2002/07/31 by Da-Ming Chen
Physics and Astronomy · #Binary black hole #Black hole (networking) #Cosmology and Gravitation Theories #Dark matter #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gravitational lens #Mass distribution #Pulsars and Gravitational Waves Research #Stellar black hole #Supermassive black hole #Weak gravitational lensing #astro-ph
paper · pdf · doi:10.1051/0004-6361:20021552
published as Astron.Astrophys. 397 (2003) 415 · 6 pages, 2 figures, accepted for publication in A&A. Some references added and errors corrected according to the referee and language editor
arxiv created 2002/09/09 · openalex publication_date 2002/12/17 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We investigate how central black holes (BHs) in galactic dark halos could affect strong gravitational lensing. The distribution of integral lensing probability with image separations are calculated for quasars of redshift 1.5 by foreground dark matter halos. The mass density of dark halos is taken to be the Navarro-Frenk-White (NFW) profile such that, when the mass of a halo is less than , its central black holes or a bulge is included as a point mass. The relationship between the masses of supermassive black holes and the total gravitational mass of their host galaxy is adopted from the most recent literature. Only a flat ΛCDM model is considered here. It is shown that, while a single black hole for each galaxy contributes considerable but not sufficient lensing probabilities at small image separations compared with those without black holes, the bulges (which are about 100–1000 times larger in mass than a typical black hole) would definitely contribute enough probability at small image separations, although it gives too high probabilities at large separation angles compared with lensing observations.