Planets, Stars and Stellar Systems

By T. Oswalt, L. French, P. Kalas. 2013

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THE MBH–LSPHEROID RELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES (2012, methodology): “Springer-Verlag, Berlin (RC3) de Vaucouleurs, G. & Olson, D. W. 1982, ApJ, 256, 346 Devereux, N.A., Ford, H.C., Tsvetanov, Z., & Jacoby, G. 2003, AJ, 125, 1226 Djorgovski, S., & Davis, M. 1987, ApJ, 313, 59 Dong, X.-B., Ho, L.C., Yuan, W., et al. 2012, ApJ, 755, 167 Dong, X.Y., & De Robertis, M.M. 2”
Dynamical Evolution of the Early Solar System (2018, background): “Here we are therefore not primarily concerned with the growth and gas-driven migration of planets (for that, see reviews of Kley & Nelson 2012 and Youdin & Kenyon 2013).”
The Evolution of Galaxy Structure Over Cosmic Time (2014, methodology): “The concentration index however has to be measured very carefully, as different regions and radii used can produce very different values that systematically do not reproduce well when observed under degraded conditions (e.g., Graham et al. 2001; Graham et al. 2005).”
CARBON-ENHANCED METAL-POOR STAR FREQUENCIES IN THE GALAXY: CORRECTIONS FOR THE EFFECT OF EVOLUTIONARY STATUS ON CARBON ABUNDANCES (2014, background): “These stars belong to the broader class of very metal-poor ([Fe/H]5 < −2.0, e.g., Beers & Christlieb 2005; Frebel & Norris 2013) stars, which have been vigorously searched for and analyzed over the past quarter century.”