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  Revisiting the stellar velocity ellipsoid-Hubble-type relation: observations versus simulations

Pinna, F., Falcón-Barroso, J., Martig, M., Martínez-Valpuesta, I., Méndez-Abreu, J., van de Ven, G., et al. (2018). Revisiting the stellar velocity ellipsoid-Hubble-type relation: observations versus simulations. Monthly Notices of the Royal Astronomical Society, 475, 2697-2712.

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Item Permalink: https://hdl.handle.net/21.11116/0000-0005-CBBA-5 Version Permalink: https://hdl.handle.net/21.11116/0000-0005-CBBB-4
Genre: Journal Article

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https://ui.adsabs.harvard.edu/abs/2018MNRAS.475.2697P (Any fulltext)
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 Creators:
Pinna, F.1, Author
Falcón-Barroso, J.1, Author
Martig, M.1, Author
Martínez-Valpuesta, I.1, Author
Méndez-Abreu, J.1, Author
van de Ven, G.1, Author
Leaman, R.1, Author
Lyubenova, M.1, Author
Affiliations:
1Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners, ou_2421692              

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Free keywords: galaxies: evolution galaxies: kinematics and dynamics galaxies: spiral galaxies: structure Astrophysics - Astrophysics of Galaxies
 Abstract: The stellar velocity ellipsoid (SVE) in galaxies can provide important information on the processes that participate in the dynamical heating of their disc components (e.g. giant molecular clouds, mergers, spiral density waves, and bars). Earlier findings suggested a strong relation between the shape of the disc SVE and Hubble type, with later-type galaxies displaying more anisotropic ellipsoids and early types being more isotropic. In this paper, we revisit the strength of this relation using an exhaustive compilation of observational results from the literature on this issue. We find no clear correlation between the shape of the disc SVE and morphological type, and show that galaxies with the same Hubble type display a wide range of vertical-to-radial velocity dispersion ratios. The points are distributed around a mean value and scatter of σz/σR = 0.7 ± 0.2. With the aid of numerical simulations, we argue that different mechanisms might influence the shape of the SVE in the same manner and that the same process (e.g. mergers) does not have the same impact in all the galaxies. The complexity of the observational picture is confirmed by these simulations, which suggest that the vertical-to-radial axis ratio of the SVE is not a good indicator of the main source of disc heating. Our analysis of those simulations also indicates that the observed shape of the disc SVE may be affected by several processes simultaneously and that the signatures of some of them (e.g. mergers) fade over time.

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 Dates: 2018
 Publication Status: Issued
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Title: Monthly Notices of the Royal Astronomical Society
Source Genre: Journal
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Pages: - Volume / Issue: 475 Sequence Number: - Start / End Page: 2697 - 2712 Identifier: -