**Table 2:** Physical parameters of the $z_{\rm abs}$ = 1.8073 metal absorber towards HS 0747+4259 derived by the MCI procedure with the Haardt & Madau and modified UV background spectra (marked, respectively, by HM96 and S1 in Fig. 2). Column densities are given in cm^-2.
	subsystem A		subsystem B		subsystem C^d
	-90 km s^-1 < v < 0 km s^-1		0 km s^-1 < v < 80 km s^-1		-20 km s^-1 < v < 20 km s^-1
Parameter^a	HM96	S1	HM96	S1
(1)	(2)	(3)	(4)	(5)	(6)
U₀	8.1E-3	4.5E-3	6.2E-3	4.1E-3
$N_{\rm H}$	1.2E18	7.7E17	7.6E18	4.7E18
$\sigma_{v}$ , km s^-1	15.0	13.0	19.8	23.5
$\sigma_{y}$	0.55	0.60	0.68	0.64
$Z_{\rm C}$	8.3E-5	1.0E-4	1.2E-5	1.7E-5
$Z_{\rm O}$	2.5E-4	3.6E-4	4.2E-5	6.0E-5
$Z_{\rm Si}$	1.1E-5	1.6E-5	1.8E-6	2.9E-6
$[Z_{\rm C}]$	-0.47	-0.37	-1.30	-1.15
$[Z_{\rm O}]$	-0.27	-0.10	-1.04	-0.90
$[Z_{\rm Si}]$	-0.46	-0.31	-1.25	-1.04
N(H I)	1.4E15	$(1.4\pm0.4)$ E15	1.0E16	$(1.2\pm0.3)$ E16	<3.0E14
N(C II)	3.6E12^b	4.3E12^b	4.8E12	$(7.0\pm2.0)$ E12	$\ldots$
N(O II)	8.1E12^b	1.0E13^b	1.2E13^b	2.2E13^b	$\ldots$
N(Si II)	4.9E11^b	5.6E11^b	6.9E11	$(9.0\pm3.0)$ E11	$\ldots$
N(C III)	7.0E13	5.5E13^c	7.3E13	6.0E13^c	$(1.0\pm0.3)$ E13^e
N(O III)	2.2E14	2.0E14^c	2.5E14	2.1E14^c	$\ldots$
N(Si III)	5.8E12	$(6.1\pm0.9)$ E12	8.4E12	$(8.1\pm1.2)$ E12	$\ldots$
N(C IV)	1.7E13	$(1.50\pm0.15)$ E13	1.1E13	$(1.1\pm0.1)$ E13	$(1.9\pm0.2)$ E13
N(O IV)	5.6E13	$(6.2\pm2.0)$ E13	4.9E13^b	5.0E13^b	$(2.9\pm0.9)$ E14^e
N(Si IV)	3.4E12	$(2.6\pm0.4)$ E12	2.2E12	$(2.0\pm0.4)$ E12	$\ldots$
N(N V)	$\ldots$	$\ldots$	$\ldots$	$\ldots$	$\leq$ 2.0E12
N(O VI)	$\ldots$	$\ldots$	$\ldots$	$\ldots$	$(1.10\pm0.25)$ E14
$\langle T \rangle$ , K	1.3E4	1.5E4	2.0E4	2.0E4
$n_{\rm H}$ , cm^-3	3.3E-3	6.6E-3	5.0E-3	7.6E-3
L, kpc	0.13	0.04	0.5	0.2

$^aZ_{\rm X} = N_{\rm X}/N_{\rm H}$ ; $[Z_{\rm X}] = \log~ (N_{\rm X}/N_{\rm H}) - \log~ (N_{\rm X}/N_{\rm H})_\odot$ ; ^b calculated using the velocity and density distributions estimated from the metal profiles marked by the horizontal bold lines in Fig. 1; ^c uncertainty cannot be estimated since line is corrupted by background subtraction; ^d column densities for putative O VI absorption at -70 km s^-1 < v < -20 km s^-1 and at 30 km s^-1 < v < 50 km s^-1 are not given because of probable blending with some Ly $\alpha$ forest lines (observed intensities of O VI $\lambda1032$ and $\lambda1037$ are inconsistent); ^e can be blended.

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