A&A 370, 407-408 (2001)
DOI: 10.1051/0004-6361:20010396

Erratum: Radio galaxies at $z\sim$ 2.5: Results from Keck spectropolarimetry

J. Vernet ¹ - R. A. E. Fosbury ² - M. Villar-Martín ³ - M. H. Cohen ⁴ - A. Cimatti ⁵ -
S. di Serego Alighieri ⁵ - R. W. Goodrich ⁶

1 - European Southern Observatory, Karl Schwarzschild Str. 2, 85748 Garching-bei-München, Germany
2 - Space Telescope European Coordination Facility, Karl Schwarzschild Str. 2, 85748 Garching-bei-München, Germany
3 - Dept. of Natural Sciences, Univ. of Hertfordshire, College Lane, Hatfield, Herts AL10 9AB, UK
4 - California Institute of Technology, Mail Stop 105-24, Pasadena, CA 91125, USA
5 - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
6 - W.M. Keck Observatory 65-1120 Mamalahoa Highway, Kamuela, HI 96742, USA

A&A, 366, 7-25 (2001), DOI: 10.1051/0004-6361:20000076

Due to technical problem, Figs. 9 to 12 were misprinted in the paper version. Please find bellow the corrected figures.

Figure 9: The N V/He II vs. N V/C IV diagram as plotted and modelled by HF93 for the BELR of QSOs - which clearly have much higher densities than the gas we are sampling in the narrow lines. The dashed line represents the locus of one of their chemical evolution models: M4a which covers a range of 2-10 times solar for the primary elements in this frame. The sequences implies solar or supersolar metallicities in the extended gas of many HzRG and different levels of enrichment in different objects. The three objects from the literature (see Table 4) are plotted with different symbols (triangles)

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Figure 10: Diagnostic diagrams involving some important UV emission line ratios including the intercombination lines NIV] $\lambda$ 1486, OIII] $\lambda \lambda$ 1661,1666 and CIII] $\lambda$ 1909. These include only data points from our sample. The model metallicity sequence that best reproduces the data trend (solid line) shows good agreement with the data in most diagnostic diagrams although the N IV] line predictions are substantially displaced (lower left, see text). The numerical labels show the metallicity sequence from 0.4 to 4 times solar for elements other than nitrogen which increases quadratically. The top two frames show the small variation in ionization state within the sample while the oxygen diagram (lower right) confirms the existence of the metallicity sequence. In this and the associated figures, only emission line components with a FWHM of $\le 3000$ km s-1 are included

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Figure 11: The relationship between the strength of Ly${\alpha }$- expressed as a ratio to C IV - and the continuum fractional polarization measured in the bin just longward of Ly${\alpha }$. The error bars represent 1$\sigma$ statistical uncertainties in P but, for the line ratios, are derived from uncertainties in the continuum fitting (see text). For values of $P\lesssim 3$%, the points are plotted as $3\sigma$ upper limits

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	Figure 12: The relationship between the narrow line ratio N V/C IV and the continuum fractional polarization measured in the bin just longward of Ly${\alpha }$
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