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CO (7-6), [C I] 370 mu m, and [N II] 205 mu m Line Emission of the QSO BRI1335-0417 at Redshift 4.407
Lu, Nanyao1,2; Cao, Tianwen1,2,3; Diaz-Santos, Tanio4; Zhao YH(赵应和)5,6,7; Privon, George C.8,9,10; Cheng, Cheng1,2,11; Gao, Yu12; Xu, C. Kevin1,2; Charmandaris, Vassilis13,14; Rigopoulou, Dimitra15; van der Werf, Paul P.16; Huang, Jiasheng1,2; Wang, Zhong1,2; Evans, Aaron S.17,18; Sanders, David B.19
发表期刊ASTROPHYSICAL JOURNAL
2018-09-01
卷号864期号:1页码:12
DOI10.3847/1538-4357/aad3c9
产权排序第5完成单位
收录类别SCI
关键词galaxies: active galaxies: ISM galaxies: star formation infrared: galaxies ISM: molecules submillimeter: galaxies
摘要

We present the results from our Atacama Large Millimeter/submillimeter Array (ALMA) imaging observations of the CO(7-6), [C I] 370 mu m (hereafter [C I]), and [N II] 205 mu m (hereafter [N II]) lines and their underlying continuum emission of BRI 1335-0417, an infrared bright quasar at z = 4.407. At the achieved resolutions of similar to 1.'' 1 to 1.'' 2 (or 7.5-8.2 kpc), the continuum at 205 and 372 mu m (rest frame), the CO(7-6), and the [C I] emissions are at best barely resolved whereas the [N II] emission is well resolved with a beam-deconvolved major axis of 1.'' 3 (+/- 0.'' 3) or 9(+/- 2) kpc. As a warm dense gas tracer, the CO(7-6) emission shows a more compact spatial distribution and a significantly higher peak velocity dispersion than the other two lines that probe lower density gas, a picture favoring a merger-triggered star formation (SF) scenario over an orderly rotating SF disk. The CO(7 -6) data also indicate a possible QSO-driven gas outflow that reaches a maximum line-of-sight velocity of 500-600 km s(-1). The far-infrared (FIR) dust temperature (T-dust) of 41.5 K from a graybody fit to the continuum agrees well with the average T-dust inferred from various line luminosity ratios. The resulting LCO(7-6)/L-FIR luminosity ratio is consistent with that of local luminous infrared galaxies powered predominantly by SF. The LCO(7-6)-inferred SF rate is 5.1(+/- 1.5) x 10(3) M-circle dot yr(-1). The system has an effective star-forming region of 1.7(-0.8)(+1.7) kpc in diameter and a molecular gas reservoir of similar to 5 x 10(11) M-circle dot.

资助项目National Key R&D Program of China[2017YFA0402704] ; NSFC[11673028] ; Chinese Academy of Sciences (CAS) ; CAS through the CASSACA postdoc and visiting scholarship
项目资助者National Key R&D Program of China[2017YFA0402704] ; NSFC[11673028] ; Chinese Academy of Sciences (CAS) ; CAS through the CASSACA postdoc and visiting scholarship
语种英语
学科领域天文学
学科门类理学 ; 理学::天文学
文章类型Article
出版者IOP PUBLISHING LTD
出版地TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS记录号WOS:000443165600011
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]ULTRALUMINOUS INFRARED GALAXIES ; STAR-FORMING GALAXIES ; MOLECULAR GAS ; SUBMILLIMETER GALAXIES ; ABSORPTION SYSTEMS ; EARLY UNIVERSE ; MAJOR MERGERS ; ATOMIC CARBON ; BRI 1202-0725 ; BLACK-HOLE
引用统计
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/17892
专题丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
通讯作者Lu, Nanyao
作者单位1.National Astronomical Observatories, Chinese Academy of Sciences (CAS), Beijing 100012, People's Republic of China
2.China-Chile Joint Center for Astronomy, Camino El Observatorio 1515, Las Condes, Santiago, Chile
3.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, People's Republic of China
4.Nucleo de Astronomia de la Facultad de Ingenieria, Universidad Diego Portales, Av. Ejercito Libertador 441, Santiago, Chile
5.Yunnan Observatories, Chinese Academy of Sciences, Kun-ming 650011, People's Republic of China
6.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, People's Republic of China
7.Center for Astronomical Mega-Science, CAS, 20A Datun Road, Chaoyang District, Beijing 100012, People's Republic of China
8.Department of Astronomy, University of Florida, 211 Bryant Space Sciences Center, Gainesville, 32611 FL, USA
9.Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
10.Pontificia Universidad Católica de Chile, Instituto de Astrofisica, Casilla 306, Santiago 22, Chile
11.Instituto de Física y Astronomía, Universidad de Valparaíso, Avda. Gran Bretanã 1111, Valparaíso, Chile
12.Purple Mountain Observatory, CAS, Nanjing 210008, People's Republic of China
13.Department of Physics, University of Crete, GR-71003 Heraklion, Greece
14.IAASARS, National Observatory of Athens, GR-15236, Penteli, Greece
15.Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
16.Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands
17.Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904, USA
18.National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
19.University of Hawaii, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
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GB/T 7714
Lu, Nanyao,Cao, Tianwen,Diaz-Santos, Tanio,et al. CO (7-6), [C I] 370 mu m, and [N II] 205 mu m Line Emission of the QSO BRI1335-0417 at Redshift 4.407[J]. ASTROPHYSICAL JOURNAL,2018,864(1):12.
APA Lu, Nanyao.,Cao, Tianwen.,Diaz-Santos, Tanio.,Zhao YH.,Privon, George C..,...&Sanders, David B..(2018).CO (7-6), [C I] 370 mu m, and [N II] 205 mu m Line Emission of the QSO BRI1335-0417 at Redshift 4.407.ASTROPHYSICAL JOURNAL,864(1),12.
MLA Lu, Nanyao,et al."CO (7-6), [C I] 370 mu m, and [N II] 205 mu m Line Emission of the QSO BRI1335-0417 at Redshift 4.407".ASTROPHYSICAL JOURNAL 864.1(2018):12.
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