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Our Fossil Galaxy

population. The halo and the bulge are supported mainly by their velocity dispersion. In a famous and influential paper, Eggen, Lynden-Bell and Sandage (1962) proposed that these pressure supported components formed before the disk, through the rapid collapse of part of the protogalaxy. This proposal was based on evidence at that time that the orbital and chemical properties of halo stars are tightly related, in the sense that the most metal weak halo stars have the largest orbital eccentricities and the lowest systemic rotation. In this picture, the stellar abundances and the kinematics are both measures of the time elapsed since the beginning of the collapse: as the collapse proceeds, the mean chemical abundance of the interstellar medium increases, and so does the mean systemic rotation of the stars forming at each stage of the collapse. An alternative view of the formation of the metal weak halo and bulge developed during the 1970's, and crystallized at the Yale conference in 1977. Toomre (1977) commented: "It seems almost inconceivable that there wasn't a great deal of merging of sizeable bits and pieces (including quite a few lesser galaxies) early in the career of every major galaxy, no matter what it now looks like. The process would obviously have yielded halos from the stars already born, whereas any leftover gas would have settled quickly into new disks embedded within such piles of stars. More or less simultaneously though, any compact and presumably more metal rich partners or galaxy cores should have sunk quite deep into this brew before losing their separate identities, thereby contributing to what we call central bulges." At about the same time, Searle and Zinn (1978: SZ) showed that there was no radial chemical gradient among the outer galactic globular clusters (i. e. the chemical and dynamical properties of the globular clusters are apparently decoupled), and they proposed that the galactic halo formed by the accretion of small metal weak "fragments", such as gas rich dwarf galaxies. SZ then showed that the shape of the chemical abundance distribution expected in this accretion picture agrees well with the distribution observed for the galactic globular clusters. Mass