We report detailed analysis of high-resolution spectra of nine high velocity metal-rich dwarfs in the solar neighborhood , selected from the proper motion samples of Grenon .
The stars are super metal-rich , and 5 of them have [ Fe/H ] \geq + 0.4 , making them the most metal-rich stars currently known .

We find that \alpha -elements decrease with increasing metallicity ; s-elements are underabundant by about [ s-elements/Fe ] \approx - 0.3 ; the \ion Eu2 line was measurable for 6 stars , showing [ Eu/Fe ] \approx 0.0 , except for G161-29 where [ Eu/Fe ] = + 0.50 .

All calculations followed the same methods used by Castro et al . ( 1996 ) [ AJ , 111 , 2439 ] for the analysis of the well-known metal-rich prototype \mu Leo and the very strong-lined bulge star BW IV-167 , for which [ Fe/H ] = + 0.46 and + 0.47 were found respectively .

While exceeding the [ Fe/H ] of current bulge samples , the chemistry of these stars has important similarities and differences .
The near-solar abundances of the alpha-capture elements places these stars on the metal-rich extension of McWilliam & Rich ( 1994 ) [ ApJS , 91 , 749 ] , but their s-process abundances are much lower than those of the bulge giants .
These low s-process values have been interpreted as the hallmark of an ancient stellar population .
We are unable to convincingly assign these stars to a known Galactic population and we urge further studies of larger samples .