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Journal articles on the topic 'Black hole population'

Author: Grafiati

Published: 26 October 2024

Last updated: 31 July 2025

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1

Nomoto, K., K. Maeda, H. Umeda, and N. Tominaga. "Nucleosynthesis in Population III Supernovae." Highlights of Astronomy 13 (2005): 560–65. http://dx.doi.org/10.1017/s1539299600016580.

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AbstractStars more massive than ~ 20–25 M⊙ form a black hole at the end of their evolution. Stars with non-rotating black holes are likely to collapse ”quietly” ejecting a small amount of heavy elements (Faint supernovae). In contrast, stars with rotating black holes are likely to give rise to very energetic supernovae (Hypernovae). Nucleosynthesis in Hypernovae is characterized by larger abundance ratios (Zn,Co,V,Ti)/Fe and smaller (Mn,Cr)/Fe than normal supernovae, which can explain the observed trend of these ratios in extremely metal-poor stars. Nucleosynthesis in Faint supernovae is chara

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Stevenson, Simon. "Biases in Estimates of Black Hole Kicks from the Spin Distribution of Binary Black Holes." Astrophysical Journal Letters 926, no. 2 (2022): L32. http://dx.doi.org/10.3847/2041-8213/ac5252.

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Abstract A population of more than 50 binary black hole mergers has now been observed by the LIGO and Virgo gravitational-wave observatories. While neutron stars are known to have large velocities associated with impulsive kicks imparted to them at birth in supernovae, whether black holes receive similar kicks, and of what magnitude, remains an open question. Recently, Callister et al. analyzed the binary black hole population under the hypothesis that they were all formed through isolated binary evolution and claimed that large black hole kicks (greater than 260 km s−1 at 99% confidence) were

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Pesce, Dominic W., Daniel C. M. Palumbo, Angelo Ricarte, et al. "Expectations for Horizon-Scale Supermassive Black Hole Population Studies with the ngEHT." Galaxies 10, no. 6 (2022): 109. http://dx.doi.org/10.3390/galaxies10060109.

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We present estimates for the number of supermassive black holes (SMBHs) for which the next-generation Event Horizon Telescope (ngEHT) can identify the black hole “shadow”, along with estimates for how many black hole masses and spins the ngEHT can expect to constrain using measurements of horizon-resolved emission structure. Building on prior theoretical studies of SMBH accretion flows and analyses carried out by the Event Horizon Telescope (EHT) collaboration, we construct a simple geometric model for the polarized emission structure around a black hole, and we associate parameters of this mo

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Callister, Thomas A., Simona J. Miller, Katerina Chatziioannou, and Will M. Farr. "No Evidence that the Majority of Black Holes in Binaries Have Zero Spin." Astrophysical Journal Letters 937, no. 1 (2022): L13. http://dx.doi.org/10.3847/2041-8213/ac847e.

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Abstract The spin properties of merging black holes observed with gravitational waves can offer novel information about the origin of these systems. The magnitudes and orientations of black hole spins offer a record of binaries’ evolutionary history, encoding information about massive stellar evolution and the astrophysical environments in which binary black holes are assembled. Recent analyses of the binary black hole population have yielded conflicting portraits of the black hole spin distribution. Some works suggest that black hole spins are small but nonzero and exhibit a wide range of mis

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Rees, Martin J., and Marta Volonteri. "Massive black holes: formation and evolution." Proceedings of the International Astronomical Union 2, S238 (2006): 51–58. http://dx.doi.org/10.1017/s1743921307004681.

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AbstractSupermassive black holes are nowadays believed to reside in most local galaxies. Observations have revealed us vast information on the population of local and distant black holes, but the detailed physical properties of these dark massive objects are still to be proven. Accretion of gas and black hole mergers play a fundamental role in determining the two parameters defining a black hole: mass and spin. We briefly review here the basic properties of the population of supermassive black holes, focusing on the still mysterious formation of the first massive black holes, and their evoluti

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Bartos, Imre, Bence Kocsis, Zoltán Haiman, and Szabolcs Márka. "Rapid and Bright Stellar-mass Binary Black Hole Mergers in Active Galactic Nuclei." Astrophysical Journal 835, no. 2 (2016): 165. https://doi.org/10.5281/zenodo.437531.

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The Laser Interferometer Gravitational-wave Observatory (LIGO) found direct evidence for double black hole binaries emitting gravitational waves. Galactic nuclei are expected to harbor the densest population of stellar-mass black holes. A significant fraction (&sim; 30 % ) of these black holes can reside in binaries. We examine the fate of the black hole binaries in active galactic nuclei, which get trapped in the inner region of the accretion disk around the central supermassive black hole. We show that binary black holes can migrate into and then rapidly merge within the disk well within a S

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Doctor, Zoheyr, Ben Farr, and Daniel E. Holz. "Black Hole Leftovers: The Remnant Population from Binary Black Hole Mergers." Astrophysical Journal Letters 914, no. 1 (2021): L18. http://dx.doi.org/10.3847/2041-8213/ac0334.

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Reynolds, Christopher S. "Observational Constraints on Black Hole Spin." Annual Review of Astronomy and Astrophysics 59, no. 1 (2021): 117–54. http://dx.doi.org/10.1146/annurev-astro-112420-035022.

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The spin of a black hole is an important quantity to study, providing a window into the processes by which a black hole was born and grew. Furthermore, spin can be a potent energy source for powering relativistic jets and energetic particle acceleration. In this review, I describe the techniques currently used to detect and measure the spins of black holes. It is shown that: ▪ Two well-understood techniques, X-ray reflection spectroscopy and thermal continuum fitting, can be used to measure the spins of black holes that are accreting at moderate rates. There is a rich set of other electromagne

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Treister, Ezequiel, Claudia M. Urry, Kevin Schawinski, Brooke D. Simmons, Priyamvada Natarajan, and Marta Volonteri. "The Multiwavelength AGN Population and the X-ray Background." Proceedings of the International Astronomical Union 9, S304 (2013): 188–94. http://dx.doi.org/10.1017/s1743921314003731.

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AbstractIn order to fully understand galaxy formation we need to know when in the cosmic history are supermassive black holes (SMBHs) growing more intensively, in what type of galaxies this growth is happening and what fraction of these sources are invisible at most wavelengths due to obscuration. Active Galactic Nuclei (AGN) population synthesis models that can explain the spectral shape and intensity of the cosmic X-ray background (CXRB) indicate that most of the SMBH growth occurs in moderate-luminosity (LX~ 1044 erg/s) sources (Seyfert-type AGN), at z~ 0.5−1 and in heavily obscured but Com

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Zevin, Michael, and Daniel E. Holz. "Avoiding a Cluster Catastrophe: Retention Efficiency and the Binary Black Hole Mass Spectrum." Astrophysical Journal Letters 935, no. 1 (2022): L20. http://dx.doi.org/10.3847/2041-8213/ac853d.

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Abstract The population of binary black hole mergers identified through gravitational waves has uncovered unexpected features in the intrinsic properties of black holes in the universe. One particularly surprising and exciting result is the possible existence of black holes in the pair-instability mass gap, ∼50–120 M ⊙. Dense stellar environments can populate this region of mass space through hierarchical mergers, with the retention efficiency of black hole merger products strongly dependent on the escape velocity of the host environment. We use simple toy models to represent hierarchical merg

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Ricarte, Angelo, Fabio Pacucci, Nico Cappelluti, and Priyamvada Natarajan. "The clustering of undetected high-redshift black holes and their signatures in cosmic backgrounds." Monthly Notices of the Royal Astronomical Society 489, no. 1 (2019): 1006–22. http://dx.doi.org/10.1093/mnras/stz1891.

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ABSTRACT There exist hitherto unexplained fluctuations in the cosmic infrared background on arcminute scales and larger. These have been shown to cross-correlate with the cosmic X-ray background, leading several authors to attribute the excess to a high-redshift growing black hole population. In order to investigate potential sources that could explain this excess, in this paper, we develop a new framework to compute the power spectrum of undetected sources that do not have constant flux as a function of halo mass. In this formulation, we combine a semi-analytic model for black hole growth and

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Netzer, Hagai. "Black Hole Demographics: Statistical Characteristics of Accreting Black Holes." Proceedings of the International Astronomical Union 5, S267 (2009): 213–22. http://dx.doi.org/10.1017/s1743921310006319.

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This review summarizes the important properties of active black holes (BHs) up to z ~ 2; their mass, accretion rate, and growth rate. At higher redshifts, such information is only available for small samples that do not represent the entire population of active galactic nuclei (AGNs). Black hole spin is still unknown; it is speculated to change with redshift, but with little experimental evidence. The available data sets also enable a direct comparison of BH accretion rates and host galaxy star-formation rates (SFRs). The ratio of the BH growth rate g(BH) and the bulge growth rate g(bulge), su

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Payne, Ethan, Ling Sun, Kyle Kremer, Paul D. Lasky, and Eric Thrane. "The Imprint of Superradiance on Hierarchical Black Hole Mergers." Astrophysical Journal 931, no. 2 (2022): 79. http://dx.doi.org/10.3847/1538-4357/ac66df.

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Abstract Ultralight bosons are a proposed solution to outstanding problems in cosmology and particle physics: they provide a dark-matter candidate while potentially explaining the strong charge-parity problem. If they exist, ultralight bosons can interact with black holes through the superradiant instability. In this work we explore the consequences of this instability on the evolution of hierarchical black holes within dense stellar clusters. By reducing the spin of individual black holes, superradiance reduces the recoil velocity of merging binary black holes, which, in turn, increases the r

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Haas, J., P. Kroupa, L. Šubr, and M. Singhal. "The star grinder in the Galactic centre." Astronomy & Astrophysics 695 (March 2025): L19. https://doi.org/10.1051/0004-6361/202453324.

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Context. Various past theoretical considerations and observational efforts suggest the presence of a population of stellar-mass black holes in the innermost parsec of the Galactic centre. Aims. In this Letter, we investigate the impact of these black holes on the composition of the embedding stellar population through their direct collisions with the individual stars. Based on the estimated collision rates, we derive an order of magnitude radial density profile of the black hole cluster. Methods. The estimates were obtained analytically, considering various possible formation channels for the

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Broekgaarden, Floor S., Simon Stevenson, and Eric Thrane. "Signatures of Mass Ratio Reversal in Gravitational Waves from Merging Binary Black Holes." Astrophysical Journal 938, no. 1 (2022): 45. http://dx.doi.org/10.3847/1538-4357/ac8879.

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Abstract The spins of merging binary black holes offer insights into their formation history. Recently it has been argued that in the isolated binary evolution of two massive stars the firstborn black hole is slowly rotating, while the progenitor of the second-born black hole can be tidally spun up if the binary is tight enough. Naively, one might therefore expect that only the less massive black hole in merging binaries exhibits nonnegligible spin. However, if the mass ratio of the binary is “reversed” (typically during the first mass transfer episode), it is possible for the tidally spun up

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Hong, Jongsuk, Abbas Askar, Mirek Giersz, Arkadiusz Hypki, and Suk-Jin Yoon. "mocca-survey Database I: Binary black hole mergers from globular clusters with intermediate mass black holes." Monthly Notices of the Royal Astronomical Society 498, no. 3 (2020): 4287–94. http://dx.doi.org/10.1093/mnras/staa2677.

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ABSTRACT The dynamical formation of black hole binaries in globular clusters that merge due to gravitational waves occurs more frequently in higher stellar density. Meanwhile, the probability to form intermediate mass black holes (IMBHs) also increases with the density. To explore the impact of the formation and growth of IMBHs on the population of stellar mass black hole binaries from globular clusters, we analyse the existing large survey of Monte Carlo globular cluster simulation data (mocca-survey Database I). We show that the number of binary black hole mergers agrees with the prediction

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Mezcua, Mar. "Feeding and feedback from little monsters: AGN in dwarf galaxies." Proceedings of the International Astronomical Union 15, S359 (2020): 238–42. http://dx.doi.org/10.1017/s1743921320002240.

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AbstractDetecting the seed black holes from which quasars formed is extremely challenging; however, those seeds that did not grow into supermassive should be found as intermediate-mass black holes (IMBHs) of 100 – 105 M⊙ in local dwarf galaxies. The use of deep multiwavelength surveys has revealed that a population of actively accreting IMBHs (low-mass AGN) exists in dwarf galaxies at least out to z ˜3. The black hole occupation fraction of these galaxies suggests that the early Universe seed black holes formed from direct collapse of gas, which is reinforced by the possible flattening of the

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Fryer, C. L. "Population Synthesis of GRB Progenitors: Problems With Kicks." Symposium - International Astronomical Union 195 (2000): 339–46. http://dx.doi.org/10.1017/s0074180900163119.

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Accretion disks around stellar-mass black holes are now thought to be the engines which power classical gamma-ray bursts (GRBs). These disks are formed almost exclusively in binaries, and to study the characteristics of the progenitors of these black-hole accretion disk (BHAD) GRBs, we must understand the uncertainties in binary population synthesis calculations. Kicks imparted onto nascent neutron stars and black holes are among the most misunderstood concepts of binary population synthesis. In this paper, we outline the current understanding (or lack of understanding) of these kicks and disc

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Thomas, Nicole, Romeel Davé, Matt J. Jarvis, and Daniel Anglés-Alcázar. "The radio galaxy population in the simba simulations." Monthly Notices of the Royal Astronomical Society 503, no. 3 (2021): 3492–509. http://dx.doi.org/10.1093/mnras/stab654.

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ABSTRACT We examine the 1.4 GHz radio luminosities of galaxies arising from star formation and active galactic nuclei (AGNs) within the state-of-the-art cosmological hydrodynamic simulation Simba. Simba grows black holes via gravitational torque limited accretion from cold gas and Bondi accretion from hot gas, and employs AGN feedback including jets at low Eddington ratios. We define a population of radio loud AGNs (RLAGNs) based on the presence of ongoing jet feedback. Within RLAGN, we define high and low excitation radio galaxies (HERGs and LERGs) based on their dominant mode of black hole a

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Mukherjee, Suvodip, and Joseph Silk. "Can we distinguish astrophysical from primordial black holes via the stochastic gravitational wave background?" Monthly Notices of the Royal Astronomical Society 506, no. 3 (2021): 3977–85. http://dx.doi.org/10.1093/mnras/stab1932.

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ABSTRACT One of the crucial windows for distinguishing astrophysical black holes from primordial black holes is through the redshift evolution of their respective merger rates. The low redshift population of black holes of astrophysical origin is expected to follow the star formation rate. The corresponding peak in their merger rate peaks at a redshift smaller than that of the star formation rate peak (zp ≈ 2), depending on the time delay between the formation and mergers of black holes. Black holes of primordial origin are going to be present before the formation of the stars, and the merger

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Häberle, Maximilian, Nadine Neumayer, Anil Seth та ін. "Fast-moving stars around an intermediate-mass black hole in ω Centauri". Nature 631, № 8020 (2024): 285–88. http://dx.doi.org/10.1038/s41586-024-07511-z.

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AbstractBlack holes have been found over a wide range of masses, from stellar remnants with masses of 5–150 solar masses (M☉), to those found at the centres of galaxies with M > 105M☉. However, only a few debated candidate black holes exist between 150M☉ and 105M☉. Determining the population of these intermediate-mass black holes is an important step towards understanding supermassive black hole formation in the early universe1,2. Several studies have claimed the detection of a central black hole in ω Centauri, the most massive globular cluster of the Milky Way3–5. However, these studies ha

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Zhou, Shuying, Mouyuan Sun, Tong Liu, Jian-Min Wang, Jun-Xian Wang, and Yongquan Xue. "Stellar Black Holes Can “Stretch” Supermassive Black Hole Accretion Disks." Astrophysical Journal Letters 966, no. 1 (2024): L9. http://dx.doi.org/10.3847/2041-8213/ad3c3f.

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Abstract Stellar black holes (sBHs) are widely believed to exist in the accretion disks of active galactic nuclei (AGNs). Previous studies often focus on the transient emission produced by embedded sBHs. Here, we explore the possible observational consequences of an AGN accretion disk that contains a population of accreting sBHs. Embedded accreting sBHs change the effective temperature distribution of the AGN accretion disk by heating gas in the outer regions. Two possible observational consequences are presented. First, the spectral energy distribution has a turnover feature at ∼4700 Å when t

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Fusco, Michael S., Benjamin L. Davis, Julia Kennefick, Daniel Kennefick, and Marc S. Seigar. "Probing the Low-Mass End of the Black Hole Mass Function via a Study of Faint Local Spiral Galaxies." Universe 8, no. 12 (2022): 649. http://dx.doi.org/10.3390/universe8120649.

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We present an analysis of the pitch angle distribution function (PADF) for nearby galaxies and its resulting black hole mass function (BHMF) via the well-known relationship between pitch angle and black hole mass. Our sample consists of a subset of 74 spiral galaxies from the Carnegie-Irvine Galaxy Survey with absolute B-band magnitude MB>−19.12 mag and luminosity distance DL≤25.4 Mpc, which is an extension of a complementary set of 140 more luminous (MB≤−19.12 mag) late-type galaxies. We find the PADFs of the two samples are, somewhat surprisingly, not strongly dissimilar; a result that ma

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Ellis, Sebastian A. R. "Premature black hole death of Population III stars by dark matter." Journal of Cosmology and Astroparticle Physics 2022, no. 05 (2022): 025. http://dx.doi.org/10.1088/1475-7516/2022/05/025.

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Abstract Population III stars were the first generation of stars, formed in minihalos of roughly primordial element abundances, and therefore metal-free. They are thought to have formed at the cores of dense dark matter clouds. Interactions between baryons and dark matter can therefore have had an important impact on their evolution. In this paper we consider the capture of non- or weakly-annihilating dark matter by these early massive stars. In a wide region of parameter space, interactions of dark matter with baryons lead to premature death of the star as a black hole. We sketch how this mod

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Casares, Jorge. "Observational evidence for stellar-mass black holes." Proceedings of the International Astronomical Union 2, S238 (2006): 3–12. http://dx.doi.org/10.1017/s1743921307004590.

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AbstractRadial velocity studies of X-ray binaries provide the most solid evidence for the existence of stellar-mass black holes. We currently have 20 confirmed cases, with dynamical masses in excess of 3 M⊙. Accurate masses have been obtained for a subset of systems which gives us a hint at the mass spectrum of the black hole population. This review summarizes the history of black hole discoveries and presents the latest results in the field.

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Kauffmann, Guinevere, and Timothy M. Heckman. "The formation of bulges and black holes: lessons from a census of active galaxies in the SDSS." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 363, no. 1828 (2005): 621–43. http://dx.doi.org/10.1098/rsta.2004.1516.

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We examine the relationship between galaxies, supermassive black holes and AGN using a sample of 23 000 narrow–emission–line (‘type 2’) active galactic nuclei (AGN) drawn from a sample of 123 000 galaxies from the Sloan Digital Sky Survey. We have studied how AGN host properties compare with those of normal galaxies and how they depend on the luminosity of the active nucleus. We find that AGN reside in massive galaxies and have distributions of sizes and concentrations that are similar to those of the early–type galaxies in our sample. The host galaxies of low–luminosity AGN have stellar popul

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Gallegos-Garcia, Monica, Christopher P. L. Berry, Pablo Marchant, and Vicky Kalogera. "Binary Black Hole Formation with Detailed Modeling: Stable Mass Transfer Leads to Lower Merger Rates." Astrophysical Journal 922, no. 2 (2021): 110. http://dx.doi.org/10.3847/1538-4357/ac2610.

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Abstract Rapid binary population synthesis codes are often used to investigate the evolution of compact-object binaries. They typically rely on analytical fits of single-star evolutionary tracks and parameterized models for interactive phases of evolution (e.g., mass transfer on a thermal timescale, determination of dynamical instability, and common envelope) that are crucial to predict the fate of binaries. These processes can be more carefully implemented in stellar structure and evolution codes such as MESA. To assess the impact of such improvements, we compare binary black hole mergers as

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Nitta, S. "Statistical Properties of Kerr BH Flywheel Model of QSOs/AGNs." Symposium - International Astronomical Union 195 (2000): 417–18. http://dx.doi.org/10.1017/s0074180900163351.

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The aim of this work is to demonstrate the properties of the magnetospheric model around Kerr black holes, so-called the “flywheel” (rotation powered) model. The fly-wheel engine of the BH accretion disk system is applied to the statistics of QSOs/AGNs. Nitta, Takahashi, & Tomimatsu clarified the individual evolution of the Kerr black-hole fly-wheel engine, which is parameterized by black-hole mass, initial Kerr parameter, magnetic field near the horizon, and a dimensionless small parameter. We impose a statistical model for the initial mass function of an ensemble of black holes using the

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Edelman, Bruce, Zoheyr Doctor, and Ben Farr. "Poking Holes: Looking for Gaps in LIGO/Virgo’s Black Hole Population." Astrophysical Journal Letters 913, no. 2 (2021): L23. http://dx.doi.org/10.3847/2041-8213/abfdb3.

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Sadler, Elaine M., Scott M. Croom, John H. Y. Ching, Helen M. Johnston, Russell D. Cannon, and Tom Mauch. "Radio-Mode Feedback in Massive Galaxies at Redshift 0 < z < 1." Proceedings of the International Astronomical Union 5, S267 (2009): 377–82. http://dx.doi.org/10.1017/s1743921310006745.

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AbstractWe have carried out a large observational study of the radio luminosities, stellar populations, and environments of massive galaxies over the redshift range 0 < z < 1. Radio jets powered by an accreting central black hole are common in massive galaxies, and there is a large class of “optically quiet AGN,” with radio emission but no optical/IR signature of black-hole accretion. The central black holes in these galaxies are probably accreting in a radiatively inefficient mode, and our results suggest that “radio-mode feedback” as described by Croton et al. is likely to occur in all

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Shojaie, H., and M. Farhoudi. "Black holes in the varying speed of light theory." Canadian Journal of Physics 85, no. 12 (2007): 1409–15. http://dx.doi.org/10.1139/p07-131.

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We consider the effect of the varying speed of light theory on nonrotating black holes. We show that in any varying-c theory, the Schwarzschild solution is neither static nor stationary. For a no-charged black hole, the singularity in the Schwarzschild horizon cannot be removed by coordinate transformation. Hence, no matter can enter the horizon, and the interior part of the black hole is separated from the rest of the Universe. If ċ < 0, then the size of the Schwarzschild radius increases with time. The higher value of the speed of light in the very early Universe may have caused a large r

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Mummery, Andrew, and Steven A. Balbus. "An upper observable black hole mass scale for tidal destruction events with thermal X-ray spectra." Monthly Notices of the Royal Astronomical Society 505, no. 2 (2021): 1629–44. http://dx.doi.org/10.1093/mnras/stab1141.

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ABSTRACT We comprehensively model the X-ray luminosity emergent from time-dependent relativistic accretion discs, developing analytical models of the X-ray luminosity of thermal disc systems as a function of black hole mass M, disc mass Md, and disc α-parameter. The X-ray properties of these solutions will be directly relevant for understanding tidal disruption event (TDE) observations. We demonstrate an extremely strong suppression of thermal X-ray luminosity from large mass black holes, LX ∼ exp (− m7/6), where m is a dimensionless mass, roughly the black hole mass in unity of 106M⊙. This st

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Ng, Ken K. Y., Gabriele Franciolini, Emanuele Berti, Paolo Pani, Antonio Riotto, and Salvatore Vitale. "Constraining High-redshift Stellar-mass Primordial Black Holes with Next-generation Ground-based Gravitational-wave Detectors." Astrophysical Journal Letters 933, no. 2 (2022): L41. http://dx.doi.org/10.3847/2041-8213/ac7aae.

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Abstract The possible existence of primordial black holes in the stellar-mass window has received considerable attention because their mergers may contribute to current and future gravitational-wave detections. Primordial black hole mergers, together with mergers of black holes originating from Population III stars, are expected to dominate at high redshifts (z ≳ 10). However, the primordial black hole merger rate density is expected to rise monotonically with redshift, while Population III mergers can only occur after the birth of the first stars. Next-generation gravitational-wave detectors

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Mummery, Andrew. "A maximum X-ray luminosity scale of disc-dominated tidal destruction events." Monthly Notices of the Royal Astronomical Society 504, no. 4 (2021): 5144–54. http://dx.doi.org/10.1093/mnras/stab1187.

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ABSTRACT We develop a model describing the dynamical and observed properties of disc-dominated tidal disruption events (TDEs) around black holes with the lowest masses (M ≲ few × 106M⊙). TDEs around black holes with the lowest masses are most likely to reach super-Eddington luminosities at early times in their evolution. By assuming that the amount of stellar debris that can form into a compact accretion disc is set dynamically by the Eddington luminosity, we make a number of interesting and testable predictions about the observed properties of bright soft-state X-ray TDEs and optically bright

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Postnov, Konstantin, and Alexander Kuranov. "Progenitors of binary black hole mergers detected by LIGO." Proceedings of the International Astronomical Union 12, S329 (2016): 118–25. http://dx.doi.org/10.1017/s1743921317002964.

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AbstractPossible formation mechanisms of massive close binary black holes that can merge in the Hubble time to produce powerful gravitational wave bursts detected during advanced LIGO O1 science run are briefly discussed. The pathways include the evolution from field low-metallicity massive binaries, the dynamical formation in globular clusters and primordial black holes. Low effective black hole spins inferred for LIGO GW150914 and LTV151012 events are discussed. Population synthesis calculations of the expected spin and chirp mass distributions from the standard field massive binary formatio

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Nitz, Alexander H., Collin D. Capano, Sumit Kumar, et al. "3-OGC: Catalog of Gravitational Waves from Compact-binary Mergers." Astrophysical Journal 922, no. 1 (2021): 76. http://dx.doi.org/10.3847/1538-4357/ac1c03.

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Abstract We present the third open gravitational-wave catalog (3-OGC) of compact-binary coalescences, based on the analysis of the public LIGO and Virgo data from 2015 through 2019 (O1, O2, O3a). Our updated catalog includes a population of 57 observations, including 4 binary black hole mergers that had not been previously reported. This consists of 55 binary black hole mergers and the 2 binary neutron star mergers, GW170817 and GW190425. We find no additional significant binary neutron star or neutron star–black hole merger events. The most confident new detection is the binary black hole mer

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Golomb, Jacob, Maximiliano Isi, and Will M. Farr. "Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources." Astrophysical Journal 976, no. 1 (2024): 121. http://dx.doi.org/10.3847/1538-4357/ad8572.

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Abstract Gravitational-wave observations of binary black holes have revealed unexpected structure in the black hole mass distribution. Previous studies employ physically motivated phenomenological models and infer the parameters that control the features of the mass distribution that are allowed in their model, associating the constraints on those parameters with their physical motivations a posteriori. In this work, we take an alternative approach in which we introduce a model parameterizing the underlying stellar and core-collapse physics and obtaining the remnant black hole distribution as

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Wong, Thomas Hong Tsun, Hugo Pfister, and Lixin Dai. "Revisiting the Rates and Demographics of Tidal Disruption Events: Effects of the Disk Formation Efficiency." Astrophysical Journal Letters 927, no. 1 (2022): L19. http://dx.doi.org/10.3847/2041-8213/ac5823.

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Abstract Tidal disruption events (TDEs) are valuable probes of the demographics of supermassive black holes as well as the dynamics and population of stars in the centers of galaxies. In this Letter, we focus on studying how debris disk formation and circularization processes can impact the possibility of observing prompt flares in TDEs. First, we investigate how the efficiency of disk formation is determined by the key parameters, namely, the black hole mass M BH, the stellar mass m ⋆, and the orbital penetration parameter β that quantifies how close the disrupted star would orbit around the

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Shao, Yong, and Xiang-Dong Li. "Population Synthesis of Black Hole X-Ray Binaries." Astrophysical Journal 898, no. 2 (2020): 143. http://dx.doi.org/10.3847/1538-4357/aba118.

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Tiwari, Vaibhav. "Exploring Features in the Binary Black Hole Population." Astrophysical Journal 928, no. 2 (2022): 155. http://dx.doi.org/10.3847/1538-4357/ac589a.

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Abstract Vamana is a mixture model framework that infers the astrophysical distribution of chirp mass, mass ratio, and spin component aligned with the orbital angular momentum for the binary black holes (BBH) population. We extend the mixing components in this framework to also model the redshift evolution of merger rate and report all the major one- and two-dimensional features in the BBH population using the 69 gravitational-wave signals detected with a false alarm rate <1 yr−1 in the third Gravitational-Wave Transient Catalog (GWTC-3). Endorsing our previous report and a recent corrobora

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Dolgov, A., and K. Postnov. "Globular cluster seeding by primordial black hole population." Journal of Cosmology and Astroparticle Physics 2017, no. 04 (2017): 036. http://dx.doi.org/10.1088/1475-7516/2017/04/036.

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Ohsuga, Ken, Hajime Susa, and Yosuke Uchiyama. "Instability of Population III Black Hole Accretion Disks." Publications of the Astronomical Society of Japan 59, no. 6 (2007): 1235–41. http://dx.doi.org/10.1093/pasj/59.6.1235.

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Ziółkowski, Janusz, and Krzysztof Belczyński. "On the apparent lack of Be X-ray binaries with black holes in the galaxy and in the Magellanic Clouds." Proceedings of the International Astronomical Union 6, S275 (2010): 329–30. http://dx.doi.org/10.1017/s1743921310016340.

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AbstractIn the Galaxy there are 67 Be X-ray binaries known to-date. Out of those, 45 host a neutron star, and for the reminder the nature of a companion is not known. None, so far, is known to host a black hole. This disparity is referred to as a missing Be – black hole X-ray binary problem. The stellar population synthesis calculations following the formation of Be X-ray binaries (Belczyński & Ziółkowski 2009) predict that the ratio of the binaries with neutron stars to the ones with black holes is rather high FNS/BH ~ 30–50. A comparison of this ratio with the number of confirmed Be – ne

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Porras-Valverde, Antonio J., and John C. Forbes. "On the Signature of Black Holes on the Quenched Stellar Mass Function." Astrophysical Journal 984, no. 2 (2025): 96. https://doi.org/10.3847/1538-4357/adcc2d.

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Abstract As star-forming galaxies approach or exceed a stellar mass of around 1011 M ⊙, they are increasingly likely to be quenched in a process generically called mass quenching. Central galaxies, which are quenched via mass rather than environmental quenching, therefore accumulate in a peak around this characteristic mass. While a number of processes may influence the shape of the quenched central stellar mass function, we find that its low-mass slope is strongly affected by the scatter in the mass of black holes at a given stellar mass, with higher scatters in the black hole population yiel

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Chen, Nianyi, Yueying Ni, Michael Tremmel, et al. "Dynamical friction modelling of massive black holes in cosmological simulations and effects on merger rate predictions." Monthly Notices of the Royal Astronomical Society 510, no. 1 (2021): 531–50. http://dx.doi.org/10.1093/mnras/stab3411.

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ABSTRACT In this work, we establish and test methods for implementing dynamical friction (DF) for massive black hole pairs that form in large volume cosmological hydrodynamical simulations that include galaxy formation and black hole growth. We verify our models and parameters both for individual black hole dynamics and for the black hole population in cosmological volumes. Using our model of DF from collisionless particles, black holes can effectively sink close to the galaxy centre, provided that the black hole’s dynamical mass is at least twice that of the lowest mass resolution particles i

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Davis, Benjamin L., and Zehao 泽灏 Jin 金. "Discovery of a Planar Black Hole Mass Scaling Relation for Spiral Galaxies." Astrophysical Journal Letters 956, no. 1 (2023): L22. http://dx.doi.org/10.3847/2041-8213/acfa98.

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Abstract Supermassive black holes (SMBHs) are tiny in comparison to the galaxies they inhabit, yet they manage to influence and coevolve along with their hosts. Evidence of this mutual development is observed in the structure and dynamics of galaxies and their correlations with black hole mass (M •). For our study, we focus on relative parameters that are unique to only disk galaxies. As such, we quantify the structure of spiral galaxies via their logarithmic spiral-arm pitch angles (ϕ) and their dynamics through the maximum rotational velocities of their galactic disks (v max). In the past, w

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Greene, Jenny E., and Luis C. Ho. "Local active black hole mass functions." Proceedings of the International Astronomical Union 2, S238 (2006): 87–90. http://dx.doi.org/10.1017/s1743921307004747.

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AbstractWhile black holes (BHs) are apparently a ubiquitous component of the nuclei of local spheroids, their role in galaxy evolution remains largely unknown. The tight correlations between galaxy spheroid properties and BH mass provide an important boundary condition for models of the coevolution of BHs and galaxies. Here we consider another important boundary condition: the local mass function of broad-line active galaxies. We use standard virial mass estimation techniques to examine the distribution of BH masses and accretion rates for active galaxies in the local universe, and we also com

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Bavera, Simone S., Tassos Fragos, Michael Zevin, et al. "The impact of mass-transfer physics on the observable properties of field binary black hole populations." Astronomy & Astrophysics 647 (March 2021): A153. http://dx.doi.org/10.1051/0004-6361/202039804.

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We study the impact of mass-transfer physics on the observable properties of binary black hole populations that formed through isolated binary evolution. We used the POSYDON framework to combine detailed MESA binary simulations with the COSMIC population synthesis tool to obtain an accurate estimate of merging binary black hole observables with a specific focus on the spins of the black holes. We investigate the impact of mass-accretion efficiency onto compact objects and common-envelope efficiency on the observed distributions of the effective inspiral spin parameter χeff, chirp mass Mchirp,

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Baron, Dalya. "Probing black hole - host galaxy scaling relations with obscured type II AGN." Proceedings of the International Astronomical Union 15, S356 (2019): 365. http://dx.doi.org/10.1017/s1743921320003373.

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AbstractThe scaling relations between supermassive black holes and their host galaxy properties are of fundamental importance in the context black hole-host galaxy co-evolution throughout cosmic time. Beyond the local universe, such relations are based on black hole mass estimates in type I AGN. Unfortunately, for this type of objects the host galaxy properties are more difficult to obtain since the AGN dominates the observed flux in most wavelength ranges. In this poster I will present a new correlation we discovered between the narrow L([OIII])/L(Hβ) line ratio and the FWHM(broad Hα). This s

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Langer, N., C. Schürmann, K. Stoll, et al. "Properties of OB star−black hole systems derived from detailed binary evolution models." Astronomy & Astrophysics 638 (June 2020): A39. http://dx.doi.org/10.1051/0004-6361/201937375.

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Context. The recent gravitational wave measurements have demonstrated the existence of stellar mass black hole binaries. It is essential for our understanding of massive star evolution to identify the contribution of binary evolution to the formation of double black holes. Aims. A promising way to progress is investigating the progenitors of double black hole systems and comparing predictions with local massive star samples, such as the population in 30 Doradus in the Large Magellanic Cloud (LMC). Methods. With this purpose in mind, we analysed a large grid of detailed binary evolution models

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