2008/11/12 by Hiroshi Nakajima, Takeshi Go Tsuru, Masayoshi Nobukawa +5 · 24 citations
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Doubly ionized oxygen #Emission spectrum #Equivalent width #Galactic Center #Galaxy #Ion #Ionization #K-alpha #Line (geometry) #Milky Way #Optics #Physics #Planetary nebula #Reflection (computer programming) #Reflection nebula #Sagittarius #Sagittarius A* #Spectral line #Stars #X-ray #astro-ph
paper · pdf · doi:10.1093/pasj/61.sp1.s233
published in Publications of the Astronomical Society of Japan 61(sp1), S233-S240 (Oxford University Press) · Accepted for publication in PASJ
arxiv created 2008/11/12 · openalex publication_date 2009/01/30 · arxiv updated 2016/06/08 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract This paper reports on the first results of a Suzaku observation in the Sgr C region. We detected four diffuse clumps with strong line emission at 6.4 keV, Kα from neutral or low-ionized Fe. One of them, M359.38-0.00, was newly discovered with Suzaku. The X-ray spectra of the two bright clumps, M359.43-0.07 and M359.47-0.15, after subtracting the galactic center diffuse X-ray emission (GCDX), exhibit a strong Kα line from Fe i with large equivalent widths (EWs) of 2.0–2.2 keV and a clear Kβ of Fe i. The GCDX in the Sgr C region is composed of the 6.4 keV- and 6.7 keV-associated components. These were phenomenologically decomposed by taking relations between the EWs of the 6.4 keV and 6.7 keV lines. Then, the former EWs against the associated continuum in bright clump regions were estimated to be 2.4+2.3-0.7keV. Since the two different approaches give similar large EWs of 2 keV, we strongly suggest that the 6.4 keV clumps in the Sgr C region are due to X-ray reflection/fluorescence (the X-ray reflection nebulae).