Normal Galaxies ASTR 2120 Sarazin
|
|
- Malcolm Rice
- 5 years ago
- Views:
Transcription
1 Normal Galaxies ASTR 2120 Sarazin
2 Test #2 Monday, April 8, 11-11:50 am ASTR 265 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other materials or any person You may bring a 3x5 card with equations ~2/3 Quantitative Problems (like homework problems) ~1/3 Qualitative Questions Multiple Choice, Short Answer, Fill In the Blank questions No essay questions
3 Normal Galaxies ASTR 2120 Sarazin
4 Edwin Hubble (1923) Andromeda Galaxy (M31)
5 Galaxy Hubble Types
6 Galaxy Hubble Types
7 Morphology (shape) Elliptical Galaxies Label En n = 10 (a-b)/a E0 (round) to E7 b a
8 Elliptical Galaxies M87 E0 pec in Virgo cluster
9 Elliptical Galaxies M49 = NGC4472 E2 in Virgo cluster
10 Elliptical Galaxies NGC4697 E6 in Virgo cluster
11 Galaxy Hubble Types unbarred barred
12 Morphology (shape) Spiral Galaxies Label Sx or SBx B = barred, = unbarred unbarred x = a, ab, b, bc, c, cd, d barred
13 Galaxy Hubble Types
14 Unbarred Spiral Galaxies M51 Unbarred spiral
15 Unbarred Spiral Galaxies M74 Unbarred spiral
16 Galaxy Hubble Types
17 Barred Spiral Galaxies M83 Barred spiral
18 Barred Spiral Galaxies M109 Barred spiral
19 Barred Spiral Galaxies M91 Barred spiral
20 Galaxy Hubble Types early late
21 Morphology (shape) Spiral Galaxies Label Sx or SBx B = barred, = unbarred unbarred x = a, ab, b, bc, c, cd, d a = tightly wound, smooth spiral arms, large nuclear bulge c = open, patchy spiral arms (H II regions), small nuclear bulge barred
22 Early vs. Late Spiral Galaxies M81 Sab
23 Early vs. Late Spiral Galaxies M31 Andromeda Sb
24 Early vs. Late Spiral Galaxies M51 Sbc
25 Early vs. Late Spiral Galaxies M33 Scd
26 Early vs. Late Spiral Galaxies M104 Sombrero Sa edge on
27 Early vs. Late Spiral Galaxies Sb edge on
28 Early vs. Late Spiral Galaxies Sc edge on
29 Galaxy Hubble Types S0 = Lenticular late
30 S0 = Lenticular Galaxies Morphology (shape) Label S0 or SB0 B = barred, = unbarred Very large bulge Disk, but no (strong) spiral arms
31 S0 = Lenticular Galaxies M102 S0 edge on
32 S0 = Lenticular Galaxies NGC5866 S0 edge on
33 S0 = Lenticular Galaxies NGC2784 S0 more face on No spiral arms
34 Galaxy Hubble Types
35 Irregular Galaxies Messy, full of gas and dust, young stars Hints of disk, spiral arms Galaxies in the process of forming Today, nearly all irregular galaxies are small In past (at high redshift), large irregular galaxies
36 Irregular Galaxies Large Magellanic Cloud LMC Irregular
37 Irregular Galaxies Small Magellanic Cloud SMC Irregular
38 Elliptical Galaxies M87 Only old stars Nearly no cool gas or dust No star formation Ellipticals are: Red and Dead
39 Spiral Galaxies M51 Young and old stars Spiral arms Bluer Lots of cool gas or dust Lots of star formation
40 Irregular Galaxies LMC Mainly young stars Very blue Lots of cool gas or dust Lots of star formation Hints of disk, spiral arms
41 Elliptical, S0 vs. Spiral, Irr color E, S0: red clump Sp, Irr: blue cloud Abs. Mag
42 Elliptical and S0 Galaxies Found in dense environments Clusters of galaxies
43 Sp and Irr Galaxies Found in low density environments Isolated and groups
44 Hubble Tuning Fork Diagram
45 Hubble Tuning Fork Diagram
46 Hubble Tuning Fork Diagram
47 Hubble Classes Sequence in: round (spheroid) flat (disk) random orbits circular orbits in disk red blue old stars young stars little cool gas and dust lots of cool gas and dust dense environments sparse environments
48
49 Hubble sequence as discussed
50
51 Galaxy Properties 1) Luminosity, Mass, Diameter Ellipticals: Very large range: dwarf ellipticals, 10 5 L (globular clusters?) giant ellipticals brightest cluster galaxies (BCGs or cds), L BCGs are the largest galaxies in Universe Spirals: Smaller range of sizes
52 Galaxy Properties (Cont.) 2) Light Distributions E, Sp & S0 Bulges: r I(r) = I(0) exp[ (r / r e ) 1/4 ] De Vaucouleurs Law r e = effective radius, 1/2 of light comes inside of r e in projection r e = kpc I(0) ~ constant for normal ellipticals (Freeman s Law)
53 Galaxy Properties (Cont.) 2) Light Distributions (cont.) Sp & S0 Disks: I(r) = I(0) exp( - r / r o ) r o = 1-5 kpc I(0) ~ constant for spirals
54 Galaxy Properties (Cont.) 3) Motions Sp & S0 Disks: Nearly circular orbits in the plane of the disk, all in the same direction
55 Galaxy Properties (Cont.) Sp & S0 Disks: View at inclination i v r = v rot (r) sin f sin i radial velocity, Doppler shift Apparent disk = ellipse us i b a f Along major axis a v r = v rot (r) sin i cos i = b/a for very thin disk, no dust
56 Galaxy Properties (Cont.) Sp & S0 Disks: v rot (r) ~ constant outside of center (same as MW)
57 Galaxy Properties (Cont.) 3) Motions Ellipticals: Why are ellipticals elliptical? What is their 3D shape? a) Rotation? No Shape would be oblate spheroid v r would vary across galaxy, not true b) Random stellar motions
58 Galaxy Properties (Cont.) Elliptical motions s r2 b) Random stellar motions No rotation, but many different v r along line-of sight broaden spectral lines º <v r2 > in CM frame If spherical, s 2 = 3 s r 2
59 Galaxy Properties (Cont.) Elliptical motions: Why not spherical? Stars move different speeds in different directions Can be different in all 3 directions triaxial ellipsoids slower faster
60 Galaxy Properties (Cont.) 4) Masses Sp & S0 Disks: v rot (r) = GM (r) r M (r) = v 2 rot (r) r G v rot (r) constant M tot (r) r, most mass at large radii ρ tot (r) 1 r 2, but light and stars e r /r 0
61 Galaxy Properties (Cont.) 4) Masses Sp & S0 disks: Massive Dark Matter Halos Extend out to ~ 100 kpc M(Dark Matter) > 10 x M(stars and gas)
62 Galaxy Properties (Cont.) 4) Masses Es, Sp & S0 bulges: Random velocities σ r = radial velocity dispersion σ = 3D velocity dispersion Virial Theorem : KE = - PE/2 1 2 Mσ 2 = 1 2 M = σ 2 R G GM 2 R
Galaxy 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 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 informationASTRO504 Extragalactic Astronomy. 2. Classification
ASTRO504 Extragalactic Astronomy 2. Classification Morphological classification Elliptical (E) galaxies Lenticular (SO) galaxies Spiral (S) galaxies Irregular (Im) galaxies The realm of nebulae Hubble
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 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 informationAn Introduction to Galaxies and Cosmology. Jun 29, 2005 Chap.2.1~2.3
An Introduction to Galaxies and Cosmology Jun 29, 2005 Chap.2.1~2.3 2.1 Introduction external galaxies normal galaxies - majority active galaxies - 2% high luminosity (non-stellar origin) variability
More informationGalaxies. Early Attempts to catalog and classify. Messier Catalog. "The Great Debate" PHY galaxies - J. Hedberg
Galaxies 1. Early Attempts to catalog and classify 1. Messier Catalog 2. "The Great Debate" 3. Spiral: Andromeda 4. Ellipticals 2. Updates to the scheme 1. NGC1300 2. Grand Design Spiral 3. Grand Design
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 informationGalaxies The Hubble Sequence Different Types of Galaxies 4 broad Morphological Types created by Edwin Hubble Galaxies come is a variety of shapes and
Galaxies The Hubble Sequence Different Types of Galaxies 4 broad Morphological Types created by Edwin Hubble Galaxies come is a variety of shapes and sizes Edwin Hubble classified the galaxies into four
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 informationGalaxies. Early Attempts to catalog and classify. Messier Catalog. "The Great Debate"
Galaxies 1. Early Attempts to catalog and classify 1. Messier Catalog 2. "The Great Debate" 3. Spiral: Andromeda 4. Ellipticals 2. Updates to the scheme 1. NGC1300 2. Grand Design Spiral 3. Flocculent
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 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 informationLecture 27 Galaxy Types and the Distance Ladder December 3, 2018
Lecture 27 Galaxy Types and the Distance Ladder December 3, 2018 1 2 Early Observations Some galaxies had been observed before 1900 s. Distances were not known. Some looked like faint spirals. Originally
More information2 Galaxy morphology and classification
2 Galaxy morphology and classification Galaxy classification is an important first step towards a physical understanding of the nature of these objects. For a detailed description of classification systems
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 informationmidterm exam thurs june 14 morning? evening? fri june 15 morning? evening? sat june 16 morning? afternoon? sun june 17 morning? afternoon?
Prof. Jeff Kenney Class 11 June 11, 2018 midterm exam thurs june 14 morning? evening? fri june 15 morning? evening? sat june 16 morning? afternoon? sun june 17 morning? afternoon? observing session tomorrow
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 informationOutline. The Rotation of the Galaxy. Astronomy: The Big Picture
I decided to cancel class next week! No homework until you get back. Honor credit need to have those papers soon! Exam 2 Grades are posted. Nighttime observing should be posted today. Interest in grade
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 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 informationClicker Question: Galaxy Classification. What type of galaxy do we live in? The Variety of Galaxy Morphologies Another barred galaxy
Galaxies Galaxies First spiral nebula found in 1845 by the Earl of Rosse. Speculated it was beyond our Galaxy. 1920 - "Great Debate" between Shapley and Curtis on whether spiral nebulae were galaxies beyond
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 informationOn Today s s Radar. ASTR 1040 Accel Astro: Stars & Galaxies. Sb) Andromeda M31 (Sb( Andromeda surprises with Spitzer in IR
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TAs: Nicholas Nelson, Zeeshan Parkar Lecture 24 Thur 8 Apr 2010 zeus.colorado.edu/astr1040-toomre toomre NGC 1232 Spiral Sb On Today s s Radar
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 informationThe Milky Way - 2 ASTR 2110 Sarazin. Center of the Milky Way
The Milky Way - 2 ASTR 2110 Sarazin Center of the Milky Way Final Exam Tuesday, December 12, 9:00 am noon Ruffner G006 (classroom) You may not consult the text, your notes, or any other materials or any
More informationGalaxies. What is a Galaxy? A bit of History. A bit of History. Three major components: 1. A thin disk consisting of young and intermediate age stars
What is a Galaxy? Galaxies A galaxy is a collection of billions of stars, dust, and gas all held together by gravity. Galaxies are scattered throughout the universe. They vary greatly in size and shape.
More informationHow did the universe form? 1 and 2
Galaxies How did the universe form? 1 and 2 Galaxies Astronomers estimate that 40 billion galaxies exist in the observable universe The universe may contain over 100 billion galaxies Even a modest-sized
More informationGalaxies. Nebulae. Virgo Cluster of Galaxies sky.google.com
Virgo Cluster of Galaxies sky.google.com Galaxies Mid 18th century, Kant and Wright suggested that the Milky Way is a finite system of stars. Turns out this is accurate. Kant went on to suggest that the
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 information4/10/18. Our wide world (universe) of Galaxies. Spirals ~80% of galaxies
ASTR 1040: Stars & Galaxies Prof. Juri Toomre TAs: Peri Johnson, Ryan Horton Lecture 23 Tues 10 Apr 2018 zeus.colorado.edu/astr1040-toomre Our wide world (universe) of Galaxies The rich range of galaxies:
More informationMorphology The Study of the Basic Pattern of Things
Morphology The Study of the Basic Pattern of Things Fundamental Considerations Different libraries of galaxies are liable to lead to the ID of different classes Images in library must be homogeneous (filter,
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 informationTuesday, Thursday 2:30-3:45 pm. Astronomy 100. Tom Burbine
Astronomy 100 Tuesday, Thursday 2:30-3:45 pm Tom Burbine tburbine@mtholyoke.edu www.xanga.com/astronomy100 OWL assignment (Due Today) There is be an OWL assignment due on Thursday April 14 at 11:59 pm.
More informationLET S MAKE A PORTRAIT OF A GALAXY
LET S MAKE A PORTRAIT OF A GALAXY Veselka S. Radeva EAAE Summer School Working Group (Bulgaria) Abstract The goal of the exercise is for students to learn about the different types of galaxies, about the
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 informationLecture 15: Galaxy morphology and environment
GALAXIES 626 Lecture 15: Galaxy morphology and environment Why classify galaxies? The Hubble system gives us our basic description of galaxies. The sequence of galaxy types may reflect an underlying physical
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 informationMore on Galaxy Classifcation
More on Galaxy Classifcation Trends within the Hubble Sequence E0 --> S0 --> Sb Decreasing bulge to disk ratio Decreasing stellar age Increasing gas content Increasing star formation rate Problems Constructed
More informationLecture 2: Galaxy types, spectra
Lecture 2: Galaxy types, spectra Galaxies AS 3011 1 Hubble tuning fork this is really just descriptive, but Hubble suggested galaxies evolve from left to right in this picture not unreasonable, perhaps
More informationLecture 2: Galaxy types, spectra. Galaxies AS
Lecture 2: Galaxy types, spectra Galaxies AS 3011 1 Hubble tuning fork this is really just descriptive, but Hubble suggested galaxies evolve from left to right in this picture not unreasonable, perhaps
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 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 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 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 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 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 informationApril 11, Astronomy Notes Chapter 16.notebook. Types of Galaxies
The Milky Way is just one of about 50 billion galaxies that are thought to exist. Just as stars can be classified using an H R diagram, galaxies can also be classified according to certain physical properties.
More informationMajor Review: A very dense article" Dawes Review 4: Spiral Structures in Disc Galaxies; C. Dobbs and J Baba arxiv "
The Components of a Spiral Galaxy-a Bit of a Review- See MBW chap 11! we have discussed this in the context of the Milky Way" Disks:" Rotationally supported, lots of gas, dust, star formation occurs in
More informationLecture 14: Other Galaxies A2020 Prof. Tom Megeath. The Milky Way in the Infrared 3/17/10. NGC 7331: the Milky Way s Twins. Spiral Galaxy bulge halo
Lecture 14: Other Galaxies A2020 Prof. Tom Megeath Our Galaxy: Side View We see our galaxy edge-on Primary features: Disk: young and old stars where we live. Bulge: older stars Halo: oldest stars, globular
More informationChapter 17. Galaxies. Copyright The McGraw-Hill Companies, Inc. Permission required for reproduction or display.
Chapter 17 Galaxies Copyright The McGraw-Hill Companies, Inc. Permission required for reproduction or display. Galaxies Beyond the Milky Way are billions of other galaxies Some galaxies are spiral like
More informationGalaxies: Classification. Galaxy Classification. galaxies; late types : spiral galaxies, Not an evolutionary sequence!
17 1 Galaxies: lassification Galaxy lassification 17 2 1920s: Hubble and others: classification of galaxies orphology: ppearance on photographs, photographic emulsion is blue sensitive Warning: scheme
More informationToday in Astronomy 142
! The epicyclic frequency Today in Astronomy 142! Summary of spiral structure, density waves! Elliptical, lenticular and irregular galaxies! Distribution of mass and light in normal galaxies Background:
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 informationAS1001:Extra-Galactic Astronomy
AS1001:Extra-Galactic Astronomy Lecture 5: Dark Matter Simon Driver Theatre B spd3@st-andrews.ac.uk http://www-star.st-and.ac.uk/~spd3 Stars and Gas in Galaxies Stars form from gas in galaxy In the high-density
More informationThe Milky Way. Finding the Center. Milky Way Composite Photo. Finding the Center. Milky Way : A band of and a. Milky Way
The Milky Way Milky Way : A band of and a The band of light we see is really 100 billion stars Milky Way probably looks like Andromeda. Milky Way Composite Photo Milky Way Before the 1920 s, astronomers
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 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 informationLecture Two: Observed Properties of Galaxies
Lecture Two: Observed Properties of Galaxies http://www.astro.rug.nl/~etolstoy/gfe14/index.html Longair, chapter 3 Wednesday 5th Feb Binney & Merrifield, chapter 4 1 From pretty picture to science 2 Galaxies
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 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 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 informationThis week at Astro Lecture 06, Sep 13, Pick up PE#6. Please turn in HW#2. HW#3 is posted
This week at Astro 3303 Lecture 06, Sep 13, 2017 Pick up PE#6 Please turn in HW#2 HW#3 is posted Today: Introduction to galaxy photometry Quantitative morphology Elliptical galaxies Reading: Continue reading
More informationLecture 28: Spiral Galaxies Readings: Section 25-4, 25-5, and 26-3
Lecture 28: Spiral Galaxies Readings: Section 25-4, 25-5, and 26-3 Key Ideas: Disk & Spheroid Components Old Stars in Spheroid Old & Young Stars in Disk Rotation of the Disk: Differential Rotation Pattern
More informationThe physical properties of galaxies in Universe
The physical properties of galaxies in Universe Iurii Babyk, Dublin Institute for Advanced Studies, Dublin City University, Main Astronomical Observatory of the NAS of Ukraine. Introduction Large-Scale
More informationThe Discovery of Other Galaxies. 24. Normal Galaxies
24. Normal Galaxies The discovery of other galaxies Edwin Hubble proved galaxies are very distant Edwin Hubble classified galaxies by shape Methods for determining distances to galaxies The Hubble Law
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 informationtuning fork ellipticals, spirals, irregulars. Hubble Sequence.
Hubble arranged his sequence on a tuning fork diagram. Originally he (incorrectly) hypothesized that galaxies evolved from the Left to the Right of this sequence. Early types Later types Hubble went on
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 informationLecture 33: Announcements
Lecture 33: Announcements 1) Pick up graded hwk 5. Good job: Jessica, Jessica, and Elizabeth for a 100% score on hwk 5 and the other 25% of the class with an A. 2) Article and homework 7 were posted on
More informationGalaxies Guiding Questions
Galaxies Guiding Questions How did astronomers first discover other galaxies? How did astronomers first determine the distances to galaxies? Do all galaxies have spiral arms, like the Milky Way? How do
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 informationInternational Herald Tribune, November 1, 1907
Recently reports have been current in certain newspapers that Mr. Thomas A. Edison, the inventor, has at last perfected the storage battery, and that within a few months electrically propelled vehicles,
More informationIt is about 100,000 ly across, 2,000 ly thick, and our solar system is located 26,000 ly away from the center of the galaxy.
The Galaxies The Milky Way Galaxy Is a spiral galaxy in which our solar system is located. The center of the galaxy lies in the Sagittarius Constellation. It is about 100,000 ly across, 2,000 ly thick,
More informationSTRUCTURE AND DYNAMICS OF GALAXIES
STRUCTURE AND DYNAMICS OF GALAXIES 3., classification of galaxies Piet van der Kruit Kapteyn Astronomical Institute University of Groningen, the Netherlands www.astro.rug.nl/ vdkruit Beijing, September
More informationTHE HUBBLE SEQUENCE. This use case explores the morphology of galaxies and their classification according to the Hubble Sequence.
THE HUBBLE SEQUENCE G. Iafrate (a), M. Ramella (a) e V. Bologna (b) (a) INAF - Astronomical Observatory of Trieste (b) Istituto Comprensivo S. Giovanni - Sc. Sec. di primo grado M. Codermatz" - Trieste
More informationA100H Exploring the Universe: Discovering Galaxies. Martin D. Weinberg UMass Astronomy
A100H Exploring the Universe: Discovering Galaxies Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 05, 2016 Read: Chap 19 04/05/16 slide 1 Exam #2 Returned by next class meeting
More informationASTR 100. Lecture 28: Galaxy classification and lookback time
ASTR 100 Lecture 28: Galaxy classification and lookback time Galaxies in general: Ch. 15, [16.2], in Essential Tuesday: Hubble s law Today: Types of galaxies The Hubble tuning fork Galaxy classification
More informationGALACTIC DYNAMICS AND INTERSTELLAR MATTER
GALACTIC DYNAMICS AND INTERSTELLAR MATTER Isaac Shlosman Department of Physics and Astronomy University of Kentucky at Lexington, USA and Theoretical Astrophysics Osaka University, Japan The goal: Explain
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 and Cosmology
4/28/17 The Discovery of Galaxies Up to the 1920 s, astronomers were not sure exactly how far away galaxies were, and thus didn t know how big they are! Spiral Nebulae could be assumed to be inside our
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 informationDark Matter: Observational Constraints
Dark Matter: Observational Constraints Properties of Dark Matter: What is it? And what isn t it? Leo Blitz UC Berkeley Stanford July 31, 2007 How much is there? WMAP results Rotation curves of Galaxies
More informationLecture #21: Plan. Normal Galaxies. Classification Properties Distances
Lecture #21: Plan Normal Galaxies Classification Properties Distances Messier 31 = M31 Early 20 th Century The Great Debate (4/26/1920): Harlow Shapley (Mt Wilson) vs Heber Curtis (Lick Observatory) Smithsonian
More informationAy 127 Systematics of Galaxy Properties and Scaling Relations
Ay 127 Systematics of Galaxy Properties and Scaling Relations Morphological Classification and Galaxy Types The first step in any empirical science: look for patterns and trends, then try to understand
More informationHW#4 is due next Monday Part of it is to read a paper and answer questions about what you read If you have questions, ask me!
Sep 21, 2015 Elliptical galaxies overview Shapes: evidence for triaxiality, isophotal twists, structure What causes flattening in ellipticals? Classes of ellipticals: Disky vs boxy Flat core vs cuspy/power-law
More informationSpiral Structure. m ( Ω Ω gp ) = n κ. Closed orbits in non-inertial frames can explain the spiral pattern
Spiral Structure In the mid-1960s Lin and Shu proposed that the spiral structure is caused by long-lived quasistatic density waves The density would be higher by about 10% to 20% Stars, dust and gas clouds
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 informationThe Milky Way. Mass of the Galaxy, Part 2. Mass of the Galaxy, Part 1. Phys1403 Stars and Galaxies Instructor: Dr. Goderya
Foundations Chapter of Astronomy 15 13e Our Milky Way Seeds Phys1403 Stars and Galaxies Instructor: Dr. Goderya Selected Topics in Chapter 15 A view our Milky Way? The Size of our Milky Way The Mass of
More informationPractice Test: ES-5 Galaxies
Class: Date: Practice Test: ES-5 Galaxies Multiple Choice Identify the letter of the choice that best completes the statement or answers the question. Light Years * The distance between stars and galaxies
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 informationWhittle : EXTRAGALACTIC ASTRONOMY 5. SPIRAL GALAXIES
Whittle : EXTRAGALACTIC ASTRONOMY 1 : Preliminaries 6 : Dynamics I 11 : Star Formation 16 : Cosmology : Morphology 7 : Ellipticals 1 : Interactions 17 : Structure Growth 3 : Surveys 8 : Dynamics II 13
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 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 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 informationSurface Brightness of Spiral Galaxies
Surface Brightness of Spiral Galaxies M104: SA N4535: SAB LMC: dwarf irregular,barred Normal 1/4-law+exp fits An example of surface brightness profile. The top curve is the sum of exp disk+1/4-bulge. The
More informationClassification Distribution in Space Galaxy Clusters. Formation and Evolution Hubble s Law
The American astronomer Edwin Hubble in 1924, according to appearance of galaxies categorized them into four basic types. Classification Distribution in Space Galaxy Clusters Masses Formation and Evolution
More informationThe Universe o. Galaxies. The Universe of. Galaxies. Ajit Kembhavi IUCAA
Hello! The Universe of Galaxies The Universe o Galaxies Ajit Kembhavi IUCAA Galaxies: Stars: ~10 11 Mass: ~10 11 M Sun Contain stars, gas and dust, possibly a supermassive black hole at the centre. Much
More informationSummary: Nuclear burning in stars
Summary: Nuclear burning in stars Reaction 4 1 H 4 He 3 4 He 12 C 12 C + 4 He 16 O, Ne, Na, Mg Ne O, Mg O Mg, S Si Fe peak Min. Temp. 10 7 o K 2x10 8 8x10 8 1.5x10 9 2x10 9 3x10 9 Evolution through nuclear
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 information