11, 1324796, pp. 1-23. https://doi.org/10.3389/fspas.2024.1324796

TY - JOUR

T1 - The high energy X-ray probe (HEX-P): constraining supermassive black hole growth with population spin measurements

AU - Piotrowska, J. M.

AU - García, J. A.

AU - Walton, D. J.

AU - Beckmann, R. S.

AU - Stern, D.

AU - Ballantyne, D. R.

AU - Wilkins, D. R.

AU - Bianchi, S.

AU - Boorman, P. G.

AU - Buchner, J.

AU - Chen, C.-T.

AU - Coppi, P.

AU - Dauser, T.

AU - Fabian, A.C.

AU - Kammoun, E.

AU - Madsen, K.

AU - Mallick, L.

AU - Matt, G.

AU - Matzeu, G.

AU - Nardini, E.

AU - Pizzetti, A.

AU - Puccetti, S.

AU - Ricci, C.

AU - Tombesi, F.

AU - Torres-Albà, N.

AU - Wong, K.-W.

PY - 2024/3/28

Y1 - 2024/3/28

N2 - Constraining the primary growth channel of supermassive black holes (SMBHs) remains one the most actively debated questions in the context of cosmological structure formation. Owing to the expected connection between SMBH spin parameter evolution and the accretion and merger history of individual black holes, population spin measurements offer a rare observational window into the cosmic growth of SMBHs. As of today, the most common method for estimating SMBH spin relies on modeling the relativistically broaden atomic profiles in the reflection spectrum observed in X-rays. In this paper, we study the observational requirements needed to confidently distinguish between the primary SMBH growth channels based on their distinct spin-mass distributions predicted by the Horizon-AGN cosmological simulation. Indoing so, we characterize outstanding limitations associated with the existing measurements and discuss the landscape of future observational campaigns which could be planned and executed with future X-ray observatories. We focus our attention on the High-Energy X-ray Probe (HEX-P), a proposed probe-class mission designed to serve the high-energy community in the 2030s.

AB - Constraining the primary growth channel of supermassive black holes (SMBHs) remains one the most actively debated questions in the context of cosmological structure formation. Owing to the expected connection between SMBH spin parameter evolution and the accretion and merger history of individual black holes, population spin measurements offer a rare observational window into the cosmic growth of SMBHs. As of today, the most common method for estimating SMBH spin relies on modeling the relativistically broaden atomic profiles in the reflection spectrum observed in X-rays. In this paper, we study the observational requirements needed to confidently distinguish between the primary SMBH growth channels based on their distinct spin-mass distributions predicted by the Horizon-AGN cosmological simulation. Indoing so, we characterize outstanding limitations associated with the existing measurements and discuss the landscape of future observational campaigns which could be planned and executed with future X-ray observatories. We focus our attention on the High-Energy X-ray Probe (HEX-P), a proposed probe-class mission designed to serve the high-energy community in the 2030s.

KW - future X-ray observatories

KW - black hole growth

KW - AGN

KW - supermassive black holes

KW - black hole spin

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DO - 10.3389/fspas.2024.1324796

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JO - Frontiers in Astronomy and Space Sciences

JF - Frontiers in Astronomy and Space Sciences

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The high energy X-ray probe (HEX-P): constraining supermassive black hole growth with population spin measurements

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