Course Work
Course work will consist of
- Problem sets (at least 4)
- 2 exams: a midterm and a final
- A course project (433 only - see below)
Students enrolled in 433 will enounter additional problems on the
homeworks and exams over and above what is required for 333.
Assignments will be posted on the course web page
http://astroweb.case.edu/ssm/ASTR333/.
Late Homework Policy
- Don't be.
- Late homeworks suffer a minimum 20% mark down.
- Further arbitrary and capricious penalties will apply to homeworks that are more than one day late.
Missed Exam Policy
- Don't.
- If there is an extraordinarily good reason to miss the scheduled exam,
arrangements must be agreed with Prof. McGaugh prior to the exam date.
Grades
Course grades will be based on the weighting scheme in the table:
| Work | ASTR 333 | ASTR 433 |
|---|
| Problem Sets | 50% | 40% |
| Midterm | 25% | 25% |
| Final | 25% | 25% |
| Project | - | 10% |
Final grades will be curved: there is no absolute standard.
Those who score highest according to the tabulated weighting scheme will get the highest grades,
and vice-versa.
Grades for ASTR 333 will be whole letter grades.
Grades for ASTR 433 will have +/- values.
You will receive the grade that you earn.
Course Project
The project will explore some current aspect of the mass discrepancy
problem: observational clues, experimental searches, or theoretical
developments. It will culminate in
an oral presentation on it to the class.
Prior to the presentation, you will write an absract for distribution
to the class. Presentations will be scheduled towards the end of the semester.
Projects must be selected in consultation with Prof. McGaugh.
Ideas for projects (this list is meant to be suggestive. It is neither complete
nor exclusive.)
- Dark Matter candidates (hypotheses & motivations)
- WIMPs & Supersymmetry
- Axions
- Strange Nuggets
- MACHOs
- Cold molecular gas
- &c.
- Dark Matter detection experiments
- Direct detection, e.g., CDMS, LUX, DAMA, etc.
- Indirect detection, e.g., Fermi (γ-rays); Ice Cube (neutrinos)
- Microlensing searches for MACHOs
- Collider constraints (i.e., should the LHC see evidence for DM particles)
- &c.
- Astronomical constraints
- There are many, many possibilities here
- Individual galaxies
- Classes of galaxies (e.g., dwarf Spheroidals)
- Clusters of galaxies
- Gravitational lensing
- Large scale structure
- The cosmic microwave background
- &c.
- &c.