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Table 2

Summary of the sources detected by XMM-Newton.

Src UVW1 UVW2 UVM2 U B V Poss. ident.
mag mag mag mag mag mag

X1 x x x x x x 1RXS J150841.2-621006
X2 x x x x x x 1RXS J150841.2-621006
GSC2.3 S7QP006140
GSC2.3 S7QP006099
X3 12.4082 ± 0.0003 14.22 ± 0.02 13.942 ± 0.003 11.96 ± 0.01 ± 11.39 ± 0.03 TYC 9024.1705.1
X4 x x x x x x TYC 9024.1615.1
X5 20.7 ± 0.2 18.8 ± 0.1 GSC2.3 S7QP084521
X6 21.4 ± 0.6 20.2 ± 0.1 18.5 ± 0.1 GSC2.3 S7QP035739
X7 19.67 ± 0.09 17.92 ± 0.06 GSC2.3 S7QP002061

src UVW1 UVM2 UVW2 U B V poss. ident.
mag mag mag mag mag mag

X8 x x x x x x GSC2.3 S7QP007261
X9 x x x x x x GSC2.3 S7QP084895

Notes. The brightness detected with the optical monitor (OM) is given when the source was in the field of view of this detector and bright enough for a detection. x marks the sources that are outside of the FoV of the OM detector. For source 1 only the probable identification 1RXS J150841.2-621006 (Voges et al. 2000) is mentioned (the possible identification with the ROSAT source is underlined by the flux of CXOU J150850.6-621018/XMMU J150851.1-621017 and its spectral shape). The Tycho-2 catalog (Hog et al. 2000) and the second-generation guide star catalog (Lasker et al. 2008) have been inspected when searching for possible counterparts. The search for reasonable counterparts included not only the three standard deviations uncertainty in the X-ray position (which is determined with a PSF fit), but also the extension of the source. Considering the systematics (Harris et al. 1998), X2 is spatially also compatible with the ROSAT source 1RXS J150841.2-621006.

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