ner_tags: O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O B-Instrument O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Instrument O O O O O O O O O O O O O O O O O O O O O O O O B-Instrument O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: mostly the and lines, and Mg for XMM2235. We note that the S/N significantly decreases in the blue part of the spectrum because of the lower throughput of KMOS in the bluer part of the YJ band, which affects the uncertainties of our measurements. Moreover, the blue part of the spectrum we fit covers a shorter wavelength range than the red part. This could potentially affect the set of templates applied by the fitting procedure. To circumvent this issue, we adopt the same combination of templates derived in the fit of the full spectrum in both the fit of the blue and red part. As discussed in Section 3.3 , before performing the kinematic fit, we smooth the KMOS spectrum with a variable kernel to a common FWHM to match the maximum FWHM. This should prevent us from adding systematics related to the KMOS resolution in the blue and red part of the spectrum. Figure 9 shows a comparison of the results obtained by fitting the full spectrum and the blue part (left panels), the full spectrum and the red part (central panels), and red and blue part (right panels). The actual value is determined as the mode of the distribution over the 100 bootstrap realizations and the error as the standard deviation. The actual value of the stellar velocity dispersion from our spectra is consistent within the errors with the mode of the distribution of derived from the bootstrap realizations. Figure 9. Comparison between the stellar velocity dispersion measurements in the blue and red part of the spectrum for XMM2235 (upper panel) and XMM2215 (lower panel). From left to right, the panels show the comparison between the fit in the full spectrum and the blue part, the full spectrum and the red part, and between blue and red part, respectively. For XMM2235, we find that the kinematics derived from the blue part and from the full spectrum have a median difference () and a scatter of 70.11 , while by fitting the red region of the spectrum, we find an offset () and a scatter of 56.20 from the fit of the full spectrum. The median difference between the fit of the blue and red part of the spectrum is () with a scatter of 72.54 . In XMM2235 the quality of some data in the “blue” part is particularly poor, resulting in a few objects with systematically higher than in the full sample. For XMM2215, we find that the kinematics derived from the blue part and from the full spectrum have a median difference () and a scatter of 60.80 , while by fitting the red region of the spectrum, we find an offset of () and a scatter of 60.00 from the fit of the full spectrum. The median difference between the fit of the blue and red part of the spectrum is () with a scatter of 121.41 . This test aims at assessing the systematic effect we can have from deriving stellar velocity dispersions from different absorption lines at different redshift. It did not result in a rejection of galaxies, which were mostly discarded at the stage of fitting the full spectrum through all the bootstrap