[
    {
        "id": "authors:dv41z-5c870",
        "collection": "authors",
        "collection_id": "dv41z-5c870",
        "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190610-085930794",
        "type": "publication_whitepaper",
        "title": "The Chemical Evolution of the Galactic Bulge",
        "author": [
            {
                "family_name": "Rich",
                "given_name": "R. Michael",
                "orcid": "0000-0003-0427-8387",
                "clpid": "Rich-R-M"
            },
            {
                "family_name": "Clarkson",
                "given_name": "Will",
                "clpid": "Clarkson-W-I"
            },
            {
                "family_name": "Cohen",
                "given_name": "Judith",
                "orcid": "0000-0002-8039-4673",
                "clpid": "Cohen-J-G"
            },
            {
                "family_name": "Howard",
                "given_name": "Christian",
                "clpid": "Howard-C"
            },
            {
                "family_name": "McWilliam",
                "given_name": "Andy",
                "clpid": "McWilliam-A"
            },
            {
                "family_name": "Johnson",
                "given_name": "Jennifer",
                "clpid": "Johnson-Jennifer-A"
            },
            {
                "family_name": "Johnson",
                "given_name": "Christian",
                "clpid": "Johnson-C-I"
            },
            {
                "family_name": "Cunha",
                "given_name": "Katia",
                "clpid": "Cunha-K"
            },
            {
                "family_name": "Smith",
                "given_name": "Verne",
                "clpid": "Smith-V-V"
            },
            {
                "family_name": "Fulbright",
                "given_name": "Jon",
                "clpid": "Fulbright-J"
            }
        ],
        "abstract": "This science white paper addresses the issue of discovering the chemical evolution of the\nGalactic bulge, from which we may learn the initial mass function at the time of the formation of\nthe bulge, the timescale for the initial burst of star formation, any evidence supporting an\nextended era of star formation, evidence of very early mergers of massive subcomponents, and\nthe fraction of its mass that was contributed by late mergers. A further immediate problem\nconcerns the composition of dwarfs measured from microlensing events versus the abundance\nscale measured from giants. A companion White Paper (Clarkson & Rich) addresses a set of\nbulge science questions that require observations at very high angular resolution.",
        "publisher": "Caltech Library",
        "publication_date": "2009"
    },
    {
        "id": "authors:wjaqf-26f12",
        "collection": "authors",
        "collection_id": "wjaqf-26f12",
        "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190607-161647635",
        "type": "publication_whitepaper",
        "title": "Extremely Metal-Poor Stars: The Local High Redshift Universe",
        "author": [
            {
                "family_name": "Cohen",
                "given_name": "Judith",
                "orcid": "0000-0002-8039-4673",
                "clpid": "Cohen-J-G"
            },
            {
                "family_name": "Beers",
                "given_name": "Timothy C.",
                "orcid": "0000-0003-4573-6233",
                "clpid": "Beers-T-C"
            },
            {
                "family_name": "Frebel",
                "given_name": "Anna",
                "orcid": "0000-0002-2139-7145",
                "clpid": "Frebel-A"
            },
            {
                "family_name": "Johnson",
                "given_name": "Jennifer",
                "clpid": "Johnson-J"
            },
            {
                "family_name": "Lai",
                "given_name": "David",
                "clpid": "Lai-David"
            },
            {
                "family_name": "McWilliam",
                "given_name": "Andrew",
                "clpid": "McWilliam-A"
            },
            {
                "family_name": "Rockosi",
                "given_name": "Constance",
                "clpid": "Rockosi-C-M"
            },
            {
                "family_name": "Shectman",
                "given_name": "Stephen",
                "clpid": "Shectman-S-A"
            },
            {
                "family_name": "Sneden",
                "given_name": "Christopher",
                "orcid": "0000-0002-3456-5929",
                "clpid": "Sneden-C"
            }
        ],
        "abstract": "Extremely metal-poor (EMP) stars can only have formed early in the history of the Galaxy, and\nrepresent the local equivalent of the high redshift universe. With them, we can study the early\nsupernovae, the early chemical evolution of the Galaxy, and the history of star formation in the\nMilky Way. By analogy we can learn about those epochs of galaxy formation in the distant past\nthat are currently at such high redshifts that they are beyond the reach of even the largest existing\ntelescopes, a technique some call \"near-field cosmology\".\nWhile H, He, and some Li came out of the Big Bang, all other elements were formed in stars,\nand were dispersed by supernovae and stellar winds into the gas from which subsequent stellar\ngenerations formed. The ejecta from supernovae played the most important role in the early\nUniverse. SN models have many parameters, including the history of the progenitor star (initial\nmass, mass loss history, internal nucleosynthesis history prior to the explosion, etc), the details of\nthe explosion (energy, ejected mass, mixing) etc. There are vigorous groups pursuing the details of\nthese models both theoretically and computationally in the US and abroad. But there are so many\nfree or poorly known parameters that these efforts are best guided by observations of metal-poor\nstars.",
        "publisher": "Caltech Library",
        "publication_date": "2005"
    }
]