Table 1: Physical and observational parameters of the 6 HFP galaxies observed with WSRT. Columns 1, 2: source names; Col. 3: projected linear sizes (Orienti et al. 2006); Col. 4: optical redshift; Col. 5: central frequency; Col. 6: channel resolution; Col. 7: 1 $\sigma$ noise level in the line cube; Col. 8: continuum flux density taken from our WSRT data at the observed frequency; Col. 9: peak flux density of the absorption line, measured on the spectral image; Col. 10: optical depth; Col. 11: the width of the H I absorption line: for J0111+3906 the FWHM is given, in the case of OQ 208 we give the FWZI, due to the complexity of the line profile; Col. 12: H I column density derived from $N_{\rm {H {\sc i}}} = 1.82 \times 10^{18} T_{\rm spin} \tau _{\rm peak} \Delta V$ cm^-2, a $T_{\rm spin}$ of 100 K has been assumed; Col. 13: the redshift of the peak H I absorption. The line flux density, the optical depth and the H I column density upper limits have been computed assuming the 2 $\sigma$ noise level, a line width of 100 km s^-1 and $T_{\rm spin}$ of 100 K, as in Vermeulen et al. (2003). a: For the source J0111+3906, the projected linear size is taken from Owsianik et al. (1998).
Source Other LS $z_{\rm opt}$ $\nu_{\rm obs}$ Resol. rms $S_{\rm obs}$ $S_{\rm HI}$ $\tau_{\rm peak}$ $\Delta v$ Log( $N_{\rm HI}$ ) $z_{\rm HI,peak}$

J2000 name pc MHz km s^-1 mJy/b/ch mJy mJy km s^-1

(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)

J0003+2129 22 0.452 977.96 4.3 6.1 50 <12.2 <0.15 <21.43

J0111+3906 OC 314 22^a 0.668 851.32 6.9 2.8 170 52.7 0.44 100 21.90 0.6687

J0655+4100 <1 0.02156 1390.03 4.3 0.7 239 <1.4 <0.006 <20.0

J1407+2827 OQ 208 10 0.0773 1318.60 4.5 1.1 826 5 0.005 1800 20.9 0.0769

J1511+0518 7 0.084 1309.96 9.5 1.1 80 <2.2 <0.02 <20.6

J1623+6624 <1 0.203 1180.38 4.5 0.7 129 <1.4 <0.01 <20.3

**Table 1:** Physical and observational parameters of the 6 HFP galaxies observed with WSRT. Columns 1, 2: source names; Col. 3: projected linear sizes (Orienti et al. 2006); Col. 4: optical redshift; Col. 5: central frequency; Col. 6: channel resolution; Col. 7: 1 $\sigma$ noise level in the line cube; Col. 8: continuum flux density taken from our WSRT data at the observed frequency; Col. 9: peak flux density of the absorption line, measured on the spectral image; Col. 10: optical depth; Col. 11: the width of the H I absorption line: for J0111+3906 the *FWHM* is given, in the case of OQ 208 we give the *FWZI*, due to the complexity of the line profile; Col. 12: H I column density derived from $N_{\rm {H {\sc i}}} = 1.82 \times 10^{18} T_{\rm spin} \tau _{\rm peak} \Delta V$ cm^-2, a $T_{\rm spin}$ of 100 K has been assumed; Col. 13: the redshift of the peak H I absorption. The line flux density, the optical depth and the H I column density upper limits have been computed assuming the 2 $\sigma$ noise level, a line width of 100 km s^-1 and $T_{\rm spin}$ of 100 K, as in Vermeulen et al. (2003). a: For the source J0111+3906, the projected linear size is taken from Owsianik et al. (1998).
Source	Other	LS	$z_{\rm opt}$	$\nu_{\rm obs}$	Resol.	rms	$S_{\rm obs}$	$S_{\rm HI}$	$\tau_{\rm peak}$	$\Delta v$	Log( $N_{\rm HI}$ )	$z_{\rm HI,peak}$
J2000	name	pc		MHz	km s^-1	mJy/b/ch	mJy	mJy		km s^-1
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)
J0003+2129		22	0.452	977.96	4.3	6.1	50	<12.2	<0.15		<21.43
J0111+3906	OC 314	22^a	0.668	851.32	6.9	2.8	170	52.7	0.44	100	21.90	0.6687
J0655+4100		<1	0.02156	1390.03	4.3	0.7	239	<1.4	<0.006		<20.0
J1407+2827	OQ 208	10	0.0773	1318.60	4.5	1.1	826	5	0.005	1800	20.9	0.0769
J1511+0518		7	0.084	1309.96	9.5	1.1	80	<2.2	<0.02		<20.6
J1623+6624		<1	0.203	1180.38	4.5	0.7	129	<1.4	<0.01		<20.3

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