Astronomy 323/423: The Local Universe
Admininistrative stuff: grading scheme, textbook and reference books
Problem set 1 (review of stellar evolution and luminosity functions) Part (1) is due in class Friday August 28, part (2) in class Tuesday Sept 1, part (3) in class Friday Sept 4. 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 Sept 15, in class.
Problem set 3 (Population synthesis) Due Tues Sept 29 in class.
Midterm in class time Tuesday 13 October
Problem set 4 (Galaxy colors and environment) Due 5pm Tues Oct 27.
Problem set 5 (Galaxy formation theory) Due in class Fri Nov 13.
Problem set 6 (Stellar LF and star count modeling of the Galaxy) Due in class Tues Dec 1.
Final Exam: Wed December 9 4-7pm
Course Outline:
(0) Review:
(1) Overview of galaxies, their structure and how we quantify it. Learning the language we use to describe galaxies. 1.1 Hubble classification
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 and the mass-metallicity relation
Chemical evolution
(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) Ellipticals and kinematical scaling relations
What causes the shape of elliptical galaxies?>
The virial theorem and the fundamental plane
(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
Multi-wavelength Milky Way
Stellar populations in
the Galaxy; measuring ages of stars
5.2 The thin disk
The thin disk (Powerpoint)
5.3 The thick disk
Properies and formation of thick
disk (Powerpoint)
5.4 The stellar halo
Halo kinematics and formation
Dynamical friction (Mihos javalab)
5.5 Dynamics of disks
Stellar
kinematics
(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
The Local Group
Dwarf galaxies in the Local Group 1.
Dwarf galaxies in the Local Group 2.
Star formation in Local Group dwarfs
