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Figure 1: The spectrum of XMMU J004215.8+411924 ( top) from observation 4, with absorbed power-law fits. The spectrum obtained from the pn (black) and the MOS2 (red) detectors are shown. The source is located in a gap on the MOS1 detector. The spectrum of SWIFT J004217.4+411532 ( bottom) from observations 5 (highest observed luminosity, black) and 12 (lowest observed luminosity, red), with absorbed disc black-body fits.

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In the text

	Figure 2: The light curves of the three sources, XMMU J004215.8+411924 (red), SWIFT J004217.4+411532 (black), and M31N 2006-11a (blue). The arrows signify upper limits, the squares indicate data points where fits with spectral information were employed, and the circles correspond to luminosities estimated from spectra with model parameters fixed at expected values.
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In the text

	Figure 3: The position of XMMU J004215.8+411924 in X-rays and optical. Observation 3 with Chandra ACIS-I ( left), observation 4 with MOS2 ( middle), and the B-band image from the LGS ( right). The red circle has a radius of 2 arcsec and marks the previously identified optical counterpart to the X-ray source.
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In the text

Figure 4: The hardness ratios at the highest observed luminosities of 41 transients observed in M 31. The sources are divided into three subcategories: very soft (VS), soft (S) and hard (H). Open squares are data points from (Williams et al. 2006), while circles are data points from our analysis of transients listed in Voss & Gilfanov (2007). The three sources analysed in this paper are marked with triangles and have thick error-bars. The displayed errors correspond to 1-sigma confidence intervals.

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In the text