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R.A. Lucas, S. A. Baum, S. Casertano, D. de Mello, M. Dickinson, H. C. Ferguson, A. S. Fruchter, R. Gonzalez-Lopezlira, I. Heyer, J. Mack, R. Makidon, C. L. Martin, M. Mutchler, E. Smith, M. Stiavelli, H. I. Teplitz, M. S. Wiggs, R. Williams, D. Zurek (STScI), T.M. Brown, J. P. Gardner (GSFC), M. E. Kaiser (JHU), R. N. Hook (ESO/ST-ECF)
Due to the availability of the STIS and NICMOS instruments at the time of the observations, the Hubble Deep Field - South Flanking Fields are more complex and varied than those of the Hubble Deep Field - North. In addition to the WFPC2 Flanking Fields, there are parallel observations in STIS and NICMOS for each, and there are also a series of STIS observations of the NICMOS deep field, and associated WFPC2 and NICMOS parallels as well. In this paper, we will present the data and describe the data reduction process used for the HDF-S Flanking Fields.
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