Dates of the courses. Sterrenstelsels en Cosmologie. Docent: M. Franx, kamer 425. Usually on Monday, 11:15-13:00, but also on Thursdays 13:45-15:30
|
|
- Angel Mosley
- 6 years ago
- Views:
Transcription
1 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-2 Sterrenstelsels en Cosmologie Docent: M. Franx, kamer 425 College assistent: Marcel van Daalen, kamer 438 Two books are relevant for this course. None are obligatory: Binney and Tremaine: Galactic Dynamics (B&T) (2nd edition) (40 dollars amazon, 30 dollars on kindle) Dates of the courses Usually on Monday, 11:15-13:00, but also on Thursdays 13:45-15:30 Feb 11,18,21,25, Mar 4,11,18,21,25, Apr 8,15, May 6,13,22 Always room room 106 Huygens Lab. Introduction into theory of galaxy dynamics, i.e. potential theory, orbits, distribution functions, equilibria, disks, mergers, etc. Extragalactic Astronomy and Cosmology Peter Schneider 79 euro bij bol, $70 bij kindle (50 euro equivalent) These books are not obligatory. Their level is very high (advanced Master course), but this means they remain useful throughout your career. 1 other book is also sometimes used: Binney and Merrifield: Galactic Astronomy (indicated with BM ) Het cijfer voor het college wordt voor 66% bepaald door het tentamen, en voor 33% door de ingeleverde huiswerk opgaven. Die moeten bij het begin van het volgende college worden ingeleverd. Een minimum cijfer van een 6 voor de huiswerk opgaves is nodig om deel te kunnen nemen aan het tentamen. Te laat inleveren van de huiswerk opgaven betekent het cijfer 0.
2 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-4 Brief content of the course 1) Introduction What is a galaxy? Classifications Photometry, exponentials, r1/4 profiles, luminosity function 2) Keeping a galaxy together: Gravity Potentials 3) Galactic Dynamics Equilibrium collisions, Virial Theorem Universe expansion Growth of galaxies by gravity Galaxy scaling relations 9) Galaxy formation - forming the stars Gas cooling and star formation formation of disks dynamical friction and mergers tidal tails in mergers 10) Observing galaxy formation High redshift galaxies from HST Fair samples of galaxies at high redshift 4) Galactic Dynamics continued Timescales Orbits 5) Collisionless Boltzmann Equation equilibrium, phase mixing derivation of distribution function 6) Velocity Moments Jeans equations comparison to observations 7) Mass distribution and dark matter Evidence for dark matter from rotation curves Solar neighborhood, Oort limit Elliptical galaxies and hot gas Clusters of galaxies, the universe Candidate dark matter particles 8) Galaxy formation
3 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c General Introduction Content Handout 1: i) What is a galaxy? Optical Radio X-Ray Dark Matter (halo) ii) Why do we study galaxies? iii) Optical Photometry iv) Luminosity Function v) Selection Effects Read from B&M: 4.1, (4.1.2), to page 165, (4.1.4) 4.2, (4.2.2), not , to page , (not 4.4.2), to page , to page 244 (4.6.2) subsection in brackets means for reading only i) What is a galaxy? Galaxies emit in many wavelengths [See the multiwavelength color show! (separate handout, also on website)] Radio: Continuum emission follows spiral arms Active nuclei produce jets, radio lobes... Line emission: HI 21 cm, CO, molecular lines Infrared: Continuum emission by dust Star forming regions, active nuclei Near Infrared: Red super giants, some extinction Optical-UV: Visible stars, dust absorbtion Emission lines Blue active nuclei X-Ray: (Double) stars, neutron stars, star forming regions Very hot gas
4 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-8 Active Nuclei produce emission at all wavelengths at all lengthscales: from very close to the nucleus ( pc) to the largest scale (> 10 kpc) Conclusion a Galaxy consists of several components: stars bulge red, old (?) r 1/4 law disk blue or red spiral arms, rings, bars exponential profile gas H I gas H 2 gas dust Hot Gas active nucleus black hole Dark Halo
5 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-10 Why study galaxies? What are the main questions? Optical images of galaxies and classification See the color handout for nice pictures! What is the structure of galaxies? What is their equilibrium? What are they made off? What is their mass distribution? All classification systems are idealizations. Independent of true size of the galaxy! Often used systems: How do they evolve in time? 1. Hubble-Sandage 2. de Vaucouleurs or How have they formed? Numerical types T (based on 2.) often used Disadvantages of ALL classifications Only based on optical image > independent of true size! Galaxies vary in more than one dimension Many galaxies are peculiar, i.e. inclassifiable
6 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-12
7 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-14
8 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-16
9 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-18 Homework Questions: 1) Describe in your own words 3 criteria which are used to classify spirals into Sa, Sb to Sd. 2) What is the type of the Milky Way? 3) Why do we classify the Magellanic CLouds not as ellipticals? They don t have spiral arms. 4) What is the type of the galaxy on the cover of BM? Give the reasons for your classification 5) How do you recognize mergers?
10 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-20 Quantitative photometry of galaxies First: photographic plates: Limited dynamic range Now: CCDs (= very sensitive TV camera s) Sizes 2048x2048 pixels Quantum efficiency 90 % Very good dynamic range Photometry > Imaging galaxies and measuring their brightness distribution Usually NOT resolved in stars Measure average surface brightness profile Ellipticals: King profile de Vaucouleurs law (r 1/4 ) Spirals: Disks: exponential profile Bulges: r 1/4 For elliptical galaxies we often find the r 1/4 law: I(R) = I e exp( 7.67[(R/R e ) 1/4 1]) where R e is the half light radius: half the light is emitted inside R e. Because of uncertainties in the background subtraction, we never know the exact half light radius. The parameter I e is the surface brightness at R = R e. No galaxy follows the r 1/4 law exactly!
11 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-22 An exponential disk has I(R) = I 0 exp( R/R d ) where R d is the disk scalelength. Many galaxies are modelled well by fitting an r 1/4 law to the bulge and an exponential model to the disk.
12 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-24 Luminosity Function Determine for each galaxy the intrinsic luminosity from apparent luminosity and distance. Correct for bandpass, internal absorbtion and absorbtion by the Milky Way. The luminosity function is defined by Φ dm = number density of galaxies in magnitude range (M,M + dm) The distribution of luminosities is given by a Schechter function Φ(L) = (Φ 0/L ) (L/L ) α exp( L/L ) Typical values: Φ = (1.6 ± 0.3) 10 2 h 3 Mpc 3 MB = 19.7 ± log h α = 1.07 ± 0.07 L B = (1.2 ± 0.1) h L Sun where H 0 = h100km/s The number of galaxies with a luminosity larger than L is given by N(> L) = L Φ(L )dl = N 0 Γ(1 + α, L/L )
13 see franx/college/ mf-sts-2013-c see franx/college/ mf-sts-2013-c01-26 Total amount of light produced l tot = 0 Φ(L )L dl = Φ L Γ(2 + α) = Φ L for α = 1 Hence, huge numbers of low luminosity galaxies expected, but finite luminosity. Most of the luminosity comes from galaxies with L = L. A simple approximation is that the universe is filled with L galaxies with a density Φ
14 see franx/college/ mf-sts-2013-c01-27 Catalogs of galaxies most catalogs based on optical surveys e.g.: Revised Shapley-Ames Catalog Sandage and Tammann Third Reference Catalogue of Bright Galaxies de Vaucouleurs et al Sloan Digital Sky Survey 1 million galaxies + spectra! see franx/college/ mf-sts-2013-c01-28 Selection effects in optical catalogs Consider galaxy with certain luminosity If galaxy too small: misclassified as star if galaxy too big: surface brightess is too low > not detected! Very important were Palomar Sky Survey Plates, these have been used for systematische surveys UGC: northern galaxies ESO catalog: southern galaxies Lauberts, Lauberts en Valentijn
15 see franx/college/ mf-sts-2013-c01-29 Homework questions 6) Given a galaxy with an exponential profile I(R) = I 0 exp( R/R d ) a) what is the total emount of light emitted? (Express in terms of I 0 and R d.) (Hint: integrate the light emitted over radius from 0 to infinity) b) what is the half light radius? (i.e., the radius in which half the light is emitted) (Hint: use the integral from 6, now to Re instead of infinity) 7) How can we attempt to classify galaxies automatically (i.e., by computer)? 8) What is the luminosity function? 9) Given a Schechter Luminosity function, what is the luminosity at which half of the total luminosity density is emitted by galaxies brighter than that luminosity? Assume α = 1. 10) What is the luminosity of a typical galaxy in terms of solar luminosities? 11) How can the total number of galaxy be infinite (per Mpc 3 )? Would that produce an infinite amount of light? 12) Find the website of a catalogue with more than galaxies (and NOT the Sloan Digital Sky Survey ).
Sterrenstelsels en Cosmologie. Dates of the courses. on Monday, 11:15-13:00 Jan 26 - June 1, room 414, (exceptions April 8 and June 1)
23-1-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c01-1 23-1-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c01-2 Sterrenstelsels en Cosmologie Docent: M. Franx,
More informationA galaxy is a self-gravitating system composed of an interstellar medium, stars, and dark matter.
Chapter 1 Introduction 1.1 What is a Galaxy? It s surprisingly difficult to answer the question what is a galaxy? Many astronomers seem content to say I know one when I see one. But one possible definition
More informationThe Classification of Galaxies
Admin. 11/9/17 1. Class website http://www.astro.ufl.edu/~jt/teaching/ast1002/ 2. Optional Discussion sections: Tue. ~11.30am (period 5), Bryant 3; Thur. ~12.30pm (end of period 5 and period 6), start
More informationStellar Dynamics and Structure of Galaxies
Stellar Dynamics and Structure of Galaxies Gerry Gilmore H47 email: gil@ast.cam.ac.uk Lectures: Monday 12:10-13:00 Wednesday 11:15-12:05 Friday 12:10-13:00 Books: Binney & Tremaine Galactic Dynamics Princeton
More informationLecture Outlines. Chapter 24. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 24 Astronomy Today 8th Edition Chaisson/McMillan Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble
More informationAn analogy. "Galaxies" can be compared to "cities" What would you like to know about cities? What would you need to be able to answer these questions?
An analogy "Galaxies" can be compared to "cities" What would you like to know about cities? how does your own city look like? how big is it? what is its population? history? how did it develop? how does
More informationNormal Galaxies (Ch. 24) + Galaxies and Dark Matter (Ch. 25) Symbolically: E0.E7.. S0..Sa..Sb..Sc..Sd..Irr
Normal Galaxies (Ch. 24) + Galaxies and Dark Matter (Ch. 25) Here we will cover topics in Ch. 24 up to 24.4, but then skip 24.4, 24.5 and proceed to 25.1, 25.2, 25.3. Then, if there is time remaining,
More informationGalaxies. With a touch of cosmology
Galaxies With a touch of cosmology Types of Galaxies Spiral Elliptical Irregular Spiral Galaxies Spiral Galaxies Disk component where the spiral arms are Interstellar medium Star formation Spheroidal
More informationQuestion 1. Question 2. Correct. Chapter 16 Homework. Part A
Chapter 16 Homework Due: 11:59pm on Thursday, November 17, 2016 To understand how points are awarded, read the Grading Policy for this assignment. Question 1 Following are a number of distinguishing characteristics
More informationAstronomy 113. Dr. Joseph E. Pesce, Ph.D. Distances & the Milky Way. The Curtis View. Our Galaxy. The Shapley View 3/27/18
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Distances & the Milky Way 14-2 Historical Overview: the Curtis-Shapley Debate ³What is the size of our galaxy? ³What is the nature of spiral nebula? The Curtis
More informationAstronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Distances & the Milky Way Historical Overview: the Curtis-Shapley Debate ³What is the size of our galaxy? ³What is the nature of spiral nebula? 14-2 ³Occurred in
More informationGalaxy Morphology. - a description of the structure of galaxies
Galaxy Morphology - a description of the structure of galaxies Galaxy Morphology - a description of the structure of galaxies Galaxy Morphology - a description of the structure of galaxies Clearly astronomical
More informationChapter 15 2/19/2014. Lecture Outline Hubble s Galaxy Classification. Normal and Active Galaxies Hubble s Galaxy Classification
Lecture Outline Chapter 15 Normal and Active Galaxies Spiral galaxies are classified according to the size of their central bulge. Chapter 15 Normal and Active Galaxies Type Sa has the largest central
More informationLECTURE 1: Introduction to Galaxies. The Milky Way on a clear night
LECTURE 1: Introduction to Galaxies The Milky Way on a clear night VISIBLE COMPONENTS OF THE MILKY WAY Our Sun is located 28,000 light years (8.58 kiloparsecs from the center of our Galaxy) in the Orion
More informationQuasars and Active Galactic Nuclei (AGN)
Quasars and Active Galactic Nuclei (AGN) Astronomy Summer School in Mongolia National University of Mongolia, Ulaanbaatar July 21-26, 2008 Kaz Sekiguchi Hubble Classification M94-Sa M81-Sb M101-Sc M87-E0
More informationUNIVERSITY OF SOUTHAMPTON
UNIVERSITY OF SOUTHAMPTON PHYS2013W1 SEMESTER 1 EXAMINATION 2012/13 GALAXIES Duration: 120 MINS Answer all questions in Section A and two and only two questions in Section B. Section A carries 1/3 of the
More informationAstronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION
Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION CHAPTER 14 The Milky Way Galaxy Lecture Presentation 14.0 the Milky Way galaxy How do we know the Milky Way exists? We can see it even though
More informationLecture 19: Galaxies. Astronomy 111
Lecture 19: Galaxies Astronomy 111 Galaxies What is a galaxy? Large assembly of stars, gas and dust, held together by gravity Sizes: Largest: ~1 Trillion stars (or more) Smallest: ~10 Million stars Milky
More informationThe Milky Way Galaxy
1/5/011 The Milky Way Galaxy Distribution of Globular Clusters around a Point in Sagittarius About 00 globular clusters are distributed in random directions around the center of our galaxy. 1 1/5/011 Structure
More informationASTRONOMY II Spring 1995 FINAL EXAM. Monday May 8th 2:00pm
ASTRONOMY II - 79202 Spring 1995 FINAL EXAM Monday May 8th 2:00pm Name: You have three hours to complete this exam. I suggest you read through the entire exam before you spend too much time on any one
More informationDistance Measuring Techniques and The Milky Way Galaxy
Distance Measuring Techniques and The Milky Way Galaxy Measuring distances to stars is one of the biggest challenges in Astronomy. If we had some standard candle, some star with a known luminosity, then
More informationLecture Outlines. Chapter 23. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 23 Astronomy Today 8th Edition Chaisson/McMillan Chapter 23 The Milky Way Galaxy Units of Chapter 23 23.1 Our Parent Galaxy 23.2 Measuring the Milky Way Discovery 23-1 Early Computers
More information1. Overview. Theory lags behind and there are many unsolved problems, including the nature of dark matter and dark energy.
PC2491: Galaxies 1. Overview The aim of this course is to understand the observed properties of galaxies in the hierarchical structure formation model. This is a particular exciting time to study galaxies
More informationStar systems like our Milky Way. Galaxies
Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in
More informationThe Milky Way & Galaxies
The Milky Way & Galaxies The Milky Way Appears as a milky band of light across the sky A small telescope reveals that it is composed of many stars (Galileo again!) Our knowledge of the Milky Way comes
More informationGalaxies. Need a (physically) meaningful way of describing the relevant properties of a galaxy.
Galaxies Aim to understand the characteristics of galaxies, how they have evolved in time, and how they depend on environment (location in space), size, mass, etc. Need a (physically) meaningful way of
More informationGalaxies -- Introduction. Classification -- Feb 13, 2014
Galaxies -- Introduction Classification -- Feb 13, 2014 Why Begin with Classification? The Hubble system forms the basic vocabulary of the subject. The sequence of galaxy types reflects an underlying physical
More informationHubble sequence galaxy classification scheme, originally based on appearance, but correlates with other properties as well.
Normal Galaxies (Ch. 24) Here we will cover topics in Ch. 24 up to 24.4, but then skip 24.4, 24.5. The sections we are skipping are all about processes that occur in the centers of galaxies, so I d like
More informationGalaxies. Lecture Topics. Lecture 23. Discovering Galaxies. Galaxy properties. Local Group. History Cepheid variable stars. Classifying galaxies
Galaxies Lecture 23 APOD: NGC 3628 (The Hamburger Galaxy) 1 Lecture Topics Discovering Galaxies History Cepheid variable stars Galaxy properties Classifying galaxies Local Group 2 23-1 Discovering Galaxies
More informationGalaxy clusters. Dept. of Physics of Complex Systems April 6, 2018
Galaxy clusters László Dobos Dept. of Physics of Complex Systems dobos@complex.elte.hu É 5.60 April 6, 2018 Satellite galaxies Large galaxies are surrounded by orbiting dwarfs approx. 14-16 satellites
More informationExam 4 Review EXAM COVERS LECTURES 22-29
Exam 4 Review EXAM COVERS LECTURES 22-29 Theoretically is there a center of the universe? Is there an edge? Do we know where Earth is on this? There is no center to the Universe, What kind of light we
More informationLaboratory: Milky Way
Department of Physics and Geology Laboratory: Milky Way Astronomy 1402 Equipment Needed Quantity Equipment Needed Quantity Milky Way galaxy Model 1 Ruler 1 1.1 Our Milky Way Part 1: Background Milky Way
More informationChapter 30. Galaxies and the Universe. Chapter 30:
Chapter 30 Galaxies and the Universe Chapter 30: Galaxies and the Universe Chapter 30.1: Stars with varying light output allowed astronomers to map the Milky Way, which has a halo, spiral arm, and a massive
More informationThe Galaxy. (The Milky Way Galaxy)
The Galaxy (The Milky Way Galaxy) Which is a picture of the Milky Way? A A is what we see from Earth inside the Milky Way while B is what the Milky Way might look like if we were far away looking back
More informationThe Milky Way. Overview: Number of Stars Mass Shape Size Age Sun s location. First ideas about MW structure. Wide-angle photo of the Milky Way
Figure 70.01 The Milky Way Wide-angle photo of the Milky Way Overview: Number of Stars Mass Shape Size Age Sun s location First ideas about MW structure Figure 70.03 Shapely (~1900): The system of globular
More informationLecture 30. The Galactic Center
Lecture 30 History of the Galaxy Populations and Enrichment Galactic Evolution Spiral Arms Galactic Types Apr 5, 2006 Astro 100 Lecture 30 1 The Galactic Center The nature of the center of the Galaxy is
More information1.4 Galaxy Light Distributions
26 1.4 Galaxy Light Distributions List of topics Hubble classification scheme see Binney & Merrifield text Galaxy surface brightness profiles (JL 2.3.1, plus additional material) Galaxy luminosity function
More informationGalaxies. CESAR s Booklet
What is a galaxy? Figure 1: A typical galaxy: our Milky Way (artist s impression). (Credit: NASA) A galaxy is a huge collection of stars and interstellar matter isolated in space and bound together by
More informationChapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo
Chapter 19 Galaxies Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past halo disk bulge Barred Spiral Galaxy: Has a bar of stars across the bulge Spiral Galaxy 1
More informationReminders! Observing Projects: Both due Monday. They will NOT be accepted late!!!
Reminders! Website: http://starsarestellar.blogspot.com/ Lectures 1-15 are available for download as study aids. Reading: You should have Chapters 1-14 read. Read Chapters 15-17 by the end of the week.
More information24.1 Hubble s Galaxy Classification
Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble s Law 24.4 XXActive Galactic Nuclei XXRelativistic Redshifts and Look-Back
More informationView of the Galaxy from within. Lecture 12: Galaxies. Comparison to an external disk galaxy. Where do we lie in our Galaxy?
Lecture 12: Galaxies View of the Galaxy from within The Milky Way galaxy Rotation curves and dark matter External galaxies and the Hubble classification scheme Plotting the sky brightness in galactic coordinates,
More informationTour of Galaxies. Sgr A* VLT in IR + adaptive optics. orbits. ASTR 1040 Accel Astro: Stars & Galaxies VLT IR+AO
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Kyle Augustson Lecture 23 Tues 8 Apr 08 zeus.colorado.edu/astr1040-toomre toomre Tour of Galaxies Briefly revisit Monster in the Milky Way
More informationASTR 101 Introduction to Astronomy: Stars & Galaxies
We observe star-gas-star cycle operating in Milky Way s disk using many different wavelengths of light! ASTR 101 Introduction to Astronomy: Stars & Galaxies Infrared light reveals stars whose visible light
More information2. Can observe radio waves from the nucleus see a strong radio source there Sagittarius A* or Sgr A*.
7/7 The Nucleus of the MW its center 1. Can t see the nucleus in visible light too much stuff in the way. 2. Can observe radio waves from the nucleus see a strong radio source there Sagittarius A* or Sgr
More informationGalaxies with Active Nuclei. Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes
Galaxies with Active Nuclei Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes Active Galactic Nuclei About 20 25% of galaxies do not fit well into Hubble categories
More informationChapter 23 The Milky Way Galaxy Pearson Education, Inc.
Chapter 23 The Milky Way Galaxy The Milky Way is our own galaxy viewed from the inside. It is a vast collection of more than 200 billion stars, planets, nebulae, clusters, dust and gas. Our own sun and
More informationGalaxies. The majority of known galaxies fall into one of three major classes: spirals (78 %), ellipticals (18 %) and irregulars (4 %).
Galaxies Collection of stars, gas and dust bound together by their common gravitational pull. Galaxies range from 10,000 to 200,000 light-years in size. 1781 Charles Messier 1923 Edwin Hubble The distribution
More informationGalaxies. Galaxy Diversity. Galaxies, AGN and Quasars. Physics 113 Goderya
Galaxies, AGN and Quasars Physics 113 Goderya Chapter(s): 16 and 17 Learning Outcomes: Galaxies Star systems like our Milky Way Contain a few thousand to tens of billions of stars. Large variety of shapes
More informationAy162, Spring 2006 Week 8 p. 1 of 15
Astronomy 162, Week 8 Milky Way Galaxy, continued Patrick S. Osmer Spring, 2006 Rotation of Galaxy How do we know the galaxy is rotating, and how do we measure its rotation? Measure radial velocities of
More informationGalaxy classification
Galaxy classification Questions of the Day What are elliptical, spiral, lenticular and dwarf galaxies? What is the Hubble sequence? What determines the colors of galaxies? Top View of the Milky Way The
More informationLecture Two: Galaxy Morphology:
Lecture Two: Galaxy Morphology: Looking more deeply at the Hubble Sequence Galaxy Morphology How do you quantify the properties of galaxies? and how do you put them in groups which allow you to study physically
More informationBROCK UNIVERSITY. Test 2, March 2018 Number of pages: 9 Course: ASTR 1P02, Section 1 Number of Students: 465 Date of Examination: March 12, 2018
BROCK UNIVERSITY Page 1 of 9 Test 2, March 2018 Number of pages: 9 Course: ASTR 1P02, Section 1 Number of Students: 465 Date of Examination: March 12, 2018 Number of hours: 50 min Time of Examination:
More informationSTRUCTURE OF GALAXIES
STRUCTURE OF GALAXIES 2., classification, surface photometry Piet van der Kruit Kapteyn Astronomical Institute University of Groningen the Netherlands February 2010, classification, surface photometry
More informationASTR 101 Introduction to Astronomy: Stars & Galaxies
ASTR 101 Introduction to Astronomy: Stars & Galaxies We observe star-gas-star cycle operating in Milky Way s disk using many different wavelengths of light Infrared light reveals stars whose visible light
More informationASTRON 449: Stellar (Galactic) Dynamics. Fall 2014
ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools
More informationBROCK UNIVERSITY. Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015
BROCK UNIVERSITY Page 1 of 9 Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015 Number of hours: 50 min Time of Examination: 18:00 18:50
More informationSurvey of Astrophysics A110
Goals: Galaxies To determine the types and distributions of galaxies? How do we measure the mass of galaxies and what comprises this mass? How do we measure distances to galaxies and what does this tell
More informationDark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab
Dark Matter ASTR 2120 Sarazin Bullet Cluster of Galaxies - Dark Matter Lab Mergers: Test of Dark Matter vs. Modified Gravity Gas behind DM Galaxies DM = location of gravity Gas = location of most baryons
More informationIntroduction to Galaxies
Introduction to Galaxies History Famous Galaxies Catalogs and Atlases Classification Schemes What is a galaxy? - A gravitationally bound collection of stars - A galaxy has 10 6 to 10 12 stars - Participates
More informationGALAXIES. I. Morphologies and classification 2. Successes of Hubble scheme 3. Problems with Hubble scheme 4. Galaxies in other wavelengths
GALAXIES I. Morphologies and classification 2. Successes of Hubble scheme 3. Problems with Hubble scheme 4. Galaxies in other wavelengths 5. Properties of spirals and Irregulars. Hubble tuning-fork diagram.
More information4/6/17. SEMI-WARM stuff: dust. Tour of Galaxies. Our Schedule
ASTR 1040: Stars & Galaxies Super-bubble blowout in NGC 3709 Prof. Juri Toomre TAs: Piyush Agrawal, Connor Bice Lecture 22 Thur 6 Apr 2017 zeus.colorado.edu/astr1040-toomre Tour of Galaxies Look at complex
More informationGalaxies & Introduction to Cosmology
Galaxies & Introduction to Cosmology Other Galaxies: How many are there? Hubble Deep Field Project 100 hour exposures over 10 days Covered an area of the sky about 1/100 the size of the full moon Probably
More informationLESSON 1. Solar System
Astronomy Notes LESSON 1 Solar System 11.1 Structure of the Solar System axis of rotation period of rotation period of revolution ellipse astronomical unit What is the solar system? 11.1 Structure of the
More informationOur Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky.
Our Galaxy Our Galaxy We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky. Early attempts to locate our solar system produced erroneous results.
More informationWhat is the solar system?
Notes Astronomy What is the solar system? 11.1 Structure of the Solar System Our solar system includes planets and dwarf planets, their moons, a star called the Sun, asteroids and comets. Planets, dwarf
More informationLecture Outlines. Chapter 25. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 25 Astronomy Today 7th Edition Chaisson/McMillan Chapter 25 Galaxies and Dark Matter Units of Chapter 25 25.1 Dark Matter in the Universe 25.2 Galaxy Collisions 25.3 Galaxy Formation
More informationOther Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies
Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at
More informationASTRO 310: Galactic & Extragalactic Astronomy Prof. Jeff Kenney
ASTRO 310: Galactic & Extragalactic Astronomy Prof. Jeff Kenney Class 3 January 23, 2017 The Milky Way Galaxy: Vertical Distributions of Stars & the Stellar Disk disks exist in many astrophysical systems
More informationGalaxies: Structure, formation and evolution
Galaxies: Structure, formation and evolution Lecture 1 Yogesh Wadadekar Jan-Feb 2017 IUCAA-NCRA Grad School 1 / 29 Galaxies are a very active field of research today! About 25% of papers published on ADS
More information11/8/18. Tour of Galaxies. Our Schedule
ASTR 1040: Stars & Galaxies Super-bubble blowout in NGC 3709 Prof. Juri Toomre TAs: Ryan Horton, Loren Matilsky Lecture 22 Thur 8 Nov 2018 zeus.colorado.edu/astr1040-toomre Tour of Galaxies Look at complex
More informationGalaxy Classification
Galaxies Galaxies are collections of billons of stars; our home galaxy, the Milky Way, is a typical example. Stars, gas, and interstellar dust orbit the center of the galaxy due to the gravitational attraction
More informationAstronomy 114. Lecture 27: The Galaxy. Martin D. Weinberg. UMass/Astronomy Department
Astronomy 114 Lecture 27: The Galaxy Martin D. Weinberg weinberg@astro.umass.edu UMass/Astronomy Department A114: Lecture 27 18 Apr 2007 Read: Ch. 25,26 Astronomy 114 1/23 Announcements Quiz #2: we re
More informationASTR 1120 General Astronomy: Stars & Galaxies
ASTR 1120 General Astronomy: Stars & Galaxies!NNOUNCEMENTS HOMEWORK #6 DUE TODAY, by 5pm HOMEWORK #7 DUE Nov. 10, by 5pm Dark matter halo for galaxies Dark matter extends beyond visible part of the galaxy
More informationChapter 15 The Milky Way Galaxy. The Milky Way
Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our
More informationActive Galaxies & Quasars
Active Galaxies & Quasars Normal Galaxy Active Galaxy Galactic Nuclei Bright Active Galaxy NGC 5548 Galaxy Nucleus: Exact center of a galaxy and its immediate surroundings. If a spiral galaxy, it is the
More informationASTR 1120 General Astronomy: Stars & Galaxies
ASTR 1120 General Astronomy: Stars & Galaxies!NNOUNCEMENTS HOMEWORK #6 DUE TODAY, by 5pm HOMEWORK #7 DUE Nov. 10, by 5pm Dark matter halo for galaxies REVIEW Dark matter extends beyond visible part of
More informationM31 - Andromeda Galaxy M110 M32
UNIT 4 - Galaxies XIV. The Milky Way galaxy - a huge collection of millions or billions of stars, gas, and dust, isolated in space and held together by its own gravity M110 M31 - Andromeda Galaxy A. Structure
More informationAST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation!
AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation! Bring pencil #2 with eraser No use of calculator or any electronic device during the exam We provide the scantrons
More informationThe distance modulus in the presence of absorption is given by
Problem 4: An A0 main sequence star is observed at a distance of 100 pc through an interstellar dust cloud. Furthermore, it is observed with a color index B-V = 1.5. What is the apparent visual magnitude
More informationAstr 5465 Feb. 13, 2018 Distribution & Classification of Galaxies Distribution of Galaxies
Astr 5465 Feb. 13, 2018 Distribution & Classification of Galaxies Distribution of Galaxies Faintest galaxies are distributed ~ uniformly over the sky except for the Galactic plane (zone of avoidance) Brighter
More informationActive Galactic Nuclei (AGNs): A type of AGNs: Quasars. Whatever is powering these QSO s must be very small!!
Active Galactic Nuclei (AGNs): Galaxies with lots of activity AST 101 General Astronomy: Stars & Galaxies Some galaxies at high redshift (large lookback times) have extremely active centers More than 1000
More informationBHS Astronomy: Galaxy Classification and Evolution
Name Pd Date BHS Astronomy: Galaxy Classification and Evolution This lab comes from http://cosmos.phy.tufts.edu/~zirbel/ast21/homework/hw-8.pdf (Tufts University) The word galaxy, having been used in English
More informationA100 Exploring the Universe: The Milky Way as a Galaxy. Martin D. Weinberg UMass Astronomy
A100 Exploring the Universe: The Milky Way as a Galaxy Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu November 12, 2014 Read: Chap 19 11/12/14 slide 1 Exam #2 Returned and posted tomorrow
More informationOur Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye
Our Galaxy Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust Held together by gravity! The Milky Way with the Naked Eye We get a special view of our own galaxy because we are part of it!
More informationAddition to the Lecture on Galactic Evolution
Addition to the Lecture on Galactic Evolution Rapid Encounters In case the encounter of two galaxies is quite fast, there will be not much dynamical friction due to lack of the density enhancement The
More informationOur Galaxy. Chapter Twenty-Five. Guiding Questions
Our Galaxy Chapter Twenty-Five Guiding Questions 1. What is our Galaxy? How do astronomers know where we are located within it? 2. What is the shape and size of our Galaxy? 3. How do we know that our Galaxy
More informationGalaxies and Cosmology
F. Combes P. Boisse A. Mazure A. Blanchard Galaxies and Cosmology Translated by M. Seymour With 192 Figures Springer Contents General Introduction 1 1 The Classification and Morphology of Galaxies 5 1.1
More informationSTRUCTURE OF GALAXIES
STRUCTURE OF GALAXIES CONTENTS OF THE COURSE 1. Structure, kinematics and dynamics of the Galaxy 2. Stellar populations, classification, surface photometry 3. Luminosity distributions and component analysis
More informationGalaxies and the Universe. Our Galaxy - The Milky Way The Interstellar Medium
Galaxies and the Universe Our Galaxy - The Milky Way The Interstellar Medium Our view of the Milky Way The Radio Sky COBE Image of our Galaxy The Milky Way Galaxy - The Galaxy By Visual Observation
More informationGalaxies. Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations
Galaxies Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations Cepheids in M31 Up to 1920s, the Milky Way was thought by
More informationChapter 19 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Our Galaxy Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition Our Galaxy 19.1 The Milky Way Revealed What does our galaxy look like? How do stars orbit in our galaxy? Where are globular clusters located
More informationBig Galaxies Are Rare! Cepheid Distance Measurement. Clusters of Galaxies. The Nature of Galaxies
Big Galaxies Are Rare! Potato Chip Rule: More small things than large things Big, bright spirals are easy to see, but least common Dwarf ellipticals & irregulars are most common Faint, hard to see Mostly
More informationThe Milky Way - Chapter 23
The Milky Way - Chapter 23 The Milky Way Galaxy A galaxy: huge collection of stars (10 7-10 13 ) and interstellar matter (gas & dust). Held together by gravity. Much bigger than any star cluster we have
More informationAS1001:Extra-Galactic Astronomy. Lecture 3: Galaxy Fundamentals
AS1001:Extra-Galactic Astronomy Lecture 3: Galaxy Fundamentals Galaxy Fundamentals How many stars are in a galaxy? How did galaxies form? How many galaxies are there? How far apart are they? How are they
More informationSKINAKAS OBSERVATORY. Astronomy Projects for University Students PROJECT GALAXIES
PROJECT 7 GALAXIES Objective: The topics covered in the previous lessons target celestial objects located in our neighbourhood, i.e. objects which are within our own Galaxy. However, the Universe extends
More informationLecture 25 The Milky Way Galaxy November 29, 2017
Lecture 25 The Milky Way Galaxy November 29, 2017 1 2 Size of the Universe The Milky Way galaxy is very much larger than the solar system Powers of Ten interactive applet 3 Galaxies Large collections of
More informationThe King's University College Astronomy 201 Mid-Term Exam Solutions
The King's University College Astronomy 201 Mid-Term Exam Solutions Instructions: The exam consists of two sections. Part A is 20 multiple choice questions - please record answers on the sheet provided.
More informationQuasars: Back to the Infant Universe
Quasars: Back to the Infant Universe Learning Objectives! What is a quasar? What spectral features tell us quasars are very redshifted (very distant)? What spectral features tell us they are composed of
More informationOur View of the Milky Way. 23. The Milky Way Galaxy
23. The Milky Way Galaxy The Sun s location in the Milky Way galaxy Nonvisible Milky Way galaxy observations The Milky Way has spiral arms Dark matter in the Milky Way galaxy Density waves produce spiral
More information