Table 1: Fit results for the RGS spectra extracted from a 1.1 $\hbox {$^\prime $ }$ wide strip centred on the core of M 87. The iron abundance is given with respect to the proto-solar values by Lodders (2003) and the other abundances with respect to iron. Emission measures ( $Y = \int n_{{\rm e}} n_{{\rm H}} {\rm d}V$ ) are given in 10⁶⁴ cm^-3.
Parameter 2T-model wdem-model

Y₁ $0.86\pm0.03$

Y₂ $9.97\pm0.13$

$Y_{{\rm wdem}}$ $11.56\pm0.17$

kT₁ (keV) $0.80\pm0.01$

kT₂ (keV) $1.67\pm0.02$

$kT_{{\rm max}}$ $2.38\pm0.05$

$\alpha$ $0.47\pm0.02$

c $0.22\pm0.01$

$kT_{{\rm mean}}$ $1.82\pm0.04$

C/Fe $0.73\pm0.11$ $0.74\pm0.13$

N/Fe $1.62\pm0.19$ $1.62\pm0.21$

O/Fe $0.60\pm0.03$ $0.59\pm0.04$

Ne/Fe $1.40\pm0.11$ $1.25\pm0.12$

Mg/Fe $0.70\pm0.05$ $0.60\pm0.06$

Fe $0.98\pm0.02$ $1.06\pm0.03$

$\chi^{2}$ / $\nu$ 2737/1905 2728/1905

**Table 1:** Fit results for the RGS spectra extracted from a 1.1 $\hbox {$^\prime $ }$ wide strip centred on the core of M 87. The iron abundance is given with respect to the proto-solar values by Lodders (2003) and the other abundances with respect to iron. Emission measures ( $Y = \int n_{{\rm e}} n_{{\rm H}} {\rm d}V$ ) are given in 10⁶⁴ cm^-3.
Parameter	2T-model	wdem-model
Y₁	$0.86\pm0.03$
Y₂	$9.97\pm0.13$
$Y_{{\rm wdem}}$		$11.56\pm0.17$
kT₁ (keV)	$0.80\pm0.01$
kT₂ (keV)	$1.67\pm0.02$
$kT_{{\rm max}}$		$2.38\pm0.05$
$\alpha$		$0.47\pm0.02$
c		$0.22\pm0.01$
$kT_{{\rm mean}}$		$1.82\pm0.04$
C/Fe	$0.73\pm0.11$	$0.74\pm0.13$
N/Fe	$1.62\pm0.19$	$1.62\pm0.21$
O/Fe	$0.60\pm0.03$	$0.59\pm0.04$
Ne/Fe	$1.40\pm0.11$	$1.25\pm0.12$
Mg/Fe	$0.70\pm0.05$	$0.60\pm0.06$
Fe	$0.98\pm0.02$	$1.06\pm0.03$
$\chi^{2}$ / $\nu$	2737/1905	2728/1905

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