Astronomy 323/423: The Local Universe
Admininistrative stuff: grading scheme, textbook and reference books
Errata for Sparke and Gallagher Second Edition
Problem set 1 (review of stellar evolution and luminosity functions) Part (1) is due in class Friday Jan 17, part (2) in class Tuesday Jan 21, part (3) in class Friday Jan 24. I will choose one or more students at random on each day to present their solution(s) to the class.
Problem set 2 (Galaxy classification) Due Tuesday Feb 4, in class.
Problem set 3 (Population synthesis) Due Tues Feb 18 in class.
Midterm in class time Friday 7 March
Problem set 4 (Galaxy colors and environment) Due 5pm Thurs Mar 20.
Problem set 5 (Galaxy formation theory) Due in class Tues April 1.
Problem set 6 (Stellar LF and star count modeling of the Galaxy) Due in class Fri April 18.
Final Exam: Friday 2 May 12:30-3:30pm
Course Outline:
(0) Review: reddening and filter systems
(1) Overview of galaxies, their structure and how we quantify it. Learning the language we use to describe galaxies.
Galaxy classification using morphology
ESO page on
sky brightness
1.2 Quantifying galaxy properties: photometry
Slides on galaxy luminosity profile measurement, originally from Prof Andreas Berlind, Vanderbilt University
Moving away from morphology: using SDSS imaging
1.3 Quantifying galaxy properties: galaxy spectra
Galaxy spectra compared to stellar spectra
Spectral synthesis
(2) Cosmology meets galaxy formation: Does environment matter?
Reading: Sparke and Gallagher Ch 7, p278-297
2.1 The morphology-density relation
Galaxy morphology and environment
Causes of galaxy trends with environment.
2.2 The galaxy luminosity function and its variation with environment
(3) Dark matter, ellipticals and kinematical scaling relations
Dark matter: constraints and possible types
What causes the shape of elliptical galaxies?>
The virial theorem and the fundamental plane
Tully Fisher relations: from Prof Stacy McGaugh
(4) Galaxy formation
Reading: Sparke and Gallagher section 4.3. Longair Ch 11, Mihos 328 notes.
Galaxy formation: theory
How gas cooling plays into galaxy formation,
and how disks get angular momentum
(5) A late-type spiral in a poor group -- the Milky Way
5.1 Techniques of stellar populations:
Reading: Sparke and Gallagher Ch 2.1, pp 58-66
Distance measurement:
Absolute and relative distance
indicators. Main sequence fitting and Cepheid variables.
Reading: Binney and
Merrifield Section 7.2, 7.2.1
Stellar luminosity function and initial mass
function
5.2 Milky Way structure:
Disk populations: ISM, thin disk, thick disk, bar.
Mapping the Galaxy with star counts. Disk
kinematics. Rotation. Epicycles, disk heating, spiral
structure.
Multi-wavelength Milky Way
Stellar populations in
the Galaxy; measuring ages of stars
5.2 The thin disk
The thin disk
5.3 The thick disk
Properties and formation of thick disk
5.4 The stellar halo
Halo kinematics and formation
Dynamical friction (Mihos javalab)
5.5 Kinematics and Dynamics of disks
Disk kinematics and a little dynamics
(6) The Local Group.
Reading: Sparke and Gallagher Ch 4, 4.1
The three spirals: M31, Milky Way, M33. Reading: text Ch 4.2
Dwarf galaxies in the Local Group. Reading: S and G Ch 4.4
