Number Density Distribution of Near-Infrared Sources on a Sub-Degree Scale in the Galactic Center: Comparison with the Fe XXV Ka Line at 6.7 keV (1510.06832v2)

Abstract: The stellar distribution derived from an $H$ and $K_{\mathrm S}$-band survey of the central region of our Galaxy is compared with the Fe XXV K$\alpha$ (6.7 keV) line intensity observed with the Suzaku satellite. The survey is for the Galactic coordinates $|l| \lesssim 3^{\circ}.0$ and $|b| \lesssim 1^{\circ}.0$ (equivalent to 0.8 kpc $\times$ 0.3 kpc for $R_0 = 8$ kpc), and the number-density distribution $N(K_{\mathrm S,0}; l, b)$ of stars is derived using the extinction-corrected magnitude $K_{\mathrm S,0}=10.5$. This is deep enough to probe the old red giant population and in turn to estimate the ($l$, $b$) distribution of faint X-ray point sources such as coronally active binaries and cataclysmic variables. In the Galactic plane ($b=0^{\circ}$), $N(10.5; l, b)$ increases to the Galactic center as $|l|^{-0.30 \pm 0.03}$ in the range of $-0^{\circ}.1 \geq l \geq -0^{\circ}.7$, but this increase is significantly slower than the increase ($|l|^{-0.44 \pm 0.02}$ ) of the Fe XXV K$\alpha$ line intensity. If normalized with the ratios in the outer region $1^{\circ}.5 \leq |l| \leq 2^{\circ}.8$, where faint X-ray point sources are argued to dominate the diffuse Galactic X-ray ridge emission, the excess of the Fe XXV K$\alpha$ line intensity over the stellar number density is at least a factor of two at $|l| = 0^{\circ}.1$. This indicates that a significant part of the Galactic center diffuse emission arises from a truly diffuse optically-thin thermal plasma, and not from an unresolved collection of faint X-ray point sources related to the old stellar population.