  With the XMM-Newton and Suzaku observations, for the first time, we acquired
broad-band spectra of two unidentified X-ray sources towards the Galactic
bulge: 1RXS J180556.1$-$343818 and 1RXS J173905.2$-$392615. The 1RXS
J180556.1$-$343818 spectrum in the $0.3$-$7$ keV band was explained by X-ray
emission originated from an optically-thin thermal plasma with temperatures of
$0.5$ and $1.7$ keV. The estimated absorption column density of $N_{\rm H} \sim
4 \times 10^{20}$ cm$^{-2}$ was significantly smaller than the Galactic HI
column density towards the source. A candidate of its optical counterpart, HD
321269, was found within $4''$. In terms of the X-ray properties and the
positional coincidence, it is quite conceivable that 1RXS J180556.1$-$343818 is
an active G giant. We also found a dim X-ray source that was positionally
consistent with 1RXS J173905.2$-$392615. Assuming that the X-ray spectrum can
be reproduced with an absorbed optically-thin thermal plasma model with $kT =
1.6$ keV, the X-ray flux in the $0.5$-$8$ keV band was $8.7 \times 10^{-14}$
erg s$^{-1}$ cm$^{-2}$, fainter by a factor of $\sim 7$ than that of 1RXS
J173905.2$-$392615 during the ROSAT observation. The follow-up observations we
conducted revealed that these two sources would belong to the Galactic disk,
rather than the Galactic bulge.
