Proceedings of the Particle Physics and Early Universe Conference (PPEUC).
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1 Introduction  

The properties of the population and the individual appearance of distant galaxies can both be modified significantly by the gravitational lensing effect of foreground masses (Schneider et al. (1992)). Gravitational lensing has been investigated in most detail in the near-infrared/optical and radio wavebands, in which faint distant galaxies can be observed with sub-arcsecond resolution. However, there are excellent prospects for extending these studies into the submillimetre waveband (Blain (1996a), Blain (1996b), Blain (1997a), Blain (1997c)). The fraction of gravitational lenses expected in a sample of galaxies selected in the submillimetre waveband can be up to three orders of magnitude larger as compared with a sample selected in other wavebands.

The concept of magnification bias provides a useful way of describing the effects of lensing on a population of distant galaxies (Borgeest et al. (1991)). If the surface density of galaxies with flux densities greater than per unit redshift is at redshift , then magnification by a factor due to gravitational lensing would predict a modified count,

If locally, then the magnification bias is given by . Hence, if then the surface density of galaxies is increased and the magnification bias is positive; if then the surface density is decreased and the bias is negative. Magnification bias was first discussed in the context of samples of bright quasars; however, counts of galaxies at faint flux densities in the submillimetre waveband are expected to be uniquely steep, with or less (Blain & Longair (1996), Blain & Longair (1993)), and so the magnification bias for faint galaxies in this waveband is expected to be very significant (Blain (1996b)). At brighter flux densities the submillimetre-wave counts are expected to be less steep, and to follow the Euclidean slope, with . The magnification bias is expected to be largest at flux densities at which the counts begin to rise above the Euclidean slope. If the population of dusty star-forming galaxies evolves strongly, then the largest magnification bias is predicted to occur at flux densities (Blain (1997a)), flux densities that are comparable with the sensitivity of Planck (Bersanelli et al. (1996)).

The submillimetre-wave counts of gravitationally-lensed galaxies are expected to be very sensitive to changes in both the world models and scenarios of galaxy formation and evolution that are assumed. Hence, the properties of the lensed galaxies or quasars detected in a Planck survey would allow both the evolution of galaxies and the values of cosmological parameters to be investigated. A value of Hubble's constant is assumed throughout this paper.

PPEUC Proceedings
Thu Jun 19 14:22:31 BST 1997