2016 η Car’s FEROS spectrum (blue-solid line). The image displays our best-fit CMFGEN model (red-dashed line) and the model described in Groh et al. (2012a; black-dashed line). The Balmer lines of the FEROS spectrum are too strong. They include large contributions of the circumstellar emission as a result of the bad seeing of ∼2″ at the time of the observation. The black synthetic spectrum matches the Fe II and Si II lines. The absorption component of the P-Cygni profiles are filled in and the He I emission lines are not reproduced by the model, which has been already observed and discussed in detail by Hillier et al. (2001). The hotter red model can hardly fit the spectral lines observed at FEROS’ wavelengths.