Joint mass and anisotropy modeling of the. Fornax Dwarf Spheroidal
|
|
- Hester Perkins
- 5 years ago
- Views:
Transcription
1 Joint mass and anisotropy modeling of the Fornax Dwarf Spheroidal Fornax Dwarf Spheroidal with Chris GORDON (Oxford) Andrea BIVIANO (Trieste) DSS 1
2 Motivations Large velocity data sets in Dwarf Spheroidals Walker et al member velocities in Fornax! constraints on Dark Matter normalization constraints on Dark Matter inner slope constraints on velocity anisotropy of stars 2
3 Mass anisotropy degeneracy Spherical stationary Jeans equation anisotropic dynamical pressure tracer density d ( ) νσr 2 dr +2 β(r) r β(r) = 1 σ2 θ (r) σ 2 r(r) νσ 2 r = ν GM(r) r 2 = velocity anisotropy isotropic orbits: β = 0 radial orbits: β = 1 circular orbits: β Mass / Anisotropy Degeneracy MAD 3
4 Exploratory Mass-Anisotropy Modeling 1) Model-fitting of Line-of-Sight velocity dispersion profile Mtot(r) + β(r) σlos(r) 4
5 1) assume both M(r) & β(r) & fit the LOS velocity dispersions for β = 0 line-of-sight velocity dispersion Tremaine et al. 94; Prugniel & Simien 97 R Σ(R) σ 2 los (R) = 2G R r 2 R 2 r 2 ν(r)m(r)dr tracer surface density kernels for other simple β(r) Mamon & Łokas 05b 5
6 Exploratory Mass-Anisotropy Modeling 1) Model-fitting of Line-of-Sight velocity dispersion profile Mtot(r) + β(r) σlos(r) 2) Anisotropy inversion { Σ(R) + Mtot(r) β(r) σlos(r) Binney & Mamon 82 Tonry 83; Bicknell et al. 89 Solanes & Salvador-Solé 90 Dejonghe & Merritt 92 6
7 Exploratory Mass-Anisotropy Modeling 1) Model-fitting of Line-of-Sight velocity dispersion profile Mtot(r) + β(r) σlos(r) 2) Anisotropy inversion { Σ(R) + Mtot(r) β(r) σlos(r) 3) Mass inversion { Σ(R) σlos(r) + β(r) Mtot(r) Mamon & Boué 10 Wolf et al. 10 7
8 3) Mass inversion Mamon & Boué 10; Wolf et al. 10 Kinematic deprojection & mass inversion of spherical systems with known anisotropy anisotropic kinematic projection p = ρ σ r2 = dynamical pressure P(R) = 2 R 1 β R2 r 2 p r dr r 2 R 2 P = Σ σ los2 = projected pressure deprojection MB10: simple β(r) (1 β) p = = r r K[β(s)] s dp dr L β (R, r) dp dr dr R dr R2 r 2 insert dynamical pressure into Jeans equation mass profile simple β(r): single integral! vc 2 1 { R d 2 P (r) = π [1 β(r)] ρ(r) R2 r 2 dr 2 C β(r, r) dp } dr r 8 dr
9 Radius where mass is independent of anisotropy Wolf et al. 10 Sérsic (or similar): at r -3 r1/2 Mamon & Boué 10 NFW: at 7 rs or 3 rs 9
10 Exploratory Mass-Anisotropy Modeling 1) Model-fitting of Line-of-Sight velocity dispersion profile Mtot(r) + β(r) σlos(r) 2) Anisotropy inversion { Σ(R) + Mtot(r) β(r) σlos(r) 3) Mass inversion { Σ(R) σlos(r) + β(r) Mtot(r) 4) Fitting stars in Projected Phase Space MAMPOSSt Mamon, Biviano & Boué 11, to be subm ν(r) + M tot (r) + β(r) + {v}(r) g(r,vlos) 10
11 Other popular modeling methods gaussian {vlos(r)} lose info on β ν(r) + M tot (r) + β[r] + {vlos}(r) g(r,vlos) dispersion-kurtosis Łokas 02; see Łokas, Mamon & Prada 05 Mtot(r) + β σlos(r) + κlos(r) must assume β = cst distribution function modeling Dejonghe & Merritt 92; Merritt & Saha 93 M tot (r) + f(e,j) or {fi(e,j)} g(r,vlos) don t know f(e,j); not sure that {fi(e,j)} = basis set orbit modeling Schwarzschild 79; de Lorenzi et al. 09 M tot (r) + {orbits} g(r,vlos) too slow for MCMC investigation of parameter space 11
12 Mass modeling of the Fornax dwarf spheroidal 12
13 LV = 1.9 x 10 7 Lsun Irwin & Hatzimiditriou 95 LV = 0.9 x 10 7 Lsun Walcher et al. 03 Fornax data Fornax metallicity 2633 velocities 2278 Fornax members Milky Way metallicity 2 Re m = 0.7 Sersic distribution Walcher et al. 03; Battaglia et al. 06 ellipticity: Battaglia et al. 06 main starburst: age = 5.4 Gyr Saviane et al. 00 Mstars/LV = 4.8 Walcher et al. 03 (uncertain) center: Battaglia et al. 06 data & MW flags: Walker et al. 09 Magellan/MMFS rejected outlier 13
14 Fornax: velocity dispersion profile out to 2 Reff Łokas 09 isotropic, M/LV = 7.3 order 2 fit M/LV = 8.8 isotropic, M/LV = 4.8 isotropic, M/LV = 4.8, low LV order 3 fit Reff order 4 fit 1/3 fraction of dark matter in inner regions? OR LV underestimated by 40%? M/L increases outwards? OR tangential outer orbits? 14
15 Fornax: anisotropy inversion INPUT stars radial OUTPUT isotropic moderately tangential cst M/L radial (low M/L) or tangential (high M/L) orbits 15
16 Fornax: isotropic mass inversion stars dark matter, even in inner regions? luminosity and/or Mstars/L too low? fit order 4 σ los (R) falls too fast! stars stars radial outer orbits! 16
17 low LV log total mass (1.5kpc)( M ) std LV max stars 1σ 2σ 3σ 4σ low LV (P=0.95 MAMPOSSt with MCMC well-defined Mtot(2Re) gaussian 3D velocities cst β cst Mstars/L Kazantzidis DM: ρ ~ exp(-r/a) / r MCMC: 9 chains of log DM scale radius (kpc) a > 2 kpc (95% conf.) anisotropy: -0.5 log(1-β) Isotropic orbits! β = -0.03±
18 log total mass (1.5kpc)( M ) std LV low LV max stars 1σ 2σ 3σ 4σ std LV Free inner dark matter slope... gaussian 3D velocities cst β cst Mstars/L gen l Kazantzidis DM: ρ ~ r γ exp(-r/a) MCMC: 11 chains of log DM scale radius (kpc) anisotropy: -0.5 log(1-β) inner DM slope inner DM slope: not too steep! 18
19 log total mass (1.5kpc)( M ) 1σ 2σ 3σ 4σ Increasing anisotropy... gaussian 3D velocities β=r 2 /(r 2 +a 2 ) Osipkov-Merritt cst Mstars/L gen l Kazantzidis DM: ρ ~ r γ exp(-r/a) MCMC: 11 chains of log DM scale radius (kpc) anisotropy: -0.5 log(1-β) inner DM slope anisotropy radius: 1.6 < ranis < 25 kpc (1σ) 19
20 Radial variations Wolf+10 mass pinch stars P=95% DM total P=98% appreciable velocity anisotropy at 2 Re but β=0 is consistent w data 20
21 Comparison with previous work Łokas 09 this work Walker+09 Walker et al. 09 Łokas 09 anisotropy poorly constrained: < β < β < σ limits vs < β < 0.13 inner slope not constrained γ < -0.3 vs. γ >
22 Conclusions Mass modelling = exploratory data analysis: try methods: mass & β inversions, & MAMPOSSt Fornax MAMPOSSt stronger constraints Isotropic inner orbits, radial outer orbits Dark matter present: likely > 50% at all radii seen in simulations: Klimentowski+07; Lokas+10 Dark matter inner slope shallower than -1.1 see Pennarubia for tidal effects on GCs 22
23 Perspectives MAMPOSSt with non-gaussian 3D velocity distributions model rotation & metallicity effects Battaglia+06 in Fornax higher-parameter MCMC fits 23
MAMPOSSt modeling of true & mock dwarf spheroidal galaxies
MAMPOSSt modeling of true & mock dwarf spheroidal galaxies Gary Mamon (IAP), 30 Oct 2014, GAIA Challenge in Heidelberg, MAMPOSSt modeling of true & mock dwarf spheroidals 1 Motivations Mass profiles of
More informationMass modelling of dwarf spheroidals. Jorge Peñarrubia
Mass modelling of dwarf spheroidals Jorge Peñarrubia Santiago de Chile 13 April 2015 Universe Composition Assumption: GR is correct WMAP7 DM particle models: Constraints 63 orders 51 orders DM particle
More informationThe 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 informationCluster density profiles and orbits of galaxies from dynamical analysis. Andrea Biviano, INAF/Oss.Astr.Trieste
Cluster density profiles and orbits of galaxies from dynamical analysis Andrea Biviano, INAF/Oss.Astr.Trieste Collaborators & papers: on the observational side: A.B. & M. Girardi 2003, P. Katgert, A.B.
More informationMilky 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 informationConnecting observations to simulations arxiv: Joe Wolf (UC Irvine)
Connecting observations to simulations arxiv: 0908.2995 Joe Wolf (UC Irvine) University of Maryland December 8 th, 2009 Team Irvine: Greg Martinez James Bullock Manoj Kaplinghat Erik Tollerud Quinn Minor
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 informationMASS PROFILES OF GALAXY CLUSTERS from dynamics. Andrea Biviano INAF - Trieste
MASS PROFILES OF GALAXY CLUSTERS from dynamics Andrea Biviano INAF - Trieste MASS PROFILES OF GALAXY CLUSTERS from dynamics Meaning: from the study of the projected phase-space distribution of cluster
More informationOverview 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 informationKinematic, lensing & X-ray mass estimates of a poor cluster
Kinematic, lensing & X-ray mass estimates of a poor cluster A. Biviano (Trieste, I) + P. Popesso, J.P.Dietrich, Y.-Y. Zhang, G. Erfanianfar, M. Romaniello, B. Sartoris Introduction Bower+97: optically
More informationarxiv: v6 [astro-ph.co] 21 Sep 2010
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 9 May 018 (MN LATEX style file v.) Accurate masses for dispersion-supported galaxies arxiv:0908.995v6 [astro-ph.co] 1 Sep 010 Joe Wolf 1, Gregory D.
More informationConnecting observations to simulations arxiv: Joe Wolf (UC Irvine)
Connecting observations to simulations arxiv: 0908.2995 Joe Wolf (UC Irvine) September, 2009 Team Irvine: Greg Martinez James Bullock Manoj Kaplinghat Erik Tollerud Quinn Minor Team Irvine: Greg Martinez
More informationMade-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 informationA 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 informationSummary 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 informationDynamical 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 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 informationA tool to test galaxy formation theories. Joe Wolf (UC Irvine)
A tool to test galaxy formation theories Joe Wolf (UC Irvine) SF09 Cosmology Summer Workshop July 7 2009 Team Irvine: Greg Martinez James Bullock Manoj Kaplinghat Frank Avedo KIPAC: Louie Strigari Haverford:
More informationarxiv: v1 [astro-ph] 31 Jul 2007
Mon. Not. R. Astron. Soc. 000, 1?? (1994) Printed 1 February 8 (MN LATEX style file v1.4) Origin of lower velocity dispersions of ultra-compact dwarf galaxy populations in clusters of galaxies K. Bekki
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 informationMilky Way s Anisotropy Profile with LAMOST/SDSS and Gaia
Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia Shanghai Astronomical Observatory In collaboration with Juntai Shen, Xiang Xiang Xue, Chao Liu, Chris Flynn, Chengqun Yang Contents 1 Stellar Halo
More informationGalaxy evolution in clusters from the CLASH-VLT survey
Galaxy evolution in clusters from the CLASH-VLT survey Andrea Biviano INAF-Osservatorio Astronomico di Trieste (on behalf of the CLASH-VLT team) (part of) The CLASH-VLT team M. Nonino, co-i I. Balestra
More informationThe Milky Way Part 3 Stellar kinematics. Physics of Galaxies 2011 part 8
The Milky Way Part 3 Stellar kinematics Physics of Galaxies 2011 part 8 1 Stellar motions in the MW disk Let s continue with the rotation of the Galaxy, this time from the point of view of the stars First,
More informationDark matter annihilation and decay factors in the Milky Way s dwarf spheroidal galaxies
Dark matter annihilation and decay factors in the Milky Way s dwarf spheroidal galaxies Vincent Bonnivard bonnivard@lpsc.in2p3.fr TAUP 2015 07/09/15 Collaborators: D. Maurin, C. Combet, M. G. Walker, A.
More informationThe 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 informationThe Milky Way Part 2 Stellar kinematics. Physics of Galaxies 2012 part 7
The Milky Way Part 2 Stellar kinematics Physics of Galaxies 2012 part 7 1 Stellar motions in the MW disk Let s look at the rotation of the Galactic disk First, we need to introduce the concept of the Local
More informationMasses of Dwarf Satellites of the Milky Way
Masses of Dwarf Satellites of the Milky Way Manoj Kaplinghat Center for Cosmology UC Irvine Collaborators: Greg Martinez Quinn Minor Joe Wolf James Bullock Evan Kirby Marla Geha Josh Simon Louie Strigari
More informationStructure and substructure in dark matter halos
Satellites and Tidal Streams ING IAC joint Conference La Palma, May 2003 Structure and substructure in dark matter halos Simon D.M. White Max Planck Institute for Astrophysics 500 kpc A CDM Milky Way Does
More informationThe 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 informationDynamics of Galaxies: Practice. Frontiers in Numerical Gravitational Astrophysics July 3, 2008
Dynamics of Galaxies: Practice Frontiers in Numerical Gravitational Astrophysics July 3, 2008 http://xkcd.com/323/ Outline 1. Initial Conditions a) Jeans Theorem b) Exact solutions for spheres c) Approximations
More informationCoordinate Systems! The geometry of the stream requires an oblate near-spherical halo!
Milky Way Galaxy (blue/ white points and orange bulge) with the Sun (yellow sphere), inner and outer Sgr stream models (yellow/red points respectively), Monoceros tidal stream model(violet points), and
More informationFor 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 informationBayesian Mass Estimates of the Milky Way: incorporating incomplete data
Bayesian Mass Estimates of the Milky Way: incorporating incomplete data Gwendolyn Eadie, PhD Candidate Dr. William Harris (McMaster), Dr. Lawrence Widrow (Queen's) AstroStat Seminar - March 23, 2015 Measuring
More informationThe Caustic Technique An overview
The An overview Ana Laura Serra Torino, July 30, 2010 Why the mass of? Small scales assumption of dynamical equilibrium Mass distribution on intermediate scales (1 10 Mpc/h) Large scales small over densities
More informationThe Distribution Function
The Distribution Function As we have seen before the distribution function (or phase-space density) f( x, v, t) d 3 x d 3 v gives a full description of the state of any collisionless system. Here f( x,
More information4. Structure of Dark Matter halos. Hence the halo mass, virial radius, and virial velocity are related by
6-4-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c04-1 6-4-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c04-2 4. Structure of Dark Matter halos Obviously, we cannot
More informationAstronomy 330 Lecture 7 24 Sep 2010
Astronomy 330 Lecture 7 24 Sep 2010 Outline Review Counts: A(m), Euclidean slope, Olbers paradox Stellar Luminosity Function: Φ(M,S) Structure of the Milky Way: disk, bulge, halo Milky Way kinematics Rotation
More informationDark Matter Dominated Objects. Louie Strigari Stanford
Dark Matter Dominated Objects Louie Strigari Stanford Milky Way Circa 2009 Satellite Year Discovered LMC 1519 SMC 1519 Sculptor 1937 Fornax 1938 Leo II 1950 Leo I 1950 Ursa Minor 1954 Draco 1954 Carina
More informationCollisionless Boltzmann Eq (Vlasov eq)" S+G sec 3.4! Collisionless Boltzmann Eq S&G 3.4!
Collisionless Boltzmann Eq (Vlasov eq)" S+G sec 3.4 When considering the structure of galaxies cannot follow each individual star (10 11 of them), Consider instead stellar density and velocity distributions.
More informationFabrizio Nesti. LNGS, July 5 th w/ C.F. Martins, G. Gentile, P. Salucci. Università dell Aquila, Italy. The Dark Matter density. F.
Global The Dark Matter Fabrizio Nesti Università dell Aquila, Italy LNGS, July 5 th 2012 w/ C.F. Martins, G. Gentile, P. Salucci Global Dark Matter? A number of indirect supporting evidences Modify Gravity
More informationUMa II and the Orphan Stream
UMa II and the Orphan Stream M. Fellhauer The Cambridge Mafia Field of Streams Belokurov et al. 2006 A short The Bifurcation of the Sagittarius stream: (a typical Sagittarius like simulation) Fellhauer
More informationConstraining self-interacting dark matter with scaling laws of observed halo surface densities
Constraining self-interacting dark matter with scaling laws of observed halo surface densities Anastasia Sokolenko, T.Bringmann (University of Oslo) K.Bondarenko and A.Boyarsky (Leiden University) Rencontres
More informationDark Matter Halos of M31. Joe Wolf
Dark Matter Halos of M31 Galaxies Joe Wolf TASC October 24 th, 2008 Dark Matter Halos of M31 Galaxies Joe Wolf Team Irvine: Louie Strigari, James Bullock, Manoj Kaplinghat TASC October 24 th, 2008 Dark
More informationThe distribution and kinematics of early high-σ peaks in present-day haloes: implications for rare objects and old stellar populations
Mon. Not. R. Astron. Soc. 000, 1 19 (2005) Printed 20 April 2006 (MN LATEX style file v2.2) The distribution and kinematics of early high-σ peaks in present-day haloes: implications for rare objects and
More information4. Structure of Dark Matter halos. Hence the halo mass, virial radius, and virial velocity are related by
13-4-12see http://www.strw.leidenuniv.nl/ franx/college/galaxies12 12-c04-1 13-4-12see http://www.strw.leidenuniv.nl/ franx/college/galaxies12 12-c04-2 4. Structure of Dark Matter halos Obviously, we cannot
More informationFirenze (JPO: 28/07/17) Small Scale Crisis for CDM: Fatal or a Baryon Physics Fix
Firenze (JPO: 28/07/17) Small Scale Crisis for CDM: Fatal or a Baryon Physics Fix CBR Spectrum Planck and all-a Perfect Fit to the CDM Expectation Precise measurements of the CBR specify the cosmological
More informationNMAGIC 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 informationA novel JEAnS analysis of the Fornax dwarf using evolutionary algorithms: mass follows light with signs of an off-centre merger
Advance Access publication 2017 May 20 doi:10.1093/mnras/stx1219 A novel JEAnS analysis of the Fornax dwarf using evolutionary algorithms: mass follows light with signs of an off-centre merger Foivos I.
More informationStructure formation in the concordance cosmology
Structure formation in the Universe, Chamonix, May 2007 Structure formation in the concordance cosmology Simon White Max Planck Institute for Astrophysics WMAP3 team WMAP3 team WMAP3 team WMAP3 team In
More informationSUPPLEMENTARY INFORMATION
doi:10.1038/nature10445 Measuring gravitational redshift of galaxies in clusters The gravitational potential depth in typical galaxy clusters, expressed in terms of the velocity shift, is estimated at
More informationStellar 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 informationWhat are the best constraints on theories from galaxy dynamics?
What are the best constraints on theories from galaxy dynamics? TDG in MOND DM MOND Françoise Combes Observatoire de Paris Tuesday 29 June 2010 O.Tiret Still most baryons are unidentified 6% in galaxies
More informationOverview spherical accretion
Spherical accretion - AGN generates energy by accretion, i.e., capture of ambient matter in gravitational potential of black hole -Potential energy can be released as radiation, and (some of) this can
More informationStellar 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 informationProbing Gravity in the Low Acceleration Regime with Globular Clusters
Probing Gravity in the Low Acceleration Regime with Globular Clusters By Riccardo Scarpa Instituto de astrofisica de Canarias Gran Telescopio Canarias The idea for this study sparked from the desire of
More informationarxiv: v2 [astro-ph.ga] 18 Nov 2016
Mon. Not. R. Astron. Soc. 000,???? (2016) Printed 11 September 2018 (MN LATEX style file v2.2) Tidal features of classical Milky Way satellites in aλcdm universe arxiv:1611.00778v2 [astro-ph.ga] 18 Nov
More informationDistinguishing Between Warm and Cold Dark Matter
Distinguishing Between Warm and Cold Dark Matter Center for Cosmology Aspen Workshop Neutrinos in Physics & Astrophysics 2/2/2007 Collaborators: James Bullock, Manoj Kaplinghat astro-ph/0701581.. Motivations
More informationDA(z) from Strong Lenses. Eiichiro Komatsu, Max-Planck-Institut für Astrophysik Inaugural MIAPP Workshop on Extragalactic Distance Scale May 26, 2014
DA(z) from Strong Lenses Eiichiro Komatsu, Max-Planck-Institut für Astrophysik Inaugural MIAPP Workshop on Extragalactic Distance Scale May 26, 2014 This presentation is based on: Measuring angular diameter
More informationRobust estimate of the dark matter halo of the Milky-way's dwarf spheroidal galaxies
Robust estimate of the dark matter halo of the Milky-way's dwarf spheroidal galaxies Koji Ichikawa arxiv:1701.xxxxx arxiv:1608.01749 (submitted in MNRAS) MNRAS, 461, 2914 (1603.08046 [astroph.ga]) In collaboration
More informationA novel determination of the local dark matter density. Riccardo Catena. Institut für Theoretische Physik, Heidelberg
A novel determination of the local dark matter density Riccardo Catena Institut für Theoretische Physik, Heidelberg 28.04.2010 R. Catena and P. Ullio, arxiv:0907.0018 [astro-ph.co]. Riccardo Catena (ITP)
More informationHubble Space Telescope survey of the Perseus Cluster I. The structure and dark matter content of cluster dwarf spheroidals
Mon. Not. R. Astron. Soc. 393, 1054 1062 (2009) doi:10.1111/j.1365-2966.2008.14269.x Hubble Space Telescope survey of the Perseus Cluster I. The structure and dark matter content of cluster dwarf spheroidals
More informationKinematics of the Solar Neighborhood
Chapter 15 Kinematics of the Solar Neighborhood Unlike an elliptical galaxy, the Milky Way rotates with a speed much larger than the random velocities of typical stars. Our position inside the disk of
More informationarxiv: v1 [astro-ph.ga] 3 Nov 2015
Mon. Not. R. Astron. Soc., 1 14 (15) Printed 1 August 18 (MN LATEX style file v.) Assessing the Jeans Anisotropic Multi-Gaussian Expansion method with the Illustris simulation arxiv:1511.789v1 [astro-ph.ga]
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 informationSurface Brightness of Spiral Galaxies
Surface Brightness of Spiral Galaxies M104: SA N4535: SAB LMC: dwarf irregular,barred Normal 1/4-law+exp fits An example of surface brightness profile. The top curve is the sum of exp disk+1/4-bulge. The
More informationLecture 7: the Local Group and nearby clusters
Lecture 7: the Local Group and nearby clusters in this lecture we move up in scale, to explore typical clusters of galaxies the Local Group is an example of a not very rich cluster interesting topics include:
More informationWhat can M2M do for Milky Way Models?
What can M2M do for Milky Way Models? Ortwin Gerhard Max-Planck-Institut für Extraterrestrische Physik, Garching gerhard@mpe.mpg.de Thanks to F. de Lorenzi, V. Debattista, P. Das, L. Morganti I. Made-to-Measure
More informationAstro 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 informationThe Hernquist model revisited: completely analytical anisotropic dynamical models
The Hernquist model revisited: completely analytical anisotropic dynamical models Maarten Baes and Herwig Dejonghe Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 28-S9, B-9 Gent, Belgium e-mail:
More informationDark Matter Detection Using Pulsar Timing
Dark Matter Detection Using Pulsar Timing ABSTRACT An observation program for detecting and studying dark matter subhalos in our galaxy is propsed. The gravitational field of a massive object distorts
More informationI. 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 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 informationThe Milky Way s rotation curve out to 100 kpc and its constraint on the Galactic mass distribution
I S I The Milky Way s rotation curve out to 100 kpc and its constraint on the Galactic mass distribution Yang Huang (LAMOST Fellow, yanghuang@pku.edu.cn) N G U N I V E R P E K T Y 1 8 9 8 Peking University
More informationSpatial 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 informationAY202a Galaxies & Dynamics Lecture 7: Jeans Law, Virial Theorem Structure of E Galaxies
AY202a Galaxies & Dynamics Lecture 7: Jeans Law, Virial Theorem Structure of E Galaxies Jean s Law Star/Galaxy Formation is most simply defined as the process of going from hydrostatic equilibrium to gravitational
More informationarxiv: v1 [astro-ph.ga] 10 May 2016
Mon. Not. R. Astron. Soc. 000, 1 16 (2043) Printed 2 July 2018 (MN LATEX style file v2.2) arxiv:1605.03191v1 [astro-ph.ga] 10 May 2016 Globular Cluster Scale Sizes in Giant Galaxies: Orbital Anisotropy
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 informationExtra Gal 9: Photometry & Dynamics
Extra Gal 9: Photometry & Dynamics Two books, among many others, that can be used by the studenys for extensive references and details are: Binney and Merrifield: Galactic Astronomy Binney and Tremaine
More informationDetermining the Nature of Dark Matter with Astrometry
Determining the Nature of Dark Matter with Astrometry Louie Strigari UC Irvine Center for Cosmology Fermilab, 4.16.2007 Collaborators: James Bullock, Juerg Diemand, Manoj Kaplinghat, Michael Kuhlen, Piero
More informationMASS PROFILES OF X-RAY BRIGHT RELAXED GROUPS: METHODS AND SYSTEMATICS
MASS PROFILES OF X-RAY BRIGHT RELAXED GROUPS: METHODS AND SYSTEMATICS FABIO GASTALDELLO IASF-INAF MILANO & UC IRVINE D. BUOTE UCI P. HUMPHREY UCI L. ZAPPACOSTA TRIESTE J. BULLOCK UCI W. MATHEWS UCSC F.
More informationVeilleux! see MBW ! 23! 24!
Veilleux! see MBW 10.4.3! 23! 24! MBW pg 488-491! 25! But simple closed-box model works well for bulge of Milky Way! Outflow and/or accretion is needed to explain!!!metallicity distribution of stars in
More informationThe 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 informationPeculiar (Interacting) Galaxies
Peculiar (Interacting) Galaxies Not all galaxies fall on the Hubble sequence: many are peculiar! In 1966, Arp created an Atlas of Peculiar Galaxies based on pictures from the Palomar Sky Survey. In 1982,
More informationarxiv:astro-ph/ v1 24 Feb 2005
DRAFT VERSION 20TH JUNE 2018 Preprint typeset using LATEX style emulateapj v. 6/22/04 A UNIVERSAL DENSITY PROFILE FOR DARK AND LUMINOUS MATTER? DAVID MERRITT 1, JULIO F. NAVARRO 2,3,, AARON LUDLOW 2 AND
More informationGalaxy 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 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 informationConstraining Dark Matter Equation of State with CLASH Clusters
Constraining Dark Matter Equation of State with CLASH Clusters Barbara Sartoris, Andrea Biviano, Piero Rosati and the CLASH team University of Trieste The Equation of state No direct observations of the
More informationGalaxies. Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations
Galaxies Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations Cepheids in M31 Up to 1920s, the Milky Way was thought by
More informationMilky Way disc dynamics and kinematics from mock data
Milky Way disc dynamics and kinematics from mock data Laurent Chemin CNES Postdoctoral Fellow (Lab. Astro. of Bordeaux) DPAC CU6 member: Gaia RVS calibrations and commissioning CU9 member: validation of
More information1 [3 p.] First things first. 4 [2p.] Mass to light II. 5 [3p.] Merger remnants
Name and student number: [will be needed in the real exam] ASTC22 (GALACTIC AND EXTRAGALACTIC ASTROPHYSICS) PREPARATION SETFOR FINAL EXAM (#7) - PROBLEMS. SOLVED, SOME NOT. SOME FULLY Points in the square
More informationSecular Evolution of Galaxies
Secular Evolution of Galaxies Outline:!Disk size evolution! Bar fraction vs mass & color! AM transfers, radial migrations! Bulges, thick disks Françoise Combes Durham, 19 July 2011 Two modes to assemble
More informationPhenomenological 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 informationarxiv: v1 [astro-ph.co] 22 Nov 2012
ACCEPTED TO APJ: 11 NOVEMBER 2012 Preprint typeset using LATEX style emulateapj v. 5/2/11 MEASURING DARK MATTER PROFILES NON-PARAMETRICALLY IN DWARF SPHEROIDALS: AN APPLICATION TO DRACO JOHN R. JARDEL
More informationThe Geometry of Sagittarius Stream from PS1 3π RR Lyrae
The Geometry of Sagittarius Stream from PS1 3π RR Lyrae Nina Hernitschek, Caltech collaborators: Hans-Walter Rix, Branimir Sesar, Judith Cohen Swinburne-Caltech Workshop: Galaxies and their Halos, Sept.
More informationMatteo Barnabè & Léon Koopmans Kapteyn Astronomical Institute - Groningen (NL)
Joint Gravitational Lensing and Stellar Dynamics Analysis of Early-Type Galaxies Matteo Barnabè & Léon Koopmans Kapteyn Astronomical Institute - Groningen (NL) Leiden, 04 August 2006 What is the mass structure
More informationEquations of Stellar Structure
Equations of Stellar Structure Stellar structure and evolution can be calculated via a series of differential equations involving mass, pressure, temperature, and density. For simplicity, we will assume
More informationE. not enough information given to decide
Q22.1 A spherical Gaussian surface (#1) encloses and is centered on a point charge +q. A second spherical Gaussian surface (#2) of the same size also encloses the charge but is not centered on it. Compared
More informationPotential-Density pair: Worked Problem In a spherical galaxy, the density of matter varies with radius as. a r 2 (r+a) 2, ρ(r) = M 4π
15 Potential-Density pair: Worked Problem In a spherical galaxy, the density of matter varies with radius as where M and a are constants. ρ(r) = M 4π a r 2 (r+a) 2, (a) Verify that the total mass of the
More informationBrief update (3 mins/2 slides) on astrophysics behind final project
Nov 1, 2017 Brief update (3 mins/2 slides) on astrophysics behind final project Evidence for Dark Matter Next Wed: Prelim #2, similar to last one (30 mins). Review especially lecture slides, PEs and non-project
More informationAxisymmetric orbit-based models of a mock dwarf spheroidal galaxy
Axisymmetric orbit-based models of a mock dwarf spheroidal galaxy Author: Jorrit Hagen Under supervision of: Amina Helmi Maarten Breddels Affiliation: Kapteyn Astronomical Institute October 6, 2015 Abstract
More information