By Hans-Walter Rix (auth.), C. S. Kochanek, J. N. Hewitt (eds.)
EDWIN TURNER AND RACHEL WEBSTER Co-Chairs, clinical Organizing Committee lAU Symposium 173, Astrophysical functions of Gravitational Lenses, was once held in Melbourne, Australia from July 9-14, 1995. The Symposium used to be subsidized by way of lAU Commissions forty seven and forty. With the invention by way of Walsh and collaborators of the 1st example of a gravitational lens, the multiply imaged quasar 0957+561, the realm of grav itational lensing moved from speculative thought to an important astrophysical device. because that point, there were common, nearly biennial in ternational conferences either in Europe and in North the US, that have in particular focussed on gravitational lensing. in this get together, with the blessing of the l. a. U, the assembly was once held on the college of Melbourne in Australia. It was once the 1st foreign astronomical assembly to be held on the collage of Melbourne, and desire totally has given the astronomical neighborhood a few enthusiasm for hiking half-way around the globe to Australia to debate their newest work.
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8 Mpc for M100 (Freedman et al. 1994). These distances (summarized in Table 2) support the high value of Ho. On the other hand, Sandage & Tammann (Sandage 1995; Sandage & Tammann 1994; 1990) have been claiming differently, as summarized in Table 3. 5 Mpc. I believe only two methods, the distances from the TF relation and from supernovae, deserve serious attention, since the other indicators are not well qualified. The distance from globular cluster luminosity functions (GCLF) depends on how it is derived.
Koclumek and J. N. Hewitt (eds), Astrophysical Applications o/Gravitational Lensing, 37-42. © 1996IAU. A. CORBETT ET AL. 96 for the lensed object. In this contribution we report the successful determination of a time delay in 0218+357. 2. 4GHz on 25 irregularly spaced occasions during 3-months in 1992/3. 335 arcsec apart. We set out to monitor the total flux densities, the polarized flux densities and polarization position angles of the compact images. As well as 0218+357, three calibration sources and a "control source" were observed during the 45 minutes allocated to each epoch.
J. , 1991, MNRAS, 253, 99 Kochanek, C. , 1993, ApJ, 403,517 NOTE ON A SUPER-HORIZON-SCALE INHOMOGENEOUS COSMOLOGICAL MODEL K. TOMITA Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-01, Japan 1. Introduction Many observations oflarge-scale and cosmological structures in the universe have been collected, but so far there is no consistent theoretical explanation. In the region within 100 Mpc from us, the observed two-point correlations of galaxies and clusters of galaxies can be described well by low-density homogeneous cosmological models (Bahcall & Cen 1993; Suto 1993).