An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z=3.717 "Passive" System, ZF 20115
文献类型：期刊论文
| 作者 | Simpson, J. M.1; Smail, Ian2; Wang, Wei-Hao1; Riechers, D.3; Dunlop, J. S.4; Ao, Y.5; Bourne, N.4; Bunker, A.6; Chapman, S. C.7; Chen, Chian-Chou8 |
| 刊名 | ASTROPHYSICAL JOURNAL LETTERS
 |
| 出版日期 | 2017-07-20 |
| 卷号 | 844期号:1页码:5 |
| ISSN号 | 2041-8205 |
| 关键词 | galaxies: high-redshift galaxies: starburst |
| DOI | 10.3847/2041-8213/aa7cf2 |
| 通讯作者 | Simpson, J. M.(jsimpson@asiaa.sinica.edu.tw) |
| 英文摘要 | The identification of high-redshift, massive galaxies with old stellar populations may pose challenges to some models of galaxy formation. However, to securely classify a galaxy as quiescent, it is necessary to exclude significant ongoing star formation, something that can be challenging to achieve at high redshifts. In this Letter, we analyze deep ALMA/870 mu m and SCUBA-2/450 mu m imaging of the claimed "post-starburst" galaxy ZF 20115 at z = 3.717 that exhibits a strong Balmer break and absorption lines. The rest-frame far-infrared imaging identifies a luminous starburst 0.'' 4 +/- 0.'' 1 (similar to 3 kpc in projection) from the position of the ultraviolet/optical emission and is consistent with lying at the redshift of ZF 20115. The star-forming component, with an obscured star formation rate of 100(-70)(+15) M-circle dot yr(-1), is undetected in the rest-frame ultraviolet but contributes significantly to the lower angular resolution photometry at rest-frame wavelengths greater than or similar to 3500 angstrom. This contribution from the obscured starburst, especially in the Spitzer/IRAC wavebands, significantly complicates the determination of a reliable stellar mass for the ZF 20015 system, and we conclude that this source does not pose a challenge to current models of galaxy formation. The multi-wavelength observations of ZF 20115 unveil a complex system with an intricate and spatially varying star formation history. ZF 20115 demonstrates that understanding high-redshift obscured starbursts will only be possible with multi-wavelength studies that include high-resolution observations, available with the James Webb Space Telescope, at mid-infrared wavelengths. |
| WOS关键词 | DEEP FIELD SOUTH ; ALMA SURVEY ; REDSHIFT DISTRIBUTION ; QUIESCENT GALAXIES ; MASSIVE GALAXIES ; STELLAR ; ULTRAVIOLET ; EVOLUTION ; CONSTRAINTS ; STARBURST |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| 出版者 | IOP PUBLISHING LTD |
| WOS记录号 | WOS:000406027700003 |
| 源URL | [http://libir.pmo.ac.cn/handle/332002/22883]  |
| 专题 | 中国科学院紫金山天文台 |
| 通讯作者 | Simpson, J. M. |
| 作者单位 | 1.Acad Sinica, Inst Astron & Astrophys, 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan 2.Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England 3.Cornell Univ, Dept Astron, 220 Space Sci Bldg, Ithaca, NY 14853 USA 4.Univ Edinburgh, Inst Astron, Royal Observ, Blackford HIll, Edinburgh EH9 3HJ, Midlothian, Scotland 5.NAOJ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan 6.Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England 7.Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada 8.European Southern Observ, Karl Schwarzschild Str 2, Garching, Germany 9.IAC, E-38205 Tenerife, Spain 10.Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain |
| 推荐引用方式 GB/T 7714 | Simpson, J. M.,Smail, Ian,Wang, Wei-Hao,et al. An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z=3.717 "Passive" System, ZF 20115[J]. ASTROPHYSICAL JOURNAL LETTERS,2017,844(1):5. |
| APA | Simpson, J. M..,Smail, Ian.,Wang, Wei-Hao.,Riechers, D..,Dunlop, J. S..,...&Zheng, X. Z..(2017).An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z=3.717 "Passive" System, ZF 20115.ASTROPHYSICAL JOURNAL LETTERS,844(1),5. |
| MLA | Simpson, J. M.,et al."An Imperfectly Passive Nature: Bright Submillimeter Emission from Dust-obscured Star Formation in the z=3.717 "Passive" System, ZF 20115".ASTROPHYSICAL JOURNAL LETTERS 844.1(2017):5. |
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