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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{aa3060TEST.eps} \end{figure}$ Figure 1: a) and b) ( left and centre panels): the soft band (0.5-2 keV) XMM-Newton X-ray image centred on KUG 0214-057. Data shown is for the 3 EPIC cameras combined in both colour and contour representations. The circles, plotted with nominal 5 arcsec radius, mark the 5 sources discussed in the text, labelled with source identifiers as in Table 1. Note that source E is strongly saturated in the image shown in a). The location of the nucleus of KUG 0214-057 is marked with a diamond in each panel. The X-ray image has been smoothed with a Gaussian with $\sigma =5$ arcsec. c) ( right-hand panel): optical R-band image of region containing KUG 0214-057 obtained with Subaru SuprimeCam. The smaller galaxy to the E is APMUKS(BJ) B021449.37-054240.9; the nebulosity discussed in the text is the faint feature to the SE marked with an arrow. Each panel has dimensions $\sim$ $3 \times 3$ arcmin.
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In the text

$\begin{figure} \par\includegraphics[height=5.5cm]{3060fig2a.eps}\includegraphics... ...=5.5cm]{3060fig2d.eps}\includegraphics[height=5.5cm]{3060fig2e.eps} \end{figure}$ Figure 2: Optical B-band ( top row) and R-band ( bottom row) finding charts for the four ULX candidate X-ray sources (A, B, C, D from left to right) and the background AGN (E). The finding charts are based on the Subaru SuprimeCam SXDS imaging. X-ray error-circles, plotted with nominal 5 arcsec radius, are shown in green. Note that the two right hand images are displayed with different colour table to enhance the visibility of faint objects.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{3060fig3.eps} \end{figure}$ Figure 3: X-ray colour-colour plots for the five X-ray sources: the four ULX candidates (red points and error bars) and the source identified with an AGN (E; blue square, error bars are $\sim$ 2 times smaller than the symbol plotted). The background grey-scale shows the density of colour values for $\sim$ 500 SXDS X-ray sources with relatively low errors in the X-ray colour. Left: HR2 vs. HR1; right: HR3 vs. HR2. The HR values are defined as follows: $\rm HR1 = (B-A)/(A+B)$ ; $\rm HR2 = (C-B)/(B+C)$ ; $\rm HR3 = (D-C)/(C+D)$ where A = $C_{\rm X}(0.3{-}0.5$ keV); B = $C_{\rm X}(0.5{-}2$ keV); C = $C_{\rm X}(2{-}4.5$ keV) and D = $C_{\rm X}(4.5{-}10$ keV) and the $C_{\rm X}$ values are the vignetting-corrected EPIC count rates. The grid overlaid on each panel corresponds to the hardness ratios for power law spectra with indexes $\Gamma = [1, 2, 3]$ ( top to bottom) and $N_{\rm H} = [10^{20}, 10^{21}, 10^{22}, 10^{23}]\rm\ cm^{-2}$ ( left to right).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3060fig4.eps} \end{figure}$ Figure 4: FOCAS optical spectrum of brightest knot in nebulosity within error-circle of source B (see Fig. 2). The bright emission lines are identified as H $\alpha$ (+ [NII]), [OIII] $\lambda 4959, 5007~$ Å, H $\beta$ , [SII] $\lambda~6716, 6731~$ Å and [SIII] $\lambda 9069~$ Å at z=0.018.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3060fig4.eps} \end{figure}$	Figure 4: FOCAS optical spectrum of brightest knot in nebulosity within error-circle of source B (see Fig. 2). The bright emission lines are identified as H $\alpha$ (+ [NII]), [OIII] $\lambda 4959, 5007~$ Å, H $\beta$ , [SII] $\lambda~6716, 6731~$ Å and [SIII] $\lambda 9069~$ Å at z=0.018.
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