Fig. 9.

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Observed UVJ diagram (Williams et al. 2009), showing restframe U − V and V − J colors (calculated using EAzY; Brammer et al. 2008), for objects at 1.5 < z < 2.4 with M⋆ > 109 M⊙ in the AEGIS pointings of Wide. Upper panel: Solid orange points are the observed sample and transparent grey points are the parent sample. While objects located within the boundary in the upper-left corner are often considered to be quiescent in nature (e.g. Whitaker et al. 2011; Muzzin et al. 2013), Wide spectroscopy reveals Hα emission in some of them (squares) indicating some source of ionizing photons (e.g. residual star formation, heating by old stellar populations, and/or an AGN; Byler et al. 2019; Maseda et al. 2021). Lower panels: Wide PRISM spectra for the two objects denoted by stars in the upper panel; sources close to the boundary between star-forming and quiescent. While the characteristic uncertainty in the restframe colors is large (shown in the lower-right corner of the upper panel), spectroscopy can unambiguously differentiate via e.g. a detection of Hα emission at 6563 Å in excess of the BAGPIPES-determined stellar continuum.
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