$V$ and $B$ was described by @Piotto02. We identified UCAC2 standards to place the NTT $R$ astrometric frame onto the ICRS frame, and then by identifying common stars in the WFPC2 and NTT frames, to place the  astrometric frame onto the ICRS frame, with an uncertainty of 0.2” (1$\sigma$). No star can be identified within 4$\sigma$ of the transient position on the NTT and WFPC2 $B$ frames, but one star in the WFPC2 $V$ frame is located 0.4” from the transient position (Fig. \[fig:optical\]). Calibrating our photometry with that in @Piotto02, we find a magnitude of $V$=21.0$\pm0.2$ for this object. Based on objects in the  image that are just barely detected in $B$, we estimate $B>22.0$. These images were probably taken during quiescence, and NGC 6440 X-2’s 57-minute orbital period indicates it will be very faint. As the ultracompact LMXB XTE J0929-314 in quiescence may have been detected with $M_V=13.2$ (D’Avanzo et al. 2009; thus it would have $V=31$ in NGC 6440), we think it unlikely that this star is the true counterpart.

Outburst and Decay
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@Li09 reported that unfiltered images were taken of NGC 6440 on July 30 and 31, 2009 with the 0.76-m Katzman Automatic Imaging Telescope 