Predicting Stellar-mass Black Hole Populations in Globular Clusters

• DOI: 10.3847/1538-4357/aad63d
• Publication Date: 2018-08-27T13:13:17Z
• Authors: Newlin C. Weather...; Sourav Chatterjee; Carl L. Rodriguez; Frederic A. Rasio
• Keywords: Astrophysics - Solar and Stellar Astrophysics; Astrophysics of Galaxies (astro-ph.GA); 0103 physical sciences; FOS: Physical sciences; General Relativity and Quantum Cosmology (gr-qc); Astrophysics - Astrophysics of Galaxies; 01 natural sciences; General Relativity and Quantum Cosmology; Solar and Stellar Astrophysics (astro-ph.SR)

Abstract Recent discoveries of black hole (BH) candidates in Galactic and extragalactic globular clusters (GCs) have ignited interest understanding how BHs dynamically evolve a GC the number ( <?CDATA ${N}_{\mathrm{BH}}$?> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>N</mml:mi> </mml:mrow> <mml:mi>BH</mml:mi> </mml:msub> </mml:math> ) that may still be retained by today’s GCs. Numerical models show even if stellar-mass are GCs, they typically configurations not directly detectable. We suitably defined measure mass segregation (Δ) between, e.g., giants low-mass main-sequence stars, can an effective probe to indirectly estimate aided calibrations from numerical models. Using models, including all relevant physics, we first is strongly anticorrelated with Δ between giant stars stars. apply distributions versus obtained three Milky Way GCs predict them at present. calculate using publicly available Advanced Camera for Surveys’ survey data 47 Tuc, M10, M22, identified BH candidates. these measured as calibration expected For M22 our predicted peak ≈ 20, 24, 50, whereas, within 2 σ confidence level, up ∼150, 200, respectively.