Table 1: Rms line widths ( FWHM) of the strongest emission lines, their cross-correlation lags with respect to continuum variations, and the derived central black hole masses (see text for details).
Line FWHM(rms) $\tau_{\rm cent}$ M

[km s^-1] [days] [ $10^7~M_{\odot}$ ]

(1) (2) (3) (4)

HeII $\lambda 4686$ 4444. $\pm$ 200 $\rm 3.5^{+2.}_{-2.}$ $\rm 2.25^{+1.63}_{-0.45}$

HeI $\lambda 5876$ 2404. $\pm$ 100 $\rm 10.8^{+4.}_{-4.}$ $\rm 1.81^{+1.36}_{-0.33}$

H $\beta$ 1515. $\pm$ 100 $\rm 23.5^{+4.}_{-4.}$ $\rm 1.63^{+0.33}_{-0.31}$

H $\alpha$ 1315. $\pm$ 100 $\rm 32.5^{+4.}_{-4.}$ $\rm 1.64^{+0.33}_{-0.35}$

**Table 1:** Rms line widths ( *FWHM*) of the strongest emission lines, their cross-correlation lags with respect to continuum variations, and the derived central black hole masses (see text for details).
Line	FWHM(rms)	$\tau_{\rm cent}$	M
	[km s^-1]	[days]	[ $10^7~M_{\odot}$ ]
(1)	(2)	(3)	(4)
HeII $\lambda 4686$	4444. $\pm$ 200	$\rm 3.5^{+2.}_{-2.}$	$\rm 2.25^{+1.63}_{-0.45}$
HeI $\lambda 5876$	2404. $\pm$ 100	$\rm 10.8^{+4.}_{-4.}$	$\rm 1.81^{+1.36}_{-0.33}$
H $\beta$	1515. $\pm$ 100	$\rm 23.5^{+4.}_{-4.}$	$\rm 1.63^{+0.33}_{-0.31}$
H $\alpha$	1315. $\pm$ 100	$\rm 32.5^{+4.}_{-4.}$	$\rm 1.64^{+0.33}_{-0.35}$

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