tokens: side and top histograms show that our SINFONI targets (red-hatched histogram) form a fair sub-sample of the full CARLA sample (blue-shaded histogram) in radio power, UV luminosity, and BH mass, even though the SINFONI sample covers a more limited range in redshift. A list of the targets and relevant observational information in our quasar sample is given in Table 1 . Table 2 summarizes the main parameters determined for the six broad-line radio galaxies from Nesvadba et al. ( 2011 ) that were used in our analysis. The available parameters include H α-based BH mass estimates and Eddington ratios that were determined in a similar fashion to the analysis performed on the CARLA quasars in this paper. Table 1. Sample information. Note . a Redshifts are from SDSS. Table 2. Broad-line radio galaxies from Nesvadba et al. ( 2011 ). Notes . a Redshifts based on H α taken from Nesvadba et al. ( 2011 ). † Radio luminosity at 325 MHz taken from De Breuck et al. ( 2000 ). ‡ Radio luminosity at 500 MHz taken from Wylezalek et al. ( 2013 ). 2.2 Observations We used SINFONI at UT4 of the VLT at the European Southern Observatory (ESO) to observe a sample of 35 high-redshift quasars. The purpose of the project was to obtain NIR spectra probing the rest-frame optical region around H α in order to obtain more accurate BH masses for quasars selected from the CARLA survey and SDSS. The data were taken over 6 yer (2009–2015) as part of programmes 095.B-0323(A), 094.B-0105(A), 093.B-0084(A), 092.B-0565(A), 091.B-0112(A), 090.B-0674(A), and 089.B-0433(A) (PI: Jaron Kurk). Except for 089.B-0433(A), all programmes targeted radio-loud quasars from CARLA. The 089.B-0433(A) targets were selected from SDSS on the basis of their very high (C iv -based) BH masses but are not part of the CARLA sample (see Section 2.1 ). We used the SINFONI K band (1.95–2.45 μ m) with the spatial scale of 125 × 250 mas (without adaptive optics). This setup delivers a spatial aperture of 8 × 8 arcsec 2 with a spectral resolution of ∼400 km s −1 , allowing a robust sky subtraction. The observational strategy includes on-source dithering (ABBA pattern) in order to optimize the exposure time on the source and sky subtraction, and a telluric standard star for telluric band removal and flux calibration. We took 14–16 individual exposures of 300 s each, resulting in total integration times of 4200–4800 s. 2.3 Data reduction The data reduction was performed using the SINFONI pipeline v2.9.0 (Modigliani et al. 2007 ) with the Reflex interface. The pipeline creates master calibration images and applies them to the observations, starting with a non-linearity map constructed from the flat-field frames. A master dark frame is created from the dark frames and the hot pixels are mapped. Individual flat-field images are combined into a master flat. Optical distortion and slitlet distances are computed, and the dispersion solution for the wavelength calibration is determined from arc spectra. Finally,
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