Key points are not available for this paper at this time.
As part of our survey for substructure in the Milky Way halo as traced by giant stars, and to look for tidal stellar debris in the halo viable for measurement of the Galactic mass potential with the Space Interferometry Mission (SIM), we explore the distribution of stars beyond the nominal tidal radius of, but still associated with, the Carina dwarf spheroidal galaxy. We make use of the photometric technique described in Majewski et al. (1999b, AJ, submitted) to identify giant star candidates at the distance and metallicity of the Carina dwarf spheroidal across the entire extent of a photometric survey covering some 2.2 deg 2 on and around Carina. These Carina-associated giant candidates are identified by a combination of (1) their M − DDO51 colors, which are a measure of both surface gravity and metallicity at given M − T2 colors, and (2) by locations in the color-magnitude diagram commensurate with the Carina red giant branch in the core of the galaxy. The density distribution of the extratidal giant candidates bears resemblance to the outer isopleths of Carina presented by Irwin Hatzidimitriou (1995, MNRAS, 277, 1354). However, in contrast to previous, statistical star-counting approaches,
Majewski et al. (Wed,) studied this question.