Dancing in the dark: Galactic properties trace spin swings along the cosmic web

Y. Dubois, C. Pichon, C. Welker, D. Le Borgne, J. Devriendt, C. Laigle, S. Codis, D. Pogosyan, S. Arnouts, K. Benabed, E. Bertin, J. Blaizot, F. Bouchet, J. F. Cardoso, S. Colombi, V. De Lapparent, V. Desjacques, R. Gavazzi, S. Kassin, T. KimmH. McCracken, B. Milliard, S. Peirani, S. Prunet, S. Rouberol, J. Silk, A. Slyz, T. Sousbie, R. Teyssier, L. Tresse, M. Treyer, D. Vibert, M. Volonteri

Research output: Contribution to journalArticle

230 Citations (Scopus)

Abstract

A large-scale hydrodynamical cosmological simulation, Horizon-AGN, is used to investigate the alignment between the spin of galaxies and the cosmic filaments above redshift 1.2. The analysis of more than 150 000 galaxies per time step in the redshift range 1.2 < z <1.8 with morphological diversity shows that the spin of low-mass blue galaxies is preferentially aligned with their neighbouring filaments, while high-mass red galaxies tend to have a perpendicular spin. The reorientation of the spin of massive galaxies is provided by galaxy mergers, which are significant in their mass build-up. We find that the stellar mass transition from alignment to misalignment happens around 3×1010M⊙.Galaxies form in the vorticity-rich neighbourhood of filaments, and migrate towards the nodes of the cosmic web as they convert their orbital angular momentum into spin. The signature of this process can be traced to the properties of galaxies, as measured relative to the cosmic web. We argue that a strong source of feedback such as active galactic nuclei is mandatory to quench in situ star formation in massive galaxies and promote various morphologies. It allows mergers to play their key role by reducing post-merger gas inflows and, therefore, keeping spins misaligned with cosmic filaments.

Original languageEnglish
Pages (from-to)1453-1468
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume444
Issue number2
DOIs
Publication statusPublished - 2014 Jan 1

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merger
galaxies
filaments
vorticity
angular momentum
inflow
alignment
gas
stellar mass
simulation
active galactic nuclei
misalignment
retraining
horizon
star formation
signatures
orbitals
gases
in situ
analysis

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Dubois, Y., Pichon, C., Welker, C., Le Borgne, D., Devriendt, J., Laigle, C., ... Volonteri, M. (2014). Dancing in the dark: Galactic properties trace spin swings along the cosmic web. Monthly Notices of the Royal Astronomical Society, 444(2), 1453-1468. https://doi.org/10.1093/mnras/stu1227
Dubois, Y. ; Pichon, C. ; Welker, C. ; Le Borgne, D. ; Devriendt, J. ; Laigle, C. ; Codis, S. ; Pogosyan, D. ; Arnouts, S. ; Benabed, K. ; Bertin, E. ; Blaizot, J. ; Bouchet, F. ; Cardoso, J. F. ; Colombi, S. ; De Lapparent, V. ; Desjacques, V. ; Gavazzi, R. ; Kassin, S. ; Kimm, T. ; McCracken, H. ; Milliard, B. ; Peirani, S. ; Prunet, S. ; Rouberol, S. ; Silk, J. ; Slyz, A. ; Sousbie, T. ; Teyssier, R. ; Tresse, L. ; Treyer, M. ; Vibert, D. ; Volonteri, M. / Dancing in the dark : Galactic properties trace spin swings along the cosmic web. In: Monthly Notices of the Royal Astronomical Society. 2014 ; Vol. 444, No. 2. pp. 1453-1468.
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title = "Dancing in the dark: Galactic properties trace spin swings along the cosmic web",
abstract = "A large-scale hydrodynamical cosmological simulation, Horizon-AGN, is used to investigate the alignment between the spin of galaxies and the cosmic filaments above redshift 1.2. The analysis of more than 150 000 galaxies per time step in the redshift range 1.2 < z <1.8 with morphological diversity shows that the spin of low-mass blue galaxies is preferentially aligned with their neighbouring filaments, while high-mass red galaxies tend to have a perpendicular spin. The reorientation of the spin of massive galaxies is provided by galaxy mergers, which are significant in their mass build-up. We find that the stellar mass transition from alignment to misalignment happens around 3×1010M⊙.Galaxies form in the vorticity-rich neighbourhood of filaments, and migrate towards the nodes of the cosmic web as they convert their orbital angular momentum into spin. The signature of this process can be traced to the properties of galaxies, as measured relative to the cosmic web. We argue that a strong source of feedback such as active galactic nuclei is mandatory to quench in situ star formation in massive galaxies and promote various morphologies. It allows mergers to play their key role by reducing post-merger gas inflows and, therefore, keeping spins misaligned with cosmic filaments.",
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Dubois, Y, Pichon, C, Welker, C, Le Borgne, D, Devriendt, J, Laigle, C, Codis, S, Pogosyan, D, Arnouts, S, Benabed, K, Bertin, E, Blaizot, J, Bouchet, F, Cardoso, JF, Colombi, S, De Lapparent, V, Desjacques, V, Gavazzi, R, Kassin, S, Kimm, T, McCracken, H, Milliard, B, Peirani, S, Prunet, S, Rouberol, S, Silk, J, Slyz, A, Sousbie, T, Teyssier, R, Tresse, L, Treyer, M, Vibert, D & Volonteri, M 2014, 'Dancing in the dark: Galactic properties trace spin swings along the cosmic web', Monthly Notices of the Royal Astronomical Society, vol. 444, no. 2, pp. 1453-1468. https://doi.org/10.1093/mnras/stu1227

Dancing in the dark : Galactic properties trace spin swings along the cosmic web. / Dubois, Y.; Pichon, C.; Welker, C.; Le Borgne, D.; Devriendt, J.; Laigle, C.; Codis, S.; Pogosyan, D.; Arnouts, S.; Benabed, K.; Bertin, E.; Blaizot, J.; Bouchet, F.; Cardoso, J. F.; Colombi, S.; De Lapparent, V.; Desjacques, V.; Gavazzi, R.; Kassin, S.; Kimm, T.; McCracken, H.; Milliard, B.; Peirani, S.; Prunet, S.; Rouberol, S.; Silk, J.; Slyz, A.; Sousbie, T.; Teyssier, R.; Tresse, L.; Treyer, M.; Vibert, D.; Volonteri, M.

In: Monthly Notices of the Royal Astronomical Society, Vol. 444, No. 2, 01.01.2014, p. 1453-1468.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Dancing in the dark

T2 - Galactic properties trace spin swings along the cosmic web

AU - Dubois, Y.

AU - Pichon, C.

AU - Welker, C.

AU - Le Borgne, D.

AU - Devriendt, J.

AU - Laigle, C.

AU - Codis, S.

AU - Pogosyan, D.

AU - Arnouts, S.

AU - Benabed, K.

AU - Bertin, E.

AU - Blaizot, J.

AU - Bouchet, F.

AU - Cardoso, J. F.

AU - Colombi, S.

AU - De Lapparent, V.

AU - Desjacques, V.

AU - Gavazzi, R.

AU - Kassin, S.

AU - Kimm, T.

AU - McCracken, H.

AU - Milliard, B.

AU - Peirani, S.

AU - Prunet, S.

AU - Rouberol, S.

AU - Silk, J.

AU - Slyz, A.

AU - Sousbie, T.

AU - Teyssier, R.

AU - Tresse, L.

AU - Treyer, M.

AU - Vibert, D.

AU - Volonteri, M.

PY - 2014/1/1

Y1 - 2014/1/1

N2 - A large-scale hydrodynamical cosmological simulation, Horizon-AGN, is used to investigate the alignment between the spin of galaxies and the cosmic filaments above redshift 1.2. The analysis of more than 150 000 galaxies per time step in the redshift range 1.2 < z <1.8 with morphological diversity shows that the spin of low-mass blue galaxies is preferentially aligned with their neighbouring filaments, while high-mass red galaxies tend to have a perpendicular spin. The reorientation of the spin of massive galaxies is provided by galaxy mergers, which are significant in their mass build-up. We find that the stellar mass transition from alignment to misalignment happens around 3×1010M⊙.Galaxies form in the vorticity-rich neighbourhood of filaments, and migrate towards the nodes of the cosmic web as they convert their orbital angular momentum into spin. The signature of this process can be traced to the properties of galaxies, as measured relative to the cosmic web. We argue that a strong source of feedback such as active galactic nuclei is mandatory to quench in situ star formation in massive galaxies and promote various morphologies. It allows mergers to play their key role by reducing post-merger gas inflows and, therefore, keeping spins misaligned with cosmic filaments.

AB - A large-scale hydrodynamical cosmological simulation, Horizon-AGN, is used to investigate the alignment between the spin of galaxies and the cosmic filaments above redshift 1.2. The analysis of more than 150 000 galaxies per time step in the redshift range 1.2 < z <1.8 with morphological diversity shows that the spin of low-mass blue galaxies is preferentially aligned with their neighbouring filaments, while high-mass red galaxies tend to have a perpendicular spin. The reorientation of the spin of massive galaxies is provided by galaxy mergers, which are significant in their mass build-up. We find that the stellar mass transition from alignment to misalignment happens around 3×1010M⊙.Galaxies form in the vorticity-rich neighbourhood of filaments, and migrate towards the nodes of the cosmic web as they convert their orbital angular momentum into spin. The signature of this process can be traced to the properties of galaxies, as measured relative to the cosmic web. We argue that a strong source of feedback such as active galactic nuclei is mandatory to quench in situ star formation in massive galaxies and promote various morphologies. It allows mergers to play their key role by reducing post-merger gas inflows and, therefore, keeping spins misaligned with cosmic filaments.

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U2 - 10.1093/mnras/stu1227

DO - 10.1093/mnras/stu1227

M3 - Article

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EP - 1468

JO - Monthly Notices of the Royal Astronomical Society

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