1999/05/03 by Atsunori Yonehara · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1086/312107
15 pages LaTeX, 3 figures, accepted to ApJ Letter. e-mail: [email protected]
arxiv created 1999/05/03 · openalex publication_date 1999/07/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
In the case of gravitationally lensed quasars, it is well known that there is a time delay between the occurrence of the intrinsic variabilities in each split image. Generally, the source of variabilities has a finite size, and there are time delays even in one image. If the origin of variabilities is widely distributed, say over ≳100 pc as a whole, variabilities between split images will not show a good correlation even though their origin is identical. Using this fact, we are able to limit the whole source size of variabilities in a quasar below the limit of direct resolution by today's observational instruments.