MIGHTEE-Hi: The relation between the Hi gas in galaxies and the cosmic web
dc.contributor.author | Tudorache, Madalina N. | |
dc.contributor.author | Jarvis, Matthew J. | |
dc.contributor.author | Heywood, Ian | |
dc.date.accessioned | 2022-07-21T10:06:49Z | |
dc.date.available | 2022-07-21T10:06:49Z | |
dc.date.issued | 2022 | |
dc.description.abstract | We study the 3D axis of rotation (3D spin) of 77 Hi galaxies from the MIGHTEE-Hi Early Science observations, and its relation to the filaments of the cosmic web. For this Hi-selected sample, the alignment between the spin axis and the closest filament (|cos 𝜓|) is higher for galaxies closer to the filaments, with h|cos 𝜓|i = 0.66 ± 0.04 for galaxies < 5 Mpc from their closest filament compared to h|cos 𝜓|i = 0.37±0.08 for galaxies at 5 < 𝑑 < 10 Mpc. We find that galaxies with a low Hi-to-stellar mass ratio (log10 (𝑀HI/𝑀★) < 0.11) are more aligned with their closest filaments, with h|cos 𝜓|i = 0.58 ± 0.04; whilst galaxies with (log10 (𝑀HI/𝑀★) > 0.11) tend to be mis-aligned, with h|cos 𝜓|i = 0.44 ± 0.04. We find tentative evidence that the spin axis of Hi-selected galaxies tend to be aligned with associated filaments (𝑑 < 10 Mpc), but this depends on the gas fractions. Galaxies that have accumulated more stellar mass compared to their gas mass tend towards stronger alignment. | en_US |
dc.identifier.citation | Tudorache, M. N. et al. (2022). MIGHTEE-Hi: The relation between the Hi gas in galaxies and the cosmic web. Monthly Notices of the Royal Astronomical Society, 513(2), 2168-2177. 10.1093/mnras/stac996 | en_US |
dc.identifier.issn | 1365-2966 | |
dc.identifier.uri | 10.1093/mnras/stac996 | |
dc.identifier.uri | http://hdl.handle.net/10566/7623 | |
dc.language.iso | en | en_US |
dc.publisher | Oxford University Press | en_US |
dc.subject | Kinematics | en_US |
dc.subject | Galaxies | en_US |
dc.subject | Science | en_US |
dc.subject | Astrophysics | en_US |
dc.title | MIGHTEE-Hi: The relation between the Hi gas in galaxies and the cosmic web | en_US |
dc.type | Article | en_US |
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