Dwarf Spheroidal Galaxies : From observations to models and vice versa. Yves Revaz
|
|
- Jason Price
- 5 years ago
- Views:
Transcription
1 Dwarf Spheroidal Galaxies : From observations to models and vice versa Yves Revaz
2 The good reasons to study dsphs : Test for the LCDM paradigm : small structures are predicted in abundance Galaxy luminosity function Bower et al. 2003
3 The good reasons to study dsphs : The missing satellite problem LCDM simulations predict the existence of a high number of dwarf galaxies orbiting around Andromeda and the MilkyWay......but only a modest population is observed. Via Lactea (Diemand et al. 2007) Simon & Geha 2007
4 The good reasons to study dsphs : In the hierarchical LCDM paradigm, dsphs are the building blocks of larger objects Dwarf galaxies Spiral galaxies time Elliptical galaxies Galaxy clusters
5 The good reasons to study dsphs : Much more complex than usually thought Tinguely 1970
6 Agenda What is a dsph galaxy? How do we model these objects? The driving parameters Intrinsic or extrinsic evolution? Can we predict the stellar mass for a given halo mass Some conclusions
7 What is a dsph galaxy? Faint stellar system (Mv < -15) Low velocity dispersion (~10 km/s) Evidence for dark matter No clear rotation (dominated by random motions) No ongoing star formation No gas (or at least not detected) [Fe/H] follows luminosity
8 clustered around spiral galaxies dsphs are interior to transition systems, themselves interior to dirrs Mateo 2008
9 diffuse objects core core tidal tidal Fornax Carina Piatek, 2007; 2003
10 they form a sequence Adapted from Tolstoy, Hill & Tosi 2009
11 ...but are also very different Sculptor Carina Vt=198 ±50 km/s Vr=79 ±6 km/s Peri : 68 kpc (33, 83) Apo :122 kpc (97,133) Period : 2.2 Gyr Vt=85 ±39 km/s Vr=22 ±24 km/s Peri : 20 kpc (3, 63) Apo :102 kpc (102,113) Period : 1.4 Gyr today today Piatek et al. 2006, 2003
12 disparate, structures, diff. stellar pop as fct of r Carina Time Rizzi et al also Tolstoy et al. 2004; Battaglia et al Out In Star Formation Rate Sculptor Time
13 What is at the origin of the diversity? Is the environment the driving parameter? Chance encounters produce a variety of properties Can we think otherwise? How much of the variety is intrinsic? When and how is interaction required? Sequence = single framework of formation?
14
15 Current limitations Too simplistic chemical evolution Arbitrary fixed SFH Small number of simulations Evolution stopped at high z Confront results only with global relations
16 Global relations are not all... Objects with very similar : - Lv - [Fe/H] - [M/Lv]...
17 ... may have completely different stellar and chemical properties! SFR, M* AGE [Fe/H] [Mg/Fe]
18 Observations : Where do we stand? Accurate abundances measurement from individual stars for: Fornax Sculptor Sextans Carina Team DART (Letarte et al. 2010) (Hill et al. in prep.) (Shetrone et al., 2001, Aoki et al.,2009, Jablonka et al., in prep.) (Koch et al., 2008, Lesmale et al., 2011, Venn et al., in prep.)
19 Modelisation Code & physical processes The initial conditions Tests and Robustness
20 GEAR : a self-consistent Tree/SPH code (Revaz & Jablonka 2012) Skeleton : Gadget-2 (Springel 2005) Gravity : -> treecode (Barnes & Hut 86) NlogN instead of N2 Hydrodynamics : -> SPH : Smooth Particles Hydrodynamics (Lucy 77, Gingold & Monaghan 77) Hydrodynamics values are obtained by convolution of neighbors particles with a kernel function the resolution follows the mass
21 GEAR : a self-consistent Tree/SPH code The baryon physics Cooling function (metal dependent) : - above 104K (Sutherland & Dopita 93) - below 104K, H2, HD, OI, CII, SiII, FeII (Maio et al. 07) Star formation : classical recipes : Schmidt law (Schmidt 59) (Katz 92) + star formation density (0.1 a/cm3) + starformation temperature (3x104K)
22 GEAR : a self-consistent Tree/SPH code Chemical evolution SSP scheme : (Poirier 03, PhD thesis) - SNIa, SNII nucleosynthesis + feedback from SN explosions - elements followed : Fe, Mg
23 Time Kodama & Arimoto 97 Formation time of a stellar particle (SSP) mass fraction yields energy Injection into the system : nearest neighbors IMF : Krupa 01
24 SNII : yields of massive stars (Iwamoto et al. 99) Energy : esn 1051 ergs/sn (thermal)
25 SNIa : model from Kobayashi et al yields from Tsujimoto et al. 95, updated models Energy : esn 1051 ergs/sn (thermal)
26 Outputs of models and observables stellar particles : Fe, Mg, Z, age -> Lv (Vasdekis et al. 96) gas particles : Fe, Mg, Z, density, temperature all particles : positions, velocities, mass
27 Initial conditions
28 Initial conditions - 2 Mpc/h3 box, dark matter only (WMAP V) - 134'217'728 particles => resolution of 150 pc/h, Msol/h more than 150 dsph haloes with masses between 108 > M > 109 Msol
29 Z=
30 Z=
31 50% of the haloes have their density profiles already in place at z=6 (in physical coordinate) 98% have an NFW profile, wich central densities varying by a fractor ~3 only (for masses between 108 and 109 Msol)
32 Initial conditions : isolated models Models of dsphs in a static Euclidean space, where the expansion of the universe is neglected, are justified. The physics of baryons that depends on the density in physical coordinates is correct. The densities of haloes with mass between 108 and 109 Msol exhibit a small dispersion, a factor 3 to 4, which could help understanding the variety in the observed properties of the dsphs Core profile supported by the observations (Blais-Ouellette et al. 2001; de Blok & Bosma 2002; Swaters et al. 2003; Gentile et al. 2004, 2005; Spekkens et al. 2005; de Blok 2005; de Blok et al. 2008; Spano et al. 2008)
33 Energy conservation, Robustness & Convergence tests
34 9.5x108Msol Conservation better than 5% over more than 250 dynamical times!
35
36 chemical properties : - metallicity distribution - abundances density profile
37 Results
38 Parameters (see also Revaz et al. 2009) More than 400 simulations, Exploring the effect of the parameters
39
40 Efficiency of supernova energy : Mass = 4x108Msol esn= 100% esn= 1% If esn=100% (1051 ergs per SN) no Fe/H enhancement (need to be below 10%) no strong winds : the gas is kept around the system 107 Msol of gas linked to the dsph (see also Marcolini et al. 06, Valcke et al. 08)
41 Mass or density? density x 5 : Δ[Fe/H]= 1.0 dex mass x 9 : Δ[Fe/H]= 0.5 dex density c*=0.05 esn=0.03 Cooling stronger for larger densities Mass increases luminosity but has negligible impact on the chemical evolution mass
42
43 Fornax 7x108Msol Sculptor 8 5x10 Msol Sextans 8 3x10 Msol Carina 8 1x10 Msol
44 Do we observe a sequence? Yes The dominant driving parameters are the mass and density (compatible with the cosmology) More massive and dense systems, forms stars continuously high [Fe/H] high Lv Less massive and less dense sytems forms stars episodically low [Fe/H] But we need outer physical processes to truncate the star formation to get rid of the remaining gas low Lv
45 Metallicity gradients Sextans (Battaglia et al. 2011) Fornax (Battaglia et al 2006) Sculptor (Tolstoy et al. 2004)
46 Metallicity gradients metalicity gradients?
47 Metallicity gradients : the effect of gas motion High resolution model : M= Msol, 4x106 of particles hot gas heated by SNs accumulates at the center due to strong Archimedes forces this gas is driven outside high metallic gas is ejected into the IGM ( Msol)
48 Metallicity gradients : the effect of gas motion High resolution model : M= Msol, 4x106 of particles
49 How galaxies populates their dark matter halo?
50 Abundance matching Millennium Simulation (MS; Springel et al. 2005) High resolution MS (Boylan-Kolchin et al. 2009) SDSS/DR7 Assume main subhaloes and satellite subhaloes have galaxies at their centres, Guo et al the stellar masses of these galaxies are directly related to the maximum dark matter mass ever attained by the subhalo during its evolution. In practice, this mass is usually the mass at z= 0. one-to-one and monotonic relationship between Mhalo and M* n(>mhalo) = n(>m*)
51 Abundance matching : Sawala et al 2011 SDSS+Millenium Guo et al 2010 Extrapolation Sawala et al 2011
52 Abundance matching Sawala et al 2011 SDSS+Millenium Guo et al 2010 Who is right? Who is wrong?
53 Faber-Jackson / Tully-Fisher relation SDSS+Millenium Guo et al 2010
54 Faber-Jackson / Tully-Fisher relation SDSS+Millenium Guo et al 2010
55 Faber-Jackson / Tully-Fisher relation SDSS+Millenium Guo et al 2010
56 Can we find 10 km/s stellar systems in Msol halos?
57 Large sample of halo populated by stars with random properties (N-body systems) Halo : generalized NFW (HonhSheng Zhao 1996, Treu et al. 2002) CUSP or CORE Mh : [108,1011] Msol rs,h : [0.5-4] kpc h : [0,1] Stars : generalized NFW Mh : [105,109] Msol rs,s : [0.5-4] kpc s : [0,1] Velocities computed from the Jeans Equations
58
59 Baryonic fractions at odd with plausible star formation histories bf : [3x10-5, 3x10-4] bf : [3x10-4, 3x10-3] Maccio et al Carina-like Fornax-like
60 Conclusions GEAR : a self-consistent Tree/SPH code for dsphs simulations robust + good convergence In LCDM, the density profiles of small haloes does not evolve much betweeen z=6 and z=0 Possible to study dsph in an isolated context To fit the metallicity of dsphs, the feedback efficiency cannot be large : no strong winds but a large amount of gas left Global relations are reproduced But also the variety in stellar populations and chemical abundances for : Fornax, Sculptor, Sextans & Carina
61 Conclusions Evolution driven by : Intrinsic processes : mass+density Extrinsic processes : get rid of the remaining gas + truncate the SFR Credit : Olivier Tiret Tidal stripping? Ram pressure stripping? The low stellar content predicted by LCDM for 10 10Msol seems to be incompatible with our models
62 The futur of GEAR Cosmological simulations dirr and spiral galaxies
63 The End
Complexities in the stellar kinematics of Local Group dwarf galaxies
Complexities in the stellar kinematics of Local Group dwarf galaxies Giuseppina Battaglia Ramon y Cajal fellow Instituto de Astrofisica de Canarias, Tenerife With thanks to: J.Bermejo-Climent, N.Kacharov,
More informationSubstructure in the Galaxy
Substructure in the Galaxy Amina Helmi Kapteyn Astronomical Institute Groningen, NL Is this how our Galaxy formed? Jeffrey Gardner Hierarchical paradigm Main characteristic of model: mergers Can we find
More informationDwarf 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 informationModelling the galaxy population
Modelling the galaxy population Simon White Max Planck Institut für Astrophysik IAU 277 Ouagadougou 1 The standard model reproduces -- the linear initial conditions -- IGM structure during galaxy formation
More informationChemo-Dynamical evolution of dwarf spheroidal galaxies
11 th Russbach School on Nuclear Astrophysics Chemo-Dynamical evolution of dwarf spheroidal galaxies Yutaka Hirai! (The University of Tokyo, NAOJ)! Jun Hidaka (NAOJ), Takayuki R. Saitoh (Titech),! Michiko
More informationON THE CHEMICAL EVOLUTION OF THE MILKY WAY. The Metallicity distribution of the halo in the hierarchical merging paradigm
ON THE CHEMICAL EVOLUTION OF THE MILKY WAY The Metallicity distribution of the halo in the hierarchical merging paradigm Halo abundance patterns and stellar yields Standard chemical evolution of solar
More informationInsights into galaxy formation from dwarf galaxies
Potsdam, August 2014 Insights into galaxy formation from dwarf galaxies Simon White Max Planck Institute for Astrophysics Planck CMB map: the IC's for structure formation Planck CMB map: the IC's for structure
More informationLucio Mayer ETH Zwicky Prize Fellow
The Local Group of galaxies in a cold dark matter Universe Collaborators: Lucio Mayer ETH Zwicky Prize Fellow Fabio Governato (U. of Washinhgton) Beth Willman (NYU) James Wadsley (McMaster) Greg Stinson
More informationEffects of baryons on the circular velocities of dwarf satellites
Effects of baryons on the circular velocities of dwarf satellites Anatoly Klypin, Kenza Arraki, Surhud More NMSU, U. Chicago August 15, 2012; Santa Cruz Galaxy Workshop LCDM and dwarfs: love to hate Missing
More informationPATRICIA B. TISSERA. Institute for Astronomy and Space Physics Argentina
PATRICIA B. TISSERA Institute for Astronomy and Space Physics Argentina i Observational motivations Model Results GALAXY FORMATION In the last years, studies of chemical elements obtained in the Local
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 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 informationAGN feedback and its influence on massive galaxy evolution
AGN feedback and its influence on massive galaxy evolution Darren Croton (University of California Berkeley) Simon White, Volker Springel, et al. (MPA) DEEP2 & AEGIS collaborations (Berkeley & everywhere
More informationThe Millennium Simulation: cosmic evolution in a supercomputer. Simon White Max Planck Institute for Astrophysics
The Millennium Simulation: cosmic evolution in a supercomputer Simon White Max Planck Institute for Astrophysics The COBE satellite (1989-1993) Two instruments made maps of the whole sky in microwaves
More informationGalaxy population simulations
Aspen, February 2014 Galaxy population simulations Simon White Max Planck Institute for Astrophysics semi-analytic simulations provide a tool... To explore the statistics and interactions of the many processes
More informationFormation and growth of galaxies in the young Universe: progress & challenges
Obergurgl. April 2014 Formation and growth of galaxies in the young Universe: progress & challenges Simon White Max Planck Institute for Astrophysics Ly α forest spectra and small-scale initial structure
More informationA wide-field view of the Phoenix transition type dwarf galaxy (Battaglia et al., MNRAS accepted, airxv/ )
A wide-field view of the Phoenix transition type dwarf galaxy (Battaglia et al., MNRAS accepted, airxv/1205.2704) Giuseppina Battaglia INAF Astronomical Observatory of Bologna With thanks to M.Rejkuba,
More informationHST & Resolved Stellar Popula3ons
HST & Resolved Stellar Popula3ons Resolved stellar popula3ons provides a powerful tool to follow galaxy evolu3on consistently and directly in terms of physical parameters such as age (star forma3on history),
More informationThe Different Physical Mechanisms that Drive the Star-formation Histories of Giant and Dwarf Galaxies
The Different Physical Mechanisms that Drive the Star-formation Histories of Giant and Dwarf Galaxies Chris Haines (University of Birmingham) Adriana Gargiulo, Gianni Busarello, Francesco La Barbera, Amata
More informationGalaxies in dark matter halos: luminosity-velocity relation, abundance and baryon content
Galaxies in dark matter halos: luminosity-velocity relation, abundance and baryon content arxiv:1005.1289 arxiv:1002.3660 S. Trujillo-Gomez (NMSU) in collaboration with: A. Klypin (NMSU), J. Primack (UCSC)
More informationASTRON 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 informationNumerical simulations of dwarf galaxy merger trees
Mon. Not. R. Astron. Soc. 000, 1 19 (2014) Printed 15 November 2018 (MN LaT E X style file v2.2) Supposedly more realistic simulations of dwarf galaxies can be obtained from large ab initio cosmological
More informationSupernova Feedback in Low and High Mass Galaxies: Luke Hovey 10 December 2009
Supernova Feedback in Low and High Mass Galaxies: Luke Hovey 10 December 2009 Galactic Winds: Mathews, W. et al. 1971 Effects of Supernovae on the Early Evolution of Galaxies: Larson, R. 1974 The origin
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 informationChemodynamical Simulations Of the Universe & Elliptical Galaxies. Chiaki Kobayashi (Stromlo Fellow, RSAA, ANU)
Chemodynamical Simulations Of the Universe & Elliptical Galaxies Chiaki Kobayashi (Stromlo Fellow, RSAA, ANU) Chemodynamical Evolution AGN (negative & positive) Feedback? Gravity Hydrodynamics Star Formation?
More informationFossils of the First Galaxies in the Local Group: True Fossils and Ghost Halos
Fossils of the First Galaxies in the Local Group: True Fossils and Ghost Halos Mia S. Bovill with Massimo Ricotti University of Maryland The Smallest Galaxies Minihalos DO NOT initiate gas condensation
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 informationSelf-Interacting Dark Matter
Self-Interacting Dark Matter James Bullock UC Irvine Garrison-Kimmel, Oñorbe et al. Act I Motivations Missing Satellites Problem (1999) Theory: N>>1000 Klypin et al. 1999; Moore et al. 1999; Kauffmann
More informationDwarf galaxy Abundances and Radialvelocities. Team (DART) Large Programme A Close Look at Nearby Galaxies
The Dwarf galaxy Abundances and Radial-velocities Team (DART) Large Programme A Close Look at Nearby Galaxies Eline Tolstoy Vanessa Hill Mike Irwin 3 Amina Helmi Giuseppina Battaglia Bruno Letarte Kim
More informationWhat do we need to know about galaxy formation?
What do we need to know about galaxy formation? rachel somerville University of Michigan Hubble Science Legacy Workshop April 2002 what s next? test the CDM paradigm constrain the nature of the dark matter
More informationCosmological Puzzles: Dwarf Galaxies and the Local Group
Cosmological Puzzles: Dwarf Galaxies and the Local Group Julio F. Navarro Dark-matter-only simulations have highlighted a number of cosmological puzzles Local Group puzzles Missing satellites problem Satellite
More informationFeedback and Galaxy Formation
Heating and Cooling in Galaxies and Clusters Garching August 2006 Feedback and Galaxy Formation Simon White Max Planck Institute for Astrophysics Cluster assembly in ΛCDM Gao et al 2004 'Concordance'
More informationConnecting the small and large scales
Cosmology at the Beach Playa del Carmen, Mexico January 12 th, 2010 Connecting the small and large scales Cosmology at the Beach Playa del Carmen, Mexico January 12 th, 2010 Connecting the small and large
More informationLocal Group See S&G ch 4
Our galactic neighborhood consists of one more 'giant' spiral (M31, Andromeda), a smaller spiral M33 and lots of (>35 galaxies), most of which are dwarf ellipticals and irregulars with low mass; most are
More informationWhere to Look for Dark Matter Weirdness
Where to Look for Dark Matter Weirdness Dark Matter in Southern California (DaMaSC) - II James Bullock UC Irvine Garrison-Kimmel, Oñorbe et al. Collaborators Mike Boylan-Kolchin U. Maryland Miguel Rocha
More informationII. Morphology and Structure of Dwarf Galaxies
II. Morphology and Structure of Dwarf Galaxies Ferguson & Binggeli 1994, A&ARev 6, 67 1 1. Properties low mass : 10 6 10 10 M slow rotators : 10 100 km s -1 low luminosity : 10 6 10 10 L low surface brightness
More informationr-process enrichment traced by Pu and Ba near the sun and in the Draco
r-process enrichment traced by Pu and Ba near the sun and in the Draco Takuji Tsujimoto (Nat. Aston. Obs. Jap.) capturing electromagnetic waves earth archives stellar spectra meteorites deep-sea crusts
More informationThe HERMES project. Reconstructing Galaxy Formation. Ken Freeman RSAA, ANU. The metallicity distribution in the Milky Way discs Bologna May 2012
The HERMES project Reconstructing Galaxy Formation Ken Freeman RSAA, ANU The metallicity distribution in the Milky Way discs Bologna May 2012 HERMES is a new high-resolution fiber-fed multi-object spectrometer
More informationPrinceton December 2009 The fine-scale structure of dark matter halos
Princeton December 2009 The fine-scale structure of dark matter halos Simon White Max Planck Institute for Astrophysics The dark matter structure of CDM halos A rich galaxy cluster halo Springel et al
More informationThe degeneracy between star formation parameters in dwarf galaxy simulations and the M star M halo relation
Mon. Not. R. Astron. Soc. 423, 735 745 (2012) doi:10.1111/j.1365-2966.2012.20913.x The degeneracy between star formation parameters in dwarf galaxy simulations and the M star M halo relation A. Cloet-Osselaer,
More informationDark Matter in Galaxies
Dark Matter in Galaxies Garry W. Angus VUB FWO 3rd COSPA Meeting Université de Liège Ellipticals. Old stars. Gas poor. Low star formation rate. Spiral (disk) galaxies. Often gas rich => star formation.
More informationThe Formation and Evolution of Galaxy Clusters
Distant Clusters of Galaxies Ringberg, October, 2005 The Formation and Evolution of Galaxy Clusters Simon D.M. White Max Planck Institute for Astrophysics Bennett et al 2003 > 105 near-independent 5 temperature
More informationBright Cluster Galaxy formation and the role of AGN feedback. Romain Teyssier
Bright Cluster Galaxy formation and the role of AGN feedback Romain Teyssier KITP 2011: Monster Inc. Romain Teyssier 1 Outline - Feedback and galaxy formation - The role of AGN feedback in Milky Way halos
More informationUsing radial metallicity gradients in dwarf galaxies to study environmental processing
Mem. S.A.It. Vol. 85, 504 c SAIt 2014 Memorie della Using radial metallicity gradients in dwarf galaxies to study environmental processing R. Leaman 1,2,3, K. Venn 3, A. Brooks 4,5,6, G. Battaglia 7, A.
More informationThe Iguaçu Lectures. Nonlinear Structure Formation: The growth of galaxies and larger scale structures
April 2006 The Iguaçu Lectures Nonlinear Structure Formation: The growth of galaxies and larger scale structures Simon White Max Planck Institute for Astrophysics z = 0 Dark Matter ROT EVOL Cluster structure
More informationUpcoming class schedule
Upcoming class schedule Thursday March 15 2pm AGN evolution (Amy Barger) th Monday March 19 Project Presentation (Brad) nd Thursday March 22 postponed to make up after spring break.. Spring break March
More informationStellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
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 informationA.Klypin. Dark Matter Halos
A.Klypin Dark Matter Halos 1 Major codes: GADET N-body Hydro Cooling/Heating/SF Metal enrichment Radiative transfer Multistepping/Multiple masses Springel, SDM White PKDGRAV - GASOLINE ART ENZO Quinn,
More informationExtreme Galaxies: Part I
M87, giant elliptical in the Virgo Cluster Extreme Galaxies: Part I Looking at the extremes in galaxy properties may tell us much about the systematics of galaxy formation and evolution and can provide
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 informationSpheroidal (Elliptical) Galaxies MBW chap 13, S+G ch 6!
" The project: Due May 2!! I expect ~10 pages double spaced (250 words/page) with references from material you used (I do not expect 'densely' cited but a sufficient number).! It must be in a subject related
More informationUniversity of Groningen. On the nature of the Milky Way satellites Li, Yang-Shyang; De Lucia, Gabriella; Helmi, Amina
University of Groningen On the nature of the Milky Way satellites Li, Yang-Shyang; De Lucia, Gabriella; Helmi, Amina Published in: Monthly Notices of the Royal Astronomical Society DOI: 10.1111/j.1365-2966.2009.15803.x
More informationTheorem : Proof... Pavel Kroupa. Pavel Kroupa: AIfA, University of Bonn
Theorem : dsph = TDG = LCDM Proof... Pavel Kroupa 1 Two Zwicky Conjectures of fundamental importance : 1. Zwicky (1937) galaxies are about 500 times heavier in the Coma galaxy cluster than judged from
More informationCosmological simulations of galaxy formation
Cosmological simulations of galaxy formation Modern galaxy formation simulations Mock gri SDSS composite image with dust absorption based on Draine opacity model. NGC4622 as seen from HST Outline - Impact
More informationDwarf Galaxies - ideal Laboratories to study astrophysical Processes
Dwarf Galaxies - ideal Laboratories to study astrophysical Processes Gerhard Hensler University of Vienna Lecture 1 Lecture "Dwarf Galaxies",, Thursday 11:30 am Content/Presenter 7.3. Organization 14.3.
More informationThe Combined effects of ram pressure stripping, and tidal influences on Virgo cluster dwarf galaxies, using N body/ SPH simulation
The Combined effects of ram pressure stripping, and tidal influences on Virgo cluster dwarf galaxies, using N body/ SPH simulation Author: Rory Smith, Cardiff University Collaborators: Jonathon Davies,
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 informationSuperbubble Feedback in Galaxy Formation
Superbubble Feedback in Galaxy Formation Ben Keller (McMaster University) James Wadsley, Samantha Benincasa, Hugh Couchman Paper: astro-ph/1405.2625 (Accepted MNRAS) Keller, Wadsley, Benincasa & Couchman
More informationFeedback flows of gas, energy and momentum in and out of galaxies
Feedback flows of gas, energy and momentum in and out of galaxies Matthijs H.D. van der Wiel March 10 th 2005 a part of the course Formation and Evolution of Galaxies Feedback accretion outflow Feedback
More informationElement abundance ratios and star formation quenching: satellite versus central galaxies
Element abundance ratios and star formation quenching: satellite versus central galaxies Anna Gallazzi INAF-Osservatorio Astrofisico di Arcetri Co#funded)by)the)) European)Union) with: Anna Pasquali (ARI-Heidelberg)
More informationTesting Cosmology with Phase-Space Correlations in Systems of Satellite Galaxies. Current Studies and Future Prospects
Observed MW satellites Testing Cosmology with Phase-Space Correlations in Systems of Satellite Galaxies Current Studies and Future Prospects http://marcelpawlowski.com/research/movies-astronomy/ Marcel
More informationCDM Controversies. James Bullock (UC Irvine)
CDM Controversies James Bullock (UC Irvine) Low stellar mass: feedback can t change DM Core Cusp Tollet et al. 2015 Also: Governato+12; Penarrubia+12; Garrison-Kimmel+13, Di Cintio+14 Low stellar mass:
More informationAstro 358/Spring 2008 (49520) Galaxies and the Universe
Astro 358/Spring 2008 (49520) Galaxies and the Universe Figures + Tables for Lecture 13 on Tu Mar 18 Lectures 9 to 12 1) Evidence for DM ; CDM vs HDM 2) Surface brightness profile and v/σ of Disks, Bulges,
More informationWhat is an ultra-faint Galaxy?
What is an ultra-faint Galaxy? UCSB KITP Feb 16 2012 Beth Willman (Haverford College) Large Magellanic Cloud, M V = -18 ~ 1/10 Milky Way luminosity image credit: Yuri Beletsky (ESO) and APOD NGC 205, M
More informationStellar Populations in the Local Group
Stellar Populations in the Local Group Recall what we ve learned from the Milky Way: Age and metallicity tend to be correlated: older -> lower heavy element content younger -> greater heavy element content
More informationBaryons MaEer: Interpre>ng the Dark MaEer Model
Baryons MaEer: Interpre>ng the Dark MaEer Model Alyson Brooks Rutgers, the State University of New Jersey In collabora>on with the University of Washington s N- body Shop makers of quality galaxies Most
More informationKilling Dwarfs with Hot Pancakes. Frank C. van den Bosch (MPIA) with Houjun Mo, Xiaohu Yang & Neal Katz
Killing Dwarfs with Hot Pancakes Frank C. van den Bosch (MPIA) with Houjun Mo, Xiaohu Yang & Neal Katz The Paradigm... SN feedback AGN feedback The halo mass function is much steeper than luminosity function
More informationarxiv:astro-ph/ v1 19 Nov 1999
Where are the First Stars now? Simon D.M. White & Volker Springel Max-Planck-Institute for Astrophysics, Garching bei München, Germany arxiv:astro-ph/9911378v1 19 Nov 1999 Abstract. We use high-resolution
More informationFeedback from massive stars in dwarf galaxy formation
Highlights of Spanish Astrophysics VII, Proceedings of the X Scientific Meeting of the Spanish Astronomical Society held on July 9-13, 2012, in Valencia, Spain. J. C. Guirado, L. M. Lara, V. Quilis, and
More informationGALAXIES 626. The Milky Way II. Chemical evolution:
GALAXIES 626 The Milky Way II. Chemical evolution: Chemical evolution Observation of spiral and irregular galaxies show that the fraction of heavy elements varies with the fraction of the total mass which
More informationThe galaxy population in cold and warm dark matter cosmologies
The galaxy population in cold and warm dark matter cosmologies Lan Wang National Astronomical Observatories, CAS Collaborators: Violeta Gonzalez-Perez, Lizhi Xie, Andrew Cooper, Carlos Frenk, Liang Gao,
More informationComponents 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 informationin the Milky NOW Way AND and THEN dwarf galaxies Stefania Salvadori
CARBON-ENHANCED DWARF GALAXIES: METAL-POOR STARS in the Milky NOW Way AND and THEN dwarf galaxies Stefania Salvadori University of Groningen Kapteyn Astronomical Institute Netherlands Organization for
More informationMoment of beginning of space-time about 13.7 billion years ago. The time at which all the material and energy in the expanding Universe was coincident
Big Bang Moment of beginning of space-time about 13.7 billion years ago The time at which all the material and energy in the expanding Universe was coincident Only moment in the history of the Universe
More informationTwo Phase Formation of Massive Galaxies
Two Phase Formation of Massive Galaxies Focus: High Resolution Cosmological Zoom Simulation of Massive Galaxies ApJ.L.,658,710 (2007) ApJ.,697, 38 (2009) ApJ.L.,699,L178 (2009) ApJ.,725,2312 (2010) ApJ.,744,63(2012)
More informationPhys/Astro 689: Lecture 12. The Problems with Satellite Galaxies
Phys/Astro 689: Lecture 12 The Problems with Satellite Galaxies The Problems with Satellites (1) The Missing Satellites Problem (2) The Too Big to Fail Problem We ll examine potential solutions to each
More informationarxiv: v1 [astro-ph.ga] 29 Sep 2015
Draft version February 21, 2018 Preprint typeset using L A TEX style emulateapj v. 01/23/15 arxiv:1509.08934v1 [astro-ph.ga] 29 Sep 2015 ENRICHMENT OF R-PROCESS ELEMENTS IN DWARF SPHEROIDAL GALAXIES IN
More information2. What are the largest objects that could have formed so far? 3. How do the cosmological parameters influence structure formation?
Einführung in die beobachtungsorientierte Kosmologie I / Introduction to observational Cosmology I LMU WS 2009/10 Rene Fassbender, MPE Tel: 30000-3319, rfassben@mpe.mpg.de 1. Cosmological Principles, Newtonian
More informationThe formation and evolution of globular cluster systems. Joel Pfeffer, Nate Bastian (Liverpool, LJMU)
The formation and evolution of globular cluster systems Joel Pfeffer, Nate Bastian (Liverpool, LJMU) Introduction to stellar clusters Open clusters: few - 10 4 M few Myr - few Gyr solar metallicity disk
More informationSmall-scale problems of cosmology and how modified dynamics might address them
Small-scale problems of cosmology and how modified dynamics might address them Marcel S. Pawlowski Email: marcel.pawlowski@case.edu Twitter: @8minutesold with support from the John Templeton Foundation
More informationGalaxy Ecology. an Environmental Impact Assessment. Frank van den Bosch (MPIA)
Galaxy an Environmental Impact Assessment Frank van den Bosch (MPIA) in collaboration with Xiaohu Yang (SHAO), Houjun Mo (UMass), Simone Weinmann (Zürich) Anna Pasquali (MPIA), Daniel Aquino (MPIA) Aspen,
More informationSimulations of Cosmic Structure Formation
Simulations of Cosmic Structure Formation Volker Springel The role of simulations in cosmology High-resolution N-body simulations Millennium XXL Hydrodynamic simulations and recent results for galaxy formation
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 informationLecture 11: Ages and Metalicities from Observations A Quick Review
Lecture 11: Ages and Metalicities from Observations A Quick Review Ages from main-sequence turn-off stars Main sequence lifetime: lifetime = fuel / burning rate $ M " MS = 7 #10 9 % & M $ L " MS = 7 #10
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 informationCentral dark matter distribution in dwarf galaxies
Central dark matter distribution in dwarf galaxies Se-Heon Oh (ICRAR/UWA) Content cusp/core controversy in ΛCDM simulations Dark matter distribution of THINGS dwarf galaxies High-resolution N-body+SPH
More informationarxiv: v2 [astro-ph.ga] 27 Jul 2015
Draft version July 28, 215 Preprint typeset using L A TEX style emulateapj v. 5/2/11 MATCHING THE DARK MATTER PROFILES OF DSPH GALAXIES WITH THOSE OF SIMULATED SATELLITES: A TWO PARAMETER COMPARISON Maarten
More informationModeling Fe Enrichment in Galaxy Clusters. Jon Oiler AST 591 2/7/2008
Modeling Fe Enrichment in Galaxy Clusters Jon Oiler AST 591 2/7/2008 Outline Background to the problem Initial modeling equations (Standard Model) Results from the model Changes to the model to match ICM
More informationCurrent status of the ΛCDM structure formation model. Simon White Max Planck Institut für Astrophysik
Current status of the ΛCDM structure formation model Simon White Max Planck Institut für Astrophysik The idea that DM might be a neutral, weakly interacting particle took off around 1980, following a measurement
More informationThe Current Status of Too Big To Fail problem! based on Warm Dark Matter cosmology
The Current Status of Too Big To Fail problem! based on Warm Dark Matter cosmology 172th Astronomical Seminar Dec.3 2013 Chiba Lab.M2 Yusuke Komuro Key Word s Too Big To Fail TBTF Cold Dark Matter CDM
More informationSpiral 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 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 informationToo small to succeed: the difficulty of sustaining star formation in low-mass haloes
Advance Access publication 2017 February 8 doi:10.1093/mnras/stx315 Too small to succeed: the difficulty of sustaining star formation in low-mass haloes Claire R. Cashmore, 1 Mark I. Wilkinson, 1 Chris
More informationIAU Symposium #254, Copenhagen June 2008 Simulations of disk galaxy formation in their cosmological context
IAU Symposium #254, Copenhagen June 2008 Simulations of disk galaxy formation in their cosmological context Simon White Max Planck Institute for Astrophysics The WMAP of the whole CMB sky Bennett et al
More informationWhite dwarf dynamical interactions. Enrique García-Berro. Jornades de Recerca, Departament de Física
White dwarf dynamical interactions Enrique García-Berro Jornades de Recerca, Departament de Física CONTENTS 1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions
More informationmodified gravity? Chaire Galaxies et Cosmologie XENON1T Abel & Kaehler
Dark matter or modified gravity? Chaire Galaxies et Cosmologie Françoise Combes 11 December, 2017 XENON1T Abel & Kaehler Why modified gravity? CDM models beautifully account for LSS, CMB, galaxy formation
More informationThe Structural Properties of Milky Way Dwarf Galaxies. Ricardo Muñoz (Universidad de Chile) Collaborators:
The Structural Properties of Milky Way Dwarf Galaxies Ricardo Muñoz (Universidad de Chile) Milky Way inner 100 kpc Collaborators: Marla Geha (Yale) Patrick Côté (HIA/DAO) Peter Stetson (HIA/DAO) Josh Simon
More informationJoop Schaye (Leiden) (Yope Shea)
Overview of sub-grid models in cosmological simulations Joop Schaye (Leiden) (Yope Shea) Length Scales (cm) Subgrid models Cosmological simulations 8 0 2 11 18 20 22 24 28 interparticle distance in stars
More informationCharacterising the last 8 Gyr. The present-day Universe
Characterising the last 8 Gyr The present-day Universe 1 Luminosity and mass functions Redshift survey Apparent magnitude limited e.g., SDSS 14.5
More information