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Published online by Cambridge University Press: 25 May 2016
Mira variables span a wide range of stellar populations and have a well-defined K, log P relation (e.g. Feast et al 1989; Hughes & Wood 1990), so can be used to map out the 3-D distribution of the bulge. Using IRAS-selected Miras, Whitelock & Catchpole (1992) showed for the first time from individual stellar distances that the bulge had a bar-like structure, but there is some uncertainty as to whether they obey the same K, log P relation as optically selected Miras. Hence the need for confirmation from an optical Mira survey.