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The distribution of star formation in the SAMI Galaxy Survey: the implications for quenching mechanisms and galaxy evolution

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posted on 28.03.2022, 02:51 authored by Gregory Goldstein
The distribution of the star formation across galaxy disks is examined with integral field spectroscopy to determine if the distribution varies according to the so-called 'main sequence' locus of galaxies on the plane of integrated star-formation rate and galaxy mass. Integral field spectroscopy allows the construction of radial profiles of star formation in the disks of star forming galaxies. The profiles are here used in the testing of various mechanisms that have been proposed for galaxy quenching and evolution. A goal is to determine whether processes local to each galaxy (such as a central process) or global environmental factors such as strangulation are the prime drivers of quenching. A sample of star forming galaxies from the SAMI Galaxy Survey is used, noting that only galaxies with a majority of spaxels in the central area that are star forming are suitable for construction of a radial profile. Galaxies have been classified as main sequence, above-, and below main sequence based on their location in relation to the star formation main sequence ridgeline. The radial profiles of star formation indicate that central suppression of star formation occurs in 16-20 percent of galaxies on, above or below the main sequence. The radial profiles are generally consistent with coherent star formation, whereby whatever the quenching process is that drives reduced SFR, it acts in such a way that SF remains largely coherent across the galaxy body. Coherent star formation favors several proposed quenching mechanisms including strangulation or cosmic web detachment. Central suppression is not a signature of a quenching process, but is consistent with a central process such as the compaction scenario, and cyclic central star formation. This study has been unable to distinguish between quenching from the inside out such as the 'compaction' scenario, and strangulation as a primary quenching mechanism. A weak positive correlation between bulge size and central SF radial profile slope has been detected, however the results do not support a major role of bulges in the initiation of central suppression of star formation.

History

Table of Contents

1 Introduction -- 2 Methods and derived quantities -- 3 Sample definition and global properties -- 4 Radial profiles of star formation surface density -- 5 Discussion and conclusions

Notes

Theoretical thesis. Bibliography: pages 109-118

Awarding Institution

Macquarie University

Degree Type

Thesis PhD

Degree

PhD, Macquarie University, Faculty of Science and Engineering, Department of Physics and Astronomy

Department, Centre or School

Department of Physics and Astronomy

Year of Award

2021

Principal Supervisor

Richard McDermid

Rights

Copyright Gregory Goldstein 2021 Copyright disclaimer: http://mq.edu.au/library/copyright

Language

English

Extent

1 online resource (iv,120 pages) : illustrations

Former Identifiers

mq:72039 http://hdl.handle.net/1959.14/1280785