By S. Weinberg
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Extra resources for Gravitation and Cosmology - Prins and Applns of the Gen Theory of Relativity
Dark solid line), the elliptical model of Croft ic Metzler (upper dashed), the semi-analytic model of Crittenden et al. (fainter solid), and the tidal stretch model of Catelan et al. (lower dot-dashed). The expected lensing signal is the lowest line. noise. Analytic methods are likely to be limited by the validity or otherwise of the simplifying assumptions, and neither general method can really be expected to include non-gravitational processes reliably in the near future. Thus it is probably best to be satisfied that we know the magnitude of the effect, and therefore not attempt to do straightforward weak lensing calculations from low-redshift samples.
N. Kaiser, ApJ 537, 555 (2001). 7. N. Kaiser, G. Squires and T. Broadhurst ApJ 449, 460 (1995). 8. K. Kuijken A&A 352, 355 (1999). 9. A. Luppino and N. Kaiser ApJ 475, 20 (1997). 10. C. MacKay (2001) h t t p : / / w o l . r a . phy. cam. a c . uk/mackay/Book. html 11. K. Ratnatunga, R. Griffiths and E. Ostrander AJ 118, 86 (1999) 12. A. Refregier and D. Bacon MNRAS submitted, (astro-ph/0105179). 13. J. Rhodes, A. J. Groth ApJ 536, 79 (2000). A. co Realistic self-consistent models of galaxies can be obtained by specifying the velocity field and solving the Euler equation semi-analytically.
One component is much larger than the other, and they have opposite values of e+ (always e x = 0 ) . 5. We obtain the results shown in Fig. 4 which show that again we also have very small residuals. In fact these residuals are entirely accounted for by the errors due to the finite number of noise realizations performed. 5. 4 Conclusions We have presented a conceptually simple method for estimating galaxy ellipticities, with carefully calculated uncertainty estimates. This method is intrinsically designed to cope with high noise levels on the input data and naturally allows bad fits to be identified from the residuals map.