Galaxies

Code:

AST406

Acronym:

AST406

Keywords
Classification	Keyword
OFICIAL	Astronomy

Instance: 2012/2013 - 1S

Active?	Yes
Responsible unit:	Department of Physics and Astronomy
Course/CS Responsible:	Master in Astronomy and Astrophysics

Cycles of Study/Courses

Acronym	No. of Students	Study Plan	Curricular Years	Credits UCN	Credits ECTS	Contact hours	Total Time
M:AST	11	Plano de Estudos do Mestrado em Astronomia	1	-	7,5	64	202,5

Teaching language

English

Objectives

The aim of this course is that students acquire a thorough knowledge about different types of galaxies, their composition, physical processes which enable the formation and physical mechanisms responsible for the variety of observed properties and their evolution in different environments. Alongside the theoretical approach, existing observational evidence will be presented as well as the major future projects with scientific impact in this area.

Learning outcomes and competences

It is intended that students acquire a thorough knowledge about different types of galaxies, their composition, physical processes which enable the formation and physical mechanisms responsible for the variety of observed properties and their evolution in different environments. Alongside the theoretical approach, it is expected that students develop skills of handling and critical analysis of available data, interpreting results in connection to the subjects lectured during classes.

Working method

Presencial

Program

I. Galaxies: Types and formation I.1 The Galaxy and the Local Group of galaxies. I.2 Classification schemes based on morphology: Hubble, de Vaucouleurs, CAS. I.3 The luminosity profile of galaxies. Stellar populations and colors. Spectral energy distribution of different types of galaxies: the effect of redshift in the spectrum. The rate of star formation in different morphological types. I.4 The interstellar medium in galaxies: the ionized, atomic and molecular gas components- Detection, properties and observed correlations. Dust and extinction. I.5 Dynamics and distribution of mass in galaxies. Calculation of total mass. Formation of spiral arms and bars. I.6 luminosity functions. Relationship between mass and luminosity: Tully-Fisher, Faber-Jackson; fundamental plane for elliptical galaxies. II. Evolution of galaxies II.1 groups and clusters of galaxies: constituents, modes of detection and calculation of mass. II.2 morphological segregation of galaxies taking into account the environmental density. II.3 physical mechanisms responsible for the evolution of galaxy groups and clusters: dynamical friction, ram-pressure stripping, tidal stripping and merging. Consequences of these mechanisms on the properties of galaxies and the luminosity function. Genesis of the relationship between morphology and density of the medium. II.4 color and spectral classes as indicators of the evolution of galaxies in clusters: the Butcher-Oemler effect; K + A galaxies, the color-magnitude relation and rate of fusion between galaxies, morphological and spectral transformations. II.5 galactic evolution in the field. Techniques and results of major searches for distant galaxies. Evolution of the characteristics of the intergalactic medium with time. II.6 radiative cooling and the formation of proto-galaxies. The effect of feedback on star formation. III. Active nuclei of galaxies III.1 Introduction. Basic properties of galaxies with nuclear activity. III.2 Taxonomy and observational properties: Seyferts, LINERS, Radio Galaxies, Quasars and Blazars. The spectral energy distributions - synchrotron emission, inverse Compton and black body. The cosmological evolution. III.3 Schematic description of an active galaxy and unification scheme. The central engine: a black hole and accretion disk. Estimates of the black hole mass through flow variability and through the Eddington limit. Structure of the accretion disk.

Mandatory literature

L.S. Sparke, J.S. Gallagher; Galaxies in the Universe: An Introduction, Cambridge University Press, 2007

Complementary Bibliography

M.H. Jones, R.J. Lambourne; An Introduction to Galaxies and Cosmology, Cambridge University Press, 2004
D.M. Elmegreen; Galaxies and Galactic Structures, Prentice Hall, 1998
H. Spinrad; Galaxy Formation and Evolution, Springer-Praxis, 2005
M.B. Peterson; An Introduction to Active Galactic Nuclei, Cambridge University Press, 1997
A.K. Kembhavi, J.V. Narlikar; Quasars and Active Galactic Nuclei, Cambridge University Press, 1999
J.H. Krolik; Active Galactic Nuclei: from the central black hole to the galactic environment, Princeton University Press, 1998
B.W. Carrol, D.A. Ostlie; An Introduction to Modern Galactic Astrophysics and Cosmology, Addison-Wesley, 2007

Teaching methods and learning activities

TP classes involve the exposure by the lecturer of the contents of the program, with the help of multimedia materials, followed by examples of application and problem solving when appropriate. In tutorial classes students develop a practical work under the guidance of the teacher.

keywords

Physical sciences > Astronomy > Astrophysics

Evaluation Type

Distributed evaluation with final exam

Assessment Components

Description	Type	Time (hours)	Weight (%)	End date
Attendance (estimated)	Participação presencial	39,00
Exam	Exame		70,00
Presentation	Prova oral		30,00
	Total:	-	100,00

Calculation formula of final grade

The assessment in this discipline consists of a final exam, which contributes with a weight of 70 percent to the final classification, plus a project that contributes with 30 percent for final classification. The calculation of the final classification is then obtained as follows: Nf = 0.7 * Ex +0.3*TP where Nf is the final grade (not less than 10 values), Ex is the exam grade (Rated 0-20, and required to be no less than 7 values), TP is the grade of the practical work (rated 0 to 20).

Examinations or Special Assignments

At the end of the practical work the student must present and discuss orally his/her results.

Classification improvement

For students who are attending the course, the improvement of the classification can be made on the written exam only, that will still weigh 70 percent of the final mark. For students who have taken the course in the academic year 2011/2012, the improvement of the classification is made in the written exam only, to be rated from 0 to 20 values; the final grade will be that obtained in this exam.