All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{1666fig1.eps} \end{figure}$ Figure 1: XMM MOS1 and MOS2 raw image of Abell 85, with the regions analysed in detail superimposed. The concentric circles around the cluster centre ( white full lines) define the centre and rings used for the detailed spectral analysis; the green dashed circle defines the VSSRS region; the yellow dashed ellipse defines the impact region, where the South Blob is probably hitting the main body of Abell 85; the blue dotted circle defines the South Blob region. The small black circles are point sources that were excluded when accumulating the spectra. The VSSRS region was also excluded from the external ring.
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{1666fig2.eps} \end{figure}$ Figure 2: Left: optical "true-color'' r-g-i image from the SDSS 2nd Data Release overlayed with logarithmically spaced Chandra isocontours. Right: Chandra X-ray image in the [0.3-8.0 keV] band. The small circle on both panels indicates an X-ray point source which may be an AGN. The arrow at the bottom right shows the position of a "hole'' of X-ray emission south of the nucleus clearly visible on the Chandra image.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1666fig3.ps} \end{figure}$ Figure 3: Temperature map and XMM isocontours in the [0.5-8.0] keV band for Abell 85. The scale for the temperature is keV.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1666fig4.ps} \end{figure}$ Figure 4: Metallicity map with XMM X-ray intensity contours in the [0.5-8.0] keV band superimposed. The scale for the metallicity is in solar units.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig5.eps} \end{figure}$ Figure 5: Gas temperature as a function of radius obtained with XMM-Newton (filled circles), Chandra (empty circles) and BeppoSax (empty squares).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig6.eps} \end{figure}$ Figure 6: Gas metallicity profile from our XMM-Newton data. For comparison we also plot the De Grandi et al. (2004) data for "cool-core'' and non "cool-core'' clusters.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig7.eps} \end{figure}$ Figure 7: Hydrogen absorption column profile from our XMM-Newton data. The two horizontal dotted lines indicate the Galactic absorption columns towards the Centre of Abell 85 and towards the South Blob obtained with the FTOOLS nh task, based on Dickey & Lockman (1990, see text for details); the dot-dashed line is the galactic $N_{\rm H}$ value from Hartmann & Burton (1997), cf. Arabadjis & Bregman (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig8.eps} \end{figure}$ Figure 8: Best spectral fits with residues for XMM-Newton MOS1, MOS2 and PN. Top: central region (R < 100'') fit with a cooling-flow model (CEVMKL); middle: Ring 1 fit with a VMEKAL ( 100'' < R < 250''); bottom: Ring 2 fit with a VMEKAL ( 250'' < R < 400'').
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig9.eps} \end{figure}$ Figure 9: Spectral MEKAL fit within the central 4 arcmin using the three XMM cameras, restricted to the [5.0-8.0 keV] band. Each line corresponds to one of the 3 detectors, cf. Fig. 8. Top panel: temperature and metallicity are free and the redshift is set to 0.0555. Bottom panel, when the redshift is set free, the best fit is z = 0.0533_-0.0009^+0.0015 (90% confidence level). The reduced $\chi ^{2}$ is given in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig10.eps} \end{figure}$ Figure 10: Photon spectra for 3 individual regions. Top: the VSSRS region (2.5 arcmin radius region). Middle: the elliptical impact region. Bottom: the South Blob region (3.0 arcmin radius region). See text for region locations.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig11.eps} \end{figure}$ Figure 11: MOS1+MOS2 X-ray image with the 21 cm radio isocontours obtained by Slee et al. (2001) overlayed. The radio source seems to be anti-correlated with the west X-ray excess emission at $\alpha \sim 0^{\rm h}41^{\rm m}36^{\rm s}$ and $\delta \sim -9^\circ 22'$ approximately limited by the dashed ellipse.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig12.eps} \end{figure}$ Figure 12: Heavy element abundances relative to iron in regions Centre (filled circles), Ring 1 (empty squares), Ring 2 (filled diamonds) and South Blob (empty triangles). Various models are superimposed: SNII (full line), Hypernovae (long dashes), and SNIa WDD1 (dot-dashed), WDD2 (dotted) and W7 (spaced dots).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig13.eps} \end{figure}$ Figure 13: Emission profile of the X-ray gas obtained from the XMM-Newton MOS1 image (the profile from MOS2 is litterally indistinguishable from MOS1); three fits are superimposed: a Sérsic law, a $\beta$ -model (dashes) and a $\beta$ -model excluding the four innermost points (dot-dashes).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig14.eps} \end{figure}$ Figure 14: Top: gas mass (dotted line) and dynamical mass (solid line when including the calculation of the temperature profile, dashedline in the isothermal case) as a function of radius. The vertical dotted line indicates the limiting radius of the data. For the isothermal case, we have adopted the mean emission temperature kT = 6.5 keV. Bottom: baryon fraction in both cases.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig15.eps} \end{figure}$ Figure 15: Dynamical mass density as a function of radius derived from our data (full line) and compared to a NFW model (dashed line) and to a Moore99 profile (dotted line). $\rho _{\rm dyn}\propto r^{-1.9}$ is a good fit at small radii. The two vertical dotted lines indicate the spatial resolution ( left) and the limit of our data ( right).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1666fig3.ps} \end{figure}$	Figure 3: Temperature map and XMM isocontours in the [0.5-8.0] keV band for Abell 85. The scale for the temperature is keV.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1666fig4.ps} \end{figure}$	Figure 4: Metallicity map with XMM X-ray intensity contours in the [0.5-8.0] keV band superimposed. The scale for the metallicity is in solar units.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig5.eps} \end{figure}$	Figure 5: Gas temperature as a function of radius obtained with XMM-Newton (filled circles), Chandra (empty circles) and BeppoSax (empty squares).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig6.eps} \end{figure}$	Figure 6: Gas metallicity profile from our XMM-Newton data. For comparison we also plot the De Grandi et al. (2004) data for "cool-core'' and non "cool-core'' clusters.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig8.eps} \end{figure}$	Figure 8: Best spectral fits with residues for XMM-Newton MOS1, MOS2 and PN. Top: central region (R < 100'') fit with a cooling-flow model (CEVMKL); middle: Ring 1 fit with a VMEKAL ( 100'' < R < 250''); bottom: Ring 2 fit with a VMEKAL ( 250'' < R < 400'').
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig10.eps} \end{figure}$	Figure 10: Photon spectra for 3 individual regions. Top: the VSSRS region (2.5 arcmin radius region). Middle: the elliptical impact region. Bottom: the South Blob region (3.0 arcmin radius region). See text for region locations.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig11.eps} \end{figure}$	Figure 11: MOS1+MOS2 X-ray image with the 21 cm radio isocontours obtained by Slee et al. (2001) overlayed. The radio source seems to be anti-correlated with the west X-ray excess emission at $\alpha \sim 0^{\rm h}41^{\rm m}36^{\rm s}$ and $\delta \sim -9^\circ 22'$ approximately limited by the dashed ellipse.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig12.eps} \end{figure}$	Figure 12: Heavy element abundances relative to iron in regions Centre (filled circles), Ring 1 (empty squares), Ring 2 (filled diamonds) and South Blob (empty triangles). Various models are superimposed: SNII (full line), Hypernovae (long dashes), and SNIa WDD1 (dot-dashed), WDD2 (dotted) and W7 (spaced dots).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig13.eps} \end{figure}$	Figure 13: Emission profile of the X-ray gas obtained from the XMM-Newton MOS1 image (the profile from MOS2 is litterally indistinguishable from MOS1); three fits are superimposed: a Sérsic law, a $\beta$ -model (dashes) and a $\beta$ -model excluding the four innermost points (dot-dashes).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig14.eps} \end{figure}$	Figure 14: Top: gas mass (dotted line) and dynamical mass (solid line when including the calculation of the temperature profile, dashedline in the isothermal case) as a function of radius. The vertical dotted line indicates the limiting radius of the data. For the isothermal case, we have adopted the mean emission temperature kT = 6.5 keV. Bottom: baryon fraction in both cases.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1666fig15.eps} \end{figure}$	Figure 15: Dynamical mass density as a function of radius derived from our data (full line) and compared to a NFW model (dashed line) and to a Moore99 profile (dotted line). $\rho _{\rm dyn}\propto r^{-1.9}$ is a good fit at small radii. The two vertical dotted lines indicate the spatial resolution ( left) and the limit of our data ( right).
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