Cosmology and Structure Formation 2
This module handbook serves to describe contents, learning outcome, methods and examination type as well as linking to current dates for courses and module examination in the respective sections.
PH2276 is a semester module in German or English language at which is offered in winter semester.
This Module is included in the following catalogues within the study programs in physics.
- Specific catalogue of special courses for nuclear, particle, and astrophysics
- Complementary catalogue of special courses for condensed matter physics
- Complementary catalogue of special courses for Biophysics
- Complementary catalogue of special courses for Applied and Engineering Physics
- Specialization Modules in Elite-Master Program Theoretical and Mathematical Physics (TMP)
If not stated otherwise for export to a non-physics program the student workload is given in the following table.
|Total workload||Contact hours||Credits (ECTS)|
|150 h||60 h||5 CP|
Responsible coordinator of the module PH2276 is Mathias Garny.
Content, Learning Outcome and Preconditions
- Motivation of cosmic inflation
- Description of inflationary expansion by scalar fields
- Slow-roll approximation
- Inflation and modified gravity
- Quantum fluctuations and primordial perturbations
- Properties of cosmic density perturbations
- Isocurvature modes and non-Gaussianity
Nonlinear structure formation
- Motivation, difficulties, techniques
- Weakly nonlinear regime
- Gravitational collapse, Press-Schechter theory
- Biased tracers
After successful completion of the module the students are able to:
- explain motivations for the paradigm of cosmic inflation using quantitative arguments
- solve the equation of motion for the inflaton field, and explain the relevant approximations
- apply the slow-roll approximation to new models and derive predictions for the statistical properties of density perturbations
- compute the spectral index and tensor-to-scalar ratio
- explain mechanisms leading to isocurvature perturbations and non-Gaussianity, and apply them to new scenarios
- be able to derive a quantitative statement about the size of nonlinear effects for a given observable
- apply methods of perturbation theory for weakly nonlinear observables
- compute at which point a density perturbation collapses into a gravitationally bound object
- explain and apply statistical methods for describing biased tracers
Cosmology and structure formation (Part I)
Courses, Learning and Teaching Methods and Literature
Courses and Schedule
|VO||2||Cosmology and Structure Formation 2||Garny, M.||
Thu, 12:00–14:00, PH 3344
and singular or moved dates
|UE||2||Exercise to Cosmology and Structure Formation 2||Garny, M.||
Fri, 10:00–12:00, PH 3344
Learning and Teaching Methods
The learning contents are taught in a thematically structured lecture, with special emphasis both on technical skills as well as physical understanding. The relation to contemporary research and the connections between theory and observations are emphasized. In tutorial sessions the students practice the techniques based on examples and problems. The understanding is deepened by transfer tasks, enabling the students to explain and apply the learning contents independently.
Combination of slides/graphs and blackboard, script containing the contents of each lecture is published on moodle every week, problem sets are being corrected and then discussed interactively in the tutorials
Dodelson, Modern Cosmology, Academic Press 2003
Lyth, Liddle, The primordial density perturbation, Cambridge University Press 2009
Description of exams and course work
There will be an oral exam of about 25 minutes duration. Therein the achievement of the competencies given in section learning outcome is tested exemplarily at least to the given cognition level using comprehension questions and sample calculations.
For example an assignment in the exam might be:
- Which problems exits in cosmology without inflation, and how are the solved quantitatively via inflation?
- Waht is the slow-roll approximation? Apply it to an example potential.
- Which properties do primordial density perturbations have in various models of inflation, and how can the be tested by observations?
- How are nonlinearities described, how is the 1-loop power spectrum computed?
- What are biased tracers and how are their properties described quantitatively?
Participation in the tutorials is strongly recommended since the exercises prepare for the problems of the exam and rehearse the specific competencies.
The exam may be repeated at the end of the semester.