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B. J. Taylor (Brigham Young University)
Results are reported for an updated version of a published statistical search for super-metal-rich (SMR) stars (Taylor 1996, ApJS 102, 105). By definition, [Fe/H] > +0.2 dex is required for such stars, with false-alarm probabilities p < 0.05. The search is based on two catalogs of homogenized high-dispersion values of [Fe/H] drawn from diverse literature sources. For dwarfs, an updated version of the Taylor (1995, PASP 107, 734) catalog is consulted. For evolved stars, the Taylor (1999, A&AS 143, 523) catalog is searched.
A preliminary list of SMR subgiants and dwarfs is unchanged from 1996:
\rho1 Cnc: [Fe/H] = +0.41 ±0.046 dex (p = 7 x 10-4).
HD 112164: [Fe/H] = +0.36 ±0.052 dex (p = 4 x 10-3).
\eta Boo: [Fe/H] = +0.32 ±0.029 dex (p = 2 x 10-4).
14 Her: [Fe/H] = +0.39 ±0.046 dex (p = 2 x 10-4).
\mu Ara: [Fe/H] = +0.38 ±0.046 dex (p = 4 x 10-3).
31 Aql: [Fe/H] = +0.37 ±0.035 dex (p = 2 x 10-5).
\delta Pav: [Fe/H] = +0.41 ±0.046 dex (p = 7 x 10-4).
The product of the stated values of p is 9 x 10-21. This is the formal probability that none of the stars are actually SMR.
As in 1996, no statistically defensible examples of SMR giants are found. Mu Leo is not an exception to this statement (Taylor 1999, A&AS 344, 655; Taylor 2000, BAAS 32, 1472). The lack of known SMR giants may be due to neglect of promising candidates (listed, for example, by Deming & Butler 1979, AJ 84, 839). For this reason, the existence or nonexistence of SMR giants continues to be an open question.
This research has been supported by the BYU College of Physical and Mathematical Sciences.