2016/04/27 by Shigeo Yamauchi, Kumiko Nobukawa, Kumiko K. Nobukawa +3 · 39 citations
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Bulge #Emission spectrum #Equivalent width #Galactic Center #Galactic plane #Geometry #Line (geometry) #Nuclear physics #Physics #Ridge #Scale height #Spectral line #Stars #X-ray #astro-ph.HE
paper · pdf · doi:10.1093/pasj/psw057
published in Publications of the Astronomical Society of Japan 68(4) (Oxford University Press) · Accepted for publication in PASJ
arxiv created 2016/04/27 · openalex publication_date 2016/06/08 · arxiv updated 2016/06/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract This paper reports the analysis of the X-ray spectra of the Galactic diffuse X-ray emission (GDXE) in the Suzaku archive. The fluxes of the Fe i Kα (6.4 keV), Fe xxv Heα (6.7 keV), and Fe xxvi Lyα (6.97 keV) lines are separately determined. From the latitude distributions, we confirm that the GDXE is decomposed into the Galactic center (GCXE), the Galactic bulge (GBXE) and the Galactic ridge (GRXE) X-ray emissions. The scale heights (SHs) of the Fe xxv Heα line of the GCXE, GBXE, and GRXE are determined to be ∼40, ∼310, and ∼140 pc, while those of the Fe i Kα line are ∼30, ∼160, and ∼70 pc, respectively. The mean equivalent widths (EWs) of the sum of the Fe xxv Heα and Fe xxvi Lyα lines are ∼750 eV, ∼600 eV, and ∼550 eV, while those of the Fe i Kα line are ∼150 eV, ∼60 eV, and ∼100 eV for the GCXE, GBXE, and GRXE, respectively. The origin of the GBXE, GRXE, and GCXE is separately discussed based on the new results of the SHs and EWs, in comparison with those of the cataclysmic variables, active binaries and coronal active stars.