Clustering of Faint Galaxies: $\w $, Induced by Weak Gravitational Lensing

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dc.creatorVillumsen, Jens Verner
dc.date1995-12-01
dc.date.accessioned2026-07-07T02:20:31Z
dc.date.available2026-07-07T02:20:31Z
dc.descriptionWeak gravitational lensing by large scale structure affects the number counts of faint galaxies through the ``magnification bias'' and thus affects the measurement of the angular two-point correlation function $\w $. At faint magnitudes the clustering amplitude will decrease differently with limiting magnitude than expected from Limber's equation. The amplitude will hit a minimum and then rise with limiting magnitude. This behavior occurs because $\w$ due to clustering decreases with distance, while the ``magnification bias'' due to weak lensing increases with distance. The apparent magnitude $m_{min}$ at which the magnification bias starts to dominate the observed clustering is model and color dependent. It is given by $ω(m=m_{min},θ=5^\prime) \approx (1\ -\ 2)\times 10^{-3}(5s-2)^2 Ω_0^2 σ_8^2$, where $s$ is the logarithmic slope of the number counts. Already published measurements of $\w$ at $R=25$ may be strongly influenced by the ``magnification bias''. An experiment using the ratio of blue and red number counts across the sky can be designed such that the effects of the ``true'' clustering is minimized. The magnification bias is a measurement of the clustering of the mass. This weak lensing experiment does not require measuring shapes and position angles of galaxies. I derive a revised Limber's Equation including the effects of magnification bias.
dc.description11 pages, 2 figures, Submitted to: Monthly Notices of the Royal Astronomical Society
dc.identifierhttps://arxiv.org/abs/astro-ph/9512001
dc.identifierhttp://arxiv.org/abs/astro-ph/9512001
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/10233
dc.subjectAstrophysics
dc.titleClustering of Faint Galaxies: $\w $, Induced by Weak Gravitational Lensing
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