Non-linear violent disc instability with high Toomre's Q in high-redshift clumpy disc galaxies
Abstract
We utilize zoom-in cosmological simulations to study the nature of violent disc instability in clumpy galaxies at high redshift, z = 1–5. Our simulated galaxies are not in the ideal state assumed in Toomre instability, of linear fluctuations in an isolated, uniform, rotating disc. There, instability is characterized by a Q parameter below unity, and lower when the disc is thick. Instead, the high-redshift discs are highly perturbed. Over long periods they consist of non-linear perturbations, compact massive clumps and extended structures, with new clumps forming in interclump regions. This is while the galaxy is subject to frequent external perturbances. We compute the local, two-component Q parameter for gas and stars, smoothed on a ~1 kpc scale to capture clumps of 108-9 M⊙. The Q < 1 regions are confined to collapsed clumps due to the high surface density there, while the interclump regions show Q significantly higher than unity. Tracing the clumps back to their relatively smooth Lagrangian patches, we find that Q prior to clump formation typically ranges from unity to a few. This is unlike the expectations from standard Toomre instability. We discuss possible mechanisms for high-Q clump formation, e.g. rapid turbulence decay leading to small clumpsmore »
- Authors:
-
- The Hebrew Univ., Jerusalem (Israel)
- Centro de Astrobiologia (CSIC-INTA), Madrid (Spain); Univ. Autonoma de Madrid, Madrid (Spain)
- CEA/DSM-CNRS-Univ. Paris Diderot, Gif-sur-Yvette (France)
- Univ. of California, Santa Cruz, CA (United States)
- Publication Date:
- Research Org.:
- Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC)
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 1542105
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Volume: 456; Journal Issue: 2; Journal ID: ISSN 0035-8711
- Publisher:
- Royal Astronomical Society
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; instabilities; methods: numerical; galaxies: formation; galaxies: kinematics and dynamics
Citation Formats
Inoue, Shigeki, Dekel, Avishai, Mandelker, Nir, Ceverino, Daniel, Bournaud, Frédéric, and Primack, Joel. Non-linear violent disc instability with high Toomre's Q in high-redshift clumpy disc galaxies. United States: N. p., 2015.
Web. doi:10.1093/mnras/stv2793.
Inoue, Shigeki, Dekel, Avishai, Mandelker, Nir, Ceverino, Daniel, Bournaud, Frédéric, & Primack, Joel. Non-linear violent disc instability with high Toomre's Q in high-redshift clumpy disc galaxies. United States. https://doi.org/10.1093/mnras/stv2793
Inoue, Shigeki, Dekel, Avishai, Mandelker, Nir, Ceverino, Daniel, Bournaud, Frédéric, and Primack, Joel. Wed .
"Non-linear violent disc instability with high Toomre's Q in high-redshift clumpy disc galaxies". United States. https://doi.org/10.1093/mnras/stv2793. https://www.osti.gov/servlets/purl/1542105.
@article{osti_1542105,
title = {Non-linear violent disc instability with high Toomre's Q in high-redshift clumpy disc galaxies},
author = {Inoue, Shigeki and Dekel, Avishai and Mandelker, Nir and Ceverino, Daniel and Bournaud, Frédéric and Primack, Joel},
abstractNote = {We utilize zoom-in cosmological simulations to study the nature of violent disc instability in clumpy galaxies at high redshift, z = 1–5. Our simulated galaxies are not in the ideal state assumed in Toomre instability, of linear fluctuations in an isolated, uniform, rotating disc. There, instability is characterized by a Q parameter below unity, and lower when the disc is thick. Instead, the high-redshift discs are highly perturbed. Over long periods they consist of non-linear perturbations, compact massive clumps and extended structures, with new clumps forming in interclump regions. This is while the galaxy is subject to frequent external perturbances. We compute the local, two-component Q parameter for gas and stars, smoothed on a ~1 kpc scale to capture clumps of 108-9 M⊙. The Q < 1 regions are confined to collapsed clumps due to the high surface density there, while the interclump regions show Q significantly higher than unity. Tracing the clumps back to their relatively smooth Lagrangian patches, we find that Q prior to clump formation typically ranges from unity to a few. This is unlike the expectations from standard Toomre instability. We discuss possible mechanisms for high-Q clump formation, e.g. rapid turbulence decay leading to small clumps that grow by mergers, non-axisymmetric instability, or clump formation induced by non-linear perturbations in the disc. Alternatively, the high-Q non-linear VDI may be stimulated by the external perturbations such as mergers and counter-rotating streams. In conclusion, the high Q may represent excessive compressive modes of turbulence, possibly induced by tidal interactions.},
doi = {10.1093/mnras/stv2793},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 456,
place = {United States},
year = {Wed Dec 30 00:00:00 EST 2015},
month = {Wed Dec 30 00:00:00 EST 2015}
}
Web of Science
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Structure and stability of high-redshift galaxies in cosmological simulations
journal, March 2019
- Meng, Xi; Gnedin, Oleg Y.; Li, Hui
- Monthly Notices of the Royal Astronomical Society, Vol. 486, Issue 2
Clumpy Galaxies in CANDELS. II. Physical Properties of UV-bright Clumps at 0.5 ≤ z < 3
journal, January 2018
- Guo, Yicheng; Rafelski, Marc; Bell, Eric F.
- The Astrophysical Journal, Vol. 853, Issue 2
Two Thresholds for Globular Cluster Formation and the Common Occurrence of Massive Clusters in the Early Universe
journal, December 2018
- Elmegreen, Bruce G.
- The Astrophysical Journal, Vol. 869, Issue 2
Distinguishing Mergers and Disks in High-redshift Observations of Galaxy Kinematics
journal, March 2019
- Simons, Raymond C.; Kassin, Susan A.; Snyder, Gregory F.
- The Astrophysical Journal, Vol. 874, Issue 1
Size Scaling of Clump Instabilities in Turbulent, Feedback-regulated Disks
journal, April 2019
- Ali, Kamran; Obreschkow, Danail; Wang, Liang
- The Astrophysical Journal, Vol. 874, Issue 2
The Evolution and Origin of Ionized Gas Velocity Dispersion from z ∼ 2.6 to z ∼ 0.6 with KMOS 3D
journal, July 2019
- Übler, H.; Genzel, R.; Wisnioski, E.
- The Astrophysical Journal, Vol. 880, Issue 1
A Noncorotating Gas Component in an Extreme Starburst at z = 4.3
journal, February 2020
- Tadaki, Ken-ichi; Iono, Daisuke; Yun, Min S.
- The Astrophysical Journal, Vol. 889, Issue 2
What drives gravitational instability in nearby star-forming spirals? The impact of CO and HI velocity dispersions
text, January 2017
- Romeo, Alessandro B.; Mogotsi, Keoikantse Moses
- arXiv
A unified model for the maximum mass-scales of molecular clouds, stellar clusters, and high-redshift clumps
text, January 2017
- Reina-Campos, Marta; Kruijssen, J. M. Diederik
- arXiv
A Unified Model for Galactic Discs: Star Formation, Turbulence Driving, and Mass Transport
text, January 2017
- Krumholz, Mark R.; Burkhart, Blakesley; Forbes, John C.
- arXiv
Towards a radially-resolved semi-analytic model for the evolution of disc galaxies tuned with machine learning
text, January 2018
- Forbes, John C.; Krumholz, Mark R.; Speagle, Joshua S.
- arXiv
Distinguishing Mergers and Disks in High Redshift Observations of Galaxy Kinematics
text, January 2019
- Simons, Raymond C.; Kassin, Susan A.; Snyder, Gregory F.
- arXiv
Size-scaling of clump instabilities in turbulent, feedback regulated disks
text, January 2019
- Ali, Kamran; Obreschkow, Danail; Wang, Liang
- arXiv
Clumpy galaxies in cosmological simulations: The effect of ISM model
text, January 2019
- Inoue, Shigeki; Yoshida, Naoki
- arXiv
A contribution of star-forming clumps and accreting satellites to the mass assembly of z ~ 2 galaxies
text, January 2019
- Zanella, A.; Floc'h, E. Le; Harrison, C. M.
- arXiv
A non-corotating gas component in an extreme starburst at z=4.3
text, January 2020
- Tadaki, Ken-ichi; Iono, Daisuke; Yun, Min S.
- arXiv