in the Milky Way s dsphs
|
|
- Paul Golden
- 7 years ago
- Views:
Transcription
1 Probes of Dark Matter on Galaxy Scales Monterey, CA July 15, 2013 The Diversity of Dark Matter Profiles in the Milky Way s dsphs John Jardel, University of Texas
2 Dark Matter & Galaxy Formation Lots of substructure Springel+(2008) Universal density profiles
3 Modeling Dark Matter in Dwarf Spheroidals Multiple Populations WP11 WP11 Review by Battaglia, Helmi, & Breddels (2013) Found cored profile Found cuspy profile Results not conclusive
4 Local Group dsphs Why study Local Group dsphs? DM dominated Lowest mass products of galaxy formation Large public data sets Individual stars resolved Unanswered questions: Cores, cusps, or something else? Challenge to CDM? New details about galaxy formation? Fornax Draco
5 How I m doing this Data Publicly available individual radial velocities from multi-fiber spectroscopy (Walker+ 2009) Individual radial velocities taken with VIRUS-W (a handful in Draco) Surface brightness profiles from star counts Models Orbit-based models (Gebhardt+ 2003) but with the added d feature of specifying a density profile nonparametrically (JJ+ 2013) Usually used in big elliptical galaxies (integrated light kinematics, not individual velocities)
6 Data What form are the data in? fraction of stars r (pc) Walker+ (2009) Murphy+ (2011)
7 From RVs to LOSVDs Individual Radial Velocities * Fitting can also be done to the individual velocities (Maarten Breddels thesis) Line-of-sight Velocity Distributions (LOSVDs) Kernel Density Estimation ion of stars fracti Silverman (1986) JJ+ (2013)
8 Models How do the models work? How do they fit to the data? (courtesy J. Kormendy)
9 Why Schwarzschild modeling? Other forms of modeling subject to massanisotropy degeneracy Schwarzschild modeling picks up extra information in the LOSVD to constrain the orbits Wolf+ (2010) fraction of st tars van der Marel & Franx (1993) JJ & Gebhardt (2012)
10 Non-Parametric Schwarzschild hild Modeling (courtesy M. Cappellari) This is where the non-parametric part comes in r
11 Draco: A test case Input age and metallicity of best-fitting isochrone to SSP models (Maraston+ 2005) to get stellar density JJ usually small
12 Results for 5 dsphs Points w/error bars are point-wise 1σ density Gray band is joint 1σ profile Red band in Fornax is stellar density (only galaxy where stellar density DM density)
13 A common halo? Rescale each density profile to a common normalization and see what happens.
14 V c profiles Boylan-Kolchin, Bullock & Kaplinghat (2012)
15 Anisotropy is mildly radial Radial orbits are a generic prediction of tidal stirring formation method for dsphs
16 Summary/Conclusions There are a variety of different profile types in real galaxies. Future Work: Detailed comparison of modeled d profiles to simulations How does DM profile change with stellar mass? Unleash Non-Parametric Schwarzschild Modeling on more massive galaxies
17 Extra Slides
18 Density estimation Histogram: Kernel Density Estimator: Silverman (1986) How to choose the smoothing size h?
19 Next steps: Feedback from baryons THINGS: HI survey of late-type type field dwarfs Simulations: Governato+ (2012) N- body/hydro cosmological simulations of THINGS-like lk dwarfs core How do DM profiles change in simulations that include baryons? cusp Do more stars = more ( ) p feedback? Governato+ (2012) with dsphs added
20 Anisotropy in Draco Find orbits are mostly radial radial tangential Consistent with tidal stirring scenario for formation of dsphs (Łokas+ 2010, Kazantzidis+ 2011)
21 Draco: A test case New VIRUS-W IFU observations (55 x 105 ) Data from literature JJ+ (2012) JJ+ (2012) New observations Kleyna+ (2002) 158 (from literature) + 12 (new) radial velocities 8 LOSVDs binned in annuli from 8 pc to 500 pc
22 How does Draco compare to ΛCDM simulations? JJ+ (2012) Boylan-Kolchin, Bullock, & Kaplinghat (2012)
23 Draco velocities from VIRUS-W Iterative sigma-clipping Hard cut at 30 km/s from systemic Both methods give same 12 stars as members
24 Draco Photometry in inner region JJ+ (2012)
25 Line-of-sight Velocity Distributions (LOSVDs) LOSVDs contain information about what types of orbits the stars are on van der Marel l& Franx (1993) They are the kinematics input in our models JJ & Gebhardt (2012)
26 Maximum Entropy Regularization Typical models have >10,000 orbits and only 20 LOSVDS with 15 velocity bins (300 observables) bl Thomas et al. (2005)
27 Calculating Phase Space Volumes Evaluating the integral Voronoi Tessellation Enclose each point (site) in SOS inside a polygon Area contains all points which lie closer to site in consideration than another Thomas et al. (2004)
Class #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 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 informationarxiv:1305.5965v1 [astro-ph.co] 25 May 2013
Internal kinematics and dynamical models of dwarf spheroidal galaxies around the Milky Way arxiv:1305.5965v1 [astro-ph.co] 25 May 2013 Giuseppina Battaglia a,, Amina Helmi b, Maarten Breddels b a INAF
More informationLecture 6: distribution of stars in. elliptical galaxies
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
More informationThe Formation of Dwarf Early-Type Galaxies. Reynier Peletier Kapteyn Astronomical Institute, Groningen
The Formation of Dwarf Early-Type Galaxies Reynier Peletier Kapteyn Astronomical Institute, Groningen From Kormendy et al. (2009) Definition of dwarf ellipticals: -15 < MB < -18 Here to be discussed the
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 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 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 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 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 informationFormation Mechanisms for Spheroidal Stellar Systems
VARIABLE STARS, THE GALACTIC HALO AND GALAXY FORMATION C. Sterken, N. Samus and L. Szabados (Eds.) 2010 Formation Mechanisms for Spheroidal Stellar Systems O. K. Sil chenko 1 Sternberg Astronomical Institute
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 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 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 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 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 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 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 informationHow the properties of galaxies are affected by the environment?
How the properties of galaxies are affected by the environment? Reinaldo R. de Carvalho - DAS/INPE Marina Trevisan Reinaldo Rosa The activities in this project follow from the Tatiana Moura general context
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 informationElliptical 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 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 informationUnderstanding the size growth of massive (spheroidal) galaxies through stellar populations
Department of Space and Climate Physics Mullard Space Science Laboratory http://www.ucl.ac.uk/mssl Understanding the size growth of massive (spheroidal) galaxies through stellar populations Ignacio Ferreras
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 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 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 informationHighlights from the VLA/ANGST Survey
Highlights from the VLA/ANGST Survey Evan Skillman U. Minnesota Gas in Galaxies 2011: From Cosmic Web to Molecular Clouds Kloster Seeon, Germany 16/06/2011 VLA/ANGST The ANGST HST Treasury Project allowed
More informationarxiv:astro-ph/0407219v1 12 Jul 2004
Astronomy & Astrophysics manuscript no. 1414 December 16, 2013 (DOI: will be inserted by hand later) Line-of-sight velocity distribution corrections for Lick/IDS indices of early-type galaxies Harald Kuntschner
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 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 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 informationGravitomagnetism and complex orbit dynamics of spinning compact objects around a massive black hole
Gravitomagnetism and complex orbit dynamics of spinning compact objects around a massive black hole Kinwah Wu Mullard Space Science Laboratory University College London United Kingdom kw@mssl.ucl.ac.uk
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 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 informationarxiv:1211.3420v2 [astro-ph.ga] 26 Mar 2013
Published by the Astrophysical Journal (ApJ, 766, 71) Preprint typeset using L A TEX style emulateapj v. 03/07/07 arxiv:1211.3420v2 [astro-ph.ga] 26 Mar 2013 THE DARK HALO SPHEROID CONSPIRACY AND THE ORIGIN
More informationOn the Spin Bias of Satellite Galaxies in the Local Group-like Environment
Prepared for submission to JCAP On the Spin Bias of Satellite Galaxies in the Local Group-like Environment arxiv:1303.0674v2 [astro-ph.co] 30 Apr 2013 Jounghun Lee a and Gerard Lemson b a Astronomy Program,
More informationThe Evolution of GMCs in Global Galaxy Simulations
The Evolution of GMCs in Global Galaxy Simulations image from Britton Smith Elizabeth Tasker (CITA NF @ McMaster) Jonathan Tan (U. Florida) Simulation properties We use the AMR code, Enzo, to model a 3D
More informationThe Crafoord Prize 2005
I N F O R M A T I O N F O R T H E P U B L I C The Royal Swedish Academy of Sciences has decided to award the Crafoord Prize in Astronomy 2005 to James Gunn, Princeton University, USA, James Peebles, Princeton
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 informationVisualization and Astronomy
Visualization and Astronomy Prof.dr. Jos Roerdink Institute for Mathematics and Computing Science University of Groningen URL: www.cs.rug.nl/svcg/ Scientific Visualization & Computer Graphics Group Institute
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 information(Long-Baseline) Interferometric Measurements of Binary Stars
(Long-Baseline) Interferometric Measurements of Binary Stars A. Boden MSC/Caltech & GSU C. Hummel USNO/ESO G. Torres & D. Latham CfA H. McAlister CHARA/GSU Outline Introduction: Why study binary stars
More informationCarol and Charles see their pencils fall exactly straight down.
Section 24-1 1. Carol is in a railroad car on a train moving west along a straight stretch of track at a constant speed of 120 km/h, and Charles is in a railroad car on a train at rest on a siding along
More informationInstitut für Kern- und Teilchenphysik Neutrinos & Cosmology
Neutrinos & Cosmology 1 Cosmology: WHY??? From laboratory experiment limits can be set ONLY in neutrino mass difference No information if neutrino masses are degenerated From kinematic experiment limits
More informationDebris disks at high resolution. Mark Wyatt Rachel Smith Institute of Astronomy, Cambridge
Debris disks at high resolution Mark Wyatt Rachel Smith Institute of Astronomy, Cambridge Debris disk overview Debris disks are remnants of planet formation, planetesimals which failed to grow into planets;
More informationCold dark matter: Controversies on small scales
Cold dark matter: Controversies on small scales David H. Weinberg a,1, James S. Bullock b, Fabio Governato c, Rachel Kuzio de Naray d, and Annika H. G. Peter a,b a Department of Astronomy, Ohio State University,
More informationWIMP dark matter and the isotropic radio signal Roberto A. Lineros R. Instituto de Física Corpuscular - CSIC/U. Valencia @Roberto_Lineros Outline Introduction Cosmic ray propagation Synchrotron emission
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 informationThe Gaia Archive. Center Forum, Heidelberg, June 10-11, 2013. Stefan Jordan. The Gaia Archive, COSADIE Astronomical Data
The Gaia Archive Astronomisches Rechen-Institut am Zentrum für Astronomie der Universität Heidelberg http://www.stefan-jordan.de 1 2 Gaia 2013-2018 and beyond Progress with Gaia 3 HIPPARCOS Gaia accuracy
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 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 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 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 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 informationStructure & Kinematics of Early-Type Galaxies from Integral-Field Spectroscopy
arxiv:162.4267v1 [astro-ph.ga] 13 Feb 216 Annu. Rev. Astron. Astrophys. 216. 54:1 67 This article s doi:.1146/annurev-astro-82214-122432 Copyright c 216 by Annual Reviews. All rights reserved Structure
More informationDIRECT ORBITAL DYNAMICS: USING INDEPENDENT ORBITAL TERMS TO TREAT BODIES AS ORBITING EACH OTHER DIRECTLY WHILE IN MOTION
1 DIRECT ORBITAL DYNAMICS: USING INDEPENDENT ORBITAL TERMS TO TREAT BODIES AS ORBITING EACH OTHER DIRECTLY WHILE IN MOTION Daniel S. Orton email: dsorton1@gmail.com Abstract: There are many longstanding
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 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 informationJ-PAS: low-resolution (R 50) spectroscopy over 8000 deg 2
J-PAS: low-resolution (R 50) spectroscopy over 8000 deg 2 C. López-Sanjuan J. Cenarro, L. A. Díaz-García, J. Varela, K. Viironen, & the J-PAS team Centro de Estudio de Física del Cosmos de Aragón 10th
More informationOUTLINE The Hubble parameter After these lectures, you should be able to: Define the Hubble parameter H Sketch a(t) for k>0, k=0, k<0 assuming Λ=0 Def
Observational cosmology: The Friedman equations 2 Filipe B. Abdalla Kathleen Lonsdale Building G.22 http://zuserver2.star.ucl.ac.uk/~hiranya/phas3136/phas3136 OUTLINE The Hubble parameter After these lectures,
More informationNeutron Stars. How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967.
Neutron Stars How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967. Using a radio telescope she noticed regular pulses of radio
More informationStar Formation History of the Magellanic Clouds: a survey program with DECam@4mCTIO.
Star Formation History of the Magellanic Clouds: a survey program with DECam@4mCTIO. Lara Monteagudo Narvion 1,2, Matteo Monelli 1,2, Carme Gallart 1,2, David Nidever 3, Knut Olsen 4 and SMASH group 1
More informationI n t e r a c t i n g G a l a x i e s - Making Ellipticals Te a c h e r N o t e s
I n t e r a c t i n g G a l a x i e s - Making Ellipticals Te a c h e r N o t e s Author: Sarah Roberts Interacting - Making Ellipticals - Teacher Notes Making Ellipticals Making Ellipticals - Changing
More information6 A High Merger Fraction in the Rich Cluster MS 1054 03 at z =0:83: Direct Evidence for Hierarchical Formation of Massive Galaxies y
6 A High Merger Fraction in the Rich Cluster MS 1054 03 at z =0:83: Direct Evidence for Hierarchical Formation of Massive Galaxies y ABSTRACT We present a morphological study of the galaxy population of
More informationCAUP s Astronomical Instrumentation and Surveys
CAUP s Astronomical Instrumentation and Surveys CENTRO DE ASTROFÍSICA DA UNIVERSIDADE DO PORTO www.astro.up.pt Sérgio A. G. Sousa Team presentation sousasag@astro.up.pt CAUP's Astronomical Instrumentation
More informationAstro 102 Test 5 Review Spring 2016. See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14
Astro 102 Test 5 Review Spring 2016 See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14 Sec 14.5 Expanding Universe Know: Doppler shift, redshift, Hubble s Law, cosmic distance ladder, standard candles,
More informationPresent-day galaxies: disks vs. spheroids. Parameters of a starburst galaxy
Paul van der Werf Sterrewacht Leiden,$& 0D\ Present-day galaxies disks vs. spheroids Disks blue relatively young range in colours range in ages (age ~ 3 6 G, z f ~ 0.5 2) stars formed continually or in
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 informationBrief ideas for a long discussion
Brief ideas for a long discussion 1. Disk formation/survival in mergers 2. Bulgeless galaxies 3. Global z~2 to z~0 evolution 4. Interface between Cold flows / Disks / Outflows 5. Emergence of a bimodality
More informationTop 10 Discoveries by ESO Telescopes
Top 10 Discoveries by ESO Telescopes European Southern Observatory reaching new heights in astronomy Exploring the Universe from the Atacama Desert, in Chile since 1964 ESO is the most productive astronomical
More informationThe Search for Dark Matter, Einstein s Cosmology and MOND. David B. Cline
The Search for Dark Matter, Einstein s Cosmology and MOND David B. Cline Astrophysics Division, Department of Physics & Astronomy University of California, Los Angeles, CA 90095 USA dcline@physics.ucla.edu
More informationWeek 1-2: Overview of the Universe & the View from the Earth
Week 1-2: Overview of the Universe & the View from the Earth Hassen M. Yesuf (hyesuf@ucsc.edu) September 29, 2011 1 Lecture summary Protein molecules, the building blocks of a living organism, are made
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 and Stellar Dynamics
Ay 20 Fall 2004 Star Clusters and Stellar Dynamics (This file has a bunch of pictures deleted, in order to save space) Stellar Dynamics Gravity is generally the only important force in astrophysical systems
More informationWhat is the Sloan Digital Sky Survey?
What is the Sloan Digital Sky Survey? Simply put, the Sloan Digital Sky Survey is the most ambitious astronomical survey ever undertaken. The survey will map one-quarter of the entire sky in detail, determining
More informationExplorations of the Outer Solar System. B. Scott Gaudi Harvard-Smithsonian Center for Astrophysics
Explorations of the Outer Solar System B. Scott Gaudi Harvard-Smithsonian Center for Astrophysics The Known Solar System How big is the solar system? a tidal R 0 M Sun M Galaxy 1/3 200,000AU How big is
More informationPlanets beyond the solar system
Planets beyond the solar system Review of our solar system Why search How to search Eclipses Motion of parent star Doppler Effect Extrasolar planet discoveries A star is 5 parsecs away, what is its parallax?
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 informationClass 2 Solar System Characteristics Formation Exosolar Planets
Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System
More informationAstronomy & Physics Resources for Middle & High School Teachers
Astronomy & Physics Resources for Middle & High School Teachers Gillian Wilson http://www.faculty.ucr.edu/~gillianw/k12 A cosmologist is.... an astronomer who studies the formation and evolution of the
More informationThe Birth and Assembly of Galaxies: the Relationship Between Science Capabilities and Telescope Aperture
The Birth and Assembly of Galaxies: the Relationship Between Science Capabilities and Telescope Aperture Betsy Barton Center for Cosmology University of California, Irvine Grateful acknowledgements to:
More informationGalaxy Survey data analysis using SDSS-III as an example
Galaxy Survey data analysis using SDSS-III as an example Will Percival (University of Portsmouth) showing work by the BOSS galaxy clustering working group" Cosmology from Spectroscopic Galaxy Surveys"
More informationDelayed mergers: The contribution of ellipticals, globular clusters, and protoclusters to the LIGO detection rate
Delayed mergers: The contribution of ellipticals, globular clusters, and protoclusters to the LIGO detection rate Aug 16, 2005 Richard O Shaughnessy (with O Leary, Fregeau, Kalogera, Rasio, Ivanova, Belczynski)
More informationCosmology and Fundamental Physics with Gamma-Ray Astronomy
Cosmology and Fundamental Physics with Gamma-Ray Astronomy J.H. Buckley Washington University, Dept. Physics CB 1105, 1 Brookings Dr., St. Louis, MO. 63130 e-mail: buckleywuphys.wustl.edu phone: (314)
More informationProblem #1 [Sound Waves and Jeans Length]
Roger Griffith Astro 161 hw. # 8 Proffesor Chung-Pei Ma Problem #1 [Sound Waves and Jeans Length] At typical sea-level conditions, the density of air is 1.23 1 3 gcm 3 and the speed of sound is 3.4 1 4
More informationProbability of detecting compact binary coalescence with enhanced LIGO
Probability of detecting compact binary coalescence with enhanced LIGO Richard O Shaughnessy [V. Kalogera, K. Belczynski] GWDAW-12, December 13, 2007 Will we see a merger soon? Available predictions Isolated
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 informationNewton s Law of Gravity
Gravitational Potential Energy On Earth, depends on: object s mass (m) strength of gravity (g) distance object could potentially fall Gravitational Potential Energy In space, an object or gas cloud has
More informationDebris Disk Imaging with WFIRST-AFTA. Geoff Bryden Jet Propulsion Laboratory, California Institute of Technology
Debris Disk Imaging with WFIRST-AFTA Geoff Bryden Jet Propulsion Laboratory, California Institute of Technology What & Why What are debris disks? Remnants of planet formation Direct: Second-generation
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 informationFXA 2008. UNIT G485 Module 5 5.5.1 Structure of the Universe. Δλ = v λ c CONTENTS OF THE UNIVERSE. Candidates should be able to :
1 Candidates should be able to : CONTENTS OF THE UNIVERSE Describe the principal contents of the universe, including stars, galaxies and radiation. Describe the solar system in terms of the Sun, planets,
More informationSystematic variations of central mass density slopes in early-type galaxies
doi:10.1093/mnras/stu1616 Systematic variations of central mass density slopes in early-type galaxies C. Tortora, 1 F. La Barbera, 1 N. R. Napolitano, 1 A. J. Romanowsky, 2,3 I. Ferreras 4 andr.r.decarvalho
More informationUsing Image J to Measure the Brightness of Stars (Written by Do H. Kim)
Using Image J to Measure the Brightness of Stars (Written by Do H. Kim) What is Image J? Image J is Java-based image processing program developed at the National Institutes of Health. Image J runs on everywhere,
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 informationA: Planets. Q: Which of the following objects would NOT be described as a small body: asteroids, meteoroids, comets, planets?
Q: Which of the following objects would NOT be described as a small body: asteroids, meteoroids, comets, planets? A: Planets Q: What can we learn by studying small bodies of the solar system? A: We can
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 informationStar formation losses due to tidal debris in hierarchical galaxy formation
A&A 373, 494 510 (2001) DOI: 10.1051/0004-6361:20010656 c ESO 2001 Astronomy & Astrophysics Star formation losses due to tidal debris in hierarchical galaxy formation B. F. Roukema 1,2,3,4,, S. Ninin 1,
More informationAnswers for the Student Worksheet for the Hubble Space Telescope Scavenger Hunt
Instructions: Answers are typed in blue. Answers for the Student Worksheet for the Hubble Space Telescope Scavenger Hunt Crab Nebula What is embedded in the center of the nebula? Neutron star Who first
More information