[
    {
        "id": "authors:2g9kp-tsa16",
        "collection": "authors",
        "collection_id": "2g9kp-tsa16",
        "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161021-155705985",
        "type": "article",
        "title": "Surface Photometry and the Structure of Elliptical Galaxies",
        "author": [
            {
                "family_name": "Kormendy",
                "given_name": "John",
                "clpid": "Kormendy-J"
            },
            {
                "family_name": "Djorgovski",
                "given_name": "S.",
                "orcid": "0000-0002-0603-3087",
                "clpid": "Djorgovski-S-G"
            }
        ],
        "abstract": "This paper reviews surface photometry of bulges and elliptical galaxies. Work prior to 1982 is discussed by Kormendy (1982a; hereafter K82). Since then, the subject has gone through a revolution. CCD detectors have come into common use, providing photometry accurate enough to measure new classes of subtle properties of ellipticals. Together with improvements in seeing, CCDs have allowed the resolution and study of galaxy cores\nand nuclei (Section 2). Newly discovered structural details, such as dust, shells, and dynamical subsystems, show the importance of accretion events in galaxy evolution (Sections 3-6). Better measurements of parameter scaling laws have led to improved constraints on galaxy formation (Section 8). Finally, CCDs provide accurate measurements of departures from elliptical isophotes (Section 9) and color gradients (Section 10). These observations are currently producing a quantum jump in our understanding\nof elliptical galaxies. \nSome of the present subjects are discussed in more detail in recent reviews by Kormendy (1987a; hereafter K87), Okamura (1988), and Nieto (1988). Techniques are discussed by de Vaucouleurs (1979, 1984), Nieto (1982), Capaccioli & de Vaucouleurs (1983), Capaccioli (1985, 1987,\n1988a,b), Okamura (1988), and Djorgovski & Dickinson (1989). Compilations of photometry references for individual galaxies are found in Davoust & Pence (1982) and Pence & Davoust (1985).\n\nUnless otherwise noted, we assume that the Hubble constant is H_0 = 50 km s^(-1) Mpc^(-1).",
        "doi": "10.1146/annurev.aa.27.090189.001315",
        "issn": "0066-4146",
        "publisher": "Annual Reviews",
        "publication": "Annual Review of Astronomy and Astrophysics",
        "publication_date": "1989-09",
        "series_number": "1",
        "volume": "27",
        "issue": "1",
        "pages": "235-277"
    }
]