Keck Spectroscopy Of The Hubble Deep Field

erse, one needs only to think of the impact of the Hubble Deep Field (Williams et al. 1996), and of the projects that the HDF images have precipitated. The first results from the DEEP team's Keck LRIS observations of the HDF and its flanking fields are available in four papers, and are summarized below. The results are based on samples of galaxies selected from the HDF to meet a number of scientific goals. Structural parameters, colors, surface brightnesses Deep Extragalactic Evolutionary Probe; for further information see the DEEP home page at http://www.ucolick.org/ deep/home.html. Figure 1: An example of a galaxy at z = 0:48 is shown with its Keck LRIS slit position, the observed emission line and the measured and model rotation curve. Note that any underestimate of the rotational velocity will lead to an overestimate of the brightening! The Tully-Fisher relation derived from such measurements is shown in Vogt et al. (1997) and Vogt & Phillips (this volume). and morphological