| Item type |
紀要論文 / Departmental Bulletin Paper(1) |
| 公開日 |
2015-03-26 |
| タイトル |
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タイトル |
Chemical Evolution and Far-Infrared Emission of Galaxies |
|
言語 |
en |
| 言語 |
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言語 |
jpn |
| 資源タイプ |
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資源タイプ識別子 |
http://purl.org/coar/resource_type/c_6501 |
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資源タイプ |
departmental bulletin paper |
| 著者 |
HIRASHITA, Hiroyuki
INOUE, Akio K.
KAMAYA, Hideyuki
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| 著者所属（英） |
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en |
|
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Department of Astronomy, Faculty of Science, Kyoto University |
| 著者所属（英） |
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en |
|
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Department of Astronomy, Faculty of Science, Kyoto University |
| 著者所属（英） |
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en |
|
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Department of Astronomy, Faculty of Science, Kyoto University |
| 出版者 |
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出版者 |
宇宙科学研究所 |
| 出版者（英） |
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出版者 |
Institute of Space and Astronautical Science |
| 書誌情報 |
en : The Institute of Space and Astronautical Science report. S.P. : Mid- and Far-Infrared Astronomy and Future Space Mission
巻 14,
p. 115-122,
発行日 2000-12
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| 抄録（英） |
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内容記述タイプ |
Other |
|
内容記述 |
Infrared (IR) dust emission from galaxies is frequently used as an indicator of starformation rate (SFR). However, the effect of dust-to-gas ratio, or amount of dust, on the con-version law from IR luminosity to SFR has not been considered. In this paper, we present aconvenient formula including the effect. In order to obtain the dependence of the dust-to-gasratio, we extend the formula derived in our previous paper, in which a theoretical formula con-verting IR luminosity to SFR was derived. That formula was expressed as SFR=(M yr-1) ={3.3 ×10-10(1-η)/(0.4 - 0.2f + 0.6ε)}(LIR=L), where f is the fraction of ionizing photons ab-sorbed by hydrogen, εis the effciency of dust absorption for nonionizing photons, ηis the cirrusfraction of observed dust luminosity, and LIR is the observed luminosity of dust emission in the8-1000-μm range. Throughout the current discussion, we construct an algorithm to relate f andε, both of which depend on the dust-to-gas ratio, to the metallicity, by adopting a galactic relationbetween dust-to-gas ratio and metallicity. Thus, we estimate the metallicity dependence of ourformula. We apply the result to the cosmic star formation history and find that the comoving SFRat z ～ 3 calculated from previous empirical formulae is underestimated by the factor of 4. Finally,we comment on the HII/L2 mission (SPICA). |
| ISSN |
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収録物識別子タイプ |
ISSN |
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収録物識別子 |
0288-433X |
| 書誌レコードID |
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収録物識別子タイプ |
NCID |
|
収録物識別子 |
AA10455137 |
| 資料番号 |
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内容記述タイプ |
Other |
|
内容記述 |
資料番号: SA4588073000 |
SA4588073.pdf (235.3 kB)
