Constraints on the Cosmological Coupling of Black Holes from the Globular Cluster NGC 3201

Rodriguez, Carl L.

doi:10.3847/2041-8213/acc9b6

Cited by 14 publications

(8 citation statements)

References 80 publications

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“…Conventional assumptions about SMBH accretion, combined with estimates of the local SMBH mass density based on the M • -M bulge relation, imply an allowed range of  <k 0 2 (Figure 2). This range is in slight tension (∼90% confidence interval) with the results in Farrah et al (2023a), though it is consistent with some of the recent constraints discussed in Section 1.2 (e.g., Rodriguez 2023;Andrae & El-Badry 2023;Ghodla et al 2023;Lei et al 2024).…”

Section: Discussionsupporting

confidence: 90%

“…For stellar mass BHs, Gao & Li (2023) argue that cosmological coupling of BHs can explain the distribution of compact object masses in low mass X-ray binaries, in particular the "mass gap" between the highest-mass neutron stars and lowest-mass BHs. However, Rodriguez (2023) disfavor coupling based on observations of a BH binary in the globular cluster NGC 3201 and Andrae & El-Badry (2023) argue that two BH binaries found by Gaia are likely to have formed with BH masses that were too small if k = 3. 4 Also, Ghodla et al (2023) argue that k = 3 would result in too many BH mergers compared to observations from gravitational-wave detectors.…”

Section: Cosmologically Coupled Black Holesmentioning

confidence: 99%

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Constraints on Cosmological Coupling from the Accretion History of Supermassive Black Holes

Lacy,

Engholm,

Farrah

et al. 2024

ApJL

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Coupling of black hole mass to the cosmic expansion has been suggested as a possible path to understanding the dark energy content of the Universe. We test this hypothesis by comparing the supermassive black hole (SMBH) mass density at z = 0 to the total mass accreted in active galactic nuclei (AGN) since z = 6, to constrain how much of the SMBH mass density can arise from cosmologically coupled growth, as opposed to growth by accretion. Using an estimate of the local SMBH mass density of ≈1.0 × 106 M ⊙ Mpc−1, a radiative accretion efficiency, η, in the range 0.05 < η < 0.3, and the observed AGN luminosity density at z ≈ 4, we constrain the value of the coupling constant between the scale size of the Universe and the black hole mass, k, to lie in the range 0 < k ≲ 2, below the value of k = 3 needed for black holes to be the source term for dark energy. Initial estimates of the gravitational-wave background (GWB) using pulsar timing arrays, however, favor a higher SMBH mass density at z = 0. We show that if we adopt such a mass density at z = 0 of ≈7.4 × 106 M ⊙ Mpc−1, this makes k = 3 viable even for low radiative efficiencies, and may exclude nonzero cosmological coupling. We conclude that, although current estimates of the SMBH mass density based on the black hole mass–bulge mass relation probably exclude k = 3, the possibility remains open that, if the GWB is due to SMBH mergers, k > 2 is preferred.

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Section: Discussionsupporting

confidence: 90%

Section: Cosmologically Coupled Black Holesmentioning

confidence: 99%

Constraints on Cosmological Coupling from the Accretion History of Supermassive Black Holes

Lacy,

Engholm,

Farrah

et al. 2024

ApJL

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“…The initial low-mass BHs grew with the expansion of the Universe, resulting in a contraction of the orbit while conserving the eccentricity imparted by the supernova kick. Rodriguez (2023) argued that if k = 3, two BH candidates in the globular cluster NGC 3201 (Giesers et al 2018(Giesers et al , 2019 must have near face-on orientations or have formed from stellar collapse with NS-like masses (<2.2 M e ). While the latter is not impossible, the cosmologically coupled mass growth may shift low-mass BHs to be more massive and leave the mass gap.…”

Section: Discussionmentioning

confidence: 99%

Can Cosmologically Coupled Mass Growth of Black Holes Solve the Mass Gap Problem?

Gao,

2023

ApJ

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Observations of elliptical galaxies suggest that black holes (BHs) might serve as dark energy candidates, coupled to the expansion of the Universe. According to this hypothesis, the mass of a BH could increase as the Universe expands. BH low-mass X-ray binaries (LMXBs) in the Galactic disk were born several gigayears ago, making the coupling effect potentially significant. In this work, we calculate the evolution of BH binaries with a binary population synthesis method to examine the possible influence of cosmologically coupled growth of BHs, if it really exists. The measured masses of the compact objects in LMXBs show a gap around ∼2.5–5 M ⊙, separating the most-massive neutron stars from the least-massive BHs. Our calculated results indicate that considering the mass growth seems to (partially) account for the mass gap and the formation of compact BH LMXBs, alleviating the challenges in modeling the formation and evolution of BH LMXBs with traditional theory. However, critical observational evidence like the detection of intermediate-mass BH binaries is required to test this hypothesis.

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“…[1] that BHs could be responsible for the observed accelerated expansion of the universe (see, however, refs. [8][9][10][11][12][13][14][15][16][17]).…”

Section: Introductionmentioning

confidence: 99%

Cosmological coupling of nonsingular black holes

Cadoni,

Sanna,

Pitzalis

et al. 2023

J. Cosmol. Astropart. Phys.

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We show that — in the framework of general relativity (GR) — if black holes (BHs) are singularity-free objects, they couple to the large-scale cosmological dynamics. We find that the leading contribution to the resulting growth of the BH mass (M BH) as a function of the scale factor a stems from the curvature term, yielding M BH ∝ ak , with k = 1. We demonstrate that such a linear scaling is universal for spherically-symmetric objects, and it is the only contribution in the case of regular BHs. For nonsingular horizonless compact objects we instead obtain an additional subleading model-dependent term. We conclude that GR nonsingular BHs/horizonless compact objects, although cosmologically coupled, are unlikely to be the source of dark energy. We test our prediction with astrophysical data by analysing the redshift dependence of the mass growth of supermassive BHs in a sample of elliptical galaxies at redshift z = 0.8–0.9. We also compare our theoretical prediction with higher redshift BH mass measurements obtained with the James Webb Space Telescope (JWST). We find that, while k = 1 is compatible within 1σ with JWST results, the data from elliptical galaxies at z = 0.8–0.9 favour values of k > 1. New samples of BHs covering larger mass and redshift ranges and more precise BH mass measurements are required to settle the issue.

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Constraints on the Cosmological Coupling of Black Holes from the Globular Cluster NGC 3201

Cited by 14 publications

References 80 publications

Constraints on Cosmological Coupling from the Accretion History of Supermassive Black Holes

Constraints on Cosmological Coupling from the Accretion History of Supermassive Black Holes

Can Cosmologically Coupled Mass Growth of Black Holes Solve the Mass Gap Problem?

Cosmological coupling of nonsingular black holes

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