Unified kinematic scaling relation in the local Universe using Integral Field Spectroscopy surveys
Mass-kinematics scaling relations have always been highly morphology-specific and the observational methods for the kinematic parameter have been specialised for the scaling relation of interest. Recently, thanks to the observational industrialisation provided by integral field spectroscopy (IFS) an...
| Main Author: | |
|---|---|
| Format: | Article in Journal/Newspaper |
| Language: | English |
| Published: |
The Australian National University
2021
|
| Subjects: | |
| Online Access: | https://dx.doi.org/10.25911/qad0-es18 https://openresearch-repository.anu.edu.au/handle/1885/247822 |
| Summary: | Mass-kinematics scaling relations have always been highly morphology-specific and the observational methods for the kinematic parameter have been specialised for the scaling relation of interest. Recently, thanks to the observational industrialisation provided by integral field spectroscopy (IFS) and the availability of large IFS galaxy surveys, the possibility of constructing a unified, morphology-independent, galaxy scaling relation has emerged. In this thesis we study the dynamical scaling relation between galaxy mass (usually stellar mass, M*, but also baryonic and halo mass) and the generalised kinematic parameter S_K = \sqrt{K V_{rot}^2 + \sigma^2} that combines rotation velocity V_[rot} and velocity dispersion \sigma, and has previously shown potential for unifying galaxies of all morphologies in a single scaling relation. For the construction of this scaling relation, we make use of the data from the Sydney-AAO Multi-object Integral-field-spectroscopy (SAMI) galaxy survey. We investigate the applicability of the M*-S_K scaling relation to galaxies ranging from elliptical galaxies to late-type spiral galaxies. We also investigate the effect of using either the stars or the gas component of galaxies as the kinematic tracer, optimise the combination of V_{rot} and \sigma by varying the K value in the S_K parameter, and compare the kinematic measurements from IFS survey to single-fibre spectroscopy with the intention of applying the findings to large-scale single-fibre surveys. The linear galaxy scaling relation from SAMI shows a lower limit that may be due either to an intrinsic mass limit or to an instrumental resolution limit. To explore the origin of this apparent linearity limit, we initiated the Study of Ha from Dwarf Emissions (SHaDE), a high spectral resolution (R=13500) Ha integral field survey of 69 dwarf galaxies with stellar masses in the range 10^6 |
|---|