TERRAPUB Earth, Planets and Space

Earth Planets Space, Vol. 65 (No. 3), pp. 203-211, 2013

Star formation and dust extinction properties of local galaxies as seen from AKARI and GALEX

A. Sakurai1, T. T. Takeuchi1, F.-T. Yuan1, V. Buat2, and D. Burgarella2

1Division of Particle and Astrophysical Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan
2Laboratoire d'Astrophysique de Marseille, OAMP, Université Aix-Marseille, CNRS, 38 rue Frédéric Joliot-Curie, 13388 Marseille cedex 13, France

(Received November 7, 2011; Revised September 19, 2012; Accepted September 20, 2012; Online published March 12, 2013)

Abstract: An accurate estimation of the star formation-related properties of galaxies is crucial for understanding the evolution of galaxies. In galaxies, ultraviolet (UV) light emitted by recently formed massive stars is attenuated by dust, which is also produced by star formation (SF) activity, and is re-emitted at mid- and far- infrared (IR) wavelengths. In this study, we investigate the star formation rate (SFR) and dust extinction using UV and IR data. We selected local galaxies which are detected at AKARI FIS 90 μm and matched the IRAS IIFSCz 60 μm select catalog. We measured FUV and NUV flux densities from GALEX images. We examined the SF and extinction of Local galaxies using four bands of AKARI. Then, we calculated FUV and total IR luminosities, and obtained the SF luminosity, LLF, the total luminosity related to star formation activity, and the SFR. We find that in most galaxies, LLF is dominated by Ldust. We also find that galaxies with higher SF activity have a higher fraction of their SF hidden by dust. In fact, the SF of galaxies with SFRs > 20 M-1 is almost completely hidden by dust. Our results boast a significantly higher precision with respect to previously published works, due to the use of much larger object samples from the AKARI and GALEX all sky surveys.
Key words: Dust, galaxies: formation, galaxies: evolution, stars: formation, infrared, ultraviolet.

Corresponding author E-mail: sakurai.akane@e.mbox.nagoya-u.ac.jp

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