All Figures

$\begin{figure} \par\includegraphics[width=4.6cm,clip]{6484fg1a.ps}\hspace*{2mm} ... ...1b.ps}\hspace*{2mm} \includegraphics[width=4.4cm,clip]{6484fg1c.ps}\end{figure}$ Figure 1: LOS velocities of ICPNe, Coma galaxies, and background emission galaxies in the MSIS field. Left: histogram of the LOS velocities of ICPNe in our Coma field. The thin red line shows spectra of a star as measured through the MSIS slits, giving the filter bandpass expressed in velocity. The velocities of the two supergiant galaxies NGC 4889 and NGC 4874 in the Coma core are indicated by vertical dotted lines; that of the nearer NGC 4874 is displaced from the main peak of the ICPN distribution. Center: LOS velocity histogram for the Coma galaxies in a $6' \times 6'$ field centered on the MSIS field, whose velocities would fall in the velocity window allowed by the MSIS observing technique. The galaxy redshifts are from Adami et al. (2005b). Right: LOS velocity distribution of the line emitters associated with spatially unresolved continuum sources: these are compatible with a uniform population of background objects. Thin red line as in the left panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6484fg2.eps}\end{figure}$ Figure 2: The position of our MSIS field (red circle) on the diffuse light isodensity contours drawn by Thuan & Kormendy (1977) in the Coma cluster core. The MSIS field is about 5' south of NGC 4874. The second Coma cD galaxy NGC 4889 is 7' east (to the left) of NGC 4874. The bright object north of NGC 4874 is the star which prevented Thuan & Kormendy (1977) from reliably determining the northern parts of the isodensity curves in their photographic photometry. Note the strong elongation of the distribution of ICL in the Coma cluster core. The likely orbits of NGC 4889 and NGC 4874 up to their present positions are sketched by the yellow dotted and magenta dashed lines, respectively; see Sect. 3.5.
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In the text

$\begin{figure} \setlength{\unitlength}{0.01\columnwidth} \begin{picture} (100,8... ... {\includegraphics[width=36\unitlength]{6484fg3b.ps} } \end{picture}\end{figure}$ Figure 3: The two subcluster cores around NGC 4874 and NGC 4889. Top-left: DSS image of the Coma cluster center. Bottom-left: positions of the galaxies in this region brighter than V=17; these are concentrated around NGC 4874 and NGC 4889. Right: velocity distributions for these bright galaxies that fall within a 36 square arcmin region around NGC 4874 ( top) and NGC 4889 ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6484fg4.ps}\end{figure}$ Figure 4: The ${v}_{\rm LOS}$ distributions of Coma galaxies in 4 quadrants relative to the GMP83 Coma cluster center. Given in arcsec intervals along the -RA and DEC directions, NE is [-600:0, 0:600], NW is [0:600, 0:600], SE is [-600:0, -600:0], SW is [0:600, -600:0]. In GMP83 coordinates NGC 4889 is at [-304, 22], i.e., in the NE quadrant, and NGC 4874 is at [124, -41], i.e., in the SW quadrant. The MSIS field is in the SE, at [-15, -289].
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{6484fg5.ps}\end{figure}$ Figure 5: Spatial distribution of all cluster members with available velocities. The X and Y axes denote -RA and DEC, given in arcsec relative to the GMP83 Coma cluster center, with North up and East to the left. Green circles are Coma galaxies with $6250{\rm~km~s^{-1}}< {v}_{\rm LOS} < 6850{\rm~km~s^{-1}}$ , red triangles are galaxies with $7050{\rm~km~s^{-1}}< {v}_{\rm LOS} < 8000{\rm~km~s^{-1}}$ , blue squares are galaxies with $4800{\rm~km~s^{-1}}< {v}_{\rm LOS} < 5350{\rm~km~s^{-1}}$ . The positions of NGC 4874, NGC 4889 and the MSIS field are indicated on the plot.
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In the text

$\begin{figure} \setlength{\unitlength}{0.01\columnwidth} \begin{picture} (100,8... ... {\includegraphics[width=36\unitlength]{6484fg3b.ps} } \end{picture}\end{figure}$	Figure 3: The two subcluster cores around NGC 4874 and NGC 4889. Top-left: DSS image of the Coma cluster center. Bottom-left: positions of the galaxies in this region brighter than V=17; these are concentrated around NGC 4874 and NGC 4889. Right: velocity distributions for these bright galaxies that fall within a 36 square arcmin region around NGC 4874 ( top) and NGC 4889 ( bottom).
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