Erratum: "Is there a metallicity-luminosity relationship in active galactic nuclei? The case of narrow-line Seyfert 1 galaxies" Page: 1

                                
THE ASTROPHYSICAL JOURNAL, 569:L59-L59, 2002 April 10
2002. The American Astronomical Society. All rights reserved. Printed in U.S.A.
ERRATUM: "IS THERE A METALLICITY-LUMINOSITY RELATIONSHIP IN ACTIVE GALACTIC NUCLEI?
THE CASE OF NARROW-LINE SEYFERT 1 GALAXIES" (ApJ, 567, L19 [2002])
OHAD SHEMMER AND HAGAI NETZER
School of Physics and Astronomy and the Wise Observatory, Raymond and Beverly Sackler Faculty of Exact Sciences,
Tel Aviv University, Tel Aviv 69978, Israel; ohad@wise.tau.ac.il, netzer@wise.tau.ac.il
We found a computational error in the above Letter, affecting the calculation of the intrinsic luminosities of several objects in
our sample. As a consequence, new versions of Figure 2 and Tables 1 and 2 are presented below. This does not affect any of the
main results of the Letter.

U
Z

0

10
z

1 T
o BLAGN
0*NLS1
I           I

tt       (jr   r

10 9   101      101    L1012    1013
vL,,@ 1450A(Lsu)

101       101

FIG. 2.-HF93 metallicity indicators, N v/C Iv (top) and N v/He II
(bottom), as a function of luminosity. Empty circles mark BLAGNs, and
filled circles marks NLSis; solid lines represent the BLAGN best-fit Z-L
slope; large squares with error bars represent average line ratios in bins
of 0.5 in log zL, of the entire data set. Note the significant deviation of
the low-luminosity bins from the straight line (top) owing to the addition
of NLS1s.
TABLE 1
LINEAR REGRESSION PARAMETERS FOR N v/C IV VERSUS log zL,
Data Set     Number of   Pearson   Spearman      Slope         Constant
Codea        Objects      (r)       (rs)         (a)            (b)
B                  121       0.70       0.73     0.19  0.02    -2.86  0.23
B+N                130       0.55       0.60     0.13   0.02   -2.11   0.23
RQQ (B)            105       0.72       0.74     0.18   0.02   -2.82   0.23
RQQ (B+N)          114       0.56       0.60     0.13   0.02   -2.04   0.24
B+up.lim.          137       0.67       0.69     0.19   0.02   -2.91   0.24
B+N+up.lim.        146       0.52       0.57     0.13   0.02   -2.17   0.24
a Data set codes are B for BLAGNs, N for NLS1s, RQQ for radio-quiet quasars, and
up.lim. for upper limits on the line ratio.
TABLE 2
LINEAR REGRESSION PARAMETERS FOR N v/He ii VERSUS log PL,
Data Set     Number of   Pearson   Spearman      Slope         Constant
Codea        Objects      (r)       (rs)         (a)            (b)
B                   98       0.58       0.60     0.14  0.02    -1.37  0.27
B+N                107       0.50       0.53     0.11   0.02   -0.95   0.24
RQQ (B)             83       0.61       0.64     0.14   0.02   -1.25   0.26
RQQ (B+N)           92       0.54       0.57     0.11   0.02   -0.87   0.23
B+up.lim.          110       0.54       0.55     0.15   0.02   -1.45   0.28
B+N+up.lim.        119       0.46       0.48     0.11   0.02   -1.00   0.26
a Data set codes are identical to those in Table 1.

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