Abstract
We present the results of X-ray and Near-Infrared observations of the Galactic Ridge X-ray Emission (GRXE). We extracted 2,002 X-ray point sources in the <em>Chandra</em> Bulge Field (l =0°.113, b = 1°.424) down to ~10<sup>-14.8</sup> ergscm<sup>-2</sup>s<sup>-1</sup> in 2-8 keV band with the longest observation (900 ks) of the GRXE. Based on X-ray brightness and hardness, we classied the X-ray point sources into three groups: A (hard), B (soft and broad spectrum), and C (soft and peaked spectrum). In order to know populations of the X-ray point sources, we carried out NIR imaging and spectroscopy observation. We identied 11% of X-ray point sources with NIR and extracted NIR spectra for some of them. Based on X-ray and NIR properties, we concluded that non-thermal sources in the group A are mostly active galactic nuclei and the thermal sources are mostly white dwarf binaries such as cataclysmic variables (CVs) and Pre-CVs. We concluded that the group B and C sources are X-ray active stars in flare and quiescence, respectively.
Highlights
Since the dawn of the X-ray astronomy, an apparently diffuse emission of low surface brightness has been known to exist along the Galactic Plane (GP; |l|
What are the populations of the dim X-ray point sources? Which class of sources contribute to the Fe K emission line? We do not know the population of majority of the dim point sources due to a limited number of X-ray photons
We retrieved 10 archived data of the CBF taken with the Advanced CCD Imaging Spectrometer (ACIS)-I array on board Chandra with a total exposure time of ∼900 ks
Summary
Since the dawn of the X-ray astronomy, an apparently diffuse emission of low surface brightness has been known to exist along the Galactic Plane (GP; |l|
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