Schuurman, Berber (2023) Thickness of the gaseous discs of galaxies at z>4. Bachelor's Thesis, Astronomy.
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Abstract
Measuring the thickness of galaxy discs is a difficult task. The thickness is therefore often neglected or arbitrarily assumed, however it does have an effect on the geometric and kinematic measurements of galaxy discs. Studying disc thickness throughout cosmic time is crucial to understand disc formation. In this work, we investigate the thickness of the gaseous disc of a hydro-dynamical cosmological simulated galaxy ’Petunia’ at z = 7 using mock [CII] emission-line datacubes. This thesis builds upon former research done by Roman-Oliveira et al. [2023], that presents CANNUBI, a tool to estimate geometric parameters, to derive the thickness of galaxy discs. The aim is to test the reliability of CANNUBI by using it on simulated galaxy Petunia. First, we estimate the thickness from an idealised edge on view of the simulated galaxy, which we take as the true thickness of Petunia. Secondly, we measure the thicknesses and inclination on the mock [CII] emission-line datacubes at inclinations: 30◦, 60◦ and 80◦. Lastly, we investigate the recovery of the thickness and inclination with the true values. The results are as follows: i) We find that the thickness of Petunia is roughly constant along its redial extent, with a median thickness of 0.065+0.002−0.009 kpc. ii) CANNUBI was able to recover the thickness and inclination of the discs within the 1σ error, except for the 80◦ inclination mock data. The tests support the thickness measurements in Roman-Oliveira et al. [2023].
Item Type: | Thesis (Bachelor's Thesis) |
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Supervisor name: | Fraternali, F. and Roman de Oliveira, F.V. |
Degree programme: | Astronomy |
Thesis type: | Bachelor's Thesis |
Language: | English |
Date Deposited: | 17 Jul 2023 10:51 |
Last Modified: | 17 Jul 2023 10:51 |
URI: | https://fse.studenttheses.ub.rug.nl/id/eprint/30618 |
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