PHY3144 Galaxies and Observational Cosmology

2011-2012

Code: PHY3144
Level: 3
Title: Galaxies and Observational Cosmology
Instructors: Dr J. Hatchell
CATS Credit Value: 10
ECTS Credit Value: 5
Pre-requisites: N/A
Co-requisites: N/A
Duration: T2:01-11
Availability: unrestricted
Background Assumed: -

Total Student Study Time

100 hours, to include: 17×1-hour lectures; 6 hours directed self-study; 3×1-hour problems classes; 74 hours private study.

Aims

This module covers the physics of large-scale objects in the universe from star clusters, galaxies and quasars to the structure of the universe itself. The fascination that these objects hold is due in part to the challenge of extracting information from objects so faint and distant, and in part to the enormous range of physical processes which play a role in their formation and evolution including Newtonian and general relativistic gravitation, magnetic fields, radiation, and nucleosynthesis. The focus of the course is on applying the two main techniques of astronomy, astronomical observations and theoretical modelling, to produce a physical understanding of star clusters, galaxies and the Universe. These systems are studied at a more advanced level than in PHY2019 and the course is intended to complement PHY3142 which covers the small-scale universe (e.g. stellar astrophysics). Many of the topics discussed are applicable to a wide range of astrophysical processes. For example, the course covers gravitational dynamics which is applicable to star formation, the evolution of star clusters, galaxies, clusters of galaxies, and the formation of large-scale structure in the universe.

Intended Learning Outcomes

Students will be able to:

• Module Specific Skills:
  • describe in detail the structure and constituents of the Milky Way, galaxies, and the universe, using physical models;
  • identify and discuss observational techniques that provide evidence for these models;
  • solve problems involving, and extract information from, observational data; discuss how and why galaxies form and evolve in time and space;
• Discipline Specific Skills:
  • solve mathematical problems;
  • apply knowledge of physical processes and observing techniques to identify and explain astronomical objects;
• Personal Transferable Skills:
  • develop self-study skills;
  • work in order to meet deadlines.

Learning / Teaching Methods

Lectures, directed self-study, e-Learning resources (ELE PHY3144), and problems classes.

Assessment and Assignments

Contribution	Assessment/Assignment	Size (duration/length)	When
Formative	Guided self-study	2×3-hour packages	Weeks TBA
Formative	Problem sheets	3×1-hour sets	Weeks TBA
100%	Final examination	90 minutes	Term 3

Syllabus Plan and Content

1. Our Galaxy
   1. Introduction to the structure and constituents of our Galaxy. Disk, halo and bulge; Population I and II stars; Size; Star clusters; Galactic coordinates.
   2. Galactic Disk: Vertical and radial scales in stars, gas and dust; surface density and mass in stars; star formation and Galactic ecology.
   3. Galactic rotation curve; Potential theory and orbits; Epicyclic orbits; Dynamical mass.
   4. Galactic Halo: Globular clusters, distance to the Galactic centre, virial theorem, relaxation, mass segregation and core collapse.
   5. Galactic Bulge: Galactic centre and central black hole. Missing mass and dark matter in the Galaxy.
2. Galaxies
   1. Types of galaxy. Optical classification and Hubble types; Optical luminosity profiles; Schechter function; Distances, standard candles, Redshift, Hubble Law.
   2. Spiral and irregular galaxies. Freeman's law; Rotation curves; Dark matter; Tully-Fisher relation; Mass-to-light ratios; Black hole masses; Spiral structure and density waves; Potentials for disks and bars.
   3. Elliptical galaxies. Kormendy relation; Faber-Jackson relation; Velocity dispersion; Potentials.
   4. Active Galactic Nuclei (AGN). Quasars, blazars, radio galaxies, Seyferts. Observations and models; Unified model of AGN; Evolution and space density of quasars.
   5. Clusters of galaxies. Local group, Virgo, Coma clusters; Cluster detection, masses and dark matter, Sunyaev-Zeldovich effect;
3. Observational Cosmology
   1. Geometry of the Universe. Euclidean and curved spaces, Robertson-Walker metric; Expansion.
   2. Dynamical evolution of the Universe. Friedmann models - open, closed, Einstein-de Sitter; Benchmark model.
   3. Angular diameter distance and luminosity distance. Comoving volume.
   4. The big bang. Physics of the early universe; Time line; Matter and radiation dominated eras; Cosmic microwave radiation; Inflation, baryogenesis, primodial nucleosynthesis. Structure formation; Hot and cold dark matter.
   5. Galaxy evolution. Luminosities; Stellar populations; Chemical evolution; Galaxy interactions and the intergalactic medium; Starbursts.

Core Text

Not applicable

Supplementary Text(s)

Binney J. and Tremaine S. (1988), Galactic Dynamics, Princeton University Press, ISBN 0-691-08445-9 (UL: 523.112 BIN)
Binney J. and Merrifield M.R. (1998), Galactic Astronomy, Princeton University Press, ISBN 0-691-02565-7 (UL: 523.112 BIN)
Coles P. and Lucchin F. (2002), Cosmology - the Origin and Evolution of Cosmic Structure (2^nd edition), Wiley, ISBN 978-0-471-48909-2 (UL: On Order)
Sparke L.S. and Gallagher III J.S. (2007), Galaxies in the Universe: An Introduction (2^nd edition), CUP, ISBN 978-0521671866 (UL: 523.112 SPA)

Formative Mechanisms

This module is supported by problems classes. Students are able to monitor their own progress by attempting problems sheets provided in the lectures. Students with specific problems should first approach their tutor, and if the problem is not resolved, the lecturer.

Evaluation Mechanisms

The module will be evaluated using information gathered via the student representation mechanisms, the staff peer appraisal scheme, and measures of student attainment based on summative assessment.