2009/01/30 by Shigeo Yamauchi, Ken Ebisawa, Yasuo Tanaka +6 · 43 citations
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Emission spectrum #Flux (metallurgy) #Galactic Center #Galactic corona #Galactic halo #Galactic plane #Galaxy #Geometry #Ion #Ionization #Line (geometry) #Physics #Ridge #Spectral line #X-ray Spectroscopy and Fluorescence Analysis
paper · pdf · doi:10.1093/pasj/61.sp1.s225
published in Publications of the Astronomical Society of Japan 61(sp1), S225-S232 (Oxford University Press)
openalex publication_date 2009/01/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/23
In order to elucidate the origin of galactic ridge X-ray emission, we analyzed Suzaku data taken at various regions along the galactic plane, and studied their Fe-K emission line features. Suzaku resolved the Fe line complex into three narrow lines at ∼ 6.4 keV, ∼ 6.7 keV and ∼ 6.97 keV, which are K-lines from neutral (or low-ionized), He-like, and H-like iron respectively. The 6.7 keV line is clearly seen in all of the observed regions, and its longitudinal distribution is consistent with that determined from previous observations. The 6.4 keV emission line was also found in various galactic plane regions (b∼0∘). Differences in the flux ratios of the 6.4 keV/6.7 keV and 6.97 keV/6.7 keV lines between the galactic plane and the galactic center regions were studied and its implication was discussed.