variable stars detected this Cepheid at $0.32^\circ$ from Sgr A$^*$. In this survey, 142 fields-of-view were captured along the Galactic plane ($|l|<10^\circ$, $b=0^\circ$) by the SIRIUS camera attached to the Infrared Survey Facility (IRSF). The monitoring started in April 2007 and continued until May 2012; the numbers of phases was typically 30. The exposure time was 8 s per visit, $\sim 6$ times shorter than that in @Matsunaga-2011. Among several classical Cepheids discovered by our group (Matsunaga [et al.]{}, in prep), the coordinates of [GCC-d]{} and its distance from the Sun places this star near the NSD. The period of [GCC-d]{}, determined in the same way as in @Matsunaga-2013, approximates those of the other three Cepheids, suggesting a similar age ($\sim 25$ Myr) based on the period-age relation [@Bono-2005]. The photometric measurements and the light curve of [GCC-d]{} are presented in Table \[tab:GCCd\] and Figure \[fig:LCs\], respectively. Barycentric Julian Date (BJD) in the Barycentric Dynamical Time standard was calculated for each $JHK_{\rm s}$ dataset [@Eastman-2010], while Modified Julian Date (MJD) is also listed to make the comparison with previous publications easier.

Also at the IRSF, we conducted additional photometry of [GCC-a]{}, -b, and -c in June 2010 and July 2012 