Structure of our Galactic Bulge from CN Measurements
  The double red clumps (DRCs) are now dominantly believed to be the strong
observational line of evidence of the so-called X-shaped Galactic bar
structures. Recently, Lee et al. reported a subtle mean \ds\ difference between
the DRCs and suggested a dichotomic picture that can be seen in globular
clusters: the faint red clump is the first generation, while the bright red
clump corresponds to the second generation (SG). They argued that the magnitude
difference between the DRCs is due to different stellar populations, and is not
due to the geometric difference between the DRCs. Our reanalysis shows that
their data do not appear to support the idea of the multiple population-induced
DRCs in our Galactic bulge. We perform fully empirical Monte Carlo simulations
and find that the shape of the \ds\ distributions is the most stringent
evidence to pursue. Our results strongly suggest that the CN distributions
toward the Galactic bulge are qualitatively consistent with the X-shaped
Galactic bulge with a minor fraction of the SG of about 2 -- 3\%.
