Daniel Ceverino (HU) Potsdam, 2009 Avishai Dekel (HU), Reem Sari(HU), Tobias Goerdt(HU), Anatoly Klypin (NMSU) High-Redshift Clumpy Disks & Bulges in Cosmological.

Slides:

Advertisements

Similar presentations

arvard.edu/phot o/2007/m51/. Confronting Stellar Feedback Simulations with Observations of Hot Gas in Elliptical Galaxies Q. Daniel Wang,

Advertisements

Late gas accretion onto primordial mini-halos a model for pre-reionization dwarfs and extragalactic compact High-Velocity Clouds Massimo Ricotti (U of.

Semi-analytic Models based on Millennium II Haloes 1.

From protostellar cores to disk galaxies - Zurich - 09/2007 S.Walch, A.Burkert, T.Naab Munich University Observatory S.Walch, A.Burkert, T.Naab Munich.

Galaxy Mergers: major/minor wet/dry Hans-Walter Rix MPIA, Heidelberg … which galaxies are most shaped by mergers? … when do mergers matter for the SFR?

The main growth modes of disks, bulges, and central black holes: Mergers - Violent Instabilities - Secular Evolution Frédéric Bournaud - CEA Saclay with.

Duilia de Mello (CUA-GSFC) Amy Soto (CUA), Nick Bond (GSFC), Jon P. Gardner (GSFC), Swara Ravindranath (STScI), Claudia Scarlata (UMN), Elysse Voyer (LAM),

The Thick Disks of Spiral Galaxies as Relics from Gas-Rich, Turbulent, Clumpy Disks at High Redshifts Frédéric Bournaud, Bruce G. Elmegreen, and Marie.

Gas in the Local Group James Binney & Filippo Fraternali Oxford University.

Filippo Fraternali (Bologna University)3D - Munich - 12/06/08 Extra-planar gas at low and high z Extra-planar gas at low and high redshifts Filippo Fraternali.

A simple model to explain the high gas content of galaxy UGC 8802 Ruixiang Chang Shanghai Astronomical Observatory Collaborators: Jinliang Hou Shiyin Shen.

Subaru UM 2009/01/15 1 Extended ionized gas regions around the Coma cluster galaxies Michitoshi YOSHIDA Okayama Astrophysical Observatory, NAOJ with Masafumi.

Fu Jian Max Planck Institute for Astrophysics, Garching 18/12/

Quenched and Quenching Galaxies at Low to High Redshifts S.M. Faber & UCSC and CANDELS collaborators Dekel60 Fest December 13, 2011 M31: UV GALEX.

Formation of Globular Clusters in  CDM Cosmology Oleg Gnedin (University of Michigan)

Numerical issues in SPH simulations of disk galaxy formation Tobias Kaufmann, Lucio Mayer, Ben Moore, Joachim Stadel University of Zürich Institute for.

Anatoly Klypin New Mexico State University Also: Stefan Gottloeber (Astrophysikalisches Institut Potsdam ) Gustavo Yepes (UAM, Madrid) Andrey Kravtsov.

Particle Astrophysics & Cosmology SS Chapter 7 Dark Matter.

Early evolution of tidal dwarf galaxies Simone Recchi INAF – Trieste Observatory V Estallidos Workshop “Star Formation and Metallicity” Albayzin – Granada.

Searching for the large-scale hot gaseous Galactic halo --Observations confront theories Yangsen Yao in collaboration with Michael A. Nowak Q. Daniel Wang.

HST ACSCO on ACS in EGS at z=1.12 Molecular Gas in Star Forming Galaxies at z=1-3 Linda Tacconi, MPE Garching & Santa Cruz Galaxy Evolution Workshop.

How Galaxies Assemble Romeel Davé, Univ. of Arizona With: Dušan Kereš & Neal Katz (U.Mass), and David Weinberg (Ohio State)

Merger Histories of LCDM Galaxies: Disk Survivability and the Deposition of Cold Gas via Mergers Kyle Stewart AAS Dissertation Talk 213 th AAS Meeting.

A Multiphase, Sticky Particle, Star Formation Recipe for Cosmology

A Multiphase, Sticky Particle, Star Formation Recipe for Cosmology Craig Booth Tom Theuns & Takashi Okamoto.

Merger Histories of Dark Matter Halos in  CDM and Implications for the Evolution of Milky Way-size Galaxies Kyle Stewart NPP Fellow, JPL Astrophysics.

Simon Portegies Zwart (Univ. Amsterdam with 2 GRAPE-6 boards)

RECOILING BLACK HOLES IN GALACTIC CENTERS Michael Boylan-Kolchin, Chung-Pei Ma, and Eliot Quataert (UC Berkeley) astro-ph/

Bi-modality and Do w n s i z i n g Avishai Dekel HU Jerusalem Bernard ’ s Cosmic Stories, Valencia, June 2006 Origin of E vs S Galaxies.

Dark Matter and Galaxy Formation (Section 3: Galaxy Data vs. Simulations) Joel R. Primack 2009, eprint arXiv: Presented by: Michael Solway.

Krakow 2010 Galactic magnetic fields: MRI or SN-driven dynamo? Detlef Elstner Oliver Gressel Natali Dziourkevich Alfio Bonanno Günther Rüdiger.

Modelling Dwarf Galaxies with a Multi-Phase ISM Stefan Harfst 1,2 with: Ch. Theis 3,2 and G. Hensler 3,2 G. Hensler 3,2 1 Rochester Institute of Technology,

THE STRUCTURE OF COLD DARK MATTER HALOS J. Navarro, C. Frenk, S. White 2097 citations to NFW paper to date.

Merger Histories of LCDM Galaxies: Disk Survivability and the Deposition of Cold Gas via Mergers Kyle Stewart Ohio State CCAPP Seminar Kyle Stewart.

A.Kravtsov (U.Chicago) D. Ceverino (NMSU) O. Valenzuela (U.Washington) G. Rhee (UNLV) F. Governato, T.Quinn, G.Stinson (U.Washington) J.Wadsley (McMaster,

Superbubble Driven Outflows in Cosmological Galaxy Evolution Ben Keller (McMaster University) James Wadsley, Hugh Couchman CASCA 2015 Paper: astro-ph:

Galactic Metamorphoses: Role of Structure Christopher J. Conselice.

The Main Mode of Galaxy/Star Formation? Avishai Dekel, HU Jerusalem Leiden, September 2008 HU Flow Team Birnboim, Freundlich, Goerdt, Neistein, Zinger.

1 Lessons from cosmic history Star formation laws and their role in galaxy evolution R. Feldmann UC Berkeley see Feldmann 2013, arXiv:

Alyson Brooks Fairchild Postdoctoral Fellow in Theoretical Astrophysics Caltech In collaboration with C. Brook (JHI), F. Governato (UW), L. Mayer (ETH,

The co-evolution of massive ellipticals & their black holes Thorsten Naab University Observatory, Munich 8 th Sino-German Workshop on Galaxy Formation.

1 On star-formation compactness & bulges: the ALMA view  IR (z~2) =  IR (z~0) x 6  IR (z~4) =  IR (z~0) x 12  IR (z) =  IR (z~0) x (1+z) 2.5 vs 

Virial shocks in galaxy and cluster halos

Renaissance: Formation of the first light sources in the Universe after the Dark Ages Justin Vandenbroucke, UC Berkeley Physics 290H, February 12, 2008.

Spiral Triggering of Star Formation Ian Bonnell, Clare Dobbs Tom Robitaille, University of St Andrews Jim Pringle IoA, Cambridge.

BX663 (2.4) MD 41 (2.2) K20-9 (2.0) K20-7 (2.2) K20-8 (2.2) D3a 4751 (2.27) SA (2.3)

1 Galaxy Formation A quick overview of the key concepts.

Cool Halo Gas in a Cosmological Context Kyle Stewart “Team Irvine” UC Santa Cruz Galaxy Formation Workshop Kyle Stewart “Team Irvine” UC Santa.

野口正史（東北大学）.  Numerical simulation Disk galaxy evolution driven by massive clumps  Analytical model building Hubble sequence.

Philamentary Structure and Velocity Gradients in the Orion A Cloud

Gas Accretion and Secular Processes 1  How much mass assembled in mergers?  How much through gas accretion and secular evolution? Keres et al 2005, Dekel.

The cold component of cluster accretion Yuval Birnboim Jerusalem 2011.

联合天体物理中心 Joint Center for Astrophysics The half-light radius distribution of LBGs and their stellar mass function Chenggang Shu Joint Center for.

AST101 Lecture 20 Our Galaxy Dissected. Shape of the Galaxy.

What is EVLA? Giant steps to the SKA-high ParameterVLAEVLAFactor Point Source Sensitivity (1- , 12 hr.)10  Jy1  Jy 10 Maximum BW in each polarization0.1.

On the initial conditions and evolution of isolated galaxy models 2012 Workshop on Computational Sciences and Research Hub Induck Hall at Pusan Nat'l University.

The Physics of Galaxy Formation. Daniel Ceverino (NMSU/Hebrew U.) Anatoly Klypin, Chris Churchill, Glenn Kacprzak (NMSU) Socorro, 2008.

Arman Khalatyan AIP 2006 GROUP meeting at AIP. Outline What is AGN? –Scales The model –Multiphase ISM in SPH SFR –BH model Self regulated accretion ?!

ARCCOS Centre of Excellence in Evolutionary Cosmology University of Central Lancashire Galaxies on a Mesh Brad Gibson Stephanie Courty, Chris Brook, Patricia.

Casiana Muñoz-Tuñón Instituto de Astrofísica de Canarias (IAC) Rodrigo Hinojosa Goñi (Chile) Jairo Méndez-Abreu (St. Andrews-UK) Starbursts.

Cold streams as Lyman-alpha blobs Collaborators: Avishai Dekel, Amiel Sternberg, Daniel Ceverino, Romain Teyssier, Joel Primack Tobias Goerdt.

Towards Realistic Modeling of Massive Star Clusters Oleg Gnedin (University of Michigan) graduate student Hui Li.

Extragalactic science with adaptive optics ( a few highlights)

Formation of Globular Clusters in Hierarchical Cosmology: ART and Science Oleg Gnedin Ohio State University.

DYNAMO Survey: An up-close view of turbulent, clumpy galaxies

What is EVLA? Build on existing infrastructure, replace all electronics (correlator, Rx, IF, M/C) => multiply ten-fold the VLA’s observational capabilities.

‘3D’ Data Sets are ABSOLUTELY Crucial to Answer the Important Questions of Galaxy Formation and Evolution Galaxy dynamical masses, gas masses Spatially.

Kinemetry of High-Redshift Galaxies

Specific Star Formation Rates to z=1.5

The SINS survey of galaxy kinematics at z~2 : turbulent thick disks and evidence for rapid secular evolution Reinhard Genzel, Natascha Förster Schreiber,

Presentation transcript:

Daniel Ceverino (HU) Potsdam, 2009 Avishai Dekel (HU), Reem Sari(HU), Tobias Goerdt(HU), Anatoly Klypin (NMSU) High-Redshift Clumpy Disks & Bulges in Cosmological Simulations

From Disks to Bulges Elmegreen et al Genzel et al Rest-frame UV Rest-frame visible

Cold Streams & Hot halos at z=2.3 2R vir =140 kpc M vir = M Cold Gas (T< K)Hot Gas (T> K) R vir Disk Streams

Gravitationally Unstable Disks 15 kpc log (M /pc 2 ) Clumps !! Gas Surface Density

More Clumpy Galaxies 10 kpc Gas Surface Density Face-on viewEdge-on view

Star Formation Maps 10 kpc Face-on viewEdge-on view in log(M /yr/kpc 2 )

A Massive Bulge 10 kpc Face-on viewEdge-on view Stellar Surface Density

More Clumpy Disks Gas Surface Density 10 kpc

SINS and Simulations Data (Red circles) from Forster Schreiber et al Data (Red circles) from Cresci et al SFR vs Stellar Mass Stellar Mass vs Max. Velocity

Clumps Evolution (400 Myr)

Clump Formation 8 kpc

Clump Migration 8 kpc

Steady-State Regime z=1.9 z=1.6 z=1.3

Summary

The End

Artificial Fragmentation