Angular momentum evolution of galaxies over the past 10 Gyr: a MUSE and KMOS dynamical survey of 400 star-forming galaxies from z=0.3 to 1.7

被引：78

作者：

Swinbank, A. M. ^{[1
,2
]}

Harrison, C. M. ^{[1
,2
]}

Trayford, J. ^{[1
,2
]}

Schaller, M. ^{[1
,2
]}

Smail, Ian ^{[1
,2
]}

Schaye, J. ^{[3
]}

Theuns, T. ^{[1
,2
]}

Smit, R. ^{[1
,2
]}

Alexander, D. M. ^{[1
,2
]}

Bacon, R. ^{[4
]}

Bower, R. G. ^{[1
,2
]}

Contini, T. ^{[5
,6
]}

Crain, R. A. ^{[7
]}

de Breuck, C. ^{[8
]}

Decarli, R. ^{[9
]}

Epinat, B. ^{[5
,6
,10
]}

Fumagalli, M. ^{[1
,2
]}

Furlong, M. ^{[1
,2
]}

Galametz, A. ^{[11
]}

Johnson, H. L. ^{[1
,2
]}

Lagos, C. ^{[12
,13
,14
]}

Richard, J. ^{[4
]}

Vernet, J. ^{[8
]}

Sharples, R. M. ^{[1
,2
]}

Sobral, D. ^{[15
]}

Stott, J. P. ^{[1
,2
,16
]}

机构：

[1] Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England

[2] Univ Durham, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England

[3] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[4] Univ Lyon 1, Observ Lyon, CRAL, 9 Ave Ch Andre, F-69561 St Genis Laval, France

[5] CNRS, IRAP, 14 Ave Edouard Belin, F-31400 Toulouse, France

[6] Univ Toulouse, UPS OMP, 14 Ave Edouard Belin, F-31400 Toulouse, France

[7] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[8] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[9] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[10] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France

[11] Osservatorio Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy

[12] Univ Western Australia, ICRAR, M468,35 Stirling Hwy, Crawley, WA 6009, Australia

[13] Australian Res Council, Ctr Excellence All Sky Astrophys CAASTRO, 44 Rosehill St, Redfern, NSW 2016, Australia

[14] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Kohn Hall, Santa Barbara, CA 93106 USA

[15] Univ Lancaster, Dept Phys, Lancaster LA1 4BY, England

[16] Univ Oxford, Subdept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2017年 / 467卷 / 03期

关键词：

galaxies: evolution; galaxies: high-redshift; DARK-MATTER HALOES; II LUMINOSITY FUNCTIONS; HIGH-REDSHIFT SURVEY; H-ALPHA EMITTERS; LESS-THAN; 1.5; HUBBLE SEQUENCE; MASSIVE GALAXIES; SPIRAL GALAXIES; PHOTOMETRIC REDSHIFTS; EAGLE SIMULATIONS;

D O I：

10.1093/mnras/stx201

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a MUSE (Multi-Unit Spectroscopic Explorer) and KMOS (K-band Multi-Object Spectrograph) dynamical study 405 star-forming galaxies at redshift z = 0.28-1.65 (median redshift z = 0.84). Our sample is representative of the star-forming 'main sequence', with star formation rates of SFR = 0.1- 30 M-circle dot yr(-1) and stellar masses M-* = 10(8)-10(11) M-circle dot. For 49 +/- 4 per cent of our sample, the dynamics suggest rotational support, 24 +/- 3 per cent are unresolved systems and 5 +/- 2 per cent appear to be early-stage major mergers with components on 8-30 kpc scales. The remaining 22 +/- 5 per cent appear to be dynamically complex, irregular (or face-on systems). For galaxies whose dynamics suggest rotational support, we derive inclination-corrected rotational velocities and show that these systems lie on a similar scaling between stellar mass and specific angular momentum as local spirals with j(*) = J/M-* alpha M-*(2/ 3) but with a redshift evolution that scales as j(*) alpha M-*(2/3)(1 + z)(-1). We also identify a correlation between specific angular momentum and disc stability such that galaxies with the highest specific angular momentum (log( j(*)/M-*(2/3)) > 2.5) are the most stable, with Toomre Q = 1.10 +/- 0.18, compared to Q = 0.53 +/- 0.22 for galaxies with log( j(*)/M-*(2/3)) < 2.5. At a fixedmass, the Hubble Space Telescope morphologies of galaxies with the highest specific angular momentum resemble spiral galaxies, whilst those with lowspecific angular momentum are morphologically complex and dominated by several bright star- forming regions. This suggests that angular momentum plays amajor role in defining the stability of gas discs: at z similar to 1, massive galaxies that have discs with low specific angular momentum are globally unstable, clumpy and turbulent systems. In contrast, galaxies with high specific angular momentum have evolved into stable discs with spiral structure where star formation is a local (rather than global) process.

引用

页码：3140 / 3159

页数：20

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