**Table 4:** Chemical abundances in ellipticals from their X-ray spectra.
Galaxy	[Fe/H]	[O/Fe]	[Mg/Fe]	[S/Fe]	[Si/Fe]	[Ne/Fe]	[C/Fe]	[N/Fe]	Core	ab.	Ref.
									(kpc)
NGC 5044	${\sim} 0_c/{-}0.36_o$	-0.48	-0.06	-0.27	-0.08	-	-	-	48	GS	^a
M 87	-0.11	-0.44	-0.15	-	-	-0.26	0	-0.21	-	AG	^b
M 87	-	-0.52_c/-0.28_o	-0.28	-0.08	0_c/0.1_o	-0.52_c/-0.21_o	-	-	2.5	GS	^c
M 87	-0.009_c/-0.39_o	-0.34_c/-0.20_o	-	0_c/-0.09_o	0.05_c/-0.04_o	-	-	-	-	F	^f
NGC 1399	${\sim} 0.3_c/{\sim}{-}0.3_o$	-	-	-	-	-	-	-	20	AGm	^d
NGC 4636	-0.06	-0.24	-0.13	-	-	-0.09	-	0.07	-	AG	^e

Solar abundance used: AG: Anders & Grevesse (1989, photospheric), AGm: Anders & Grevesse (1989, meteoritic), GS: Grevesse & Sauvall (1998), F: Feldman (1992).
References: ^a: Buote et al. (2003); ^b: Sakelliou et al. (2002); ^c: Gastaldello & Molendi (2002); ^d: Buote (2002); ^e: Xu et al. (2002); ^f: Matsushita et al. (2003).
Core: radius of the region quoted as "galactic core'' in the above-mentioned paper.

Source LaTeX | All tables | In the text

	1 Introduction
	2 The model
	3 Galactic models
	4 The stellar component - photochemical properties of the models
	5 The gaseous halo - X-ray properties of the models
	6 The ICM
	7 Conclusions
	References