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  The possible hierarchical scales of observed clumps in high-redshift disc galaxies

Behrendt, M., Schartmann, M., & Burkert, A. (2019). The possible hierarchical scales of observed clumps in high-redshift disc galaxies. Monthly Notices of the Royal Astronomical Society, 488(1), 306-323. doi:10.1093/mnras/stz1717.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-4028-6 Version Permalink: http://hdl.handle.net/21.11116/0000-0005-4029-5
Genre: Journal Article

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Behrendt, M.1, Author              
Schartmann, M.1, Author              
Burkert, A.1, Author              
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1Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              

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 Abstract: Giant clumps on ∼kpc scales and with masses of 108−109M are ubiquitous in observed high-redshift disc galaxies. Recent simulations and observations with high spatial resolution indicate the existence of substructure within these clumps. We perform high-resolution simulations of a massive galaxy to study the substructure formation within the framework of gravitational disc instability. We focus on an isolated and pure gas disc with an isothermal equation of state with T = 104 K that allows capturing the effects of self-gravity and hydrodynamics robustly. The main mass of the galaxy resides in rotationally supported clumps which grow by merging to a maximum clump mass of 108M with diameter ∼120 pc for the dense gas. They group to clump clusters (CCs) within relatively short times (⁠≪50Myr⁠), which are present over the whole simulation time. We identify several mass and size scales on which the clusters appear as single objects at the corresponding observational resolution between ∼108 and 109M⁠. Most of the clusters emerge as dense groups and for larger beams they are more likely to be open structures represented by a single object. In the high-resolution runs higher densities can be reached, and the initial structures can collapse further and fragment to many clumps smaller than the initial Toomre length. In our low-resolution runs, the clumps directly form on larger scales 0.3–1 kpc with 108−109M⁠. Here, the artificial pressure floor which is typically used to prevent spurious fragmentation strongly influences the initial formation of clumps and their properties at very low densities.

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 Dates: 2019-06-21
 Publication Status: Published online
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 Rev. Method: Peer
 Identifiers: DOI: 10.1093/mnras/stz1717
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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 488 (1) Sequence Number: - Start / End Page: 306 - 323 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150