All Figures

$\begin{figure} \par\includegraphics[width=5.9cm,clip]{f1a.ps}\includegraphics[width=5.9cm,clip]{f1b.ps}\includegraphics[width=5.9cm,clip]{f1c.ps} \end{figure}$ Figure 1: Left panel. Identification of the previously reported features of M 86 on the smallest scale of the wavelet decomposition of the image in the 0.5-2 keV band. Middle panel. Wavelet-decomposed image of M 86 with contours indicating the selection of regions for the spectral analysis. Black contours denote the regions excluded from the analysis due to either low statistics or a presence of the point source. Numbers on the figure indicate the approximate location of the larger zones, reported in Table 1. Right panel. Hardness ratio map with surface brightness contours overlaid. Dark grey color corresponds to temperature of 1.1-1.2 keV, grey to 0.9-1 keV, light grey to 0.7-0.9 keV, white to 0.5-0.7 keV.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.cm,clip]{f2a.ps} \end{figure}$ Figure 2: Fe abundance map, overlaid with surface brightness contours. From left to right the panels show the best-fit values, low and upper limit on Fe abundance, ranging from 0 (light grey) to 0.7 (black) of solar.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.cm,clip]{f2b.ps} \end{figure}$ Figure 3: Temperature map, overlaid with surface brightness contours. From left to right the panels show the best-fit values, low and upper limit on temperature, ranging from 0.6 (light grey) to 1.2 (dark grey) keV.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.cm,clip]{f2c.ps} \end{figure}$ Figure 4: Pressure map, overlaid with surface brightness contours. From left to right the panels show the best-fit values, low and upper limit on pressure, ranging from $2\times 10^{-12}$ ergs cm^-3 (light grey) to $2\times 10^{-11}$ ergs cm^-3 (black).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.cm,clip]{f2d.ps} \end{figure}$ Figure 5: Entropy map, overlaid with surface brightness contours. From left to right the panels show the best-fit values, low and upper limit on entropy, ranging from 8 keV cm² (white) to 100 keV cm² (black).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{f3.ps} \par\end{figure}$ Figure 6: Pressure vs. entropy for all the regions in M 86. Only the points with significance greater than 4 sigma are shown. Open circles and filled triangles denote the points with high and low Fe abundance, respectively. Light gray lines show isotherms and a dark-gray line shows the shock adiabat of Mach number of 1.4. Dotted line shows the prediction on imposing an additional pressure of $4\times 10^{-12}$ ergs cm^-3 to an initially isothermal gas with kT=0.67 keV. Filled diamond displays the characteristics of the projected component found in the east to M 86.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{f4.ps} \end{figure}$ Figure 7: Image of M 86. Black contours indicate shocked region, while white contours indicate the preshock regions of the same entropy and similarly high metallicity.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=4.cm,clip]{f5.ps} \end{figure}$ Figure 8: Schematic view of the crossing of M 86 by the plane of the shock wave. Direction of motion of M 86 galaxy relative to the observer is indicated by a slight replacement of M 86 galaxy (filled circle) relative to the group (open circle).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{f6.ps} \end{figure}$ Figure 9: Image of the intensity of the power law component per unit extraction area in the X-ray spectra of M 86. Contours indicate the surface brightness in the infrared, derived from DSS-2 data. Gray ellipse indicates the region selected for a detailed spectral analysis, presented in Fig.10.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{f7.ps}\par \end{figure}$ Figure 10: Spectrum of the M 86 zone with enhanced hard emission. Grey crosses indicate the data points, solid line shows the combined model, consisting of normal component (dotted), hotter component (long-dashed) and a power-law (short-dashed).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[bb=79 43 570 760,height=5.8cm,angle=-90,clip... ... 43 570 760,height=5.8cm,angle=-90,clip]{f8p14.ps}\hspace*{3.4cm}}\end{figure}$ Figure 11: Spectra of 14 major zones of the M 86, in correspondence with Table 1. Spectra are assembled in rows with increasing number from left to right and from up to down.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{f9.ps} \end{figure}$ Figure 12: Large-scale structure around M 86. The wavelet-reconstructed image reproduces a part of ROSAT All-Sky Survey in the 0.5-2 keV energy band, close to M 86. Black squares indicate the galaxies falling onto Virgo from behind ( $V_{\rm M~87}-V_{\rm galaxy} > 600$ km s^-1), using the galaxy velocity data from Bingelli et al. (1985, 1993). Large rectangular region denotes the position of the excess X-ray emission identified in Böhringer et al. (1994).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.cm,clip]{f2a.ps} \end{figure}$	Figure 2: Fe abundance map, overlaid with surface brightness contours. From left to right the panels show the best-fit values, low and upper limit on Fe abundance, ranging from 0 (light grey) to 0.7 (black) of solar.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17.cm,clip]{f2b.ps} \end{figure}$	Figure 3: Temperature map, overlaid with surface brightness contours. From left to right the panels show the best-fit values, low and upper limit on temperature, ranging from 0.6 (light grey) to 1.2 (dark grey) keV.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17.cm,clip]{f2c.ps} \end{figure}$	Figure 4: Pressure map, overlaid with surface brightness contours. From left to right the panels show the best-fit values, low and upper limit on pressure, ranging from $2\times 10^{-12}$ ergs cm^-3 (light grey) to $2\times 10^{-11}$ ergs cm^-3 (black).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17.cm,clip]{f2d.ps} \end{figure}$	Figure 5: Entropy map, overlaid with surface brightness contours. From left to right the panels show the best-fit values, low and upper limit on entropy, ranging from 8 keV cm² (white) to 100 keV cm² (black).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{f4.ps} \end{figure}$	Figure 7: Image of M 86. Black contours indicate shocked region, while white contours indicate the preshock regions of the same entropy and similarly high metallicity.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=4.cm,clip]{f5.ps} \end{figure}$	Figure 8: Schematic view of the crossing of M 86 by the plane of the shock wave. Direction of motion of M 86 galaxy relative to the observer is indicated by a slight replacement of M 86 galaxy (filled circle) relative to the group (open circle).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{f6.ps} \end{figure}$	Figure 9: Image of the intensity of the power law component per unit extraction area in the X-ray spectra of M 86. Contours indicate the surface brightness in the infrared, derived from DSS-2 data. Gray ellipse indicates the region selected for a detailed spectral analysis, presented in Fig.10.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{f7.ps}\par \end{figure}$	Figure 10: Spectrum of the M 86 zone with enhanced hard emission. Grey crosses indicate the data points, solid line shows the combined model, consisting of normal component (dotted), hotter component (long-dashed) and a power-law (short-dashed).
Open with DEXTER

$\begin{figure} \par\includegraphics[bb=79 43 570 760,height=5.8cm,angle=-90,clip... ... 43 570 760,height=5.8cm,angle=-90,clip]{f8p14.ps}\hspace*{3.4cm}}\end{figure}$	Figure 11: Spectra of 14 major zones of the M 86, in correspondence with Table 1. Spectra are assembled in rows with increasing number from left to right and from up to down.
Open with DEXTER