Iron and Nickel Line Diagnostics for the Galactic Center Diffuse Emission

Koyama Katsuji

Hyodo Yoshiaki

Inui Tatsuya

Nakajima Hiroshi

Matsumoto Hironori

Tsuru Takeshi Go

Takahashi Tadayuki

Maeda Yoshitomo

Yamazaki Noriko Y.

Murakami Hiroshi

Yamauchi Shigeo

Tsuboi Yohko

Senda Atsushi

Kataoka Jun

Takahashi Hiromitsu

Holt Stephen S.

Brown Gregory V.

Publications of the Astronomical Society of Japan

We have observed the diffuse X-ray emission from the Galactic Center (GC) using the X-ray Imaging Spectrometer (XIS) on Suzaku. The high-energy resolution and the low-background orbit provided excellent spectra of the GC diffuse X-rays (GCDX). The XIS found many emission lines in the GCDX near the energy of K-shell transitions of iron and nickel. The most pronounced features are Fe I Kα at 6.4 keV and K-shell absorption edge at 7.1 keV, which are from neutral and/or low ionization states of iron, and the K-shell lines at 6.7 keV and 6.9 keV from He-like (Fe XXV Kα) and hydrogenic (Fe XXVI Lyα) ions of iron. In addition, Kα lines from neutral or low ionization nickel (Ni I Kα) and He-like nickel (Ni XXVII Kα), Fe I Kβ, Fe XXV Kβ, Fe XXVI Lyβ, Fe XXV Kγ and FeXXVI Lyγ were detected for the first time. The line center energies and widths of Fe XXV Kα and Fe XXVI Lyα favor a collisional excitation plasma for the origin of the GCDX. The electron temperature determined from the line flux ratio of Fe XXV Kα/Fe XXV Kβ is similar to the ionization temperature determined from that of Fe XXV Kα/Fe XXVI Lyα. Thus it would appear that the GCDX plasma is close to ionization equilibrium. The 6.7 keV flux and temperature distribution to the galactic longitude is smooth and monotonic, in contrast to the integrated point source flux distribution. These facts support the hypothesis that the GCDX is truly diffuse emission rather than the integration of the outputs of a large number of unresolved point sources. In addition, our results demonstrate that the chemical composition of Fe in the interstellar gas near the GC is constrained to be about 3.5 times solar abundance.

Galaxy: center

ISM: abundances

ISM: dust, extinction

X-ray spectra

天文学・宇宙科学 [ 440 ]

英語

日本天文学会

Copyright (c) 2007 Astronomical Society of Japan

[ISSN] 0004-6264

[NCID] AA1082896X

[URI] http://pasj.asj.or.jp/v59/sp1/59s121/59s121a.html