All Figures

$\begin{figure} { \psfig{file=0827fg1.eps,bbllx=40pt,bblly=30pt,bburx=482pt,bbury=470pt,width=8.5cm,clip=} } \end{figure}$ Figure 1: CFHT archival H $_{\alpha }$ image of the HoII X-1 region. The MPFS FOV and the PMAS mosaic FOV are superposed. The small black and the large red circles give the 90% confidence circles of the Chandra ACIS-S (RA: 8 $^{\rm h}$ 19 $^{\rm m}$ 29.0 $^{\rm s}$ , Dec: +70 $^{\circ }$ 42 $^{\prime }$ 19.0 $^{\prime \prime }$ ; J2000) and the ROSAT HRI positions, respectively. The small white circle shows the location of the radio peak at 6, 20, and 90 cm wavelengths (see Tongue & Westpfahl 1995). Long-slit positions (1-5) are indicated with dotted lines. The overlaid coordinate grid is given in steps of 1 $^{\rm s}$ in RA and in steps of 4 $^{\prime \prime }$ in Dec.
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In the text

$\begin{figure} \hspace*{1.0cm}\psfig{file=0827fg2.eps,width=6.5cm,clip=} \end{figure}$ Figure 2: CFHT H $\alpha , R$ , and B images of the HoII X-1 region with the marked Chandra position (a circle $1\hbox {$^{\prime \prime }$ }$ in radius) of the X-ray source. The image size is 24.5 $\hbox {$^{\prime \prime }$ }\times 14.0$ $\hbox {$^{\prime \prime }$ }$ .
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In the text

$\begin{figure} \par\psfig{file=0827fg3.ps,angle=-90,width=8.5cm,clip=} \end{figure}$ Figure 3: Surface brightness profile of the He II emission around the ULX (solid circles) together with the MPFS PSF (solid line). The error bars include both the photon noise and the error in the surface brightness determination. The He II region around the ULX is clearly extended to about 3 $^{\prime \prime }$ .
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In the text

$\begin{figure} \hspace*{0.1cm} \psfig{file=0827fg4.eps,bbllx=225pt,bblly=1pt,bburx=670pt,bbury=568pt,width=8.5cm,clip=}\par \end{figure}$ Figure 4: PMAS emission line flux maps ( upper panels), and emission line FWHM maps ( lower panels), corrected for instrumental resolution, for H $\beta$ and for [O III] $\lambda 5007$ in the HolI X-1 region. The FWHM images have been smoothed using a $3 \times 3$ pixel box. The emission line flux contour of [O III] $\lambda 5007$ is overlaid on the FHWM maps. The ACIS-S error circle of the X-ray source position is shown. The FOV of the single images is about 11 $\hbox {$^{\prime \prime }$ }\times 11.5^{\prime \prime }$ . The black color in the flux maps and in the FWHM maps mark regions with no significant line detections and unresolved lines, respectively. The white color in the same maps indicates values above the limit given in the color bars.
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In the text

$\begin{figure} \par\psfig{file=0827fg5.ps,bbllx=45pt,bblly=75pt,bburx=460pt,bbury=565pt,width=8.5cm,angle=-90,clip=} \end{figure}$ Figure 5: The co-added PMAS spectrum at the X-ray position (see Fig. 4) clearly shows an He II $\lambda 4686$ emission line.
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In the text

$\begin{figure} \par\psfig{file=0827fg6.eps,width=18.0cm,clip=} \end{figure}$ Figure 6: MPFS emission line flux, FWHM (corrected for instrumental resolution) and radial velocity maps for He II, H $\beta$ , [O III] $\lambda 4959$ and [O III] $\lambda 5007$ of the HoII X-1 region. The black color in the flux/radial velocity maps and in the FWHM maps marks regions with no significant line detection and unresolved lines, respectively. The ACIS-S error circle of the X-ray source position is marked. The FOV of the single images is about 15 $^{\prime \prime }\times 16^{\prime \prime }$ . The dotted line in each map marks the area of the H II region given by the [OIII] $\lambda 5007$ line flux larger than $\sim$ $17 \times 10^{-16}$ erg s^-1 cm^-2. The FWHM and radial velocity images have been smoothed using the mean of a $3 \times 3$ pixel box.
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In the text

$\begin{figure} \par\psfig{file=0827fg7.eps,width=8.5cm,clip=} \end{figure}$ Figure 7: Same maps as shown in Fig. 6 for H $\alpha$ and [S II] $\lambda 6717$ .
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In the text

$\begin{figure} \par {\psfig{file=0827fg8.eps,angle=-90,width=14cm,clip=} } \end{figure}$ Figure 8: The average LSS spectrum of the slit positions 2 and 3 (see Fig. 1) at the X-ray source shows, in addition to the lines found in the MPFS spectra, faint [O III] $\lambda 4363$ , He I $\lambda 4471$ and [O I] $\lambda 6364$ lines. The continuum emission seems to increase blueward of $\sim$ 5700 Å.
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In the text

$\begin{figure} \par\hspace*{2cm} \psfig{file=0827fg9.eps,width=13.0cm,clip=} \end{figure}$ Figure 9: MPFS line flux ratio maps of Ho II X-1: H $\alpha$ /H $\beta$ , [O III] $\lambda 5007$ /H $\beta$ and [S II] $\lambda 6717/$ H $\alpha$ . The [O III] $\lambda 5007$ line flux contours are overlaid.
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In the text

$\begin{figure} \hspace*{2cm} \psfig{file=0827fg10.eps,bbllx=1pt,bblly=313pt,bburx=213pt,bbury=588pt,width=4.5cm,clip=} \end{figure}$ Figure 10: Monochromatic MPFS images in He II $\lambda 4686$ smoothed with a 2 $\times$ 2 pixel kernel. The flux is given on logarithmic scale. The Chandra ACIS-S source position is overlaid. The He II image shows a second, probably extended region North-West of the X-ray source, similar to the He II emission line flux map (Fig. 6), and the line intensity plots from the long-slit spectra.
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In the text

$\begin{figure} \hspace*{1.7cm} \psfig{file=0827fg11.eps,bbllx=1pt,bblly=1pt,bburx=260pt,bbury=480pt,height=9cm,clip=} \end{figure}$ Figure 11: Isophotes of the 2d-LSS spectra at slit positions N2 and N3 in the He II $\lambda 4686$ emission line. The extended He II region coincident with the X-ray source HoII X-1 is located at an offset value of $\sim$ 14.5 $^{\prime \prime }$ . A second fainter He II region is detected in the spectrum N2 at an offset value of $\sim$ 9 $^{\prime \prime }$ in the North-West direction along the slit.
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In the text

$\begin{figure} \par\psfig{file=0827fg12.ps,width=8.5cm,angle=-90,clip=} \end{figure}$ Figure 12: Radial velocity difference derived from the HeII $\lambda 4686$ and the [O III] $\lambda 5005$ emission lines inside the He II region along the slit position for the N2 and N3. The offset (arcsec) is the same as in Fig. 11, its larger values correspond to the "heel'' of the HII region.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{0827fg13.ps}\hspace*{3mm} \includegraphics[width=6cm,height=6.3cm,clip]{0827fg14.ps} \end{figure}$ Figure 13: Left: radial profile of Holmberg II X-1 (diamonds with error bars) compared to the simulated ACIS-S PSF at 1 keV. A pixel corresponds to 0.5 $^{\prime \prime }$ . The PSF was normalized to the maximum source counts at the first annulus outside 3 $^{\prime \prime }$ (6 pixel) in radius. The counts in the radial range between $\sim$ 4-5 $^{\prime \prime }$ (5. and 6. radial bins) are marginally above the 1 keV PSF. Right: logarithmically scaled 5 ks Chandra ACIS-S image of HoII X-1 in the 0.3-8.0 keV energy band. The 5, 10, 30, 100, 300, 1000 and 3000 $\sigma$ contours above the logarithmic value of the background are shown (North is up, East is left). The FOV is about 17 $^{\prime \prime } \times 17^{\prime \prime }$ . The circles with 7 and 12 pixel radius mark the annulus with slightly larger counts than expected from to the 1 keV ACIS-S PSF.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0827fg15.eps} \end{figure}$ Figure 14: The X-ray pulse-height spectrum of XMM EPIC-PN is shown with folded models for fit (B). The lower panel shows the data/model ratios. Pulse height spectra are re-binned for display and 1 $\sigma$ error bars are attached to data points.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0827fg16.eps} \end{figure}$ Figure 15: Unfolded XMM EPIC-PN spectrum showing the best fit model (B). The thermal black body component contributes about 18% to the total 0.3-8.0 keV flux, and is clearly soft (<2 keV).
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In the text

$\begin{figure} \hspace*{1.0cm}\psfig{file=0827fg2.eps,width=6.5cm,clip=} \end{figure}$	Figure 2: CFHT H $\alpha , R$ , and B images of the HoII X-1 region with the marked Chandra position (a circle $1\hbox {$^{\prime \prime }$ }$ in radius) of the X-ray source. The image size is 24.5 $\hbox {$^{\prime \prime }$ }\times 14.0$ $\hbox {$^{\prime \prime }$ }$ .
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$\begin{figure} \par\psfig{file=0827fg3.ps,angle=-90,width=8.5cm,clip=} \end{figure}$	Figure 3: Surface brightness profile of the He II emission around the ULX (solid circles) together with the MPFS PSF (solid line). The error bars include both the photon noise and the error in the surface brightness determination. The He II region around the ULX is clearly extended to about 3 $^{\prime \prime }$ .
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$\begin{figure} \par\psfig{file=0827fg5.ps,bbllx=45pt,bblly=75pt,bburx=460pt,bbury=565pt,width=8.5cm,angle=-90,clip=} \end{figure}$	Figure 5: The co-added PMAS spectrum at the X-ray position (see Fig. 4) clearly shows an He II $\lambda 4686$ emission line.
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$\begin{figure} \par\psfig{file=0827fg7.eps,width=8.5cm,clip=} \end{figure}$	Figure 7: Same maps as shown in Fig. 6 for H $\alpha$ and [S II] $\lambda 6717$ .
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$\begin{figure} \par {\psfig{file=0827fg8.eps,angle=-90,width=14cm,clip=} } \end{figure}$	Figure 8: The average LSS spectrum of the slit positions 2 and 3 (see Fig. 1) at the X-ray source shows, in addition to the lines found in the MPFS spectra, faint [O III] $\lambda 4363$ , He I $\lambda 4471$ and [O I] $\lambda 6364$ lines. The continuum emission seems to increase blueward of $\sim$ 5700 Å.
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$\begin{figure} \par\hspace*{2cm} \psfig{file=0827fg9.eps,width=13.0cm,clip=} \end{figure}$	Figure 9: MPFS line flux ratio maps of Ho II X-1: H $\alpha$ /H $\beta$ , [O III] $\lambda 5007$ /H $\beta$ and [S II] $\lambda 6717/$ H $\alpha$ . The [O III] $\lambda 5007$ line flux contours are overlaid.
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$\begin{figure} \hspace*{2cm} \psfig{file=0827fg10.eps,bbllx=1pt,bblly=313pt,bburx=213pt,bbury=588pt,width=4.5cm,clip=} \end{figure}$	Figure 10: Monochromatic MPFS images in He II $\lambda 4686$ smoothed with a 2 $\times$ 2 pixel kernel. The flux is given on logarithmic scale. The Chandra ACIS-S source position is overlaid. The He II image shows a second, probably extended region North-West of the X-ray source, similar to the He II emission line flux map (Fig. 6), and the line intensity plots from the long-slit spectra.
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$\begin{figure} \par\psfig{file=0827fg12.ps,width=8.5cm,angle=-90,clip=} \end{figure}$	Figure 12: Radial velocity difference derived from the HeII $\lambda 4686$ and the [O III] $\lambda 5005$ emission lines inside the He II region along the slit position for the N2 and N3. The offset (arcsec) is the same as in Fig. 11, its larger values correspond to the "heel'' of the HII region.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0827fg15.eps} \end{figure}$	Figure 14: The X-ray pulse-height spectrum of XMM EPIC-PN is shown with folded models for fit (B). The lower panel shows the data/model ratios. Pulse height spectra are re-binned for display and 1 $\sigma$ error bars are attached to data points.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0827fg16.eps} \end{figure}$	Figure 15: Unfolded XMM EPIC-PN spectrum showing the best fit model (B). The thermal black body component contributes about 18% to the total 0.3-8.0 keV flux, and is clearly soft (<2 keV).
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