2002/12/31 by N. W. Evans, H. J. Witt · 6 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Flux (metallurgy) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gravitation #Gravitational lens #Lens (geology) #Observable #Pulsars and Gravitational Waves Research #Simple (philosophy) #Strong gravitational lensing #Weak gravitational lensing #astro-ph
paper · pdf · doi:10.1046/j.1365-2966.2003.07057.x
published as Mon.Not.Roy.Astron.Soc.345:1351,2003 · 16 pages, version in press at MNRAS, revisions include new treatment of the observational errors and the inclusion of external shear in the models
arxiv created 2003/07/10 · openalex publication_date 2003/11/02 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The observables in a strong gravitational lens are usually just the image positions and sometimes the flux ratios. We develop a new and simple algorithm which allows a set of models to be fitted exactly to the observations. Taking our cue from the strong body of evidence that early-type galaxies are close to isothermal, we assume that the lens is scale-free with a flat rotation curve. External shear can be easily included. Our algorithm allows full flexibility regarding the angular structure of the lensing potential. Importantly, all the free parameters enter linearly into the model and so the lens and flux ratio equations can always be solved by straightforward matrix inversion. The models are only restricted by the fact that the surface mass density must be positive. We use this new algorithm to examine some of the claims made for anomalous flux ratios. It has been argued that such anomalies betray the presence of substantial amounts of substructure in the lensing galaxy. We demonstrate by explicit construction that some of the lens systems for which substructure has been claimed can be well fitted by smooth lens models. This is especially the case when the systematic errors in the flux ratios (caused by microlensing or differential extinction) are taken into account. However, there is certainly one system (B 1422+231) for which the existing smooth models are definitely inadequate and for which substructure may be implicated. Within a few tens of kpc of the lensing galaxy centre, dynamical friction and tidal disruption are known to be very efficient at dissolving any substructure. Very little substructure is projected within the Einstein radius. The numbers of strong lenses for which substructure is currently being claimed may be so large that this contradicts rather than supports cold dark matter theories.