| Item type |
会議発表論文 / Conference Paper(1) |
| 公開日 |
2018-05-01 |
| タイトル |
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タイトル |
Herschel Observations: Constraints on Dust Attenuation and Star Formation Histories at High Redshift |
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言語 |
en |
| 言語 |
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|
言語 |
eng |
| 資源タイプ |
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資源タイプ識別子 |
http://purl.org/coar/resource_type/c_5794 |
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資源タイプ |
conference paper |
| 著者 |
Burgarella, Denis
Buat, Veronique
Gruppioni, Carlotta
Cucciati, Olga
Heinis, Sebastien
The PEP/HerMES Team
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| 著者所属（英） |
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en |
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Aix-Marseille Universite |
| 著者所属（英） |
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en |
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Aix-Marseille Universite |
| 著者所属（英） |
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en |
|
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Osservatorio Astronomico di Bologna, Instituto Nazionale di Astrofisica(INAF) |
| 著者所属（英） |
|
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en |
|
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Osservatorio Astronomico di Bologna, Instituto Nazionale di Astrofisica(INAF) |
| 著者所属（英） |
|
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en |
|
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Aix-Marseille Universite |
| 出版者 |
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出版者 |
宇宙航空研究開発機構(JAXA) |
| 出版者（英） |
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出版者 |
Japan Aerospace Exploration Agency (JAXA) |
| 書誌情報 |
宇宙航空研究開発機構特別資料
en : JAXA Special Publication: Proceedings of the SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe
巻 JAXA-SP-17-010E,
p. 53-57,
発行日 2018-03-09
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| 会議概要（会議名, 開催地, 会期, 主催者等）（英） |
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内容記述タイプ |
Other |
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内容記述 |
SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan |
| 抄録（英） |
|
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内容記述タイプ |
Other |
|
内容記述 |
SPICA is one of the key projects for the future. Not only its instrument suite will open up a discovery window but they will also allow to physically understand some of the phenomena that we still do not understand in the high-redshift universe. Using new homogeneous luminosity functions (LFs) in the Far-Ultraviolet (FUV) from VVDS and in the Far-Infrared (FIR) from Herschel/PEP and Herschel/HerMES, we studied the evolution of the dust attenuation with redshift. With this information, we are able to estimate the redshift evolution of the total (FUV + FIR) star formation rate density (SFRDTOT). Our main conclusions are that: 1) the dust attenuation AFUV is found to increase from z = 0 to z approximately 1.2 and then starts to decrease until our last data point at z = 3.6; 2) the estimated SFRD confirms published results to z approximately 2. At z greater than 2, we observe either a plateau or a small increase up to z approximately 3 and then a likely decrease up to z = 3.6; 3) the peak of AFUV is delayed with respect to the plateau of SFRDTOT but the origin of this delay is not understood yet, and SPICA instruments will provide clues to move further in the physical understanding of this delay but also on the detection and redshift measurements of galaxies at higher redshifts. This work is further detailed in Burgarella et al. (2013). |
| 内容記述 |
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内容記述タイプ |
Other |
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内容記述 |
形態: カラー図版あり |
| 内容記述（英） |
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内容記述タイプ |
Other |
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内容記述 |
Physical characteristics: Original contains color illustrations |
| ISSNONLINE |
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収録物識別子タイプ |
ISSN |
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収録物識別子 |
2433-2232 |
| 資料番号 |
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内容記述タイプ |
Other |
|
内容記述 |
資料番号: AA1730027010 |
| レポート番号 |
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内容記述タイプ |
Other |
|
内容記述 |
レポート番号: JAXA-SP-17-010E |
AA1730027010.pdf (411.0 kB)
