Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: Comparison of gas-phase N/O as a function of oxygen abundance in G1's (star) and N1's (plus) CGM (light blue filled; Section 4.2.3) and ISM (red filled; Section 3.2.2) gas. This is the first time this explicit comparison has been made at this z (to our knowledge) and shows that G1's CGM is less chemically evolved than its ISM, and that N1's ISM and CGM are comparable in oxygen abundance. An effective average of the KBSS-MOSFIRE sample is plotted as a green circle (KBSS-LM1; C. C. Steidel et al. 2016); pink squares show metal-rich DLAs compiled by T. A. M. Berg et al. (2015a); light green squares are moderate–low-metallicity DLAs compiled by M. Pettini et al. (2008) where the pentagons show points where S was converted to O assuming (O/S)⊙ = 1.57, M. Asplund et al. 2009); gray squares show very metal-poor DLAs compiled by R. Cooke et al. (2011b); gray points show nearby HII regions in SDSS galaxies from L. S. Pilyugin et al. (2012); dashed black lines show the approximate locations of the primary N plateau and the secondary N rise with similar locations and slopes as M. Pettini et al. (2008); and dashed yellow lines show solar values from M. Asplund et al. (2009). References: Metal-rich compilation by T. A. M. Berg et al. (2015a), S. Lopez et al. (1999), J. X. Prochaska & A. M. Wolfe (1999), J. X. Prochaska et al. (2001b), J. X. Prochaska et al. (2001a), M. Dessauges-Zavadsky et al. (2006), M. Dessauges-Zavadsky et al. (2007), T. A. M. Berg et al. (2013), T. A. M. Berg et al. (2015b), S. Lopez et al. (2002), M. Centurión et al. (2003), P. Petitjean et al. (2008), J. X. Prochaska et al. (2002), R. Dutta et al. (2014), C. Ledoux et al. (1998), P. Erni et al. (2006), M. Pettini et al. (2008), S. Lopez & S. L. Ellison (2003), R. Srianand et al. (2005), P. Noterdaeme et al. (2012), R. Srianand et al. (2012), R. B. C. Henry & J. X. Prochaska (2007), J. X. Prochaska et al. (2003), J. X. Prochaska et al. (2007b), C. Ledoux et al. (2006), P. Noterdaeme et al. (2008), L. Lu et al. (1996), T. Zafar et al. (2014b), S. A. Levshakov et al. (2002), and M. Dessauges-Zavadsky et al. (2001). Moderate–low-metallicity compilation by M. Pettini et al. (2008), M. Dessauges-Zavadsky et al. (2004), S. L. Ellison & S. Lopez (2001), P. Petitjean et al. (2008), S. Lopez & S. L. Ellison (2003), M. Centurión et al. (2003), R. B. C. Henry & J. X. Prochaska (2007), M. Dessauges-Zavadsky et al. (2006), L. Lu et al. (1998), M. Pettini et al. (2002), C. Ledoux et al. (2006), S. Lopez et al. (2002), and V. D’Odorico et al. (2002); very metal-poor compilation by R. Cooke et al. (2011b), R. Cooke et al. (2011a), B. E. Penprase et al. (2010), M. Pettini et al. (2008), P. Molaro et al. (2000), P. Petitjean et al. (2008), S. L. Ellison et al. (2010), M. Dessauges-Zavadsky et al. (2001), R. Srianand et al. (2010), J. M. O’Meara et al. (2006), and J. X. Prochaska & A. M. Wolfe (2002).