Computes the IMBH mass above which predicted Bondi/ADAF accretion luminosity would exceed the JWST NIRCam/MIRI bolometric upper limit for Omega Centauri's core. This is a third, independent constraint axis alongside stellar kinematics and pulsar timing.
Model-dependent result
The exclusion scales with the assumed ADAF radiative efficiency epsilon. This bound is NOT a peer of the Haberle et al. 2024 kinematic lower bound (≥ 8,200 M-sun) or the Banares-Hernandez et al. 2025 pulsar timing upper bound (≤ 6,000 M-sun). Chen et al. 2025 (arXiv:2511.20945) constrains (mass, accretion) combinations; it does not report a ~20,000 M-sun detection.
Model parameters
0.001
ADAF radiative efficiency (Pesce et al. 2021). Range 10⁻⁴–0.1.
10⁻²¹ kg/m³
Ambient gas density at Bondi radius. GC core: ~10⁻²¹–10⁻²³ kg/m³.
Accretion exclusion limit
709
M-sun (upper limit, accretion axis)
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What this tool computes
Given an ADAF radiative efficiency epsilon, ambient gas density rho_inf, and the JWST NIRCam/MIRI bolometric luminosity upper limit (fixed at 10²⁸ W, Chen et al. 2025), solves for the maximum IMBH mass consistent with non-detection:
where c_s = 10 km/s (approximate GC-core sound speed). The Bondi accretion model assumes spherical symmetry, steady state, and the ADAF radiative prescription.