Stellar Population Synthesis, a Discriminant Between Gravity Models
|
|
- Godfrey Flynn
- 5 years ago
- Views:
Transcription
1 Stellar Population Synthesis, a Discriminant Between Gravity Models Akram Hasani Zonoozi Institute for Advanced Studies in Basic Sciences, IASBS Zanjan, Iran In collaboration with: H.Haghi & Y.Sobouti
2 Introduction Most of alternative gravity models and the DM scenarios simulate the rotation curves of spirals with reasonable details. There is significant disparities in their predictions of mass-tolight ratios, M/L, of the galaxies. This feature are used as a discriminant between different alternative theories, by resorting to stellar population synthesis analysis. The rotation curve for the galaxy NGC3198 from Begeman 1989
3 Alternative gravity models MOND: Modified Newtonian Dynamics of Milgorom MOG: Modified Gravity of Moffat DM: Newtonian Gravity + Dark matter.
4 Modified Newtonian Dynamics (MOND) Based on observations of galactic rotation curves, gravity is boosted bellow a certain acceleration. (Milgrom, 1983; Milgrom & Bekenestein 1984; Bekenstein 2004) a g µ ( g a ) 0 = mond 10 mond ms 2 g N µ ( x) = x x << 1 µ ( x) = 1 x >> 1 Standard function Simple function Bekenstein function
5 Modified Gravity of Moffat (MOG) (Moffat 2005) In galactic scale: 1 [ M M ( )] 2 α( r ) = 0 r In larger scales: local group, galaxy clusters: (Brownstein & Moffat 2006, Haghi & Rahvar 2010)
6 Newtonian Gravity plus Dark Matter (DM) logarithmic halo: (Binney & Tremaine 1987) NFW halo: (Navarro, Frenk & White 1996, 1997) ρ NFW ( r) = ( r / r s ρs )(1 + r / r s 2 )
7 Constructing rotation curves Rotation speed of a test object is a function of distance from the galactic center and the distribution of the detectable matter. Sanders & McGaugh 2002 In modified gravity: In DM: 2 2 * V = V + V baryonic gas 2 2 V = V + V baryonic dark 2 2 Fitting of the calculated rotation curves to the observed data points is achieved by adjusting the stellar M/L ratio, through a least-square method.
8 All models trace the observed data with reasonable details. We analyzed 46 galaxies.
9 MOND3 MOND3
10 Color - M/L ratio correlation How realistic are the inferred M/L ratios? - Stellar population synthesis (SPS) models are tools for interpreting the integrated light that we observed from the galaxies. - SPS models predict a linear relation between colors and log(m/l) ratios of galaxies. log ( M * / L) = a ( B V ) + (Bell & de Jong (2001, 2003) and Portinari et al ) b Redder galaxies have larger M/L ratio.
11 The slope of this linear relation does not depend on exact details of the history of star formation. Different SPS models. B and K refer to different spectral band from Bell & de Jong (2001)
12 The dominant source of uncertainty in estimating stellar M/L ratios from galaxy luminosities and optical colors is the stellar IMF. Depending on how many stars are present at the low-mass end of the stellar IMF, the color- M/L curve shifts up and down. Different IMFs: Bruzual & Charlot (2001): Salpeter with x=-1.35 Salpeter with x=0 below 0.6 Scalo (1986) IMF The updated PE_GASE models with a steeper x=-1.85 and a flatter x= from Bell & de Jong (2001)
13 Initial Mass Function, IMF Low mass stars contribute significantly to the mass of a population, but not so much to its luminosity and color. An IMF richer in low-mass stars yields a higher stellar M/L ratio at a given color. dn/dlog(m) α =1.3 α = 2.3 Salpeter 1955, Kroupa Log(m)
14 M*/L - Color relation Solid line in each panel is the best-fit to the prediction of the gravity model in question. Other lines denote the theoretical predictions of SPS with different IMFs (Bell & de Jong 2001, Bell et al. 2003). They have almost the same slope but different y-intercepts.
15 Slopes of MOND are reasonably close to the prediction of SPS. Those of MOG and DM are not.
16 Results Log(M/L)=a.(B-V) b SPS predictions Salpeter IMF (Scaled) Salpeter IMF Kroupa IMF Bottema IMF Slope Y-intercept Model MOND1 MOND2 MOND3 MOG DM:NFW DM:Log Slope (Error) Y-intercept (Error)
17 Concluding Remarks The SPS scheme can differentiate between different gravity models. The slope of MOND, are reasonably close to prediction of SPS model. The y-intercept of MOND with Bekenstein function is in agreement with Kroupa's IMF, while that of MOND with other interpolating functions are somewhere between the standard Salpeter and the scaled Salpeter IMF. The slopes of MOG and DM are different from the predictions of SPS.
Direct N-body simulations of distant halo globular clusters
Direct N-body simulations of distant halo globular clusters Hosein Haghi Institute for Advanced Studies in Basic Sciences (IASBS) Zanjan, IRAN in collaboration with Akram Hasani Zonoozi (IASBS), Holger
More informationBaryonic Masses from Rotation Curves. Stacy McGaugh University of Maryland
Unveiling the Mass - Extracting and Interpreting Galaxy Masses, Kingston, Ontario, 19 June 2009 Baryonic Masses from Rotation Curves Stacy McGaugh University of Maryland Rotation curves tend to become
More informationRotation curves of spiral galaxies
Rotation curves of spiral galaxies Rotation curves Mass discrepancy Circular velocity of spherical systems and disks Dark matter halos Inner and outer regions Tully-Fisher relation From datacubes to rotation
More informationarxiv: v1 [astro-ph] 13 May 2008
Draft version May 13, 28 Preprint typeset using L A TEX style emulateapj v. 8/13/6 MOND AND THE UNIVERSAL ROTATION CURVE: SIMILAR PHENOMENOLOGIES Gianfranco Gentile 1,2 Draft version May 13, 28 arxiv:85.1731v1
More informationScaling Relations of late-type galaxies
Scaling Relations of late-type galaxies - an observational perspective - Lecture I Lecture II Trends along the Hubble sequence Galaxy rotation curves Lecture III Tully-Fisher relations Marc Verheijen Kapteyn
More informationarxiv: v2 [astro-ph.ga] 23 Nov 2017
Publ. Astron. Obs. Belgrade No. 98 (2018), 1-4 Contributed paper arxiv:1711.06335v2 [astro-ph.ga] 23 Nov 2017 INVESTIGATING THE RADIAL ACCELERATION RELATION IN EARLY-TYPE GALAXIES USING THE JEANS ANALYSIS
More informationModified Newtonian Dynamics (MOND) and the Bullet Cluster (1E )
Modified Newtonian Dynamics (MOND) and the Bullet Cluster (1E 0657-558) Alan G. Aversa ABSTRACT Modified Newtonian Dynamics (MOND) is a theory that modifies Newton s force law to explain observations that
More informationarxiv: v2 [astro-ph.ga] 12 Jan 2011
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) Distant star clusters of the Milky Way in MOND Hossein Haghi 1,2,, Holger Baumgardt 2,3, and Pavel Kroupa 2 arxiv:111.1952v2 [astro-ph.ga]
More informationStellar Population Mass Estimates. Roelof de Jong (STScI AIP) Eric Bell (MPIA Univ. of Michigan)
Stellar Population Mass Estimates Roelof de Jong (STScI AIP) Eric Bell (MPIA Univ. of Michigan) Overview Stellar Mass-to-Light (M/L) ratios from SEDs Comparing different SED fitting techniques Comparing
More informationarxiv:astro-ph/ v4 29 Sep 2004
The Mass Discrepancy-Acceleration Relation: Disk Mass and the Dark Matter Distribution Stacy S. McGaugh Department of Astronomy, University of Maryland arxiv:astro-ph/0403610v4 29 Sep 2004 College Park,
More informationDark Matter. Galaxy Counts Redshift Surveys Galaxy Rotation Curves Cluster Dynamics Gravitational Lenses ~ 0.3 Ω M Ω b.
Dark Matter Galaxy Counts Redshift Surveys Galaxy Rotation Curves Cluster Dynamics Gravitational Lenses Ω M ~ 0.3 2 1 Ω b 0.04 3 Mass Density by Direct Counting Add up the mass of all the galaxies per
More informationEverything in baryons?
Everything in baryons? Benoit Famaey (ULB) Rencontres de Blois 2007 General Relativity -> Dark Matter R αβ - 1/2 R g αβ + Λg αβ = (8πG/c 4 ) T αβ very precisely tested on solar system scales (but Pioneer)
More informationarxiv:astro-ph/ v1 22 Sep 2005
Mass Profiles and Shapes of Cosmological Structures G. Mamon, F. Combes, C. Deffayet, B. Fort (eds) EAS Publications Series, Vol.?, 2005 arxiv:astro-ph/0509665v1 22 Sep 2005 MONDIAN COSMOLOGICAL SIMULATIONS
More informationDark Matter. 4/24: Homework 4 due 4/26: Exam ASTR 333/433. Today. Modified Gravity Theories MOND
Dark Matter ASTR 333/433 Today Modified Gravity Theories MOND 4/24: Homework 4 due 4/26: Exam Not any theory will do - length scale based modifications can be immediately excluded as the discrepancy does
More informationDark Matter. ASTR 333/433 Spring 2018 T R 4:00-5:15pm Sears 552
Dark Matter ASTR 333/433 Spring 2018 T R 4:00-5:15pm Sears 552 TODAY - Laws of Galactic Rotation - Flat rotation curves - Tully-Fisher - Universal Rotation curve - central Density Relation - Renzo s Rule
More informationProbing Gravity in the Low Acceleration Regime with Globular Clusters
Probing Gravity in the Low Acceleration Regime with Globular Clusters By Riccardo Scarpa, Gianni Marconi & Roberto Gilmozzi European Southern Observatory The idea of this study sparked from the following
More informationDynamical friction, galaxy merging, and radial-orbit instability in MOND
Dynamical friction, galaxy merging, and radial-orbit instability in MOND Carlo Nipoti Dipartimento di Astronomia Università di Bologna Strasbourg, 29 June 2010 Outline MOND and Equivalent Newtonian Systems
More informationarxiv: v1 [astro-ph.ga] 13 Mar 2019
Astronomy & Astrophysics manuscript no. ETGfields-arxiv c ESO 9 March 5, 9 Study of gravitational fields and globular cluster systems of early-type galaxies M. Bílek,, S. Samurović 3, and F. Renaud 4 arxiv:93.5659v
More informationModified Dark Matter: Does Dark Matter Know about the Cosmological Constant?
Modified Dark Matter: Does Dark Matter Know about the Cosmological Constant? Douglas Edmonds Emory & Henry College (moving to Penn State, Hazleton) Collaborators Duncan Farrah Chiu Man Ho Djordje Minic
More informationarxiv: v1 [astro-ph.ga] 27 Mar 2019
Author s version, Nature BCA, 12thSept.2018 Does the galaxy NGC1052-DF2 falsify Milgromian dynamics? arxiv:1903.11612v1 [astro-ph.ga] 27 Mar 2019 Pavel Kroupa 1,2, Hosein Haghi 1,3, Behnam Javanmardi 4,
More informationLaws of Galactic Rotation. Stacy McGaugh Case Western Reserve University
Laws of Galactic Rotation Stacy McGaugh Case Western Reserve University UGC 2885 Galaxies NGC 2403 Huge dynamic range in 10 kpc Gravitationally self-bound entities composed of stars, gas, dust, [& dark
More informationMOdified Newtonian Dynamics an introductory review. Riccardo Scarpa European Southern Observatory
MOdified Newtonian Dynamics an introductory review By Riccardo Scarpa European Southern Observatory Everything started in 1933 with the work by Zwicky on the Coma cluster of galaxies, but were galaxy rotation
More informationUniversal Properties of Galactic Rotation Curves and a First Principles Derivation of the Tully-Fisher Relation
Universal Properties of Galactic Rotation Curves and a First Principles Derivation of the Tully-Fisher Relation James G. O Brien 1, Thomas L. Chiarelli 2, and Philip D. Mannheim 3 1 Department of Sciences,
More informationThe physical origin of stellar envelopes around globular clusters
The physical origin of stellar envelopes around globular clusters Phil Breen University of Edinburgh in collaboration with A. L. Varri, J. Peñarrubia and D. C. Heggie Current observational evidence Example:
More informationDark Matter. ASTR 333/433 Fall 2013 M T 4:00-5:15pm Sears 552. Prof. Stacy McGaugh Sears
Dark Matter ASTR 333/433 Fall 2013 M T 4:00-5:15pm Sears 552 Prof. Stacy McGaugh Sears 573 368-1808 stacy.mcgaugh@case.edu Empirical Laws of Galactic Rotation Homework 2 due Oct 15 midterm Oct 29 What
More informationGalaxies in the Cosmic Web
Galaxies in the Cosmic Web Empirical Constraints on Halo Profiles from Rotation Curves Stacy McGaugh University of Maryland New Mexico State University, Las Cruces, 19 May 2006 1. Global Correlations:
More informationDeriving stellar masses from SDSS
Deriving stellar masses from SDSS Reference: Bruzual and Charlot 2003MNRAS.344.1000B Kauffmann et al. 2003MNRAS.341.33 Salim et al. 2007ApJS..173..267S Bell et al. 2003ApJS..149..289B Outline! Basic idea!
More informationThe Baryonic Tully-Fisher Relation
NRAO - TF35: Global Properties of HI in Galaxies Workshop - 1 April 2012 The Baryonic Tully-Fisher Relation Stacy McGaugh University of Maryland Tully & Fisher (1977) Abs. Mag. line-width 9/30/10 3/30/10
More information11 days exposure time. 10,000 galaxies. 3 arcminutes size (0.1 x diameter of moon) Estimated number of galaxies in observable universe: ~200 billion
11 days exposure time 10,000 galaxies 3 arcminutes size (0.1 x diameter of moon) Estimated number of galaxies in observable universe: ~200 billion Galaxies with disks Clumpy spiral shapes Smooth elliptical
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationROE, Edinburgh, 20 April 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 informationDwarf Galaxy Dispersion Profile Calculations Using a Simplified MOND External Field Effect
Dwarf Galaxy Dispersion Profile Calculations Using a Simplified MOND External Field Effect On the Shoulders of Giants Workshop Case Western Reserve University June 7, 2017 Stephen Alexander Physics Department
More informationGalaxy Rotation Curves of a Galactic Mass Distribution. By: Camiel Pieterse Supervised by: Prof. dr. Wim Beenakker Theoretical High Energy Physics
Galaxy Rotation Curves of a Galactic Mass Distribution By: Camiel Pieterse Supervised by: Prof. dr. Wim Beenakker Theoretical High Energy Physics 1 Contents 1 Introduction 3 2 Mass Distribution 5 2.1 The
More informationJohn Moffat Perimeter Institute Waterloo, Ontario, Canada
New Results in Modified Gravity Without Dark Matter John Moffat Perimeter Institute Waterloo, Ontario, Canada The research was supported by the John Templeton Foundation Talk given at the topical conference
More informationGMU, April 13, The Pros and Cons of Invisible Mass and Modified Gravity. Stacy McGaugh University of Maryland
GMU, April 13, 2007 The Pros and Cons of Invisible Mass and Modified Gravity Stacy McGaugh University of Maryland What gets us into trouble is not what we don t know. It s what we know for sure that just
More informationOn MOND and dark matter in ultra compact dwarf galaxies
On MOND and dark matter in ultra compact dwarf galaxies Jörg Dabringhausen Argelander-Institut für Astronomie, University of Bonn Pavel Kroupa Michael Hilker, Michael Fellhauer, Steffen Mieske, Michael
More informationModified Dark Matter: Does Dark Matter Know about the Cosmological Constant? Douglas Edmonds Emory & Henry College
Modified Dark Matter: Does Dark Matter Know about the Cosmological Constant? Douglas Edmonds Emory & Henry College Collaborators Duncan Farrah Chiu Man Ho Djordje Minic Y. Jack Ng Tatsu Takeuchi Outline
More informationMiami Modified dark matter in galaxy clusters. Douglas Edmonds Emory & Henry College
Miami 2015 Modified dark matter in galaxy clusters Douglas Edmonds Emory & Henry College Collaboration D. Edmonds Emory & Henry College D. Farrah Virginia Tech C.M. Ho Michigan State University D. Minic
More informationarxiv: v2 [astro-ph.ga] 5 Nov 2018
MOND in galaxy groups Mordehai Milgrom Department of Particle Physics and Astrophysics, Weizmann Institute arxiv:1810.03089v2 [astro-ph.ga] 5 Nov 2018 Galaxy groups, which have hardly been looked at in
More informationRelationship Between Newtonian and MONDian Acceleration
Advances in Applied Physics, Vol. 4, 2016, no. 1, 31-37 HIKARI Ltd, www.m-hikari.com http://dx.doi.org/10.12988/aap.2016.6810 Relationship Between Newtonian and MONDian Acceleration A. S. Sarabi Department
More informationObservational Evidence for Dark Matter. Simona Murgia, SLAC-KIPAC
Observational Evidence for Dark Matter Simona Murgia, SLAC-KIPAC XXXIX SLAC Summer Institute 28 July 2011 Outline Evidence for dark matter at very different scales Galaxies Clusters of galaxies Universe???
More informationThe Stellar Initial Mass Function of Massive Galaxies
The Stellar Initial Mass Function of Massive Galaxies Aaron A. Dutton Max Planck Institute for Astronomy (MPIA), Heidelberg, Germany Quenching and Quiescence, Heidelberg, July 2014 Motivation What is the
More informationarxiv: v2 [astro-ph.ga] 3 Jul 2018
Astronomy & Astrophysics manuscript no. FitRAR c ESO 218 July 4, 218 Fitting the radial acceleration relation to individual SPARC galaxies Pengfei Li 1, Federico Lelli 2,, Stacy S. McGaugh 1, and James
More informationWeak lensing measurements of Dark Matter Halos around galaxies
Weak lensing measurements of Dark Matter Halos around galaxies Rachel Mandelbaum Carnegie Mellon University 1 Image credits: NASA, ESA, S. Beckwith (STScI), the HUDF Team 2 Image credit: ESA/Planck 3 The
More informationUniversity of Groningen. Understanding disk galaxies with the Tully-Fisher relation Ponomareva, Anastasia
University of Groningen Understanding disk galaxies with the Tully-Fisher relation Ponomareva, Anastasia IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationUsing globular clusters to test gravity in the weak acceleration regime
Using globular clusters to test gravity in the weak acceleration regime Riccardo Scarpa 1, Gianni Marconi 2, Roberto Gilmozzi 2, and Giovanni Carraro 3 1 Instituto de Astrofísica de Canarias, Spain 2 European
More informationAngular Momentum Problems in Disk Formation
Angular Momentum Problems in Disk Formation MPIA Theory Group Seminar, 07/03/2006 The Standard Picture Disks galaxies are systems in centrifugal equilibrium Structure of disks is governed by angular momentum
More informationInsights on galaxy evolution from the dark matter content of massive early-type galaxies Crescenzo Tortora
Insights on galaxy evolution from the dark matter content of massive early-type galaxies Crescenzo Tortora ITP Zurich What is fun with dark matter (DM)? DARK MATTER DC comics Futurama come back to talk
More informationClusters and groups of galaxies: internal structure and dynamics
Clusters and groups of galaxies: internal structure and dynamics Strong constraints on cosmological theories and on the nature of dark matter can be obtained from the study of cluster masses, mass distribution,
More informationMOND + 11eV sterile neutrinos
MOND + 11eV sterile neutrinos PPC10 - Day 2 13 -July-2010 th Garry Angus Caustic Group @ UTorino (INFN) In collaboration with Antonaldo Diaferio & Benoit Famaey Modified Newtonian Dynamics MOND new physical
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationTesting Verlinde's emergent gravity in early-type galaxies Tortora, Crescenzo; Koopmans, L.V.E.; Napolitano, N. R.; Valentijn, E
University of Groningen Testing Verlinde's emergent gravity in early-type galaxies Tortora, Crescenzo; Koopmans, L.V.E.; Napolitano, N. R.; Valentijn, E Published in: Monthly Notices of the Royal Astronomical
More informationThe Dark Matter Problem
The Dark Matter Problem Dr. Yves Gaspar, Ph.D. ( University of Cambridge, UK) Università Cattolica del Sacro Cuore, Brescia Department of Mathematics and Physics. Implications of astronomical data. James
More informationOn the Extension of the Baryonic Tully-Fisher Relation to Galaxy Clusters and Super Massive-Cosmic Systems
Open Access Library Journal 17, Volume 4, e3686 ISSN Online: 333-971 ISSN Print: 333-975 On the Extension of the Baryonic Tully-Fisher Relation to Galaxy Clusters and Super Massive-Cosmic Systems Barbaro
More informationarxiv: v2 [astro-ph] 24 Apr 2007
Mon. Not. R. Astron. Soc. 000, 000 000 (2007) Printed 1 February 2008 (MN LATEX style file v2.2) Vertical dynamics of disk galaxies in MOND Carlo Nipoti 1, Pasquale Londrillo 2, Hong Sheng Zhao 3, and
More informationThe Need for Dark Matter in MOND on Galactic Scales
The Need for Dark Matter in MOND on Galactic Scales Muhammad Furqaan Yusaf Kings College London, Strand Campus, Department of Physics. muhammad.yusaf@kcl.ac.uk September 28, 2007 As presented by I. Ferreras,
More informationMODEL OF DARK MATTER AND DARK ENERGY BASED ON GRAVITATIONAL POLARIZATION. Luc Blanchet. 15 septembre 2008
MODEL OF DARK MATTER AND DARK ENERGY BASED ON GRAVITATIONAL POLARIZATION Luc Blanchet Gravitation et Cosmologie (GRεCO) Institut d Astrophysique de Paris 15 septembre 2008 Luc Blanchet (GRεCO) Séminaire
More informationMOND and the Galaxies
MOND and the Galaxies Françoise Combes Observatoire de Paris With Olivier Tiret Angus, Famaey, Gentile, Wu, Zhao Wednesday 1st July 2009 MOND =MOdified Newtonian Dynamics Modification at weak acceleration
More informationGalaxy mass models: MOND versus dark matter haloes
MNRAS (2014) MNRAS Advance Access published February 17, 2014 doi:10.1093/mnras/stu100 Galaxy mass models: MOND versus dark matter haloes Toky H. Randriamampandry and Claude Carignan Department of Astronomy,
More informationGaia Revue des Exigences préliminaires 1
Gaia Revue des Exigences préliminaires 1 Global top questions 1. Which stars form and have been formed where? - Star formation history of the inner disk - Location and number of spiral arms - Extent of
More informationDark Matter and/or MOND in Giant Ellipticals
Dark Matter and/or MOND in Giant Ellipticals NGC 4636 & NGC 1399 Ylva Schuberth Tom Richtler, Michael Hilker, Boris Dirsch 1 July 2010 / Strasbourg Y. Schuberth (AIfA) Strasbourg 1 / 16 Outline 1 Globular
More informationTully-Fisher relation, key to dark matter in galaxies
Invisible Universe Paris, June 29- July 3, 2009 Tully-Fisher relation, key to dark matter in galaxies Y. Sobouti Institute for Advanced Studies in Basic Sciences, Zanjan, P O Box 45195-1159, Zanjan 45195,
More informationTidal streams as gravitational experiments!
Tidal streams as gravitational experiments! Benoit Famaey CNRS - Observatoire astronomique de Strasbourg MOND paradigm MDAR: McGaugh et al. 2016 Lelli et al. 2016 Famaey & McGaugh 2012 MOND paradigm Prediction:
More informationVisible Matter. References: Ryden, Introduction to Cosmology - Par. 8.1 Liddle, Introduction to Modern Cosmology - Par. 9.1
COSMOLOGY PHYS 30392 DENSITY OF THE UNIVERSE Part I Giampaolo Pisano - Jodrell Bank Centre for Astrophysics The University of Manchester - March 2013 http://www.jb.man.ac.uk/~gp/ giampaolo.pisano@manchester.ac.uk
More informationThe dynamics of face-on galaxies in MOND
Journal of Physics: Conference Series PAPER OPEN ACCESS The dynamics of face-on galaxies in MOND To cite this article: Garry W. Angus 2016 J. Phys.: Conf. Ser. 718 032001 View the article online for updates
More informationClusters: Observations
Clusters: Observations Last time we talked about some of the context of clusters, and why observations of them have importance to cosmological issues. Some of the reasons why clusters are useful probes
More informationModified Gravity (MOG) and Dark Matter: Can Dark Matter be Detected in the Present Universe?
Modified Gravity (MOG) and Dark Matter: Can Dark Matter be Detected in the Present Universe? John Moffat Perimeter Institute, Waterloo, Ontario, Canada Talk given at the Miami 2014 topical conference on
More informationStellar Mass Estimates of Galaxies in Superclusters at z~1
Stellar Mass Estimates of Galaxies in Superclusters at z~1 Catherine Whiting The University of Iowa Advisor: Dr. Roy Gal Institute for Astronomy, University of Hawai i at Manoa Abstract. A simple method
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 informationTristan Clark. And. Dr. Stephen Alexander. Capstone Final Paper. Miami University of Ohio
1 N- Body Simulations of a Dwarf Spheroidal Galaxy Comparing Newtonian, Modified Newtonian, and Dark Matter Models. Tristan Clark And Dr. Stephen Alexander Capstone Final Paper Miami University of Ohio
More informationExploring Extended MOND in Galaxy Clusters. Alistair Hodson Supervisor Hongsheng Zhao
Exploring Extended MOND in Galaxy Clusters Alistair Hodson Supervisor Hongsheng Zhao Overview What is Extended MOND (EMOND)? What is the motivation for EMOND? What are the implications of EMOND? How successful
More informationDark Matter in Dwarf Galaxies
Maryland Center for Fundamental Physics & Joint Space-Science Institute 26-28 May 2010 Advances in Theoretical and Observational Cosmology Dark Matter in Dwarf Galaxies Stacy McGaugh University of Maryland
More informationarxiv: v1 [astro-ph.ga] 12 Dec 2018
Preprint 13 December 2018 Compiled using MNRAS LATEX style file v3.0 Is there a fundamental acceleration scale in galaxies? Zhe Chang, 1,2 Yong Zhou 1,2 1 Institute of High Energy Physics, Chinese Academy
More informationTEREZA JEŘÁBKOVÁ ESO GARCHING & UNIVERSITY OF BONN & CHARLES UNIVERSITY IN PRAGUE
1 TEREZA JEŘÁBKOVÁ ESO GARCHING & UNIVERSITY OF BONN & CHARLES UNIVERSITY IN PRAGUE www: sirrah.troja.mff.cuni.cz/~tereza email: tjerabko@eso.org 17 MODEST UNDER PRAGUE S STARRY SKIES CZECH REPUBLIC 18-22
More informationarxiv:astro-ph/ v1 10 May 1998
Testing Modified Newtonian Dynamics with Low Surface Brightness Galaxies Rotation curve fits arxiv:astro-ph/9805120v1 10 May 1998 W.J.G. de Blok 1 and S.S. McGaugh 2 1 Kapteyn Astronomical Institute, P.O.
More informationThe effect of primordial mass segregation on the size scale of the star clusters
The effect of primordial mass segregation on the size scale of the star clusters Hosein Haghi In collaboration with: HoseiniRad, Zonoozi, Kuepper Institute for Advanced Studies in Basic Sciences (IASBS),Zanjan
More informationASTR 610 Theory of Galaxy Formation Lecture 18: Disk Galaxies
ASTR 610 Theory of Galaxy Formation Lecture 18: Disk Galaxies Frank van den Bosch Yale University, spring 2017 The Structure & Formation of Disk Galaxies In this lecture we discuss the structure and formation
More informationThe Radial Acceleration Relation of Galaxies
The Radial Acceleration Relation of Galaxies Federico Lelli ESO Fellow (Garching, Germany) In collaboration with Stacy McGaugh (Case Western Reserve University) James Schombert (University of Oregon) Marcel
More informationDark Matter. ASTR 333/433 Spring Today Stars & Gas. essentials about stuff we can see. First Homework on-line Due Feb. 4
Dark Matter ASTR 333/433 Spring 2016 Today Stars & Gas essentials about stuff we can see First Homework on-line Due Feb. 4 Galaxies are made of stars - D. Silva (1990) private communication Stars Majority
More informationGalaxies Astro 530 Prof. Jeff Kenney
Galaxies Astro 530 Prof. Jeff Kenney CLASS 7 February 5, 2018 Tully-Fisher Relation (finish) & Spiral Structure (start) 1 Tully-Fisher relation M B,i Tradi7onal Tully- Fisher rela7on: Good correla7on between
More informationFitting the NGC 1560 rotation curve and other galaxies in the constant Lagrangian model for galactic dynamics.
Fitting the NGC 1560 rotation curve and other galaxies in the constant Lagrangian model for galactic dynamics. 1, a) E.P.J. de Haas Nijmegen, The Netherlands (Dated: April 24, 2018) The velocity rotation
More informationPoisson Equation. The potential-energy tensor. Potential energy: work done against gravitational forces to assemble a distribution of mass ρ(x)
Poisson Equation 1 2 Potential energy: work done against gravitational forces to assemble a distribution of mass ρ(x) The potential-energy tensor Assuming a distribution of mass is already in place, and
More informationGlobal Scaling Relations of Spiral Galaxies
Global Scaling Relations of Spiral Galaxies Aaron A. Dutton Max Planck Institute for Astronomy (MPIA), Heidelberg, Germany IAU 311, Galaxy Masses as constraints to Formation Models, Oxford, July 2014 Outline
More informationarxiv: v2 [astro-ph.co] 28 Sep 2012
Testing MOND Over a Wide Acceleration Range in X-Ray Ellipticals Mordehai Milgrom DPPA, Weizmann Institute of Science, Rehovot 76100, Israel arxiv:1205.1308v2 [astro-ph.co] 28 Sep 2012 The gravitational
More informationThe dark and visible matter content of low surface brightness disk galaxies Blok, W. J. G. de; McGaugh, S. S.
University of Groningen The dark and visible matter content of low surface brightness disk galaxies Blok, W. J. G. de; McGaugh, S. S. Published in: The Astrophysical Journal IMPORTANT NOTE: You are advised
More informationarxiv: v1 [astro-ph.co] 16 Jan 2012
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 27 December 2017 (MN LATEX style file v2.2) A QUMOND galactic N-body code I: Poisson solver and rotation curve fitting arxiv:1201.3185v1 [astro-ph.co]
More informationNumerical simulations of Modified Newtonian Dynamics
Journal of Physics: Conference Series PAPER OPEN ACCESS Numerical simulations of Modified Newtonian Dynamics To cite this article: G N Candlish et al 2016 J. Phys.: Conf. Ser. 720 012012 View the article
More informationThe mass discrepancy acceleration relation in early-type galaxies: extended mass profiles and the phantom menace to MOND
San Jose State University From the SelectedWorks of Aaron J. Romanowsky September, 2016 The mass discrepancy acceleration relation in early-type galaxies: extended mass profiles and the phantom menace
More informationMODIFIED NEWTONIAN DYNAMICS AS AN ALTERNATIVE TO DARK MATTER
MODIFIED NEWTONIAN DYNAMICS AS AN ALTERNATIVE TO DARK MATTER Robert H. Sanders 1 & Stacy S. McGaugh 2 1 Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands 2 Department
More informationMOND and the Galaxies
MOND and the Galaxies F. Combes a and O. Tiret b a Observatoire de Paris, LERMA, 61 Av de l Observatoire, F-75014 Paris, France b SISSA, via Beirut 4, I-34014 Trieste, Italy Abstract. We review galaxy
More informationIonized Hydrogen (HII)
Ionized Hydrogen (HII) While ionized hydrogen (protons, electrons) forms the majority of the ionized phase of the ISM, it also contains ionized forms of other elements: e.g., OII, OIII, CIV, MgII. Highest
More information12.1 Elliptical Galaxies
12.1 Elliptical 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
More informationMODIFIED NEWTONIAN DYNAMICS AS AN ALTERNATIVE TO DARK MATTER
Annu. Rev. Astron. Astrophys. 2002. 40:263 317 doi: 10.1146/annurev.astro.40.060401.093923 Copyright c 2002 by Annual Reviews. All rights reserved MODIFIED NEWTONIAN DYNAMICS AS AN ALTERNATIVE TO DARK
More informationHigh-redshift galaxies
High-redshift galaxies Houjun Mo May 4, 2004 Galaxies can now be observed to z 6 Normal galaxies with 0.2 < z < 1 The Lyman-break population at z 3 The sub-mm sources at z 3 Between 1 2, spectroscopy desert,
More informationCAULDRON: dynamics meets gravitational lensing. Matteo Barnabè
CAULDRON: dynamics meets gravitational lensing Matteo Barnabè KIPAC/SLAC, Stanford University Collaborators: Léon Koopmans (Kapteyn), Oliver Czoske (Vienna), Tommaso Treu (UCSB), Aaron Dutton (MPIA), Matt
More informationDARK MATTER IN GALAXIES. Deqian Yuan
DARK MATTER IN GALAXIES Deqian Yuan INTRODUCTION Dark Matter(From Merriam Webster): Nonluminous matter not yet directly detected by astronomers that is hypothesized to exist to account for various observed
More informationEvidence for/constraints on dark matter in galaxies and clusters
Nov 11, 2015 Evidence for/constraints on dark matter in galaxies and clusters HW#9 is due; please hand in your summaries; then you get to talk (I have slides of the different facilities/telescopes. HW#10
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 informationarxiv: v1 [astro-ph.ga] 31 Dec 2016
Draft version April 23, 218 Preprint typeset using L A TEX style emulateapj v. 5/2/11 MASS-TO-LIGHT VERSUS COLOR RELATIONS FOR DWARF IRREGULAR GALAXIES Kimberly A. Herrmann 1, Deidre A. Hunter 2, Hong-Xin
More information