Evidence of Multiple r-Process Sites in the Early Galaxy: New   Observations of CS 22892-052
  First results are reported of a new abundance study of neutron-capture elements in the ultra-metal-poor (UMP; [Fe/H] = -3.1) halo field giant star CS 22892-052. Using new high resolution, high signal-to-noise spectra, abundances of more than 30 neutron-capture elements (Z>30) have been determined. Six elements in the 40<Z<56 domain (Nb, Ru, Rh, Pd, Ag and Cd) have been detected for the first time in a UMP star. Abundances are also derived for three of the heaviest stable elements (Os, Ir, and Pb). A second transition of thorium, Th{4086}, confirms the abundance deduced from the standard Th{4019} line, and an upper limit to the abundance of uranium is established from the absence of the U{3859} line. As found in previous studies, the abundances of the heavier (Z>=56) stable neutron-capture elements in CS 22892-052 match well the scaled solar system r-process abundance distribution. From the observed Th abundance, an average age of ~= 16 +/- 4 Gyr is derived for cs22892-052, consistent with the lower age limit of ~= 11 Gyr derived from the upper limit on the U abundance. The concordance of scaled solar r-process and CS 22892-052 abundances breaks down for the lighter neutron-capture elements, supporting previous suggestions that different r-process production sites are responsible for lighter and heavier neutron-capture elements. 
Christopher Sneden, John J. Cowan, Inese I. Ivans, George M. Fuller,   Scott Burles, Timothy C. Beers, and James E. Lawler