Lecture 6: distribution of stars in. elliptical galaxies
|
|
- Rodger McKenzie
- 8 years ago
- Views:
Transcription
1 Lecture 6: distribution of stars in topics: elliptical galaxies examples of elliptical galaxies different classes of ellipticals equation for distribution of light actual distributions and more complex shapes later lecture: dynamics of elliptical galaxies that produce the stellar distribution Galaxies AS
2 M32 local ellipticals E2 at 750 kpc, satellite of M31 spiral NGC 205, 147, 185 de s at kpc Sagittarius, Sculptor, Fornax etc. dsph at 25 kpc these are part of the Local Group of galaxies Milky Way is a major member of this Galaxies AS
3 NGC 185 Phoenix dwarf And VI dwarf images from seds.org Galaxies AS
4 Galaxies AS image from anzwers.org
5 local dwarfs and spheroidals none of the ellipticals in the Local Group is very impressive dwarf spheroidals were discovered between 1938 and ~1998 faint excess of stars in one region of sky hardest to spot behind Galactic Plane (e.g. Sgr dsph) these are old galaxies low metallicity, [Fe/H] of -1.3 or less some have RR Lyrae stars that take 8 Gyr to evolve large M/L ratios, ~ 5-75 stars are small addition to the dark matter! Galaxies AS
6 star formation history stars are very distributed in a colourmagnitude diagram plotting isochrones for main sequence stars demonstrates a large range of ages e.g Gyr in Leo I cf. a globular cluster has ~one birth age Caputo et al. (1999) N. Drakos Galaxies AS
7 ellipticals in clusters more massive ellipticals are found in other galaxy clusters, beyond the Local Group. a typical cluster might have: > 50 galaxies cluster-core radius ~ 300 kpc but median radius ~ 3 Mpc Local Group has ~1/10 th the galaxy density of a rich cluster mass-to-light ratio ~ 200 cluster-core regions are elliptical rich: proportions 10 / 40 / 50 in spirals / ellipticals / lenticulars but in outer regions of a cluster, 80 / 10 / 10 in spirals / ellipticals /lenticulars Galaxies AS
8 luminosity classes ellipticals have a very wide range of luminosities, and for convenience are divided into luminosity sub-classes: dwarf: L < 3 x 10 9 L solar locally, from M32: 3 x 10 8 L solar down to Draco dsph: 2 x 10 5 L solar! de are diffuse, with dsph having even lower surface brightness and luminosity (only detectable nearby) midsized : L 3 x 10 9 L solar,, or M B -18 luminous: L ~ 2 x L solar or M B ~ -20 supergiant or cd: a few times more luminous still D refers to the diffuse outer envelope can be nearly 1 Mpc across! Galaxies AS
9 possibly cd s form by swallowing up other galaxies in a cluster: A1060 galaxy cluster A3827 (M. West) false colour brings out galaxy nuclei Galaxies AS
10 ε describing the structure although featureless we need ways to describe the structure of elliptical galaxies light is concentrated towards the centre most luminous (e.g. cd s) have an extended outer halo overall shape is defined by the ellipticity parameter = 1 b/a this is basically the ellipticity sub-class En where n = 10 (1 b/a) more complex examples have three symmetry axes. and/or change of shape with radius Galaxies AS
11 Σ characterising properties for typical mid-sized and luminous ellipticals, a greater luminosity is closely related to a lower surface brightness (and to a larger core region) B per arcsec E globulars S de M B Galaxies AS
12 Σ Σ Σ Σ Σ surface brightness equation we already defined surface brightness, as flux density per unit solid angle. or in magnitudes per arcsec 2 : = -2.5 log 10 + constant NB more luminous ellipticals have lower a larger number (fainter) and so describe the surface brightness by an empirical formula, (NB sometimes see I instead of ) (R) = (R e ) exp { -b [ (R/R e ) 1/n -1 ] } b is just a constant chosen so that half the light of the galaxy comes from within the effective radius R e n is the exponent describing how the light decreases with radius is Galaxies AS
13 Σ elliptical light profiles the exponent ¼ fits the rise in central light (the galaxy core) as well as the slow outer decline cd s have a diffuse outer halo which adds extra light (R) n=4 n=1 E cd R (arcsec) Galaxies AS
14 defining the edge of a galaxy we use R e because it s hard to define the true outer edge of a galaxy (the last star ) outer regions may be well below the night sky brightness!... only the isophote shows there are stars there some catalogues use e.g. D 25, where is magnitude 25 per arcsec 2 but this is really just a telescope limit de Vaucouleurs proposed an R 1/4 law fitting elliptical light profiles in this is the basis of the exponent law the half-light enclose radius idea is more useful, if all ellipticals have about this same light profile we always comparing a region with half the galaxy s stars Galaxies AS
15 Σ actual light profiles NB, (R) actually comes from an azimuthal average, i.e of the light between isophotes of the same shape as the galaxy NB we do not always see the steep rise in the core if a galaxy has a small core, the atmospheric seeing may blur it out to an apparent size equal to the seeing (e.g. 1 arcsec) hence smaller galaxies such as de may seem to have smaller n exponents azimuthal angle φ Galaxies AS
16 Σ πσφ πσ from surface brightness to luminosity luminosity is the surface brightness integrated over radius and azimuthal angle to start we have to go back a bit and define a simpler expression for the surface brightness (R) = 0 exp [ -(R/R s )1/n ] where R S is a scale length similar to that defined before for stars in spirals then integrate to get the luminosity L = 0 2 (R) R d dr, i.e. L = R exp [ -(R/R s ) 1/n ] dr Galaxies AS
17 πσ Γ πσγ πσ πσ to make this workable, substitute x = (R/R s ) 1/n i.e. R = R S x n, from which dr = n R S x (n-1) dx so now we have L = 2 0 R S 2 n 0 x (2n-1) e -x dx which can be looked up in tables of integrals the Gamma (or factorial) function is (z) = 0 t (z-1) e -t dt = (z-1)! (for integers) so using this, L = 2 0 R S 2 n (2n) or L = 0 R S 2 2n (2n-1)! but 2n (2n-1)! = 2n!, so we finally get: L = (2n)! 0 R S 2 Galaxies AS
18 πσ Σ πσ Σ however, the scale height turns out to be rather small for ellipticals because n is large this is why the half-light radius is used instead we equate: 2 0 Re 2 R (R) dr = 0 2 from which it turns out that (R) = R (R) dr (R e ) exp { -b [ (R/R e ) 1/n -1 ] } where b = 7.67 for n = 4, for ellipticals integrating to get the luminosity, as before L = [ 8! exp(7.67) / ] { R e 2 and the central surface brightness is (R e ) } 0 ~ 2000 e Galaxies AS
19 true shapes the value of b/a for a galaxy depends somewhat on what direction we see it from consider an oblate spheroid (a sphere flattened down one axis) looks round if we look down this axis looks as flat as it is if we look perpendicular to this can show that q obs2 = (b/a) 2 = (B/A) 2 sin 2 i + cos 2 i where B and A are the real axis sizes and i is the inclination of the axis to our line of sight note that it can t look flatter than it really is elliptical galaxy courtesy of cherryblossomgardens.com Galaxies AS
20 we could calculate the fraction we expect to see with any value of q, assuming only that i is random (galaxies don t know about us ) for mid-sized ellipticals q is ~ 0.75 and we deduce that the B/A range is commonly 0.55 to 0.7 (not very flat) smaller ellipticals appear more elongated but with a lot of variation so shape and dynamics not strongly related to size? luminous ellipticals have q ~ 0.85 but very few look actually circular which is unexpected break-down of simple model: these may have three symmetry axes Galaxies AS
21 isophote shapes triaxiality reflects complicated orbits of stars in ellipticals axis ratio of galaxy may be changing with radius, and this also affects the orientations of the isophotes we see long axis seems to twist Galaxies AS
22 disky, boxy, indecribable some ellipticals contain non-elliptical isophotes disky ones suggest some orbits in a disk plane boxy ones suggest some orbits that pass through the galaxy centre dynamics; next lecture lastly, NB, encounters between galaxies can distort their shapes Naab et al J. Dunlop Galaxies AS
Elliptical Galaxies. Virgo Cluster: distance 15Mpc
Elliptical Galaxies Virgo Cluster: distance 15Mpc Elliptical Galaxies Elliptical galaxies are thought to be the simplest of all types of galaxies. Yet, detailed analysis shows that they are much more complicated
More informationEllipticals. Elliptical galaxies: Elliptical galaxies: Some ellipticals are not so simple M89 E0
Elliptical galaxies: Ellipticals Old view (ellipticals are boring, simple systems)! Ellipticals contain no gas & dust! Ellipticals are composed of old stars! Ellipticals formed in a monolithic collapse,
More informationClass #14/15 14/16 October 2008
Class #14/15 14/16 October 2008 Thursday, Oct 23 in class You ll be given equations and constants Bring a calculator, paper Closed book/notes Topics Stellar evolution/hr-diagram/manipulate the IMF ISM
More informationElliptical Galaxies. Old view: ellipticals are boring, simple systems
Eliptical Galaxies Elliptical Galaxies Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals formed in a monolithic collapse,
More informationDwarf Elliptical andFP capture the Planets
Rough subdivision Normal ellipticals. Giant ellipticals (ge s), intermediate luminosity (E s), and compact ellipticals (ce s), covering a range of luminosities from M B 23 m to M B 15 m. Dwarf ellipticals
More informationElliptical Galaxies. Houjun Mo. April 19, 2004. Basic properties of elliptical galaxies. Formation of elliptical galaxies
Elliptical Galaxies Houjun Mo April 19, 2004 Basic properties of elliptical galaxies Formation of elliptical galaxies Photometric Properties Isophotes of elliptical galaxies are usually fitted by ellipses:
More informationHow Do Galeries Form?
8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-1 8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-2 Galaxy Formation Leading questions for today How do
More informationObservational properties of ellipticals
Observational properties of ellipticals Ellipticals are deceptively simple it is so tempting to treat them as a pressure supported gas of stars but this is not correct. Too bad that only dwarf ellipticals
More informationElliptical Galaxies. Galaxies and Their Properties, Part II: Fine Structure in E-Galaxies: A Signature of Recent Merging
Elliptical Galaxies Ay 21 - Lecture 12 Galaxies and Their Properties, Part II: Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals
More informationThe Size & Shape of the Galaxy
name The Size & Shape of the Galaxy The whole lab consists of plotting two graphs. What s the catch? Aha visualizing and understanding what you have plotted of course! Form the Earth Science Picture of
More informationSKINAKAS OBSERVATORY. Astronomy Projects for University Students PROJECT THE HERTZSPRUNG RUSSELL DIAGRAM
PROJECT 4 THE HERTZSPRUNG RUSSELL DIGRM Objective: The aim is to measure accurately the B and V magnitudes of several stars in the cluster, and plot them on a Colour Magnitude Diagram. The students will
More informationIn studying the Milky Way, we have a classic problem of not being able to see the forest for the trees.
In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. A panoramic painting of the Milky Way as seen from Earth, done by Knut Lundmark in the 1940 s. The
More informationPopulations and Components of the Milky Way
Chapter 2 Populations and Components of the Milky Way Our perspective from within the Milky Way gives us an opportunity to study a disk galaxy in detail. At the same time, it s not always easy to relate
More informationThe Milky Way Galaxy is Heading for a Major Cosmic Collision
The Milky Way Galaxy is Heading for a Major Cosmic Collision Roeland van der Marel (STScI) [based on work with a team of collaborators reported in the Astrophysical Journal July 2012] Hubble Science Briefing
More informationFaber-Jackson relation: Fundamental Plane: Faber-Jackson Relation
Faber-Jackson relation: Faber-Jackson Relation In 1976, Faber & Jackson found that: Roughly, L! " 4 More luminous galaxies have deeper potentials Can show that this follows from the Virial Theorem Why
More informationarxiv:astro-ph/0101553v1 31 Jan 2001
Evidence for Large Stellar Disks in Elliptical Galaxies. Andreas Burkert and Thorsten Naab Max-Planck-Institut für Astronomie, D-69242 Heidelberg, Germany arxiv:astro-ph/0101553v1 31 Jan 2001 Abstract.
More information165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars
Name Date Period 30 GALAXIES AND THE UNIVERSE SECTION 30.1 The Milky Way Galaxy In your textbook, read about discovering the Milky Way. (20 points) For each item in Column A, write the letter of the matching
More informationScience Standard 4 Earth in Space Grade Level Expectations
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
More informationOrigins of the Cosmos Summer 2016. Pre-course assessment
Origins of the Cosmos Summer 2016 Pre-course assessment In order to grant two graduate credits for the workshop, we do require you to spend some hours before arriving at Penn State. We encourage all of
More informationA Universe of Galaxies
A Universe of Galaxies Today s Lecture: Other Galaxies (Chapter 16, pages 366-397) Types of Galaxies Habitats of Galaxies Dark Matter Other Galaxies Originally called spiral nebulae because of their shape.
More informationS0 galaxy NGC 2787. Marcella Carollo, HST.
S0 galaxy NGC 2787. Marcella Carollo, HST. Dust lane in NGC 5128. Marina Rejkuba, ESO. Peculiar E galaxy NGC 1316. Paul Goudfrooij, HST. Dust-lane E galaxy NGC 5266. Carnegie Atlas of Galaxies. 1994ApJ...43
More informationChapter 22: Electric Flux and Gauss s Law
22.1 ntroduction We have seen in chapter 21 that determining the electric field of a continuous charge distribution can become very complicated for some charge distributions. t would be desirable if we
More informationModeling Galaxy Formation
Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages
More informationDirect Detections of Young Stars in Nearby Ellipticals
Direct Detections of Young Stars in Nearby Ellipticals (NRAO Green Bank) Joel N. Bregman (University of Michigan) Click icon to add picture ApJ, in press (arxiv:1205.1066) Red and Dead Conventional wisdom:
More informationData Provided: A formula sheet and table of physical constants is attached to this paper. DARK MATTER AND THE UNIVERSE
Data Provided: A formula sheet and table of physical constants is attached to this paper. DEPARTMENT OF PHYSICS AND ASTRONOMY Autumn Semester (2014-2015) DARK MATTER AND THE UNIVERSE 2 HOURS Answer question
More informationELLIPTICAL GALAXIES: ROTATIONALLY DISTORTED, AFTER ALL
Serb. Astron. J. 179 (2009), 31-47 UDC 524.7 327 DOI: 10.2298/SAJ0979031C Original scientific paper ELLIPTICAL GALAXIES: ROTATIONALLY DISTORTED, AFTER ALL R. Caimmi Dipartimento di Astronomia, Università
More informationGalaxy Classification and Evolution
name Galaxy Classification and Evolution Galaxy Morphologies In order to study galaxies and their evolution in the universe, it is necessary to categorize them by some method. A classification scheme generally
More informationHR Diagram Student Guide
Name: HR Diagram Student Guide Background Information Work through the background sections on Spectral Classification, Luminosity, and the Hertzsprung-Russell Diagram. Then complete the following questions
More informationDetailed Mass Map of CL 0024+1654 from Strong Lensing
Detailed Mass Map of CL 0024+1654 from Strong Lensing Tyson, Kochanski, & Dell Antonio (1998) HST WFPC2 image of CL0024+1654 slides based on presentation by Yue Zhao Rutgers Physics 690 February 21, 2008
More informationDYNAMICS OF GALAXIES
DYNAMICS OF GALAXIES 2. and stellar orbits Piet van der Kruit Kapteyn Astronomical Institute University of Groningen the Netherlands Winter 2008/9 and stellar orbits Contents Range of timescales Two-body
More informationThe Sun. Solar radiation (Sun Earth-Relationships) The Sun. The Sun. Our Sun
The Sun Solar Factoids (I) The sun, a medium-size star in the milky way galaxy, consisting of about 300 billion stars. (Sun Earth-Relationships) A gaseous sphere of radius about 695 500 km (about 109 times
More informationUsing Photometric Data to Derive an HR Diagram for a Star Cluster
Using Photometric Data to Derive an HR Diagram for a Star Cluster In In this Activity, we will investigate: 1. How to use photometric data for an open cluster to derive an H-R Diagram for the stars and
More informationAstronomy. Astrophysics. Isolated ellipticals and their globular cluster systems. I. Washington photometry of NGC 3585 and NGC 5812
A&A 549, A148 (2013) DOI: 10.1051/0004-6361/201220231 c ESO 2013 Astronomy & Astrophysics Isolated ellipticals and their globular cluster systems I. Washington photometry of NGC 3585 and NGC 5812 R. R.
More informationQué pasa si n = 1 y n = 4?
Galaxias Elípticas Qué pasa si n = 1 y n = 4? Isophotal Shapes For normal elliptical galaxies the axis ratio lies in the range 0.3
More informationProperties of Elliptical Galaxies
Chapter 3 Properties of Elliptical Galaxies In the last 20 years our notions about elliptical galaxies have changed radically; these galaxies are much more complex than they seemed at first. 3.1 Folklore
More informationThe Messier Objects As A Tool in Teaching Astronomy
The Messier Objects As A Tool in Teaching Astronomy Dr. Jesus Rodrigo F. Torres President, Rizal Technological University Individual Member, International Astronomical Union Chairman, Department of Astronomy,
More informationDefining Characteristics (write a short description, provide enough detail so that anyone could use your scheme)
GEMS COLLABORATON engage The diagram above shows a mosaic of 40 galaxies. These images were taken with Hubble Space Telescope and show the variety of shapes that galaxies can assume. When astronomer Edwin
More informationThe Hidden Lives of Galaxies. Jim Lochner, USRA & NASA/GSFC
The Hidden Lives of Galaxies Jim Lochner, USRA & NASA/GSFC What is a Galaxy? Solar System Distance from Earth to Sun = 93,000,000 miles = 8 light-minutes Size of Solar System = 5.5 light-hours What is
More informationChapter 15.3 Galaxy Evolution
Chapter 15.3 Galaxy Evolution Elliptical Galaxies Spiral Galaxies Irregular Galaxies Are there any connections between the three types of galaxies? How do galaxies form? How do galaxies evolve? P.S. You
More informationThis paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00
Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June
More informationThe formation and evolution of massive galaxies: A major theoretical challenge
The formation and evolution of massive galaxies: A major theoretical challenge Thorsten Naab Max-Planck-Institute for Astrophysics L. Oser, M. Hilz, P. Johansson, J. P. Ostriker Tähtitieteilijäpäivät Haikko,
More informationThe Celestial Sphere. Questions for Today. The Celestial Sphere 1/18/10
Lecture 3: Constellations and the Distances to the Stars Astro 2010 Prof. Tom Megeath Questions for Today How do the stars move in the sky? What causes the phases of the moon? What causes the seasons?
More informationarxiv:1002.0847v1 [astro-ph.co] 3 Feb 2010
Mon. Not. R. Astron. Soc. 000, 1 19 (200x) Printed 3 February 2010 (MN LATEX style file v2.2) Formation, Evolution and Properties of Isolated Field Elliptical Galaxies arxiv:1002.0847v1 [astro-ph.co] 3
More informationLow-Mass X-Ray Binary Models for Ellipticals NGC3379 and NGC4278
Low-Mass X-Ray Binary Models for Ellipticals NGC3379 and NGC4278 Tassos Fragos with V. Kalogera, K. Belczynski, G. Fabbiano et al. Department of Physics and Astronomy Northwestern University MODEST 7b
More informationAn Introduction to Astronomy and Cosmology. 1) Astronomy - an Observational Science
An Introduction to Astronomy and Cosmology 1) Astronomy - an Observational Science Why study Astronomy 1 A fascinating subject in its own right. The origin and Evolution of the universe The Big Bang formation
More informationAPPENDIX D: SOLAR RADIATION
APPENDIX D: SOLAR RADIATION The sun is the source of most energy on the earth and is a primary factor in determining the thermal environment of a locality. It is important for engineers to have a working
More information1-2. What is the name given to the path of the Sun as seen from Earth? a.) Equinox b.) Celestial equator c.) Solstice d.
Chapter 1 1-1. How long does it take the Earth to orbit the Sun? a.) one sidereal day b.) one month c.) one year X d.) one hour 1-2. What is the name given to the path of the Sun as seen from Earth? a.)
More informationFirst Discoveries. Asteroids
First Discoveries The Sloan Digital Sky Survey began operating on June 8, 1998. Since that time, SDSS scientists have been hard at work analyzing data and drawing conclusions. This page describes seven
More informationChapter 2. Mission Analysis. 2.1 Mission Geometry
Chapter 2 Mission Analysis As noted in Chapter 1, orbital and attitude dynamics must be considered as coupled. That is to say, the orbital motion of a spacecraft affects the attitude motion, and the attitude
More informationBeginning of the Universe Classwork 6 th Grade PSI Science
Beginning of the Universe Classwork Name: 6 th Grade PSI Science 1 4 2 5 6 3 7 Down: 1. Edwin discovered that galaxies are spreading apart. 2. This theory explains how the Universe was flattened. 3. All
More informationUNIT V. Earth and Space. Earth and the Solar System
UNIT V Earth and Space Chapter 9 Earth and the Solar System EARTH AND OTHER PLANETS A solar system contains planets, moons, and other objects that orbit around a star or the star system. The solar system
More informationTELESCOPE AS TIME MACHINE
TELESCOPE AS TIME MACHINE Read this article about NASA s latest high-tech space telescope. Then, have fun doing one or both of the word puzzles that use the important words in the article. A TELESCOPE
More informationIndiana University Science with the WIYN One Degree Imager
Indiana University Science with the WIYN One Degree Imager Katherine Rhode (Indiana University, WIYN SAC member) Indiana University Department of Astronomy Nine faculty members, plus active emeritus faculty
More informationEvolution of Close Binary Systems
Evolution of Close Binary Systems Before going on to the evolution of massive stars and supernovae II, we ll think about the evolution of close binary systems. There are many multiple star systems in the
More informationThe Chemical Composition of a Molecular Cloud at the Outer Edge of the Galaxy
Carnegie Observatories Astrophysics Series, Vol. 4: Origin and Evolution of the Elements, 2003 ed. A. McWilliam and M. Rauch (Pasadena: Carnegie Observatories, http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html)
More informationSolar System. 1. The diagram below represents a simple geocentric model. Which object is represented by the letter X?
Solar System 1. The diagram below represents a simple geocentric model. Which object is represented by the letter X? A) Earth B) Sun C) Moon D) Polaris 2. Which object orbits Earth in both the Earth-centered
More informationProceedings of the NATIONAL ACADEMY OF SCIENCES
Proceedings of the NATIONAL ACADEMY OF SCIENCES Volume 55 * Number 1 * January 15, 1966 DYNAMICS OF SPHERICAL GALAXIES, II* BY PHILIP M. CAMPBELL LAWRENCE RADIATION LABORATORY, LIVERMORE, CALIFORNIA Communicated
More informationPractice Final Math 122 Spring 12 Instructor: Jeff Lang
Practice Final Math Spring Instructor: Jeff Lang. Find the limit of the sequence a n = ln (n 5) ln (3n + 8). A) ln ( ) 3 B) ln C) ln ( ) 3 D) does not exist. Find the limit of the sequence a n = (ln n)6
More informationNational Aeronautics and Space Administration. Teacher s. Science Background. GalaxY Q&As
National Aeronautics and Space Administration Science Background Teacher s GalaxY Q&As 1. What is a galaxy? A galaxy is an enormous collection of a few million to several trillion stars, gas, and dust
More informationGalaxy Morphological Classification
Galaxy Morphological Classification Jordan Duprey and James Kolano Abstract To solve the issue of galaxy morphological classification according to a classification scheme modelled off of the Hubble Sequence,
More informationWhite Dwarf Properties and the Degenerate Electron Gas
White Dwarf Properties and the Degenerate Electron Gas Nicholas Rowell April 10, 2008 Contents 1 Introduction 2 1.1 Discovery....................................... 2 1.2 Survey Techniques..................................
More informationStructure formation in modified gravity models
Structure formation in modified gravity models Kazuya Koyama Institute of Cosmology and Gravitation University of Portsmouth Dark energy v modified gravity Is cosmology probing the breakdown of general
More informationCHAPTER 24 GAUSS S LAW
CHAPTER 4 GAUSS S LAW 4. The net charge shown in Fig. 4-40 is Q. Identify each of the charges A, B, C shown. A B C FIGURE 4-40 4. From the direction of the lines of force (away from positive and toward
More informationIntermediate-Mass Black Holes (IMBHs) in Globular Clusters? HST Proper Motion Constraints. Roeland van der Marel
Intermediate-Mass Black Holes (IMBHs) in Globular Clusters? HST Proper Motion Constraints Roeland van der Marel Why Study IMBHs in Globular Clusters (GCs)? IMBHs: IMBHs can probe a new BH mass range, between
More informationWhich month has larger and smaller day time?
ACTIVITY-1 Which month has larger and smaller day time? Problem: Which month has larger and smaller day time? Aim: Finding out which month has larger and smaller duration of day in the Year 2006. Format
More informationThe Star Formation Histories of Disk and E/S0 Galaxies from Resolved Stars
The Star Formation Histories of Disk and E/S0 Galaxies from Resolved Stars Knut A.G. Olsen National Optical Astronomy Observatory kolsen@noao.edu Phone: (520)-318-8555 Co-authors: Aaron J. Romanowsky (UCO/Lick)
More informationMotions of the Earth. Stuff everyone should know
Motions of the Earth Stuff everyone should know Earth Motions E W N W Noon E Why is there day and night? OR Why do the Sun and stars appear to move through the sky? Because the Earth rotates around its
More informationROE, Edinburgh, 20 April 2006. Observational Constraints on the Acceleration Discrepancy Problem. Stacy McGaugh University of Maryland
ROE, Edinburgh, 20 April 2006 Observational Constraints on the Acceleration Discrepancy Problem Stacy McGaugh University of Maryland What gets us into trouble is not what we don t know. It s what we know
More informationCoordinate Systems. Orbits and Rotation
Coordinate Systems Orbits and Rotation Earth orbit. The earth s orbit around the sun is nearly circular but not quite. It s actually an ellipse whose average distance from the sun is one AU (150 million
More informationTHE HR DIAGRAM THE MOST FAMOUS DIAGRAM in ASTRONOMY Mike Luciuk
THE HR DIAGRAM THE MOST FAMOUS DIAGRAM in ASTRONOMY Mike Luciuk 1.INTRODUCTION Late in the nineteenth century, astronomers had tools that revealed a great deal about stars. By that time, advances in telescope
More informationName Class Date. true
Exercises 131 The Falling Apple (page 233) 1 Describe the legend of Newton s discovery that gravity extends throughout the universe According to legend, Newton saw an apple fall from a tree and realized
More informationPhysics 210 Q1 2012 ( PHYSICS210BRIDGE ) My Courses Course Settings
1 of 11 9/7/2012 1:06 PM Logged in as Julie Alexander, Instructor Help Log Out Physics 210 Q1 2012 ( PHYSICS210BRIDGE ) My Courses Course Settings Course Home Assignments Roster Gradebook Item Library
More informationSolutions for Review Problems
olutions for Review Problems 1. Let be the triangle with vertices A (,, ), B (4,, 1) and C (,, 1). (a) Find the cosine of the angle BAC at vertex A. (b) Find the area of the triangle ABC. (c) Find a vector
More informationObserving the Universe
Observing the Universe Stars & Galaxies Telescopes Any questions for next Monday? Light Doppler effect Doppler shift Doppler shift Spectra Doppler effect Spectra Stars Star and planet formation Sun Low-mass
More informationarxiv:astro-ph/9908129v1 12 Aug 1999
On the Formation of Boxy and Disky Elliptical Galaxies Thorsten Naab & Andreas Burkert Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, arxiv:astro-ph/9908129v1 12 Aug 1999 Germany
More informationStudy Guide: Solar System
Study Guide: Solar System 1. How many planets are there in the solar system? 2. What is the correct order of all the planets in the solar system? 3. Where can a comet be located in the solar system? 4.
More informationStar Clusters. Star Clusters E NCYCLOPEDIA OF A STRONOMY AND A STROPHYSICS
Star Clusters Even a small telescope shows obvious local concentrations of stars scattered around the sky. These star clusters are not chance juxtapositions of unrelated stars. They are, instead, physically
More informationLesson Plan G2 The Stars
Lesson Plan G2 The Stars Introduction We see the stars as tiny points of light in the sky. They may all look the same but they are not. They range in size, color, temperature, power, and life spans. In
More informationThe CGM around Dwarf Galaxies
The CGM around Dwarf Galaxies Rongmon Bordoloi STScI + the COS-Halos Team What is the CGM? Shen et al. 212 jectedcolumndensityinacubeof5(proper)kpc Diffuse gas, including metals and dust, o2en on extending
More informationVirgo and the Stellar Populations of Planets
A Systematic Study of the Stellar Populations and ISM in Galaxies out to the Virgo Cluster: near-field cosmology within a representative slice of the local universe Rolf A. Jansen Arizona State University
More informationHW6 Solutions Notice numbers may change randomly in your assignments and you may have to recalculate solutions for your specific case.
HW6 Solutions Notice numbers may change randomly in your assignments and you may have to recalculate solutions for your specific case. Tipler 22.P.053 The figure below shows a portion of an infinitely
More informationRenewable Energy. Solar Power. Courseware Sample 86352-F0
Renewable Energy Solar Power Courseware Sample 86352-F0 A RENEWABLE ENERGY SOLAR POWER Courseware Sample by the staff of Lab-Volt Ltd. Copyright 2009 Lab-Volt Ltd. All rights reserved. No part of this
More informationIntroduction to the Solar System
Introduction to the Solar System Lesson Objectives Describe some early ideas about our solar system. Name the planets, and describe their motion around the Sun. Explain how the solar system formed. Introduction
More informationMidterm Solutions. mvr = ω f (I wheel + I bullet ) = ω f 2 MR2 + mr 2 ) ω f = v R. 1 + M 2m
Midterm Solutions I) A bullet of mass m moving at horizontal velocity v strikes and sticks to the rim of a wheel a solid disc) of mass M, radius R, anchored at its center but free to rotate i) Which of
More informationLecture 13. Gravity in the Solar System
Lecture 13 Gravity in the Solar System Guiding Questions 1. How was the heliocentric model established? What are monumental steps in the history of the heliocentric model? 2. How do Kepler s three laws
More informationBinary Stars. Kepler s Laws of Orbital Motion
Binary Stars Kepler s Laws of Orbital Motion Kepler s Three Laws of orbital motion result from the solution to the equation of motion for bodies moving under the influence of a central 1/r 2 force gravity.
More informationastronomy 2008 1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times.
1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times. 5. If the distance between the Earth and the Sun were increased,
More informationSound. References: L.D. Landau & E.M. Lifshitz: Fluid Mechanics, Chapter VIII F. Shu: The Physics of Astrophysics, Vol. 2, Gas Dynamics, Chapter 8
References: Sound L.D. Landau & E.M. Lifshitz: Fluid Mechanics, Chapter VIII F. Shu: The Physics of Astrophysics, Vol., Gas Dynamics, Chapter 8 1 Speed of sound The phenomenon of sound waves is one that
More informationCELESTIAL CLOCK - THE SUN, THE MOON, AND THE STARS
INTRODUCTION CELESTIAL CLOCK - THE SUN, THE MOON, AND THE STARS This is a scientific presentation to provide you with knowledge you can use to understand the sky above in relation to the earth. Before
More information1 Introduction. Name: 1.1 Spectral Classification of Stars. PHYS-1050 Hertzsprung-Russell Diagram Solutions Spring 2013
Name: 1 Introduction Read through this information before proceeding on with the lab. 1.1 Spectral Classification of Stars 1.1.1 Types of Spectra Astronomers are very interested in spectra graphs of intensity
More informationA TRIO OF NEW LOCAL GROUP GALAXIES WITH EXTREME PROPERTIES
The Astrophysical Journal, 688:1009Y1020, 2008 December 1 # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. A A TRIO OF NEW LOCAL GROUP GALAXIES WITH EXTREME PROPERTIES
More informationMagellanic Cloud planetary nebulae as probes of stellar evolution and populations. Letizia Stanghellini
Magellanic Cloud planetary nebulae as probes of stellar evolution and populations Letizia Stanghellini Planetary nebulae beyond the Milky Way - May 19-21, 2004 1 Magellanic Cloud PNe The known distances,
More informationAstronomy 112: The Physics of Stars. Class 1 Notes: Observing Stars
Astronomy 112: The Physics of Stars Class 1 Notes: Observing Stars Although this course will be much less oriented toward observations than most astronomy courses, we must always begin a study of any topic
More informationIf A is divided by B the result is 2/3. If B is divided by C the result is 4/7. What is the result if A is divided by C?
Problem 3 If A is divided by B the result is 2/3. If B is divided by C the result is 4/7. What is the result if A is divided by C? Suggested Questions to ask students about Problem 3 The key to this question
More informationCarbon stars in the Local Group
Carbon stars in the Local Group Martin Groenewegen groen@ster.kuleuven.ac.be Instituut voor Sterrenkunde - K.U.Leuven Torun October 2002 p.1/42 Overview Late-type stars How to find them? Inventory / Status
More informationMath 1B, lecture 5: area and volume
Math B, lecture 5: area and volume Nathan Pflueger 6 September 2 Introduction This lecture and the next will be concerned with the computation of areas of regions in the plane, and volumes of regions in
More informationSupplementary Material
Supplementary Material Contents 1. Alternative designations, celestial coordinates and apparent magnitudes 2. Stellar properties 3. Data preparation and transit modeling 4. Kepler data validation 5. Follow
More informationSTRUCTURE AND FORMATION OF ELLIPTICAL AND SPHEROIDAL GALAXIES 1,2,3
STRUCTURE AND FORMATION OF ELLIPTICAL AND SPHEROIDAL GALAXIES 1,2,3 JOHN KORMENDY 4,5,6, DAVID B. FISHER 4,5,6, MARK E. CORNELL 4, AND RALF BENDER 4,5,6 Received 2006 September 6; accepted 2008 October
More informationArjen van der Wel -- MPIA, Heidelberg
THE PATH FROM COMPACT Z = 2 GALAXY TO GIANT ELLIPTICAL Arjen van der Wel -- MPIA, Heidelberg with the 3D-HST and CANDELS teams THE PATH FROM COMPACT Z = 2 GALAXY TO GIANT ELLIPTICAL The size-mass relation
More informationCELESTIAL MOTIONS. In Charlottesville we see Polaris 38 0 above the Northern horizon. Earth. Starry Vault
CELESTIAL MOTIONS Stars appear to move counterclockwise on the surface of a huge sphere the Starry Vault, in their daily motions about Earth Polaris remains stationary. In Charlottesville we see Polaris
More information