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

A. M. Swinbank, C. M. Harrison, J. Trayford, M. Schaller, Ian Smail, J. Schaye, T. Theuns, R. Smit, D. M. Alexander, R. Bacon, R.G. Bower, T. Contini, R.A. Crain, C. De Breuck, R. Decarli, B. Epinat, M. Fumagalli, M. Furlong, M. Galametz, H. L. Johnson & 6 others Claudia Lagos Urbina, J. Richard, J. Vernet, R. M. Sharples, D. Sobral, J. P. Stott

Research output: Contribution to journalArticle

Abstract

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 \bar{z} = 0.84). Our sample is representative of the star-forming 'main sequence', with star formation rates of SFR = 0.1-30 M⊙ yr-1 and stellar masses M⋆ = 108-1011 M⊙. 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_\star ∝ M_\star ^{2/3} but with a redshift evolution that scales as j⋆ ∝ M_\star ^{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_\star ^{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_\star ^{2/3}) < 2.5. At a fixed mass, the Hubble Space Telescope morphologies of galaxies with the highest specific angular momentum resemble spiral galaxies, whilst those with low specific angular momentum are morphologically complex and dominated by several bright star-forming regions. This suggests that angular momentum plays a major role in defining the stability of gas discs: at z ∼ 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.
Original languageEnglish
Pages (from-to)3140–3159
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume467
Issue number3
Early online date25 Jan 2017
DOIs
Publication statusPublished - 1 Jun 2017

Fingerprint

extremely high frequencies
angular momentum
spectrographs
M stars
galaxies
stars
stellar mass
spiral galaxies
star formation rate
Hubble Space Telescope
merger
inclination
star formation
scaling
gases
gas

Cite this

Swinbank, A. M. ; Harrison, C. M. ; Trayford, J. ; Schaller, M. ; Smail, Ian ; Schaye, J. ; Theuns, T. ; Smit, R. ; Alexander, D. M. ; Bacon, R. ; Bower, R.G. ; Contini, T. ; Crain, R.A. ; De Breuck, C. ; Decarli, R. ; Epinat, B. ; Fumagalli, M. ; Furlong, M. ; Galametz, M. ; Johnson, H. L. ; Lagos Urbina, Claudia ; Richard, J. ; Vernet, J. ; Sharples, R. M. ; Sobral, D. ; Stott, J. P. . / 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. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 467, No. 3. pp. 3140–3159.
@article{d85a5f56ffe740e8a43dcb367f121aca,
title = "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",
abstract = "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 \bar{z} = 0.84). Our sample is representative of the star-forming 'main sequence', with star formation rates of SFR = 0.1-30 M⊙ yr-1 and stellar masses M⋆ = 108-1011 M⊙. 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_\star ∝ M_\star ^{2/3} but with a redshift evolution that scales as j⋆ ∝ M_\star ^{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_\star ^{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_\star ^{2/3}) < 2.5. At a fixed mass, the Hubble Space Telescope morphologies of galaxies with the highest specific angular momentum resemble spiral galaxies, whilst those with low specific angular momentum are morphologically complex and dominated by several bright star-forming regions. This suggests that angular momentum plays a major role in defining the stability of gas discs: at z ∼ 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.",
author = "Swinbank, {A. M.} and Harrison, {C. M.} and J. Trayford and M. Schaller and Ian Smail and J. Schaye and T. Theuns and R. Smit and Alexander, {D. M.} and R. Bacon and R.G. Bower and T. Contini and R.A. Crain and {De Breuck}, C. and R. Decarli and B. Epinat and M. Fumagalli and M. Furlong and M. Galametz and Johnson, {H. L.} and {Lagos Urbina}, Claudia and J. Richard and J. Vernet and Sharples, {R. M.} and D. Sobral and Stott, {J. P.}",
year = "2017",
month = "6",
day = "1",
doi = "10.1093/mnras/stx201",
language = "English",
volume = "467",
pages = "3140–3159",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "OXFORD UNIV PRESS UNITED KINGDOM",
number = "3",

}

Swinbank, AM, Harrison, CM, Trayford, J, Schaller, M, Smail, I, Schaye, J, Theuns, T, Smit, R, Alexander, DM, Bacon, R, Bower, RG, Contini, T, Crain, RA, De Breuck, C, Decarli, R, Epinat, B, Fumagalli, M, Furlong, M, Galametz, M, Johnson, HL, Lagos Urbina, C, Richard, J, Vernet, J, Sharples, RM, Sobral, D & Stott, JP 2017, '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' Monthly Notices of the Royal Astronomical Society, vol. 467, no. 3, pp. 3140–3159. https://doi.org/10.1093/mnras/stx201

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. / Swinbank, A. M.; Harrison, C. M.; Trayford, J.; Schaller, M.; Smail, Ian; Schaye, J.; Theuns, T.; Smit, R. ; Alexander, D. M.; Bacon, R. ; Bower, R.G.; Contini, T. ; Crain, R.A.; De Breuck, C.; Decarli, R.; Epinat, B. ; Fumagalli, M.; Furlong, M.; Galametz, M.; Johnson, H. L. ; Lagos Urbina, Claudia; Richard, J.; Vernet, J. ; Sharples, R. M. ; Sobral, D. ; Stott, J. P. .

In: Monthly Notices of the Royal Astronomical Society, Vol. 467, No. 3, 01.06.2017, p. 3140–3159.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Angular momentum evolution of galaxies over the past 10 Gyr

T2 - A MUSE and KMOS dynamical survey of 400 star-forming galaxies from z = 0.3 to 1.7

AU - Swinbank, A. M.

AU - Harrison, C. M.

AU - Trayford, J.

AU - Schaller, M.

AU - Smail, Ian

AU - Schaye, J.

AU - Theuns, T.

AU - Smit, R.

AU - Alexander, D. M.

AU - Bacon, R.

AU - Bower, R.G.

AU - Contini, T.

AU - Crain, R.A.

AU - De Breuck, C.

AU - Decarli, R.

AU - Epinat, B.

AU - Fumagalli, M.

AU - Furlong, M.

AU - Galametz, M.

AU - Johnson, H. L.

AU - Lagos Urbina, Claudia

AU - Richard, J.

AU - Vernet, J.

AU - Sharples, R. M.

AU - Sobral, D.

AU - Stott, J. P.

PY - 2017/6/1

Y1 - 2017/6/1

N2 - 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 \bar{z} = 0.84). Our sample is representative of the star-forming 'main sequence', with star formation rates of SFR = 0.1-30 M⊙ yr-1 and stellar masses M⋆ = 108-1011 M⊙. 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_\star ∝ M_\star ^{2/3} but with a redshift evolution that scales as j⋆ ∝ M_\star ^{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_\star ^{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_\star ^{2/3}) < 2.5. At a fixed mass, the Hubble Space Telescope morphologies of galaxies with the highest specific angular momentum resemble spiral galaxies, whilst those with low specific angular momentum are morphologically complex and dominated by several bright star-forming regions. This suggests that angular momentum plays a major role in defining the stability of gas discs: at z ∼ 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.

AB - 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 \bar{z} = 0.84). Our sample is representative of the star-forming 'main sequence', with star formation rates of SFR = 0.1-30 M⊙ yr-1 and stellar masses M⋆ = 108-1011 M⊙. 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_\star ∝ M_\star ^{2/3} but with a redshift evolution that scales as j⋆ ∝ M_\star ^{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_\star ^{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_\star ^{2/3}) < 2.5. At a fixed mass, the Hubble Space Telescope morphologies of galaxies with the highest specific angular momentum resemble spiral galaxies, whilst those with low specific angular momentum are morphologically complex and dominated by several bright star-forming regions. This suggests that angular momentum plays a major role in defining the stability of gas discs: at z ∼ 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.

U2 - 10.1093/mnras/stx201

DO - 10.1093/mnras/stx201

M3 - Article

VL - 467

SP - 3140

EP - 3159

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -