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Table 6.

Spearman test results for the SUPER sample.

Correlation Slope ρ P-value
(1) (2) (3) (4)
FWHM Hβ vs. FWHM Hα(1) 1.43 ± 0.49 0.88 6e−6
FWHM Hβ vs. FWHM Hα(2) 0.95 ± 0.20 0.87 2e−5
FWHM Hβ vs. FWHM MgII(1) −0.05 ± 0.70 0.39 0.15
FWHM Hβ vs. FWHM MgII(2) 2.89 ± 1.89 0.66 0.01
FWHM Hα vs. FWHM MgII(1) 1.15 ± 0.63 0.41 0.11
FWHM Hα vs. FWHM MgII(2) 0.63 ± 0.23 0.50 0.04
FWHM Hβ vs. FWHM CIV(1) −40.32 ± 0.14 −0.32 0.24
FWHM Hβ vs. FWHM CIV(2) −0.32 ± 0.14 −0.33 0.23
FWHM Hα vs. FWHM CIV −0.13 ± 0.11 −0.15 0.54
Log L vs Log L5100 0.84 ± 0.05 0.79 6e−5
Log L vs Log L5100 0.97 ± 0.06 0.94 6e−8
Log L1350 vs Log L5100 0.78 ± 0.15 0.78 7e−5
Log L3000 vs Log L5100 0.97 ± 0.19 0.86 2e−5
Log L vs Log L 1.09 ± 0.08 0.78 4e−4

Notes. We derived linear relations using the BCES (Y|X) regression (Akritas & Bershady 1996). Outlier objects showing a very broad FWHM of Hβ (J1549+1245, see Fig. 5) and MgII emission lines (X_N_4_48, see Sect. 6) have been included (1) and excluded (2) from the fit.

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