1f:T437,classical Cepheids are discussed with particular emphasis on the fact that Cepheids continue to provide the most homogeneous and reliable set of distances to many nearby galaxies. Observational programs relating to extragalactic Cepheids are also reviewed, and new distances and reddenings to individual galaxies are determined from these data using multiwavelength PL relations, based for the first time on self-consistent calibrating data sets. Three recent promising secondary extragalactic distance indicators (Tully-Fisher, planetary nebula luminosity functions, and surface-brightness fluctuations) tie their zero points to the Cepheid distance scale and give globally consistent values for the Hubble constant of about 80 km sec-1^ Mpc-1^. Tying the Faber-Jackson relation and the supernova distance scales to the Leo and Virgo clusters yields similar results. Such a value for the Hubble constant is marginally inconsistent with new estimates of the ages of globular clusters, and it may prove to be a serious problem for standard cold dark-matter models of the universe.20:T42a,We describe a relatively direct technique of determining extragalactic distances. The method relies on measuring the luminosity fluctuations that arise from the counting statistics of the stars contributing the flux in each pixel of a high-signal-to-noise CCD image of a galaxy. The amplitude of these fluctuations is inversely proportional to the distance of the galaxy. This approach bypasses most of the successive stages of calibration required in the traditional extragalactic distance ladder; the only serious drawback to this method is that it requires an accurate knowledge of the bright end (M_V_ <= 3) of the luminosity function. Potentially, this method can produce accurate distances of elliptical galaxies and spiral bulges at distances out to about 20 Mpc. In this paper, we explain how to calculate the value of the fluctuations, taking into account various sources of contamination and the effects of finite spatial resolution, and we demonstrate, via simulations and CCD images of M32 and N3379, the feasibility and limitations of this technique.21:T431,We have determined the distance to SN 1987A by comparing the angular size of its circumstellar ring, measured from an HST image obtained in a narrow [O III] 5007 A filter, with its absolute size derived from an analysis of the light curves of narrow UV lines (N V λ1240, N IV] λ1486, N III] λ1750, and C III] λ1909) measured with IUE. Our analysis confirms that the observed elliptical structure is indeed a circular ring seen at an inclination of <i> = 42.8^deg^ + 2.6^deg^ and provides a determination of its absolute diameter of (1.27 +/- 0.07) x 10^18^ cm. Its ratio to the angular diameter of 1.66''+/- 0.03'' (Jakobsen et al.) gives an accurate determination of the distance to SN 1987A, i.e., d(1987A) = 51.2 +/- 3.1 kpc. Estimating the relative position of SN 1987A within the Large Magellanic Cloud on the basis of radial velocity data, the distance to the center of the LMC turns out to be 50.1 +/- 3.1 kpc and its distance modulus 18.50 +/- 0.13. This value agrees very well with the determinations obtained from light-curve analyses of variable stars.22:T419,The authors present results from a study of the distances and velocities of elliptical galaxies out to ≡6000 km s^-1. Distances are inferred from a new relation between central velocity dispersion and an angular diameter defined by integrated surface brightness. With this residual velocities V_obs - V_pred from a smooth Hubble flow are estimated. It is found that V_obs - V_pred, in coordinates with respect to the microwave background, exhibits a systematic variation over the celestial sphere. Interpreted as a large-scale bulk flow, this variation implies a mean motion of the ellipticals with respect to the microwave background of 599±104 km s^-1 in the direction l = 312°±11°, b = 6°±10°. The data show that if the microwave dipole anisotropy is due to a motion of the

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