Left: MZR for cluster and field galaxies at z ∼ 1.5, using the N2 method of Pettini & Pagel (2004) to derive oxygen abundances. The SDSS local MZR relation is shown by the red solid line using the fit given by Kewley & Ellison (2008) for the N2 calibration. The dotted red lines show the dispersion of the SDSS relation, ±0.09 dex, as given by Kewley & Ellison (2008), while the dotted blue line is displaced by a further 0.11 dex to lower metallicities compared to the lower dotted red line, and corresponds to the location of the stacked measurements (large blue filled squares) of a larger sample of z ∼ 1.5 KMOS3D field galaxies from Wuyts et al. (2016). Red triangles are XMM2215 cluster galaxies from the SFvirialized sample, blue star symbols are XMM2215 infalling galaxies (see phase-space diagram, Fig. 2), and blue filled circles depict KMOS3D field galaxies at 1.42 <  z <  1.52 from Wuyts et al. (2016). The red filled circle is the galaxy 39683 with a relatively high [NII]/Hα ratio, and a possible contribution from an AGN to the [NII] emission. An enhancement of the oxygen abundances of about 0.1 dex for XMM2215 cluster galaxies compared to field is seen. Right: line ratios [N II] λ 6584/Hα for the SFvirialized sample (red), infalling galaxies (asterisks), and KMOS3D field galaxies (blue). A linear fit of the log([N II] λ 6584/Hα) vs. stellar mass relation for the SFvirialized sample is shown by the red dotted line, and the linear relation implied by the stacked values of the KMOS3D sample (large blue filled squares) is shown by the blue dotted line. An enhancement of the log([N II] λ 6584/Hα) ratios of 0.2 dex for XMM2215 cluster galaxies compared to field is visible.