**Table 6:** Compilation of O I and P II measurements found in the literature. The distance we report is the target distance, it is also an upper limit for the cloud distances.
Sightline	$\log N$ (O I)	$\log N$ (P II)	$\log$ P II/O I	reference	comment
WD 0004+330	$16.34\pm0.15$	$12.85\pm0.02$	$-3.50\pm0.15$	Lehner et al. (2003)	Star distance D=97 pc
WD 0131-163	$15.85\pm0.11$	$12.78\pm0.09$	$-3.07\pm0.14$	''	D=96 pc
WD 1211+332	$15.74\pm0.32$	$12.57\pm0.08$	$-3.17\pm0.32$	''	D=115 pc
WD 1528-163	$15.80\pm0.08$	$12.40\pm0.30$	$-3.40\pm0.30$	''	D=140 pc
WD 1631+781	$15.78\pm0.11$	$12.45\pm0.14$	$-3.33\pm0.17$	''	D=67 pc
WD 1634-573^a	$15.50\pm0.04$	$12.08\pm0.07$	$-3.43\pm0.08$	''	D=37 pc
WD 1800+685	$16.11\pm0.14$	$12.94\pm0.06$	$-3.17\pm0.15$	''	D=159 pc
WD 1844-223	$15.97\pm0.19$	$12.59\pm0.10$	$-3.38\pm0.20$	''	D=62 pc
WD 2004-605	$15.65\pm0.08$	$12.36\pm0.09$	$-3.29\pm0.11$	''	D=58 pc
WD 2011+395	$16.04\pm0.07$	$12.59\pm0.14$	$-3.45\pm0.15$	''	D=141 pc
WD 2124-224	$15.94\pm0.03$	$12.74\pm0.09$	$-3.20\pm0.10$	''	D=224 pc
WD 2211-495^b	$15.34\pm0.04$	$12.04\pm0.10$	$-3.30\pm0.11$	''	D=53 pc
WD 2309+105	$15.67\pm0.05$	$12.28\pm0.04$	$-3.39\pm0.07$	''	D=79 pc
WD 2331-475	$15.48\pm0.05$	$12.18\pm0.10$	$-3.30\pm0.11$	''	D=82 pc
HD 185418	$18.15\pm0.09$	$14.72\pm0.10$	$-3.43\pm0.14$	Sonnentrucker et al. (2003)	D=790 pc
GD 246	$15.67\pm0.07$	$12.29\pm0.10$	$-3.38\pm0.13$	Oliveira et al. (2003)	D=79 pc
WD 2331-475	$15.48\pm0.11$	$12.18\pm0.20$	$-3.30\pm0.25$	''	D=82 pc
HZ 121	$15.74\pm0.10$	$12.57\pm0.13$	$-3.17\pm0.17$	''	D=115 pc
$\zeta$ Pup	$16.70\pm0.20$	$13.38\pm0.05$	$-3.32\pm0.21$	Morton et al. (1978)	D=450 pc
$\zeta$ Oph	$17.38\pm0.10$	$13.98\pm0.10$	$-3.40\pm0.14$	Morton et al. (1975)	D=200 pc
$\alpha$ Vir	$15.58\pm0.10$	$12.40\pm0.15$	$-3.18\pm0.20$	York & Kinahan (1979)	D=88 pc
HD 47240	$14.86\pm0.02$	$12.60\pm0.10$	$-2.26\pm0.10$	Welsh et al. (2001)	D=1800 pc
Sk108	$16.65\pm0.06$	$13.39\pm0.04$	$-3.26\pm0.07$	Mallouris (2003)	(SMC star)
					Metallicity $Z\sim Z_\odot$ /4
Q0347-383^c	$16.18\pm0.18$	$12.48\pm0.09$	$-3.70\pm0.21$	Ledoux et al. (2003)	(DLA)
					Redshift $z_{\rm abs}=3.02485$ ,
					$Z\sim Z_\odot$ /10
Q0347-383^c	$16.12\pm0.12$	$12.34\pm0.19$	$-3.78\pm0.24$	''	(DLA) $z_{\rm abs}=3.02463$ ,
					$Z\sim Z_\odot$ /10
LLIV Arch	$16.42\pm0.23$	$13.21\pm0.12$	$-3.21\pm0.28$	Richter et al. (2001)	Z $\sim$ Z $_\odot$
QSO HE 2243-6031	$16.79\pm0.21$	$13.42\pm0.10$	$-3.37\pm0.25$	Lopez et al. (2002)	(DLA) $z_{\rm abs}=2.33$ ,
					$Z\sim Z_\odot$ /12
QSO 0000-2620	$16.42\pm0.10$	$12.63\pm0.04$	$-3.79\pm0.11$	Molaro et al. (2001)	(DLA) $z_{\rm abs}=3.3901$ ,
					$Z\sim Z_\odot$ /100 (Molaro et al. 2000)

^a Wood et al. (2002) obtained a consistent ratio $\log$ P II/O I = $-3.43\pm0.15$ for this sightline.
^b Hébrard et al. (2002) obtained a consistent ratio $\log$ P II/O I = $-3.29\pm0.23$ for this sightline.
^c Levshakov et al. (2002) found $-3.63\pm0.03$ towards this QSO. We choose to quote the measurement of Ledoux et al. (2003) who obtained significantly better VLT/UVES data and had a particular attention on the saturation of O I lines.

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations
	3 Data analysis
	4 Results
	5 Conclusions
	References