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1.4. Miras as probes of the Galactic bulge

  • S.M.G. Hughes (a1), R.M. Catchpole (a1), P.A. Whitelock (a2) and M.W. Feast (a3)

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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.

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References

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Feast, M.W., 1996, MNRAS, 278, 11.
Feast, M.W, Glass, I.S., Whitelock, P.A., Catchpole, R. 1989 MNRAS, 241, 375.
Hughes, S.M.G. 1992, IAU Coll. 139, eds. Nemec, J.M. and Matthews, J.M. (CUP), p192.
Hughes, S.M.G. & Wood, P.R. 1990, AJ, 99, 784.
van Leeuwen, F., Feast, M. W., Whitelock, P. A., Yudin, B. 1997 MNRAS 287, 955.
Whitelock, P.A. & Catchpole, R.M., 1992 in The Center, Bulge and Disk of the Milky Way, ed. Blitz, L. (Kluwer: Dordrecht), p.103.
Whitelock, P.A., et al., 1994, MNRAS, 267, 711.

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