ALMA constraints on star-forming gas in a prototypical z=1.5 clumpy galaxy: the dearth of CO(5-4) emission from UV-bright clumps

被引：27
|
作者：
Cibinel, A. [1 ,2 ]
Daddi, E. [2 ]
Bournaud, F. [2 ]
Sargent, M. T. [1 ]
le Floc'h, E. [2 ]
Magdis, G. E. [3 ,4 ]
Pannella, M. [5 ]
Rujopakarn, W. [6 ,7 ]
Juneau, S. [2 ]
Zanella, A. [8 ]
Duc, P. -A. [2 ]
Oesch, P. A. [9 ]
Elbaz, D. [2 ]
Jagannathan, P. [10 ]
Nyland, K. [11 ]
Wang, T. [2 ]
机构：
[1] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England
[2] CEA Saclay, DSM Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France
[3] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Mariesvej 30, DK-2100 Copenhagen, Denmark
[4] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, GR-15236 Athens, Greece
[5] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany
[6] Univ Tokyo, Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan
[7] Chulalongkorn Univ, Fac Sci, Dept Phys, 254 Phayathai Rd, Bangkok 10330, Thailand
[8] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany
[9] Univ Geneva, Observ Geneva, Chemin Maillettes 51, CH-1290 Versoix, Switzerland
[10] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA
[11] Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2017年 / 469卷 / 04期
基金：
英国科学技术设施理事会; 瑞士国家科学基金会;
关键词：
galaxies: evolution; galaxies: high-redshift; galaxies: ISM; galaxies: star formation; submillimetre: galaxies; ACTIVE GALACTIC NUCLEI; ULTRA DEEP FIELD; SIMILAR-TO; SPECTRAL ENERGY-DISTRIBUTION; DENSE MOLECULAR GAS; SUBMILLIMETER GALAXY; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; GIANT CLUMPS; COSMOLOGICAL SIMULATIONS;
D O I：
10.1093/mnras/stx1112
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present deep ALMA CO(5-4) observations of a main-sequence, clumpy galaxy at z = 1.5 in the HUDF. Thanks to the similar to 0 ''.5 resolution of the ALMA data, we can link stellar population properties to the CO(5-4) emission on scales of a few kiloparsec. We detect strong CO(5-4) emission from the nuclear region of the galaxy, consistent with the observed LIR-L CO(5-4) correlation and indicating ongoing nuclear star formation. The CO(5-4) gas component appears more concentrated than other star formation tracers or the dust distribution in this galaxy. We discuss possible implications of this difference in terms of star formation efficiency and mass build-up at the galaxy centre. Conversely, we do not detect any CO(5-4) emission from the UV-bright clumps. This might imply that clumps have a high star formation efficiency (although they do not display unusually high specific star formation rates) and are not entirely gas dominated, with gas fractions no larger than that of their host galaxy (similar to 50 per cent). Stellar feedback and disc instability torques funnelling gas towards the galaxy centre could contribute to the relatively low gas content. Alternatively, clumps could fall in a more standard star formation efficiency regime if their actual star formation rates are lower than generally assumed. We find that clump star formation rates derived with several different, plausible methods can vary by up to an order of magnitude. The lowest estimates would be compatible with a CO(5-4) non-detection even for main-sequence like values of star formation efficiency and gas content.
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收藏
页码：4683 / 4704
页数：22
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