PATRICIA B. TISSERA. Institute for Astronomy and Space Physics Argentina

Size: px
Start display at page:

Download "PATRICIA B. TISSERA. Institute for Astronomy and Space Physics Argentina"

Transcription

1 PATRICIA B. TISSERA Institute for Astronomy and Space Physics Argentina i

2 Observational motivations Model Results

3

4 GALAXY FORMATION In the last years, studies of chemical elements obtained in the Local Universe and at high redshifts have improved dramatically. Chemical patterns are the result of different mechanisms which contribute to galaxy formation gas cooling and condensation growth of the structure: Collapse, infall and mergers star formation and stellar evolution environmental effects:starvation strangulation, etc supernova feedback: chemical + energy release

5 THE MILKY WAY DM HALO BULGE STELLAR HALO THIN DISC THICK DISC

6 Milky Way BULGE hz ~ 2 kpc; averged age ~ 10 Gyr for stars with hz > 400 pc metallicity peak: [Fe/H] ~ -0.3 dex ( Zoccali et al. 2003). there are young stars and on-going star formation ( Van Loon et al. 2003) Stellar Halor: J/M ~ 0 (Freeman 1987); sopported by dispersion <[Fe/H] > ~ -1.5 dex (Ryan & Nories THIN DISC 1991;Chiba & Beers (2000 Rotationally supported: σ/v <<1. Scale-length ~ kpc (Siegel et al. 2001), hz ~ 280 pc (σr, σphi, σz ) ~ (141, 106, 94) km/s Stellar age distribution ~ [2,14]Gyr and [Fe/H] peaks at ~ -0.2 (Nordstrom et al. 2004) THICK DISC scale-lenght ~ 3 kpc, hz ~ 1 kpc (assuming a double exponential). t_median ~ Gyr (Liu &Chaboyer 2000) -2.2 < [Fe/H] <0.5 with <[Fe/H]> ~ -0.6 (Chiba & Beers 2000) higher [O/Fe] than the stars in the thin disc. Patricia B. Tissera

7 Luminosity-metallicity and mass-metallicity relations: There are well-known LMR and MMR in the local Universe. Observations suggest evolution in the zero point and slope of both relations. SDSS: Tremonti et al.2004 Erb et al 2006: z~2.5

8 CHEMICAL FEEDBACK Some references on chemical modeling in cosmological simulations: Raiteri et al. (1996; also Berczik 1999) SNII & SNIa; Fe & H Mosconi, Tissera, Lambas & Cora. (2001): SNII & SNIa, Eth. Lia, Portinari & Carraro (2002):detailed SE; diffusion Kawata & Gibson (2003): SNII, SNIa,IS; Eth +Ekin Springel & Hernquist (2003): Z + Twophases +Ekin Kobayashi (2004; et al. 2006):detailedSE; Eth +Ekin Scannapieco et al. (2005, 2006): SNII & SNIa + Multiphase+SNE Okamoto et al. 2006: SNII+SNIa+Twophases+Ekin (+top heavy Imf) Oppenhaimer & Dave (2006): SNII &SNIa + Twophases + Ekin Stinson et al. (2006): SNII&SNIa + cooling off Martinez-Serrano et al. (2008): detailedse; diffusion Wiersma et al. (2009): detailedse; smoothed metals+ Ekin

9 Supernova Feedback CHEMICAL ENRICHMENT SN: Main source of heavy elements Change the cooling time HYDRODYNAMICAL HEATING evaporates cold-dense gas galactic winds which can results in outflows or galactic fountains Regulates the star formation activity and enriches the ISM and IGM Affects the gas dynamics: disc formation This might leave chemical fossils which can be used to track the formation history of a galaxy

10 CHEMICAL FEEDBACK Mosconi, Tissera, Lambas & Cora 2001 Numerical space Physical space Star particles Stellar populations Type II Sne Type Ia Sne Intermediate mass stars Need IMF: SNe long-lived stars M* > 8 Mo; typical life-times: ~ 106 yr Produce most O, Si, Ca, etc Typical life-times: ~ Gyr Main source of iron (Fe) YIELDS

11 Chemical evolution: the fossil records from Zocalli 2008 Relative abundances of alfa elements over Fe: Relative abundances of SNII with respecto to SNIa Formation timescale of the systems

12 CHEMICAL FEEDBACK When SN explosions take place, they distribute metals according to the SPH technique. For a given chemical element x at a particle i, Mxi = j mj/ρj Mxi W(rij,hij) Each neigbhour will receive Mxj =mj/ρj Mxi W(rij,hij) Exploding star particle Gaseous neighbours Mosconi, Tissera, Lambas & Cora 2001 i j

13 A GADGET-3 (Springel 2005) with: Stochastic star formation (Springel & Hernquist 2002) Chemical enrichment from Type II and Ia Supernovae and metal dependent cooling Multiphase gas model: allows overlap of dense and diffuse gas Supernova feedback: distributes energy separately for cold and hot pre-defined phases (thermal feedback + reservoir for cold phases) within the context of the Multiphase gas model. All this implemented without scale-dependent parameters well suited to run cosmological simulations where systems of different mass form simultaneously. Scannapieco, Tissera, White & Springel 2005,2006,2008

14 Scannapieco et al. 2006

15 Aquarius haloes 8 galazy-sized haloes of 1012 Mo (Springel et al. 2008) selected from a Λ-CDM cosmological volume of 100 Mpc/h box, with mild isolation criterion. ICs have been modified to include baryons. approx half a millons particle per specie Run with GADGET-3 including chemical evolution. Can these simulations reproduce general trends? Can we link the chemical properties to their histories of assembly? Tissera, White & Scannapieco in prepration

16 Aquarius galaxies Scannapieco et al. 2008

17 T= (U2 +W2) Bulge V (km/s) Disc Inner H Outer H

18 Re-defining the disc components r (kpc/h) r (kpc/h) Disc cont. 16% Bar/T(p) = 0.23 [Fe/H] [Fe/H] r (kpc/h) Disc cont. 12 % Bar/T(p) = 0.34 [Fe/H] Disc cont. 7.5% Bar/T(p) = 0 r (kpc/h) r (kpc/h) r (kpc/h)

19 Star formation histories of each component Aq-A-5 Aq-C-5 Aq-D-5 Disc Bulge Inner Halo Outer Halo Age Gyr Aq-E-5 f Age Gyr Aq-G-5 Aq-F-5

20 Aq-A-5 Aq-C-5 Aq-D-5 f Aq-G-5 Aq-E-5 Aq-F-5 f Disc Bulge Inner Halo Outer Halo

21 The hierarchical building up of the structure

22 Stellar mass fraction in Inner Halo In satellites log z +1 log z + 1 Stellar mass fraction in Disc In situ Stellar mass fraction in Outer Halo Stellar mass fraction in Bulge Fraction of stellar mass formed in the progenitor and in substructure log z + 1 log z + 1

23 Median Fe enrichment for each component Disc Bulge Inner Halo Outer Halo

24

25 Median alfa-enhacement for each component Disc Bulge Inner Halo Outer Halo

26 There is a correlation between the fraction of stellar mass formed in situ and the fraction of stellar mass formed in massive satellites (M > Mo/h).

27 The level of enrichment of stars in the halo tend to correlates with the fraction of mass formed in massive satellites: the larger this fraction, the higher the median abundance of the halo

28 Metallicity gradients Observations from Dutil et al. 1997

29 Metallicity gradientes and history of formation

30 Median [O/Fe] (O/H)c S(O/H) Mean age of Bulges Median age Median age Median age The faster the bulge formed its stars, the steeper and higher its Oxygen abundances and the higher its [alfa-fe] content. Nevertheless, there is important dispersion in the correlations.

31 DISC COMPONENT Median properties of stars formed in situ and stars formed in satellites Aq-C [Fe/H] [Fe/H]sat [O/Fe] Aq-D Aq-G [O/Fe]sat 0.27 Age 8.19 Age_sat σ/vtan 0.55 σ/vtan (Gyr) Stars on the disc coming from satellites tend to have lower metallicity and higher [alfa-fe] than those formed in situ. Kinematically they are, on average, more consistent with belonging to a thick disc

32 Stellar mass fraction with very low metallicity

33 Stellar mass fraction of old and metal-rich stars The fraction of old metal-rich stars show NO correlation with the history of formation.

34 The satellite systems 100 kpc/h

35 The satellite systems: star formation histories Aq-B-5 Aq-C-5 Stellar mass fraction Aq-A-5 Stellar mass fraction Aq-D-5 Age (Gyr) Aq-F-5 Aq-G-5

36 The satellite systems: chemical properties Chemical properties of the satellites which contribute to the formation of the main galaxies are different from those of the surviving satellites. Stripped stars Surviving satellites

37 Some conclusions... Bulges formed mainly in situ. Some might receive contribution from stars formed in subtructures. The level of enrichmnet and [alfa/fe] anticorrelates with this fraction: Systems formed mainly by infall have older stellar populations, larger [alfa-fe], higher O/H abundances and speeper gradients. Haloes formed mainly by contribution from substructure. Stars tend to be old with lower level of enrichment. The median abundances correlate with the fraction of stars formed in massive satellites. It matter how they were assembly. The have very flat gradients. The disc component formed mainly in situ and in several starbursts resulting in a population with lower [O/Fe] content. There could be contribution from satellites (~15%) and these stars are older, alfa enhanced and high velocity dispersion than those stars formed on the disc. Simulated gradients are consistent with observations. Satellites that contribute to the formation of the main galaxies have very different chemical properties than those that survive in the haloes.

38 Dynamics and chemistry: new interesting results coming soon..

Chemo-dynamical disk modeling. Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP)

Chemo-dynamical disk modeling. Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP) Chemo-dynamical disk modeling Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP) Talk outline Effect of disk asymmetries on disk dynamics. Radial migration in galactic disks. Chemo-dynamical disk

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

Supernova 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 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 information

GALAXIES 626. The Milky Way II. Chemical evolution:

GALAXIES 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 information

ON 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 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 information

Disk Formation and the Angular Momentum Problem. Presented by: Michael Solway

Disk Formation and the Angular Momentum Problem. Presented by: Michael Solway Disk Formation and the Angular Momentum Problem Presented by: Michael Solway Papers 1. Vitvitska, M. et al. 2002, The origin of angular momentum in dark matter halos, ApJ 581: 799-809 2. D Onghia, E. 2008,

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

The Formation of Galaxies: connecting theory to data

The Formation of Galaxies: connecting theory to data Venice, October 2003 The Formation of Galaxies: connecting theory to data Simon D.M. White Max Planck Institute for Astrophysics The Emergence of the Cosmic Initial Conditions > 105 independent ~ 5 measurements

More information

Basics of Galactic chemical evolution

Basics of Galactic chemical evolution Basics of Galactic chemical evolution The chemical abundances of stars provide important clues as to the evolutionary history of a galaxy. Astronomers usually refer to chemical elements other than hydrogen

More information

Stellar Populations in the Galaxy

Stellar Populations in the Galaxy Stellar Populations in the Galaxy Stars are fish in the sea of the galaxy, and like fish they often travel in schools. Star clusters are relatively small groupings, the true schools are stellar populations.

More information

Zoccali et al. 2003, A&A, 399, 931. Overview of (old) Galactic components. bulge, thick disk, metal-weak halo. metallicity & age distribution

Zoccali et al. 2003, A&A, 399, 931. Overview of (old) Galactic components. bulge, thick disk, metal-weak halo. metallicity & age distribution Chap.3 The nature of Galactic components Overview of (old) Galactic components bulge, thick disk, metal-weak halo Globular clusters metallicity & age distribution Satellite galaxies spatial and metallicity

More information

The Iguaçu Lectures. Nonlinear Structure Formation: The growth of galaxies and larger scale structures

The 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 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

Trends in Intracluster Metallicity

Trends in Intracluster Metallicity Trends in Intracluster Metallicity The Right Answer ICM metallicity is ~0.3 solar with a negative gradient within ~0.15 R180, as measured from Fe K lines M Fe M gas 4 10 4 Leccardi & Molendi (2008) (For

More information

Coupling small and large scales: how massive and dying stars drive the formation of a galaxy

Coupling small and large scales: how massive and dying stars drive the formation of a galaxy Coupling small and large scales: how massive and dying stars drive the formation of a galaxy P. Monaco, Trieste University and INAF-Osservatorio Astronomico di Trieste Micro-physics of star formation and

More information

What do we need to know about galaxy formation?

What 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 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

Superbubble Feedback in Galaxy Formation

Superbubble 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 information

Formation and growth of galaxies in the young Universe: progress & challenges

Formation 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 information

THE CHEMICAL EVOLUTION OF THE MILKY WAY DISK

THE CHEMICAL EVOLUTION OF THE MILKY WAY DISK THE CHEMICAL EVOLUTION OF THE MILKY WAY DISK 1. The simple picture of disk evolution: independent ring evolution, successes and failures 2. The dynamical picture: stars (and gas) moving around 3. A model

More information

Bridging the near and the far: constraints on first star formation from stellar archaeology. Raffaella Schneider Sapienza University of Rome

Bridging the near and the far: constraints on first star formation from stellar archaeology. Raffaella Schneider Sapienza University of Rome Bridging the near and the far: constraints on first star formation from stellar archaeology Raffaella Schneider Sapienza University of Rome Kyoto,First Stars IV 2012 Kyoto,First Stars IV 2012 "As we extend

More information

Numerical Cosmology & Galaxy Formation

Numerical Cosmology & Galaxy Formation Numerical Cosmology & Galaxy Formation Lecture 13: Example simulations Isolated galaxies, mergers & zooms Benjamin Moster 1 Outline of the lecture course Lecture 1: Motivation & Historical Overview Lecture

More information

Feedback and Galaxy Formation

Feedback 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 information

arxiv: v3 [astro-ph.ga] 11 Jun 2010

arxiv: v3 [astro-ph.ga] 11 Jun 2010 Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 31 July 2018 (MN LATEX style file v2.2) An observer s view of simulated galaxies: disc-to-total ratios, bars, and (pseudo-)bulges arxiv:1001.4890v3

More information

Starburst Dwarf Galaxies

Starburst Dwarf Galaxies Starburst Dwarf Galaxies 1 Starburst Dwarf Galaxies The star-formation history does in general not show a continuous evolution but preferably an episoidal behaviour. 2 1 Definition: Starburst ( t0) 10....100

More information

Chemodynamical 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 Simulations Of the Universe & Elliptical Galaxies Chiaki Kobayashi (Stromlo Fellow, RSAA, ANU) Chemodynamical Evolution AGN (negative & positive) Feedback? Gravity Hydrodynamics Star Formation?

More information

The 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 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 information

Joop Schaye (Leiden) (Yope Shea)

Joop 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 information

high density low density Rayleigh-Taylor Test: High density medium starts on top of low density medium and they mix (oil+vinegar) Springel (2010)

high density low density Rayleigh-Taylor Test: High density medium starts on top of low density medium and they mix (oil+vinegar) Springel (2010) GAS MIXES high density Springel (2010) low density Rayleigh-Taylor Test: High density medium starts on top of low density medium and they mix (oil+vinegar) HOT HALO highest resolved density nth= 50x10

More information

Astronomy. Astrophysics. Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies

Astronomy. Astrophysics. Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies DOI: 10.1051/0004-6361/201118409 c ESO 2012 Astronomy & Astrophysics Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies M. E. De Rossi 1,2,3, P. B. Tissera

More information

Princeton December 2009 The fine-scale structure of dark matter halos

Princeton 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 information

Modeling 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 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 information

The theoretical view of high-z Clusters. Nelson Padilla, PUC, Chile Pucón, November 2009

The theoretical view of high-z Clusters. Nelson Padilla, PUC, Chile Pucón, November 2009 The theoretical view of high-z Clusters Nelson Padilla, PUC, Chile Pucón, November 2009 The Plan: 1) To see what the observations are telling us using models that agree with the cosmology, and with other

More information

Basics of chemical evolution

Basics of chemical evolution Basics of chemical evolution The chemical abundances of stars provide important clues as to the evolutionary history of a galaxy. H and He were present very early on in the Universe, while all metals (except

More information

AGN feedback and its influence on massive galaxy evolution

AGN 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 information

Origin of Bi-modality

Origin of Bi-modality Origin of Bi-modality and Downsizing Avishai Dekel HU Jerusalem Galaxies and Structures Through Cosmic Times Venice, March 2006 Summary Q: z

More information

The importance of galactic fountain in galaxy evolution

The importance of galactic fountain in galaxy evolution The importance of galactic fountain in galaxy evolution Federico Marinacci in collaboration with: L. Armillotta, A. Marasco, F. Fraternali, J. Binney, L. Ciotti & C. Nipoti Sydney, 4 November 214 Galactic

More information

Effects of feedback on the morphology of galaxy discs

Effects of feedback on the morphology of galaxy discs Mon. Not. R. Astron. Soc. 363, 1299 1314 (2005) doi:10.1111/j.1365-2966.2005.09525.x Effects of feedback on the morphology of galaxy discs Takashi Okamoto, 1,2 Vincent R. Eke, 1 Carlos S. Frenk 1 and Adrian

More information

Galactic Bulge Science

Galactic Bulge Science Galactic Bulge Science Ken Freeman Australian National University ngcfht meeting Hilo, Mar 27-29 2013 NGC 5746 1 The Galactic bulge was long thought to be a merger product. We now know that boxy bulges

More information

Gaia ITNG2013 School, Tenerife. Ken Freeman, Lecture 2: the thin disk

Gaia ITNG2013 School, Tenerife. Ken Freeman, Lecture 2: the thin disk Gaia ITNG2013 School, Tenerife Ken Freeman, Lecture 2: the thin disk September 2013 The Thick Disk Thick disk Most spirals (including our Galaxy) have a second thicker disk component The thick disk and

More information

arxiv:astro-ph/ v1 5 Feb 2003

arxiv:astro-ph/ v1 5 Feb 2003 Chemo-dynamical Evolution of the ISM in Galaxies Stefan Harfst, Gerhard Hensler and Christian Theis Institute for Theoretical Physics and Astrophysics, University Kiel, Germany arxiv:astro-ph/0302098v1

More information

Two Main Techniques. I: Star-forming Galaxies

Two Main Techniques. I: Star-forming Galaxies p.1/24 The high redshift universe has been opened up to direct observation in the last few years, but most emphasis has been placed on finding the progenitors of today s massive ellipticals. p.2/24 Two

More information

The Universe of Galaxies: from large to small. Physics of Galaxies 2012 part 1 introduction

The Universe of Galaxies: from large to small. Physics of Galaxies 2012 part 1 introduction The Universe of Galaxies: from large to small Physics of Galaxies 2012 part 1 introduction 1 Galaxies lie at the crossroads of astronomy The study of galaxies brings together nearly all astronomical disciplines:

More information

Evolving Disks in Cold Dark Matter Cosmology

Evolving Disks in Cold Dark Matter Cosmology Evolving Disks in Cold Dark Matter Cosmology C. B. Brook 1, H. Martel 1 1 Université Laval, Québec, Qc, G1K-7P4 Canada B. K. Gibson 2.3, D. Kawata 2 2 Swinburne University, Vic., Australia and 3 School

More information

stelle e galassie primordiali

stelle e galassie primordiali stelle e galassie primordiali Raffaella Schneider INAF/Osservatorio Astronomico di Roma Matteo de Bennassuti, PhD INAF/OAR Stefania Marassi, Pdoc INAF/OAR Luca Graziani, Pdoc INAF/OAR Rosa Valiante, Pdoc

More information

arxiv:astro-ph/ v1 19 Nov 1999

arxiv: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 information

Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.

Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio. More abs. Dust [1.1] kev V Wavelength Optical Infra-red More abs. Wilms et al. 000, ApJ, 54, 914 No grains Grains from http://www.astro.princeton.edu/~draine/dust/dustmix.html See DraineH 003a, column

More information

The structure and evolution of stars. Learning Outcomes

The structure and evolution of stars. Learning Outcomes The structure and evolution of stars Lecture14: Type Ia Supernovae The Extravagant Universe By R. Kirshner 1 Learning Outcomes In these final two lectures the student will learn about the following issues:

More information

Citation for published version (APA): Boomsma, R. (2007). The disk-halo connection in NGC 6946 and NGC 253 s.n.

Citation for published version (APA): Boomsma, R. (2007). The disk-halo connection in NGC 6946 and NGC 253 s.n. University of Groningen The disk-halo connection in NGC 6946 and NGC 253 Boomsma, Rense IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it.

More information

IAU 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 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 information

Star formation and feedback in smoothed particle hydrodynamic simulations - I. Isolated galaxies

Star formation and feedback in smoothed particle hydrodynamic simulations - I. Isolated galaxies University of Massachusetts - Amherst ScholarWorks@UMass Amherst Astronomy Department Faculty Publication Series Astronomy 2006 Star formation and feedback in smoothed particle hydrodynamic simulations

More information

Durham Research Online

Durham Research Online Durham Research Online Deposited in DRO: 09 November 2015 Version of attached le: Published Version Peer-review status of attached le: Peer-reviewed Citation for published item: Cooper, Andrew P. and Parry,

More information

Bright Cluster Galaxy formation and the role of AGN feedback. Romain Teyssier

Bright 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 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

Structure and substructure in dark matter halos

Structure 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 information

On the influence of environment on star-forming galaxies

On the influence of environment on star-forming galaxies On the influence of environment on star-forming galaxies Lizhi Xie 谢利智 Tianjin Normal University; INAF-OATS Collaborators: G. De Lucia; F. Fontanot; D. Wilman; M. Fossati Galaxy properties correlate with

More information

The Tempest Simulations Milky Way-type Galaxies, their Environments and Progenitors

The Tempest Simulations Milky Way-type Galaxies, their Environments and Progenitors The Tempest Simulations Milky Way-type Galaxies, their Environments and Progenitors John Wise Brian O Shea (PI, MSU) David Collins (FSU), Cameron Hummels (Caltech), Devin Silvia (MSU), Britton Smith (SDSC)

More information

arxiv: v1 [astro-ph] 15 Oct 2007

arxiv: v1 [astro-ph] 15 Oct 2007 Mon. Not. R. Astron. Soc. 000, 1 6 (2002) Printed 22 January 2008 (MN LATEX style file v2.2) Bulges versus disks: the evolution of angular momentum in cosmological simulations of galaxy formation arxiv:0710.2901v1

More information

Star formation feedback in galaxy formation models. Yu Lu (KIPAC/Stanford)

Star formation feedback in galaxy formation models. Yu Lu (KIPAC/Stanford) Star formation feedback in galaxy formation models Yu Lu (KIPAC/Stanford) Overview Galaxies form in dark matter halos. CDM model predicts too many low-mass and high-mass halos. Feedback is needed to explain

More information

Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator)

Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator) Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator) The Gaia-ESO Survey http://www.gaia-eso.eu Public spectroscopic

More information

The 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 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 information

arxiv:astro-ph/ v2 9 Aug 2005

arxiv:astro-ph/ v2 9 Aug 2005 From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution Proceedings IAU Symposium No. 228, 2005 c 2005 International Astronomical Union V. Hill, P. François & F. Primas, eds. DOI: 00.0000/X000000000000000X

More information

Moore et al Kenney et al. 2004

Moore et al Kenney et al. 2004 Moore et al. 1996 Kenney et al. 2004 (i) Interaction with other cluster members and/or with the cluster potential (ii) Interactions with the hot gas that permeates massive galaxy systems. The influence

More information

Co-Evolution of Central Black Holes and Nuclear Star Clusters

Co-Evolution of Central Black Holes and Nuclear Star Clusters Co-Evolution of Central Black Holes and Nuclear Star Clusters Oleg Gnedin (University of Michigan) Globular clusters in the Galaxy median distance from the center is 5 kpc Resolved star cluster highest

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

Lecture 11: Ages and Metalicities from Observations A Quick Review

Lecture 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 information

Carbon Enhanced Metal Poor (CEMP) Stars and the Halo System of the Milky Way

Carbon Enhanced Metal Poor (CEMP) Stars and the Halo System of the Milky Way Carbon Enhanced Metal Poor (CEMP) Stars and the Halo System of the Milky Way Daniela Carollo Sydney Castiglione della Pescaia September 2013 Carbon Enhanced Metal Poor Stars (CEMP) CEMP = Carbon Enhanced

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

Metal Enrichment of the Circum- Galactic Medium around Massive Galaxies at Redshift 3

Metal Enrichment of the Circum- Galactic Medium around Massive Galaxies at Redshift 3 Metal Enrichment of the Circum- Galactic Medium around Massive Galaxies at Redshift 3 Sijing Shen (UCSC) Santa Cruz Galaxy Workshop August 2011 In collaboration with: Javiera Guedes (ETH), Piero Madau

More information

Lucio Mayer ETH Zwicky Prize Fellow

Lucio 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 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

Two Phase Formation of Massive Galaxies

Two 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 information

Gas accretion in Galaxies

Gas accretion in Galaxies Massive Galaxies Over Cosmic Time 3, Tucson 11/2010 Gas accretion in Galaxies Dušan Kereš TAC, UC Berkeley Hubble Fellow Collaborators: Romeel Davé, Mark Fardal, C.-A. Faucher-Giguere, Lars Hernquist,

More information

Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ M gas / dyn. Log SFR. Kennicutt Log. gas / dyn

Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ M gas / dyn. Log SFR. Kennicutt Log. gas / dyn Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ 0.017 M gas / dyn Log SFR Kennicutt 1998 Log gas / dyn Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Moster 2009 No Feedback 10% of baryons Log(

More information

The enrichment history of cosmic metals

The enrichment history of cosmic metals CHAPTER 5 The enrichment history of cosmic metals Robert P. C. Wiersma, Joop Schaye, Claudio Dalla Vecchia, C. M. Booth, Tom Theuns, and Anthony Aguirre Accepted for publication in the Monthly Notices

More information

METAL DIFFUSION IN SMOOTHED PARTICLE HYDRODYNAMICS SIMULATIONS OF DWARF GALAXIES

METAL DIFFUSION IN SMOOTHED PARTICLE HYDRODYNAMICS SIMULATIONS OF DWARF GALAXIES Draft version February 17, 216 Preprint typeset using L A TEX style emulateapj v. 5/2/11 METAL DIFFUSION IN SMOOTHED PARTICLE HYDRODYNAMICS SIMULATIONS OF DWARF GALAXIES David Williamson Département de

More information

Substructure in the Galaxy

Substructure 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 information

The Great Debate: The Size of the Universe (1920)

The Great Debate: The Size of the Universe (1920) The Great Debate: The Size of the Universe (1920) Heber Curtis Our Galaxy is rather small, with Sun near the center. 30,000 LY diameter. Universe composed of many separate galaxies Spiral nebulae = island

More information

Probing the history of star formation in the Local Group using the galactic fossil record

Probing the history of star formation in the Local Group using the galactic fossil record Probing the history of star formation in the Local Group using the galactic fossil record Brian O Shea (Michigan State University) Collaborators: Tim Beers, Carolyn Peruta, Monica Derris (MSU), Jason Tumlinson

More information

Abundance distribution in the Galactic thick disk

Abundance distribution in the Galactic thick disk Abundance distribution in the Galactic thick disk omas Bensby Lund Observatory, Department of Astronomy and eoretical Physics Discovery of thick disks (Burstein 1979, ApJ, 234, 829) Discovery of the Galactic

More information

Element abundance ratios and star formation quenching: satellite versus central galaxies

Element 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 information

arxiv: v2 [astro-ph.ga] 7 May 2018

arxiv: v2 [astro-ph.ga] 7 May 2018 The Origin of the Milky Way s Halo Age Distribution Daniela Carollo Center of Exellence for All Sky Astrophysics (CAASTRO) - Australia arxiv:1803.05154v2 [astro-ph.ga] 7 May 2018 INAF, Astrophysical Observatory

More information

Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars

Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars Properties of Nearby Stars Most in orbit with the Sun around Galactic Center Stellar Kinematics Reveal Groups of Stars with Common Space Motion (Moving

More information

THE BOLSHOI COSMOLOGICAL SIMULATIONS AND THEIR IMPLICATIONS

THE BOLSHOI COSMOLOGICAL SIMULATIONS AND THEIR IMPLICATIONS GALAXY FORMATION - Durham -18 July 2011 THE BOLSHOI COSMOLOGICAL SIMULATIONS AND THEIR IMPLICATIONS JOEL PRIMACK, UCSC ΛCDM Cosmological Parameters for Bolshoi and BigBolshoi Halo Mass Function is 10x

More information

Implementing sub-grid treatments of galactic outflows into cosmological simulations. Hugo Martel Université Laval

Implementing sub-grid treatments of galactic outflows into cosmological simulations. Hugo Martel Université Laval Implementing sub-grid treatments of galactic outflows into cosmological simulations Hugo Martel Université Laval Leiden, June 19, 2013 GALACTIC OUTFLOWS Optical image of galaxy (Hubble Space Telescope)

More information

THE GHZ OF THE MILKY WAY AND M31

THE GHZ OF THE MILKY WAY AND M31 THE GHZ OF THE MILKY WAY AND M31 FROM CHEMICAL EVOLUTION MODELS WITH GAS RADIAL FLOWS Emanuele Spitoni Department of Physics, University of Trieste Astronomical Observatory of Bologna, 10 April 2014 THE

More information

Svitlana Zhukovska Max Planck Institute for Astrophysics

Svitlana Zhukovska Max Planck Institute for Astrophysics Unveiling dust properties across galactic environments with dust evolution models Svitlana Zhukovska Max Planck Institute for Astrophysics Clare Dobbs (Uni Exeter), Ed Jenkins (Princeton Uni) Ralf Klessen

More information

Empirical Evidence for AGN Feedback

Empirical Evidence for AGN Feedback Empirical Evidence for AGN Feedback Christy Tremonti MPIA (Heidelberg) / U. Wisconsin-Madison Aleks Diamond-Stanic (U. Arizona), John Moustakas (NYU) Much observational and theoretical evidence supports

More information

Abundance Constraints on Early Chemical Evolution. Jim Truran

Abundance Constraints on Early Chemical Evolution. Jim Truran Abundance Constraints on Early Chemical Evolution Jim Truran Astronomy and Astrophysics Enrico Fermi Institute University of Chicago Argonne National Laboratory MLC Workshop Probing Early Structure with

More information

Mergers and Mass Assembly of Dark Matter Halos & Galaxies

Mergers and Mass Assembly of Dark Matter Halos & Galaxies Mergers and Mass Assembly of Dark Matter Halos & Galaxies Chung-Pei Ma Onsi Fakhouri James McBride (UC Berkeley) Mike Boylan-Kolchin (MPA --> Southern UC) Claude-Andre Faucher-Giguere Dusan Keres (Harvard

More information

Cosmic Structure Formation on Supercomputers (and laptops)

Cosmic Structure Formation on Supercomputers (and laptops) Cosmic Structure Formation on Supercomputers (and laptops) Lecture 4: Smoothed particle hydrodynamics and baryonic sub-grid models Benjamin Moster! Ewald Puchwein 1 Outline of the lecture course Lecture

More information

Galaxy Evolution. Part 4. Jochen Liske Hamburger Sternwarte

Galaxy Evolution. Part 4. Jochen Liske Hamburger Sternwarte Galaxy Evolution Part 4 Jochen Liske Hamburger Sternwarte jochen.liske@uni-hamburg.de Astronomical picture of the week NGC 1275 Central galaxy of the Perseus cluster Active Source: APOD Astronomical picture

More information

Violent Disk Instability at z=1-4 Outflows; Clump Evolution; Compact Spheroids

Violent Disk Instability at z=1-4 Outflows; Clump Evolution; Compact Spheroids Violent Disk Instability at z=1-4 Outflows; Clump Evolution; Compact Spheroids Avishai Dekel The Hebrew University of Jerusalem Santa Cruz, August 2013 stars 5 kpc Outline 1. Inflows and Outflows 2. Evolution

More information

Fossils 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 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 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

Astr 5465 March 6, 2018 Abundances in Late-type Galaxies Spectra of HII Regions Offer a High-Precision Means for Measuring Abundance (of Gas)

Astr 5465 March 6, 2018 Abundances in Late-type Galaxies Spectra of HII Regions Offer a High-Precision Means for Measuring Abundance (of Gas) Astr 5465 March 6, 2018 Abundances in Late-type Galaxies Spectra of HII Regions Offer a High-Precision Means for Measuring Abundance (of Gas) Emission lines arise from permitted (recombination) and forbidden

More information

Schmidt-Kennicutt relations in SPH simulations of disc galaxies with effective SN thermal feedback

Schmidt-Kennicutt relations in SPH simulations of disc galaxies with effective SN thermal feedback Schmidt-Kennicutt relations in SPH simulations of disc galaxies with effective SN thermal feedback Pierluigi Monaco Università di Trieste & INAF-Osservatorio Astronomico di Trieste In collaboration with:

More information

Simulating Feedback-Driven Galactic Chemical Evolution with Individual Stars

Simulating Feedback-Driven Galactic Chemical Evolution with Individual Stars Simulating Feedback-Driven Galactic Chemical Evolution with Individual Stars Andrew Emerick Blue Waters Fellow NSF Graduate Research Fellow Greg Bryan Mordecai-Mark Mac Low Emerick + 18a (submitted) Emerick

More information

Multiwavelength observation campaign of Mrk 509: UV spectra of the X-ray Outflow!!!!Gerard Kriss!! STScI!!! (with N. Arav, J. Kaastra & the Mrk 509

Multiwavelength observation campaign of Mrk 509: UV spectra of the X-ray Outflow!!!!Gerard Kriss!! STScI!!! (with N. Arav, J. Kaastra & the Mrk 509 Multiwavelength observation campaign of Mrk 509: UV spectra of the X-ray Outflow!!!!Gerard Kriss!! STScI!!! (with N. Arav, J. Kaastra & the Mrk 509 Team)!! The Influence of AGN Outflows! «They may affect

More information

Dwarf Spheroidal Galaxies : From observations to models and vice versa. Yves Revaz

Dwarf Spheroidal Galaxies : From observations to models and vice versa. Yves Revaz Dwarf Spheroidal Galaxies : From observations to models and vice versa Yves Revaz The good reasons to study dsphs : Test for the LCDM paradigm : small structures are predicted in abundance Galaxy luminosity

More information