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 Wednesday August 30, part (2) in class Wednesday Sept 6, part (3) at 5pm Friday Sept 8. 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 Wed Sept 20, in class.
Problem set 3 (Population synthesis) Due Wed 4 Oct in class.
Midterm in class time Wednesday 18 October.
Problem set 4 (Galaxy colors and environment) Due in class Wed November 1.
Problem set 5 (Galaxy formation theory) Due 5pm Friday November 17.
Problem set 6 (Stellar LF and star count modeling of the Galaxy) Due in class Monday December 4.
Final Exam: Wed December 14 12-3pm
Course Outline:
(0) Review:
Readings for review:
1. HR diagram and magnitudes: Kutner, Astronomy, A Physical Perspective, Sections 2.5, 3.5; Caroll and Ostlie Sections 3.6, 8.2; Binney and Merrifield Sections 2.3, 3.3, 3.5
2. Stellar structure and evolution: Kutner Section 9.4, 10.1, Carroll and Ostlie Section 13.1, 13.2
3. Extinction and reddening: Binney and Merrifield Section 3.7
(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
Reading: Kutner 17 intro, 17.1, 17.2
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
Reading: Bruzual and Charlot (1993), ApJ, 405, 538; Kauffmann et al (2003), MNRAS 341, 33
Chemical evolution
Reading: Binney
and Merrifield Section 5.3; Binney and Tremaine, Galactic Dynamics,
NB: First Edition, Section 9.2.
(2) Cosmology meets galaxy formation: Does environment matter?
2.1 The morphology-density relation
Reading (required!): Sparke and Gallagher Section 7 intro, 7.1, 7.2, 7.3
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
New methods: asteroseismology and Gaia parallaxes
GONG helioseismology movies
Reading: Binney and
Merrifield Section 7.2, 7.2.1
Stellar luminosity function and initial mass
function
Reading: Binney and Merrifield Section 3.6
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
