Syllabus for PHYS 581-002 Advanced Topics: Observational Cosmology

Instructor: Dinesh Loomba



This class is a full 3 credit course and can serve as a A4XX elective for undergraduates.


Meeting times: The class will meet on Tuesdays and Thursdays from 12:30-1:45.


Office Hours: to be decided after first meeting.


Book(s): None required but below is a list of books which I will use as references for my lectures.  I will try to put as many of these on reserve at Centennial.

- The Early Universe by Kolb and Turner

- Physical Cosmology by Peebles

- Galaxy Formation by Longair

- Modern Cosmology by Dodelson

- Theoretical Astrophysics I, II, II, a 3 volume set by Padmanabhan

- Structure Formation in the Universe by Padmanabhan

- Cosmological Physics by Peacock

I will ask the library to put these on reserve.





                                                301 (Thermo), 405 (E&M), and 491 (QM)

Graduate Students: none but I'm assuming you are at or above the level of the courses listed above.


Cosmology is a subject that requires a wide knowledge of physics and math, so it is difficult to specify prequisites in terms of specific courses.  A senior undergraduate or beginning graduate student should have sufficient knowledge (or be willing to do some self study) to take this course. 


Preliminary outline of the course:


The course will be divided into roughly 5 parts:


I)                             The Robertson-Friedman-Walker Model of the universe.  We will begin by postulating that the Universe is isotropic and homogeneous.  This will lead us to the Robertson-Walker metric which we will use to constrain both the geometry and, at low redshift, the dynamics of the Universe.  Next we will write down the solutions to Einstein's General Relativity which fully describe the dynamics of a homogeneous and isotropic Universe.  We will examine these solutions (the Friedman Equations) and consider the various allowable cosmological world models which can result.  Possible tests of which of these models is our Universe will be discussed.

II)                          Big Bang Nucleosynthesis (BBN).  This is generally touted as one of the great successes of Big Bang cosmology (it is one of the 3 "pillar" on which the theory stands).  We will describe the epoch in the early universe when protons and neutrons are made into deuterium, the 2 isotopes of helium, and some lithium 7.  We will see how the abundances of these various elements depend on one parameter, the present matter density in baryons (i.e., protons, neutrons), within the assumptions of BBN.  We will compare the predicted abundances with data and find constraints on the baryon density.

III)                      Cosmic Microwave Background Radiation (CMB).  This is the other "pillar" on which the Big Bang stands.  We will discuss, at various levels of detail, the physics of the CMB epoch.  The properties of the CMB (temperature, anisotropies, etc) are one of the most precisely measured quantities of the early universe.  We will discuss what constraints the measurements place BOTH on what comes later in time - structure formation - as well as what took place earlier, e.g., inflation.  We will also see that the CMB data now provide independent constraints on the baryon density and show that these are consistent with the BBN prediction.

IV)                     Structure formation.  During this part we will attempt to connect the early universe constraints from the CMB, BBN, inflation, etc, with what we observe today: galaxies, clusters of galaxies, superclusters, etc.

V)                         Special Topics.  These will include: dark matter; gravitational lensing; Sunyaev-Zeldovich effect; and possibly topics of the very early universe such as bariogenesis, phase-transitions, inflation; and others.  This part provides me a buffer in case parts I-IV require more time.  This part also provides the students a chance to have input on what they'd like to hear (tell me soon!).


As noted above, this is a rough list of topics.  We can spend more time on a few of these if there's interest, or include others not on the list.


What will be required of students:


The final grade will consist of equal contributions from the following three things:


a) Homeworks (approximately 6-7 sets; i.e., about 1 set every 2 weeks)


b) A midterm exam


c) A final project involving a term paper and, depending on time and number of students enrolled in the course, I may devote several lectures to short talks given by students on their final paper topic.  I will discuss the project in more detail once the course begins.


I could be convinced by a student of a final project in theoretical cosmology; however, I would urge you to pick something that has observational consequences (i.e., it should be a testable theory) and the job done better be good!


Besides the three official contributions to your grade listed above, the following will help you but not hurt you:


d) During class I may suggest a problem for extra credit.


e) Oftentimes questions will be raised during class-time that won't be answered to everyone's satisfaction.  Students who, by whatever means, return with additional information that sheds light on the subject will be duly noted!


f) Students are strongly encouraged to ask questions, express skepticism, start discussions, and in general actively participate in the course.  If there is a single motto to follow in this course, it is that there are no "dumb" questions!  If you don't ask, you won't learn so please don't be shy.