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Suzaku observations of early-type galaxies

Published online by Cambridge University Press:  21 October 2010

K. Matsushita ,
Y. Fukazawa ,
K. Hayashi ,
S. Konami ,
R. Nagino ,
T. Ohashi ,
Y. Tawara  and
M. Tozuka
K. Matsushita
Affiliation:
Department of Physics, Tokyo University of Science, 1-3 Kagurazaka, Shinjyuku-ku, Tokyo 162-8601, Japan, email: matusita@rs.kagu.tus.ac.jp
Y. Fukazawa
Affiliation:
Department of Physical Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
K. Hayashi
Affiliation:
Department of Physical Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
S. Konami
Affiliation:
Department of Physics, Tokyo University of Science, 1-3 Kagurazaka, Shinjyuku-ku, Tokyo 162-8601, Japan, email: matusita@rs.kagu.tus.ac.jp
R. Nagino
Affiliation:
Department of Physics, Tokyo University of Science, 1-3 Kagurazaka, Shinjyuku-ku, Tokyo 162-8601, Japan, email: matusita@rs.kagu.tus.ac.jp
T. Ohashi
Affiliation:
Department of Physics, Tokyo Metropolitan University, 1-1 Minami-Osawa, Hachioji, Tokyo 192-0397, Japan
Y. Tawara
Affiliation:
Department of Physics, Nagoya University, Nagoya, Japan
M. Tozuka
Affiliation:
Department of Physics, Tokyo University of Science, 1-3 Kagurazaka, Shinjyuku-ku, Tokyo 162-8601, Japan, email: matusita@rs.kagu.tus.ac.jp
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The metal abundances in the hot X-ray emitting interstellar medium (ISM) of early-type galaxies give us important information about the present metal supply into the ISM through supernovae (SNe) Ia and stellar mass loss. In addition, O and Mg abundances should reflect the stellar metallicity and enable us to directly look into the formation history of these galaxies. The XIS instrument onboard the Suzaku satellite has an improved line spread function due to a very small low-pulse-height tail below 1 keV coupled with a very low background.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 274
Copyright
Copyright © International Astronomical Union 2010

References

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