PHYS2013 Galaxies
Module Overview
We will start from outlining fundamental questions we must answer in order to build up a picture of an astrophysical object, e.g., what is it made of? How luminous? How big? How old? How fast? How heavy? These seemingly simple questions are surprisingly difficult to answer but we will cover the different astrophysical tools used to answer them. We will then move outwards to consider the demography, spatial distribution, and environment of galaxies, in the ‘field’ and in clusters. We will then consider galaxies very distant from us in space and time, discuss galaxy formation and evolution, and have an overview of Active Galaxies, super-massive black holes and their co-evolution with their host galaxies.
Aims and Objectives
Module Aims
The aim of this course is to examine all aspects of galaxies, from what they are and how they are made up, to how we think they form and evolve.
Learning Outcomes
Knowledge and Understanding
Having successfully completed this module, you will be able to demonstrate knowledge and understanding of:
- The structural, morphological, environmental, and spectral differences of galaxies.
- The differences between the spectra of stars and galaxies.
- Environment of galaxies and its connection to galaxy evolution
- Main families of high-redshift galaxies
Subject Specific Intellectual and Research Skills
Having successfully completed this module you will be able to:
- Interpret the structural and evolutionary differences of spiral and elliptical galaxies
- Investigate the physics behind galaxy motions
- Differentiate the relevant physical processes in active galaxies
- Outline the relationships between dark matter, galaxies, and the large-scale structure of the Universe
Transferable and Generic Skills
Having successfully completed this module you will be able to:
- Develop mathematical tools for applied physics
- Formulate links between statistics and physics
Syllabus
- The make-up of galaxies: stars, gas, dust and dark matter. - Galaxy morphology: Luminosities and sizes, surface brightness, elliptical galaxies, spirals, irregular galaxies, galaxy masses. - Basic galaxy dynamics: The virial theorem - Galaxy demographics: Demographics of different types of galaxies, luminosity functions, surveys. - Galaxy environment: large-scale structure, clustering, clusters and groups, effect on galaxies. - Galaxy groups and clusters : Scaling relations, mass estimates. - The cosmological setting of galaxies: Distance measurements, cosmological redshift, Hubble expansion of the universe. - Active galaxies and supermassive black holes : Supermassive black holes in normal and active galaxies, quasars, radio galaxies, unification, the possible role of AGN in galaxy evolution. - Galaxy evolution: Hierarchical structure formation and Galaxy mergers and interactions, galaxies at high-redhisft, cosmic downsizing, star formation history of the universe.
Learning and Teaching
Teaching and learning methods
Q&As via zappers In-class group activities On-line group activities Blogs Videos, Movies
| Type | Hours |
|---|---|
| Lecture | 36 |
| Preparation for scheduled sessions | 18 |
| Follow-up work | 18 |
| Revision | 10 |
| Wider reading or practice | 52 |
| Completion of assessment task | 16 |
| Total study time | 150 |
Resources & Reading list
S S Sparke & J S Gallagher (2007). Galaxies in the universe: an introduction.
Web-sites of additional Lectures. Provided in class..
Module notes on Blackboards.
Galaxies & Galactic Structure.
Galaxy Formation and Evolution.
An introduction to modern astrophysics.
The Structure and Evolution of galaxies.
Assessment
Summative
| Method | Percentage contribution |
|---|---|
| Examination (2 hours) | 80% |
| Problem Sheets | 20% |
Repeat
| Method | Percentage contribution |
|---|---|
| Coursework marks carried forward | % |
| Examination | % |
Referral
| Method | Percentage contribution |
|---|---|
| Coursework marks carried forward | % |
| Examination | % |
Repeat Information
Repeat type: Internal & External
Linked modules
Pre-requisite: PHYS1005