What can M2M do for Milky Way Models?

Size: px
Start display at page:

Download "What can M2M do for Milky Way Models?"

Transcription

1 What can M2M do for Milky Way Models? Ortwin Gerhard Max-Planck-Institut für Extraterrestrische Physik, Garching Thanks to F. de Lorenzi, V. Debattista, P. Das, L. Morganti I. Made-to-Measure Adaptive N-body Modeling... II.... for the Milky Way 1 NGC 6946 (image from D. Block)

2 Made-to-Measure Modeling Various stellar components orbiting in one gravitational potential Each component characterized by one or more phase-space distributions; their parameters could be Z, [α /Fe], age, when measurable. Dynamical modeling: understand intrinsic properties of a stellar system from the observable data: e.g., gravitational potential, orbits of a certain group of stars, global anisotropy, then relate to formation history. Examples: elliptical galaxies, spiral bulges, Milky Way, dark halos, black hole masses Made-to-measure: adaptive N-body technique for constructing equilibrium models of stellar systems. Between std. N-body and Schwarzschild models 2

3 Made-To-Measure (M2M) Method Aim: construct an N-particle system to match a prescribed target 3

4 4

5 Galactic Bulge Target Initial Model Final Model M2M model from Bissantz et al. 2004, constrained by surface density from Bissantz & G Resimulated: Courtesy Victor Debattista Target I.C.s Target Final model 5

6 χ 2M2M Aim: construct an N-particle system to match a prescribed set of target data [(surface) density, kinematics] in a χ 2-sense 6

7 NMAGIC Flow Chart & Parallelization N-Particle Made-to-Measure AlGorithm MInimizing Chi2 Left (+): Time/χ 2M2M step Right ( ): χ 2M2M steps/unit time vs N(processors), for N= particles 7

8 NMAGIC N-Particle Made-to-Measure AlGorithm MInimizing Chi2 de Lorenzi, Debattista, Gerhard, Sambhus, 2007, MNRAS, 376, 71 Implements χ 2M2M Has been tested for spherical, axisymmetric, triaxial, rotating triaxial models Example for NMAGIC in action Spherical Initial Model Triaxial Target Wide range of applications in galaxy modelling: - triaxial E s & bulges, - rotating systems, - black hole masses, - dark halos - Milky Way 8

9 Evolution of χ 2 and particle weights Truncated Hernquist Sphere: Fit of mass structure (1st) and integral-field kinematics (2nd ); relaxation (3rd); stability test (4th phase) 9

10 Test: Recovering Maximally Rotating Oblate System Lz Lz target -E -E Int.Fld ICs slits 10

11 Discrete Velocities De Lorenzi et al

12 Efficient M/L Estimation Convergence of fitted M/L; true value M/L=5 De Lorenzi et al χ of models with different M/L 12 Ortwin Gerhard, Leiden,

13 Discussion: Schwarzschild vs χ 2M2M Schwarzschild method + orbits complete orbit sampling binning storage of orbits as symmetry work + fast in fixed potential Current state of the art e.g. for BH measurements χ 2M2M independent particles / orbit + no sampling or binning all-orbit ICs + none - on the fly + no symmetry restrictions, good. for model designing still slow + self-consistent potential evln. + std. Nbody limit: stability Great promise but work to do 13

14 Observables (NGC 3379) Kinematic data luminosity weighted GaussHermite moments of the LOSVD Photometric data SAURON data (Shapiro+06) Surfaced brightness and luminosity density Slit kinematics Deprojection, e.g., axisymmetric Magorrian (1999) (Statler & SmeckerHane 99) Figure from Douglas+07 Discrete data PNe data (Douglas+07) either binned or as discrete velocities Ortwin Gerhard, dLeiden, luminosity density

15 NMAGIC A New Way of Modeling Galaxies Basel&MPE De Lorenzi, Gerhard etal., MNRAS N-particle model approaches target data for elliptical galaxy NGC 3379 Top right: Light distribution (observer sees ~spherical image from top) Top left: radial profile of stellar velocity dispersion Left: Projected kinematics of NGC 3379 (SAURON data) v=mean line-ofsight velocity σ =velocity dispersion of the stars hn= higher order moments Lower left: Initial Final model fit (final model instead of film) Applications: black hole masses, dark matter halos, Ortwin Gerhard, Leiden,

16 Spherical Models for NGC 3379 in Different Potentials NGC 3379 model potentials range from stars only (- -. Model A), to stars plus dark halo models (, B-E). Models A, E (weakly) ruled out by likelihood analysis shaded range is from Dekel et al. (2005) star-forming merger simulations on orbits from Λ CDM cosmology de Lorenzi et al Falling PN velocity dispersion profile can be reproduced in A-D Baryons centrally concentrated, but no contradiction to Λ CDM 16

17 Halo Dynamics in NGC 3379 & NGC 4697 Best axisymmetric models for NGC 3379 (red) and N4697 (blue) have moderately falling circular velocity curves and radially anisotropic halos (de Lorenzi et al. 2008, 2009) Fig. from Napolitano et al shows virial masses and concentrations from fitted NFW models & compares with LCDM 1sigma range from Bullock et al Strongly radially falling dispersion profiles in NGC 3379, NGC 4697 do not necessarily imply non-standard diffuse halos, but may be consistent with predicted scatter. 17

18 What would we like to know? Various stellar components orbiting in one gravitational potential Each component characterized by one or more phase-space distributions; their parameters could be Z, [α /Fe], age, when measurable. Like to know about: formation and assembly history, dynamical history, history of star formation and chemical evolution, processes and events Fossil record: distribution over orbits and stellar pop. parameters; but this is snapshot, need to compare with evolutionary simulations Observations to tell us about stellar kinematics Z, [α /Fe], etc. Need to determine potential and can then invert kin.obsvs. orbits 18

19 Disk Models Problem: see only small fraction of particles from the N-body model in magnitude limited surveys (e.g., Brown et al. 2004, 2005). Suggest we can circumvent this with M2M/NMAGIC: modeling of observables can be done with time-averaging (~ N) can then forward-integrate in the potential to create and superpose multiple snapshots in the solar neighbourhood To be demonstrated. Problem: large-scale structure (disk scale lengths..) and potential Need hierarchy of models. Stellar potential through particles. Problem: get particle distribution, not phase-space DF. Under consideration.. 19

20 Bulge Models Previous bulge models: Zhao (1996), Haefner et al. (2000) Schwarzschild technique; Fux (1997) (std. Nbody) Density model: Bissantz & G. (2002), rotating bulge bar (nonparametric, penalized maximum likelihood Successes include clump giant los distributions, microlensing optical depth, gas flow. Pattern speed km/s/kpc Procedure: dissipate transients (5 Trot), evolve with M2M (25 Trot), relax (11 Trot) Debattista et al. in prep. 20

21 Preliminary Bulge Model for RCG Kinematics Match to RCG data (Rangwala)

22 Conclusions Adaptive particle methods ( made-to-measure ) can be used both in the pure N-body and Schwarzschild limits Offer a lot of power and promise, interesting new possibilities: (in principle no symmetry restriction, time evolution of particle potential, ) Still new and number of aspects still need to be understood (best force of change from data, convergence, initial conditions, noisy data & smoothing, how to increase efficiency,..) Work to do!! These methods will be great for some aspects of Milky Way research 22

NMAGIC Made-to-Measure Modeling of Elliptical Galaxies NMAGIC - 2 M2M

NMAGIC Made-to-Measure Modeling of Elliptical Galaxies NMAGIC - 2 M2M NMAGIC Made-to-Measure Modeling of Elliptical Galaxies Ortwin Gerhard, MPE, Garching gerhard@mpe.mpg.de I. Made-to-measure dynamical modeling with NMAGIC II Elliptical galaxy halo kinematics with planetary

More information

Stellar Orbits and Angular Momentum in Early-Type Galaxy Halos Ortwin Gerhard, MPE, Garching

Stellar Orbits and Angular Momentum in Early-Type Galaxy Halos Ortwin Gerhard, MPE, Garching Stellar Orbits and Angular Momentum in Early-Type Galaxy Halos Ortwin Gerhard, MPE, Garching gerhard@mpe.mpg.de 1. Preamble Arnaboldi et al 2013 2. Predictions: ETG halos in cosmological simulations 3.

More information

Made-to-Measure (M2M) Dynamical modelling of external galaxies and the Milky Way

Made-to-Measure (M2M) Dynamical modelling of external galaxies and the Milky Way Made-to-Measure (M2M) Dynamical modelling of external galaxies and the Milky Way Shude Mao (NAOC/Manchester) Oct. 31, 2012@KIAS Collaborators: Richard Long, Yougang Wang, Juntai Shen Motivation Important

More information

Overview of Dynamical Modeling. Glenn van de Ven

Overview of Dynamical Modeling. Glenn van de Ven Overview of Dynamical Modeling Glenn van de Ven glenn@mpia.de 1 Why dynamical modeling? -- mass total mass stellar systems key is to their evolution compare luminous mass: constrain DM and/or IMF DM radial

More information

Dynamical modelling of galaxies. Eugene Vasiliev

Dynamical modelling of galaxies. Eugene Vasiliev Dynamical modelling of galaxies Eugene Vasiliev DAGAL summer school, Marseille, 2014 Plan Overview of dynamical modelling problem Theoretical and observational approaches The Schwarzschild orbit superposition

More information

Inner dynamics of massive galaxies (ETG) Michele Cappellari

Inner dynamics of massive galaxies (ETG) Michele Cappellari Inner dynamics of massive galaxies (ETG) Michele Cappellari First rotation curve of an elliptical (Bertola+Capaccioli75) Elliptical galaxy NGC4697 2 hr of observations at 5-m Palomar Angular momentum much

More information

Dynamical friction, galaxy merging, and radial-orbit instability in MOND

Dynamical 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 information

Gaia Revue des Exigences préliminaires 1

Gaia 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 information

Stellar Dynamics and Structure of Galaxies

Stellar Dynamics and Structure of Galaxies Stellar Dynamics and Structure of Galaxies Gerry Gilmore H47 email: gil@ast.cam.ac.uk Lectures: Monday 12:10-13:00 Wednesday 11:15-12:05 Friday 12:10-13:00 Books: Binney & Tremaine Galactic Dynamics Princeton

More information

ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014

ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014 ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools

More information

An Introduction to Galaxies and Cosmology. Jun 29, 2005 Chap.2.1~2.3

An Introduction to Galaxies and Cosmology. Jun 29, 2005 Chap.2.1~2.3 An Introduction to Galaxies and Cosmology Jun 29, 2005 Chap.2.1~2.3 2.1 Introduction external galaxies normal galaxies - majority active galaxies - 2% high luminosity (non-stellar origin) variability

More information

Gas and Stellar Dynamical Black Hole Mass Measurements:

Gas and Stellar Dynamical Black Hole Mass Measurements: Gas and Stellar Dynamical Black Hole Mass Measurements: Revisiting M84 and a Consistency Test with NGC 3998 Jonelle Walsh (UC Irvine/UT Austin) Aaron Barth (UC Irvine) Remco van den Bosch (MPIA) Marc Sarzi

More information

A Universe in Motion: Testing the Cosmological Paradigm with Galaxy Dynamics. John Dubinski, Toronto

A Universe in Motion: Testing the Cosmological Paradigm with Galaxy Dynamics. John Dubinski, Toronto A Universe in Motion: Testing the Cosmological Paradigm with Galaxy Dynamics John Dubinski, Toronto Outline Cosmology and galaxy dynamics Tools of the trade and computational challenges Case Studies: Triaxial

More information

b a = 1 n 10. Surface brightness profile of most elliptical galaxies can be fit well by the R 1/4 (or de Vaucouleurs) law, (1 ɛ) 2 a 2 = 1.

b a = 1 n 10. Surface brightness profile of most elliptical galaxies can be fit well by the R 1/4 (or de Vaucouleurs) law, (1 ɛ) 2 a 2 = 1. 7 Elliptical Galaxies Basic properties of elliptical galaxies Formation of elliptical galaxies 7.1 Photometric Properties Isophotes of elliptical galaxies are usually fitted by ellipses: Major axis a;

More information

Galaxy Morphology. - a description of the structure of galaxies

Galaxy Morphology. - a description of the structure of galaxies Galaxy Morphology - a description of the structure of galaxies Galaxy Morphology - a description of the structure of galaxies Galaxy Morphology - a description of the structure of galaxies Clearly astronomical

More information

arxiv:astro-ph/ v1 30 Nov 2004

arxiv:astro-ph/ v1 30 Nov 2004 Probing Halos with PNe: Mass and Angular Momentum in Early-Type Galaxies Aaron J. Romanowsky arxiv:astro-ph/0411797v1 30 Nov 2004 School of Physics and Astronomy, University of Nottingham, University Park,

More information

Constraints on secular evolution in unbarred spiral galaxies: understanding bulge and disk formation

Constraints on secular evolution in unbarred spiral galaxies: understanding bulge and disk formation Constraints on secular evolution in unbarred spiral galaxies: understanding bulge and disk formation July 10 th 2012 Marja Kristin Seidel Jesús Falcón - Barroso Instituto de Astrofísica de Canarias www.iac.es/project/traces

More information

Fundamental Planes and Galaxy Formation

Fundamental Planes and Galaxy Formation Fundamental Planes and Galaxy Formation Philip Hopkins, NoviCosmo 2007 Fundamental Planes = Scaling Laws Obeyed by Galaxies vs Origin of scaling laws: Ideally, we d understand every galaxy as an individual:

More information

arxiv:astro-ph/ v1 16 Dec 2004

arxiv:astro-ph/ v1 16 Dec 2004 arxiv:astro-ph/0412433v1 16 Dec 2004 The Nuclear Orbital Distribution in Galaxies as Fossil Record of Black Hole Formation from Integral-Field Spectroscopy Michele Cappellari and Richard McDermid Leiden

More information

Modelling the Milky Way bar

Modelling the Milky Way bar Modelling the Milky Way bar Shude Mao Tsinghua University/NAOC June 25, 2015@IPMU Collaborators: Yougang Wang, Richard Long, Juntai Shen, Liang Cao, Outline! Observed properties of barred galaxies " The

More information

M31: black hole & dynamics of nucleus

M31: black hole & dynamics of nucleus M31: black hole & dynamics of nucleus John Magorrian The Great Andromeda Galaxy Princeton, 19 June 2012 1. The black hole at the centre of M31 (just P3) Photometry of P3 (Bender et al 2005) Distinct component

More information

A MUSE view of cd galaxy NGC 3311

A MUSE view of cd galaxy NGC 3311 A MUSE view of cd galaxy NGC 3311 C. E. Barbosa 1, M. Arnaboldi 2, L. Coccato 2, O. Gerhard 3, C. Mendes de Oliveira 1, M. Hilker 2, T. Richtler 4 1 Universidade de São Paulo, São Paulo, Brazil 2 European

More information

Central supermassive black holes from SINFONI observations

Central supermassive black holes from SINFONI observations Central supermassive black holes from SINFONI observations R.P Saglia, MPE with R.Bender, N.Nowak, P. Erwin, J. Thomas Gas and stars in Galaxies A Multi-Wavelength 3D Perspective Garching, 10th June 2008

More information

Volume-limited limited sample

Volume-limited limited sample Masses of Early-Type Galaxies from Atlas 3D Michele Cappellari Mass DF degeneracy SAURON Data Model Cap ppellari+07 Both orbital distribution (DF) and kinematics are 3D Given gravitational potential one

More information

CAULDRON: dynamics meets gravitational lensing. Matteo Barnabè

CAULDRON: 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 information

WHAT IS THE ORIGIN OF THE BLACK HOLE -BULGE MASS CORRELATION? By Curtis McCully

WHAT IS THE ORIGIN OF THE BLACK HOLE -BULGE MASS CORRELATION? By Curtis McCully WHAT IS THE ORIGIN OF THE BLACK HOLE -BULGE MASS CORRELATION? By Curtis McCully OUTLINE What is the Black hole-bulge mass correlation Observations Possible Theoretical Explanations BH - BULGE MASS CORRELATION

More information

Action-based Dynamical Modeling of the Milky Way Disk with Gaia & RAVE

Action-based Dynamical Modeling of the Milky Way Disk with Gaia & RAVE IAU Symposium 330 Nice, 27. April 2017 Action-based Dynamical Modeling of the Milky Way Disk with Gaia & RAVE Wilma Trick (MPIA, Heidelberg) Hans-Walter Rix (MPIA) Jo Bovy (Uni Toronto) Open Questions

More information

Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles

Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles Shanghai Astronomical Observatory In collaboration with Juntai Shen, Xiang Xiang Xue, Chao Liu, Chris Flynn, Ling Zhu, Jie Wang Contents 1

More information

Galaxies: Structure, Dynamics, and Evolution. Elliptical Galaxies (II)

Galaxies: Structure, Dynamics, and Evolution. Elliptical Galaxies (II) Galaxies: Structure, Dynamics, and Evolution Elliptical Galaxies (II) Layout of the Course Feb 5: Review: Galaxies and Cosmology Feb 12: Review: Disk Galaxies and Galaxy Formation Basics Feb 19: Disk Galaxies

More information

Quantifying the (Late) Assembly History of Galaxies. Michael Pierce (University of Wyoming)

Quantifying the (Late) Assembly History of Galaxies. Michael Pierce (University of Wyoming) Quantifying the (Late) Assembly History of Galaxies Michael Pierce (University of Wyoming) What I Think We Already Know: Morphology Density Relation (Assembly Depends on Environment) (Dressler 1980) Ratio

More information

AS1001:Extra-Galactic Astronomy

AS1001: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 information

ASTR 200 : Lecture 25. Galaxies: internal and cluster dynamics

ASTR 200 : Lecture 25. Galaxies: internal and cluster dynamics ASTR 200 : Lecture 25 Galaxies: internal and cluster dynamics 1 Galaxy interactions Isolated galaxies are often spirals One can find small galaxy `groups' (like the Local group) with only a few large spiral

More information

arxiv: v2 [astro-ph.ga] 18 Sep 2016

arxiv: v2 [astro-ph.ga] 18 Sep 2016 MNRAS, 1 (1) Preprint September 1 Compiled using MNRAS LATEX style file v3. The Stellar Halo in the Inner Milky Way: Predicted Shape and Kinematics Angeles Pérez-Villegas 1, Matthieu Portail 1 and Ortwin

More information

Astro 242. The Physics of Galaxies and the Universe: Lecture Notes Wayne Hu

Astro 242. The Physics of Galaxies and the Universe: Lecture Notes Wayne Hu Astro 242 The Physics of Galaxies and the Universe: Lecture Notes Wayne Hu Syllabus Text: An Introduction to Modern Astrophysics 2nd Ed., Carroll and Ostlie First class Wed Jan 3. Reading period Mar 8-9

More information

midterm exam thurs june 14 morning? evening? fri june 15 morning? evening? sat june 16 morning? afternoon? sun june 17 morning? afternoon?

midterm exam thurs june 14 morning? evening? fri june 15 morning? evening? sat june 16 morning? afternoon? sun june 17 morning? afternoon? Prof. Jeff Kenney Class 11 June 11, 2018 midterm exam thurs june 14 morning? evening? fri june 15 morning? evening? sat june 16 morning? afternoon? sun june 17 morning? afternoon? observing session tomorrow

More information

Using Globular Clusters to. Study Elliptical Galaxies. The View Isn t Bad... Omega Centauri. Terry Bridges Australian Gemini Office M13

Using Globular Clusters to. Study Elliptical Galaxies. The View Isn t Bad... Omega Centauri. Terry Bridges Australian Gemini Office M13 Using Globular Clusters to Omega Centauri Study Elliptical Galaxies Terry Bridges Australian Gemini Office 10,000 1,000,000 stars up to 1000 stars/pc3 typical sizes ~10 parsec Mike Beasley (IAC, Tenerife)

More information

The tidal stirring model and its application to the Sagittarius dwarf

The tidal stirring model and its application to the Sagittarius dwarf The tidal stirring model and its application to the Sagittarius dwarf Ewa L. Łokas Copernicus Center, Warsaw Stelios Kazantzidis (Ohio State) Lucio Mayer (University of Zurich) Collaborators: Steven Majewski

More information

arxiv: v1 [astro-ph.co] 21 Jul 2010

arxiv: v1 [astro-ph.co] 21 Jul 2010 Astron. Nachr. / AN 999, No. 88, 1 7 (2010) / DOI please set DOI! Schwarzschild modelling of elliptical galaxies and their black holes Jens Thomas 1,2, 1 Universitäts-Sternwarte München, Scheinerstr. 1,

More information

Major Review: A very dense article" Dawes Review 4: Spiral Structures in Disc Galaxies; C. Dobbs and J Baba arxiv "

Major Review: A very dense article Dawes Review 4: Spiral Structures in Disc Galaxies; C. Dobbs and J Baba arxiv The Components of a Spiral Galaxy-a Bit of a Review- See MBW chap 11! we have discussed this in the context of the Milky Way" Disks:" Rotationally supported, lots of gas, dust, star formation occurs in

More information

For β = 0, we have from our previous equations: d ln ν d ln r + d ln v2 r

For β = 0, we have from our previous equations: d ln ν d ln r + d ln v2 r Isotropic models Now simplify the equation, and assume β = 0, or isotropic velocity dispersions - i.e., they are the same in all directions. Below we show how the observed light distribution and observed

More information

Everything in baryons?

Everything 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 information

Phenomenological studies in dark matter direct detection: from the impact of the escape speed estimates to tests of halo models

Phenomenological studies in dark matter direct detection: from the impact of the escape speed estimates to tests of halo models Phenomenological studies in dark matter direct detection: from the impact of the escape speed estimates to tests of halo models Stefano Magni Laboratoire Univers et Particules de Montpellier (Université

More information

Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye

Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye Our Galaxy Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust Held together by gravity! The Milky Way with the Naked Eye We get a special view of our own galaxy because we are part of it!

More information

The kinematics of the extreme outer halo of. M87 as revealed by Planetary Nebulae. A.Longobardi M.Arnaboldi O.Gerhard. Garching 2015, 26th Feb.

The kinematics of the extreme outer halo of. M87 as revealed by Planetary Nebulae. A.Longobardi M.Arnaboldi O.Gerhard. Garching 2015, 26th Feb. The kinematics of the extreme outer halo of A. M.Arnaboldi O.Gerhard Max-Planck-Institut für extraterrestrische Physik Garching 2015, 26th Feb. Outer regions of galaxies and structure formation Formation

More information

Galaxies & Introduction to Cosmology

Galaxies & Introduction to Cosmology Galaxies & Introduction to Cosmology Other Galaxies: How many are there? Hubble Deep Field Project 100 hour exposures over 10 days Covered an area of the sky about 1/100 the size of the full moon Probably

More information

12.1 Elliptical Galaxies

12.1 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 information

Chapter 15 The Milky Way Galaxy. The Milky Way

Chapter 15 The Milky Way Galaxy. The Milky Way Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our

More information

Polar Ring Galaxies FINDING THE DARK HALO SHAPE BY CAROLINE VAN BORM

Polar Ring Galaxies FINDING THE DARK HALO SHAPE BY CAROLINE VAN BORM Polar Ring Galaxies FINDING THE DARK HALO SHAPE BY CAROLINE VAN BORM Papers (1) Polar ring galaxies and the Tully-Fisher relation: Implications for the dark halo shape Iodice, E.; Arnaboldi, M.; Bournaud,

More information

Dark Matter Halos of Spiral Galaxies

Dark Matter Halos of Spiral Galaxies Dark Matter Halos of Spiral Galaxies Arunima Banerjee National Centre for Radio Astrophysics Tata Institute of Fundamental Research Pune, India email: arunima@ncra.tifr.res.in Web: http://www.ncra.tifr.res.in/~arunima

More information

Structure and Mass Distribution of the Milky Way Bulge and Disk

Structure and Mass Distribution of the Milky Way Bulge and Disk Galaxy Disks and Disk Galaxies ASP Conference Series, Vol. 3 10 8, 2000 J.G. Funes, S.J., and E.M. Corsini, eds. Structure and Mass Distribution of the Milky Way Bulge and Disk Ortwin Gerhard Astronomisches

More information

The physical origin of stellar envelopes around globular clusters

The 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 information

Components of Galaxies: Dark Matter

Components of Galaxies: Dark Matter Components of Galaxies: Dark Matter Dark Matter: Any Form of matter whose existence is inferred solely through its gravitational effects. -B&T, pg 590 Nature of Major Component of Universe Galaxy Formation

More information

Galaxy dynamics with the Planetary Nebula Spectrograph

Galaxy dynamics with the Planetary Nebula Spectrograph Mem. S.A.It. Suppl. Vol. 5, 255 c SAIt 2004 Memorie della Supplementi Galaxy dynamics with the Planetary Nebula Spectrograph N.R. Napolitano 1, A.J. Romanowsky 2, N.G. Douglas 1, M. Capaccioli 3, M. Arnaboldi

More information

Black Hole Mergers at Galactic. The Final Parsec: Supermassive. Centers. Milos Milosavljevic. California Institute of Technology

Black Hole Mergers at Galactic. The Final Parsec: Supermassive. Centers. Milos Milosavljevic. California Institute of Technology The Final Parsec: Supermassive Black Hole Mergers at Galactic Centers Milos Milosavljevic California Institute of Technology MBH Binaries Form in Galaxy Mergers Borne et al 2000 by transferring binding

More information

Dynamics of the Milky Way

Dynamics of the Milky Way Dynamics of the Milky Way Part 1: Part 2: Part 3: Part 4: I. Introduction Formation of Disk Galaxies II. Fundamentals of Stellar Dynamics Stellar Orbits and Jeans Theorem The Galactic Bulge and Bar The

More information

Dark Matter: Observational Constraints

Dark Matter: Observational Constraints Dark Matter: Observational Constraints Properties of Dark Matter: What is it? And what isn t it? Leo Blitz UC Berkeley Stanford July 31, 2007 How much is there? WMAP results Rotation curves of Galaxies

More information

Galaxy Evolution Workshop Austin, TX, Nov 2008

Galaxy Evolution Workshop Austin, TX, Nov 2008 Galaxy Evolution Workshop Austin, TX, Nov 2008 LCDM is a well-specified theory which makes definite predictions about the way structures in the Universe form and evolve. most (all?) of the mass of the

More information

The Milky Way Galaxy

The Milky Way Galaxy 1/5/011 The Milky Way Galaxy Distribution of Globular Clusters around a Point in Sagittarius About 00 globular clusters are distributed in random directions around the center of our galaxy. 1 1/5/011 Structure

More information

Global Scaling Relations of Spiral Galaxies

Global 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 information

Summary So Far! M87van der Maerl! NGC4342! van den Bosch! rotation velocity!

Summary So Far! M87van der Maerl! NGC4342! van den Bosch! rotation velocity! Summary So Far Fundamental plane connects luminosity, scale length, surface brightness, stellar dynamics. age and chemical composition Elliptical galaxies are not randomly distributed within the 3D space

More information

arxiv: v1 [astro-ph] 12 Feb 2008

arxiv: v1 [astro-ph] 12 Feb 2008 Mon. Not. R. Astron. Soc. 000, 1 19 ( -) Printed 14 February 2008 (MN LATEX style file v2.2) Dark matter content and internal dynamics of NGC 4697: NMAGIC particle models from slit data and planetary nebulae

More information

Dwarf Galaxies as Cosmological Probes

Dwarf Galaxies as Cosmological Probes Dwarf Galaxies as Cosmological Probes Julio F. Navarro The Ursa Minor dwarf spheroidal First Light First Light The Planck Satellite The Cosmological Paradigm The Clustering of Dark Matter The Millennium

More information

Supermassive Black Hole Binaries as Galactic Blenders. Balša Terzić

Supermassive Black Hole Binaries as Galactic Blenders. Balša Terzić Supermassive Black Hole Binaries as Galactic Blenders Balša Terzić University of Florida January 30, 2004 Supermassive Black Hole Binaries as Galactic Blenders Kandrup, Sideris, Terzić & Bohn, 2003, ApJ,

More information

Theoretical ideas About Galaxy Wide Star Formation! Star Formation Efficiency!

Theoretical ideas About Galaxy Wide Star Formation! Star Formation Efficiency! Theoretical ideas About Galaxy Wide Star Formation Theoretical predictions are that galaxy formation is most efficient near a mass of 10 12 M based on analyses of supernova feedback and gas cooling times

More information

The Milky Way and Near-Field Cosmology

The Milky Way and Near-Field Cosmology The Milky Way and Near-Field Cosmology Kathryn V Johnston (Columbia University) Collaborators (theorists): James S Bullock (Irvine), Andreea Font (Durham), Brant Robertson (Chicago), Sanjib Sharma (Columbia),

More information

A new mechanism for the formation of PRGs

A new mechanism for the formation of PRGs A new mechanism for the formation of PRGs Spavone Marilena (INAF-OAC) Iodice Enrica (INAF-OAC), Arnaboldi Magda (ESO-Garching), Longo Giuseppe (Università Federico II ), Gerhard Ortwin (MPE-Garching).

More information

Normal Galaxies ASTR 2120 Sarazin

Normal Galaxies ASTR 2120 Sarazin Normal Galaxies ASTR 2120 Sarazin Test #2 Monday, April 8, 11-11:50 am ASTR 265 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other materials or any person

More information

Spiral Structure. m ( Ω Ω gp ) = n κ. Closed orbits in non-inertial frames can explain the spiral pattern

Spiral Structure. m ( Ω Ω gp ) = n κ. Closed orbits in non-inertial frames can explain the spiral pattern Spiral Structure In the mid-1960s Lin and Shu proposed that the spiral structure is caused by long-lived quasistatic density waves The density would be higher by about 10% to 20% Stars, dust and gas clouds

More information

Galaxies. CESAR s Booklet

Galaxies. CESAR s Booklet What is a galaxy? Figure 1: A typical galaxy: our Milky Way (artist s impression). (Credit: NASA) A galaxy is a huge collection of stars and interstellar matter isolated in space and bound together by

More information

3 The lives of galaxies

3 The lives of galaxies Discovering Astronomy : Galaxies and Cosmology 24 3 The lives of galaxies In this section, we look at how galaxies formed and evolved, and likewise how the large scale pattern of galaxies formed. But before

More information

Visible Matter. References: Ryden, Introduction to Cosmology - Par. 8.1 Liddle, Introduction to Modern Cosmology - Par. 9.1

Visible 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 information

Galaxy Formation and Evolution

Galaxy Formation and Evolution Galaxy Formation and Evolution Houjun Mo Department of Astronomy, University of Massachusetts 710 North Pleasant Str., Amherst, MA 01003-9305, USA Frank van den Bosch Department of Physics & Astronomy,

More information

Three Major Components

Three Major Components The Milky Way Three Major Components Bulge young and old stars Disk young stars located in spiral arms Halo oldest stars and globular clusters Components are chemically, kinematically, and spatially distinct

More information

Dark Matter in Disk Galaxies

Dark Matter in Disk Galaxies Chapter 14 Dark Matter in Disk Galaxies Rotation curves of disk galaxies rise steeply in their inner regions and then remain roughly flat out to the last point measured. To explain these observations within

More information

Galaxy Dynamics Galaxies Block Course 2008 Hans-Walter Rix - MPIA

Galaxy Dynamics Galaxies Block Course 2008 Hans-Walter Rix - MPIA Galaxy Dynamics Galaxies Block Course 2008 Hans-Walter Rix - MPIA For more detail on any of this Binney and Tremaine, 1996 Binney and Merrifield, 2002 1 Basic Goals of Stellar Dynamics Most Empirical:

More information

Probing Galaxy Halos with Tidal Interactions. Kyoto University Astronomy Department June 27, 2013

Probing Galaxy Halos with Tidal Interactions. Kyoto University Astronomy Department June 27, 2013 Probing Galaxy Halos with Tidal Interactions Kyoto University Astronomy Department June 27, 2013 Galaxy Formation Baryons cool & collapse in dark halo potentials. White & Rees 78 Galaxy Formation Baryons

More information

Galaxies. The majority of known galaxies fall into one of three major classes: spirals (78 %), ellipticals (18 %) and irregulars (4 %).

Galaxies. The majority of known galaxies fall into one of three major classes: spirals (78 %), ellipticals (18 %) and irregulars (4 %). Galaxies Collection of stars, gas and dust bound together by their common gravitational pull. Galaxies range from 10,000 to 200,000 light-years in size. 1781 Charles Messier 1923 Edwin Hubble The distribution

More information

arxiv:astro-ph/ v3 2 Jun 2008

arxiv:astro-ph/ v3 2 Jun 2008 Mon. Not. R. Astron. Soc. 000, 1 15 (2008) Printed 2 June 2008 (MN LATEX style file v2.2) Phase models of the Milky Way stellar disc S.A. Rodionov and V.V. Orlov Sobolev Astronomical Institute, St. Petersburg

More information

Scaling Relations of late-type galaxies

Scaling 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 information

ASTR 610 Theory of Galaxy Formation Lecture 18: Disk Galaxies

ASTR 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 information

The Formation and Evolution of Galaxy Clusters

The Formation and Evolution of Galaxy Clusters IAU Joint Discussion # 10 Sydney, July, 2003 The Formation and Evolution of Galaxy Clusters Simon D.M. White Max Planck Institute for Astrophysics The WMAP of the whole CMB sky Bennett et al 2003 > 105

More information

A M BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY. WALSH et al Akiyama Group M1 Genki Suzuki

A M BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY. WALSH et al Akiyama Group M1 Genki Suzuki A 5 10 9 M BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY WALSH et al. 2015 Akiyama Group M1 Genki Suzuki Introduction NGC 1277 is thought to harbor one of the most massive black holes in the

More information

Milky Way S&G Ch 2. Milky Way in near 1 IR H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/

Milky Way S&G Ch 2. Milky Way in near 1 IR   H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/ Why study the MW? its "easy" to study: big, bright, close Allows detailed studies of stellar kinematics, stellar evolution. star formation, direct detection of dark matter?? Milky Way S&G Ch 2 Problems

More information

BROCK UNIVERSITY. Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015

BROCK UNIVERSITY. Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015 BROCK UNIVERSITY Page 1 of 9 Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015 Number of hours: 50 min Time of Examination: 18:00 18:50

More information

Other Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies

Other Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at

More information

ASTRO 310: Galactic & Extragalactic Astronomy Prof. Jeff Kenney

ASTRO 310: Galactic & Extragalactic Astronomy Prof. Jeff Kenney ASTRO 310: Galactic & Extragalactic Astronomy Prof. Jeff Kenney Class 3 January 23, 2017 The Milky Way Galaxy: Vertical Distributions of Stars & the Stellar Disk disks exist in many astrophysical systems

More information

The motions of stars in the Galaxy

The motions of stars in the Galaxy The motions of stars in the Galaxy The stars in the Galaxy define various components, that do not only differ in their spatial distribution but also in their kinematics. The dominant motion of stars (and

More information

A tool to test galaxy formation arxiv: Joe Wolf (UC Irvine)

A tool to test galaxy formation arxiv: Joe Wolf (UC Irvine) A tool to test galaxy formation arxiv: 0908.2995 Joe Wolf (UC Irvine) Hunting for the Dark: The Hidden Side of Galaxy Formation Malta October 22 nd, 2009 Team Irvine: Greg Martinez James Bullock Manoj

More information

Supermassive Black Holes

Supermassive Black Holes Supermassive Black Holes Leiden, Modern Research: Galaxy Formation and Evolution Tom van Leth & Maarten van Dijk November 25, 2005 1 Introduction Introduction Black hole theory Characteristics of SMBH

More information

1.4 Galaxy Light Distributions

1.4 Galaxy Light Distributions 26 1.4 Galaxy Light Distributions List of topics Hubble classification scheme see Binney & Merrifield text Galaxy surface brightness profiles (JL 2.3.1, plus additional material) Galaxy luminosity function

More information

I. Basic Goals. Most galaxies are in approx. equilibrium in the present-day universe.

I. Basic Goals. Most galaxies are in approx. equilibrium in the present-day universe. Elements of Galaxy Dynamics I. Basic Goals Most galaxies are in approx. equilibrium in the present-day universe. What equilibrium i solutions exist and which h are stable? A solution entails: in which

More information

Ellipticals. Ellipticals. Huge mass range:

Ellipticals. Ellipticals. Huge mass range: Ellipticals Huge mass range: Dwarf spheroidal (Leo I) Dwarf spheroidals: 1 7-1 8 M Blue compact dwarfs: ~1 9 M Dwarf ellipticals: 1 7-1 9 M Normal (giant) ellipticals: 1 8-1 13 M cd galaxies in cluster

More information

Spatial distribution of stars in the Milky Way

Spatial distribution of stars in the Milky Way Spatial distribution of stars in the Milky Way What kinds of stars are present in the Solar neighborhood, and in what numbers? How are they distributed spatially? How do we know? How can we measure this?

More information

Galaxy Formation: Overview

Galaxy Formation: Overview Galaxy Formation: Overview Houjun Mo March 30, 2004 The basic picture Formation of dark matter halos. Gas cooling in dark matter halos Star formation in cold gas Evolution of the stellar populaion Metal

More information

The Los Cabos Lectures

The Los Cabos Lectures January 2009 The Los Cabos Lectures Dark Matter Halos: 3 Simon White Max Planck Institute for Astrophysics Shapes of halo equidensity surfaces Group Jing & Suto 2002 Galaxy δ 100 2500 6250 Shapes of halo

More information

5.1 Circular Velocities and Rotation Curves

5.1 Circular Velocities and Rotation Curves Chapter 5 otation Curves 5.1 Circular Velocities and otation Curves The circular velocity v circ is the velocity that a star in a galaxy must have to maintain a circular orbit at a specified distance from

More information

distribution of mass! The rotation curve of the Galaxy ! Stellar relaxation time! Virial theorem! Differential rotation of the stars in the disk

distribution of mass! The rotation curve of the Galaxy ! Stellar relaxation time! Virial theorem! Differential rotation of the stars in the disk Today in Astronomy 142:! The local standard of rest the Milky Way, continued! Rotation curves and the! Stellar relaxation time! Virial theorem! Differential rotation of the stars in the disk distribution

More information

The Los Cabos Lectures

The Los Cabos Lectures January 2009 The Los Cabos Lectures Dark Matter Halos: 2 Simon White Max Planck Institute for Astrophysics EPS statistics for the standard ΛCDM cosmology Millennium Simulation cosmology: Ωm = 0.25, ΩΛ

More information

arxiv:astro-ph/ v1 17 Feb 2007

arxiv:astro-ph/ v1 17 Feb 2007 Mon. Not. R. Astron. Soc. 000, 1 16 (2006) Printed 17 June 2008 (MN LATEX style file v2.2) Phase Models of the Milky Way Stellar Disk S.A. Rodionov and V.V. Orlov Sobolev Astronomical Institute, St. Petersburg

More information

Astronomy 114. Lecture 29: Internal Properties of Galaxies. Martin D. Weinberg. UMass/Astronomy Department

Astronomy 114. Lecture 29: Internal Properties of Galaxies. Martin D. Weinberg. UMass/Astronomy Department Astronomy 114 Lecture 29: Internal Properties of Galaxies Martin D. Weinberg weinberg@astro.umass.edu UMass/Astronomy Department A114: Lecture 29 20 Apr 2007 Read: Ch. 26 Astronomy 114 1/16 Announcements

More information