tokens: The authors wish to thank Sara Ellison, Crystal Martin, and George Djorgovski for aiding in collection and reduction of the Keck/ESI spectroscopy used in this study. We also wish to thank the anonymous referee for useful comments which improved the manuscript. It is our pleasure to thank Neil Crighton, Simeon Bird, Jeff Cooke, Claude-André Faucher-Giguère, Michele Fumagalli, John O’Meara, Celine Péroux, Ali Rahmati, and Sijing Shen for valuable discussion of this work, and to acknowledge Sijing Shen for sharing the results of her analysis of the CGM properties of the Eris2 simulation. Finally, we are grateful to Art Wolfe for sharing his insight on these results and for his inspiring and pioneering work in this field. K.H.R.R. acknowledges the generous support of the Clay Postdoctoral Fellowship, and J.F.H. acknowledges support from the Alexander von Humboldt foundation in the context of the Sofja Kovalevskaja Award. The Humboldt foundation is funded by the German Federal Ministry for Education and Research. J.X.P. and M.L. acknowledge support from National Science Foundation (NSF) grants AST-1010004, AST-1109452, AST-1109447, and AST-1412981. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
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