Uncertainties in Chemical Enrichment Models
|
|
|
- Tracey Simpson
- 5 years ago
- Views:
Transcription
1 Uncertainties in Chemical Enrichment Models CLUES Cas A M82 Benoit Côté (Christian Ritter, Falk Herwig, Brian O Shea) JINA Frontiers Meeting March 2015
2 Galactic Outflow M82 Abell 1689 Stripping and Disruption NGC 4676 Galaxy with a SFH Simple Stellar Population Individual Stars NGC 7293 NGC 4449 Cas A Tycho SN Nuclear Physics WR 124 Denissenkov (2012)
3 Galactic Outflow M82 Abell 1689 Stripping and Disruption NGC 4676 Galaxy with a SFH Simple Stellar Population Individual Stars NGC 7293 NGC 4449 Cas A Tycho SN Nuclear Physics WR 124 Denissenkov (2012)
4 Galactic Outflow M82 Abell 1689 Benoit Côté Stripping and Disruption NGC 4676 Galaxy with a SFH Simple Stellar Population Individual Stars NGC 7293 NGC 4449 Cas A Tycho SN Nuclear Physics WR 124 Denissenkov (2012)
5 Quick Overview of my Ph.D. Hugo Martel 40 Mpc Ph.D. project : Develop a semi-analytic model (SAM) that is going to be used as a sub-grid treatment to generate the evolution of galaxies in a cosmological simulation. 40 Mpc Dark Matter SAM (galaxy) Gas Galaxy
6 Quick Overview of my Ph.D. Hugo Martel 40 Mpc Ph.D. project : Develop a semi-analytic model (SAM) that is going to be used as a sub-grid treatment to generate the evolution of galaxies in a cosmological simulation. 40 Mpc Dark Matter SAM (galaxy) Gas Galaxy Côté et al. (2015)
7 Quick Overview of my Ph.D. Hugo Martel 40 Mpc Ph.D. project : Develop a semi-analytic model (SAM) that is going to be used as a sub-grid treatment to generate the evolution of galaxies in a cosmological simulation. 40 Mpc Dark Matter Gas Galactic Outflow Galaxy Côté et al. (2015)
8 Quick Overview of my Ph.D. Hugo Martel 40 Mpc Ph.D. project : Develop a semi-analytic model (SAM) that is going to be used as a sub-grid treatment to generate the evolution of galaxies in a cosmological simulation. 40 Mpc Gas Dark Matter How certain are we about the amount of chemical elements injected in those simulations? Galactic Outflow Galaxy Côté et al. (2015)
9 Hierarchical Growth of Uncertainties Relative uncertainty scale Nuclear Reaction Rates Stellar Hydro More uncertain results Stellar Model Stellar Population Galaxy Model Cosmological Model Model
10 Goal of the Current Project Relative uncertainty scale Nuclear Reaction Rates Stellar Hydro More uncertain results Stellar Model Stellar Population Galaxy Model Cosmological Model Model Connect stellar models and nuclear physics to a galaxy model
11 Goal of the Current Project Relative uncertainty scale Nuclear Reaction Rates Stellar Hydro More uncertain results Stellar Model Stellar Population Galaxy Model Cosmological Model Model Connect stellar models and nuclear physics to a galaxy model How the predicted chemical evolution of galaxies is affected by assumptions in stellar models Explosion prescription Mixing processes Mass-loss
12 Goal of the Current Project Relative uncertainty scale Nuclear Reaction Rates Stellar Hydro More uncertain results Stellar Model Stellar Population Galaxy Model Cosmological Model Model Connect stellar models and nuclear physics to a galaxy model How the predicted chemical evolution of galaxies is affected by assumptions in stellar models Explosion prescription Mixing processes Mass-loss How the predicted chemical evolution of galaxies is affected by uncertainties in nuclear physics Nuclear reaction rates
13 Connecting Stellar Models to a Galaxy Model Cas A WR 124 NGC 7293 Tycho SN + IMF Stellar lifetimes = Stellar yields SSP yields SYGMA (Stellar Yields for Galactic Modelling Application) See Christian Ritter s talk at 11:30 C. Ritter C. Fryer F. Herwig J. F. Navarro E. Starkenburg M. Pignatari S. Jones K. Venn P. A. Denissenkov B. Côté the collaboration
14 Connecting Stellar Models to a Galaxy Model Cas A WR 124 NGC 7293 Tycho SN + IMF Stellar lifetimes = Stellar yields SSP yields SYGMA (Stellar Yields for Galactic Modelling Application) See Christian Ritter s talk at 11:30 Many SSPs SFR (SYGMA) NGC Inflows Outflows = Time Star formation history Simple 1-zone galaxy OMEGA (One-zone Model for the Evolution of GAlaxies)
15 Uncertainties in SYGMA and OMEGA Upcoming project O Shea & Côté SYGMA OMEGA
16 Uncertainties in SYGMA and OMEGA Upcoming project O Shea & Côté SYGMA OMEGA Milky Way
17 Uncertainties in SYGMA and OMEGA Upcoming project O Shea & Côté SYGMA OMEGA Milky Way 200 runs with random parameters
18 Uncertainties in SYGMA and OMEGA Upcoming project O Shea & Côté SYGMA OMEGA Milky Way Galaxy Closed Model 200 runs with random parameters
19 Uncertainties in SYGMA and OMEGA Upcoming project O Shea & Côté SYGMA OMEGA Inflow Outflow Milky Way Galaxy Open Model 200 runs with random parameters
20 Core-Collapse SNe Prescription Core-Collapse SNe Z = Initial stellar mass > Chieffi & Limongi (2004) Initial stellar mass > Nomoto et al. (2006) Initial stellar mass > E E E E E E E E E E E E-04
21 Core-Collapse SNe Prescription Core-Collapse SNe Z = Initial stellar mass > Chieffi & Limongi (2004) Initial stellar mass > Nomoto et al. (2006) Initial stellar mass > E E E E E E E E E E E E-04
22 Core-Collapse SNe Prescription Core-Collapse SNe Z = Initial stellar mass > Fryer et al. (2012) Chieffi & Limongi (2004) Initial stellar mass > Nomoto et al. (2006) Initial stellar mass > E E E E E E E E E E E E-04
23 Core-Collapse SNe Prescription
24 Core-Collapse SNe Prescription N06
25 Core-Collapse SNe Prescription N06
26 Core-Collapse SNe Prescription Solid Dashed No ejecta for [30,100] Last model used for [30,100] N06
27 Core-Collapse SNe Prescription Solid Dashed No ejecta for [30,100] Last model used for [30,100] N06
28 Core-Collapse SNe Prescription Solid Dashed No ejecta for [30,100] Last model used for [30,100] N06 N06 Last model used for [30,100]
29 Uncertainties in Nuclear Reaction Rates Low-mass TP-AGB models Herwig et al. (2005)
30 Uncertainties in Nuclear Reaction Rates Low-mass TP-AGB models Herwig et al. (2005)
31 Conclusion Relative uncertainty scale O Shea & Côté SYGMA OMEGA Next Steps Create new sets of yields with different physical assumptions (explosion prescription, internal mixing, mass-loss, ) Create new sets of yields with different nuclear reaction rates Ultimate Goal Provide better estimates of the uncertainties related to the predicted chemical enrichment at galactic and cosmological scales
32 Conclusion Chemical Evolution in Galaxies Un-conference this afternoon Relative uncertainty scale O Shea & Côté SYGMA OMEGA Next Steps Create new sets of yields with different physical assumptions (explosion prescription, internal mixing, mass-loss, ) Create new sets of yields with different nuclear reaction rates Ultimate Goal Provide better estimates of the uncertainties related to the predicted chemical enrichment at galactic and cosmological scales
33 Open and Closed Models Galaxy Closed Model Inflow Outflow Galaxy Open Model
34 Open and Closed Models Shift toward higher [Fe/H] Dilution (inflows) Smaller gas reservoir Small initial gas reservoir Outflows Shift toward lower [Fe/H] Stronger outflows
Chemical Evolution and the Mass Function of Stellar Mass Black Holes
.. and Neutron Stars Chemical Evolution and the Mass Function of Stellar Mass Black Holes Benoit Côté Postdoctoral Fellow Collaborators C. Fryer, K. Belczynski, B. O Shea, C. Ritter, F. Herwig, M. Pignatari,
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)
THE ENERGY OF STARS NUCLEAR ASTROPHYSICS THE ORIGIN OF THE ELEMENTS
THE ENERGY OF STARS NUCLEAR ASTROPHYSICS THE ORIGIN OF THE ELEMENTS Stellar Energy Origin of the Elements Nuclear Astrophysics Astrophysics Nuclear Physics ROBERT D ESCOURT ATKINSON (1931) 1942 β MeV
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
arxiv: v2 [astro-ph.ga] 7 Dec 2016
![arxiv: v2 [astro-ph.ga] 7 Dec 2016](/thumbs/93/113587210.jpg "arxiv: v2 [astro-ph.ga] 7 Dec 2016")
Draft version December 8, 2016 Preprint typeset using L A TEX style emulateapj v. 01/23/15 THE IMPACT OF MODELING ASSUMPTIONS IN GALACTIC CHEMICAL EVOLUTION MODELS Benoit Côté, 1,2,5,6 Brian W. O Shea,
The Evolution and Explosion of Mass-Accreting Pop III Stars. Ken Nomoto (IPMU / U.Tokyo)
The Evolution and Explosion of Mass-Accreting Pop III Stars Ken Nomoto (IPMU / U.Tokyo) Pop III Stars Pop III GRBs Pop III SNe? M > 10 5 M :SMS (Super Massive Stars) GR instability Collapse M ~ 300-10
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
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
Cat's Eye Nebula, APOD 4 Sep 02, Corradi & Goncalves. Falk Herwig:»Nuclear Astrophysics with Neutron Facilities«MSU - 14 Feb 05
Cat's Eye Nebula, APOD 4 Sep 02, Corradi & Goncalves Nuclear Astrophysics with Neutron Facilities Falk Herwig Los Alamos National Laboratory, New Mexico, USA Theoretical Astrophysics and Los Alamos Neutron
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
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
Modeling abundances! in star forming galaxies!
Modeling abundances! in star forming galaxies! Chemical Enrichment Q [Fe/H] and [X/Fe] evolve in a galaxy: fossils that retain the evolution history of the galaxy Galactic Archaeology! 3 types of galaxy
formation and evolution of high-z dust
formation and evolution of high-z dust Raffaella Schneider INAF/Osservatorio Astronomico di Roma the FIRST team and collaborators Matteo Alparone, student Matteo de Bennassuti, PhD Michele Ginolfi, PhD
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
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(
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
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
Galac%c Halo. Open Cluster
Galac%c Bulge Galac%c Halo Globular Cluster Open Cluster Dwarf Galaxies Pre Solar Grains Galac%c Disk Planetary Nebulae Supernovae HII Regions QSO Distribu%on of masses at birth In general, stellar masses
Asymptotic Giant Branch stars
Asymptotic Giant Branch stars Falk Herwig Los Alamos National Laboratory Theoretical Astrophysics Group LA Neutron Science Center Falk Herwig, May 8, 2006, 1 Introduction: AGB evolution NGC 6826 (Balick
Hybrid C-O-Ne White Dwarfs as Progenitors of Diverse SNe Ia
Hybrid C-O-Ne White Dwarfs as Progenitors of Diverse SNe Ia Department of Physics & Astronomy, University of Victoria, P.O. Box 1700, STN CSC, Victoria, B.C., V8W 2Y2, Canada; The Joint Institute for Nuclear
in 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
Recent Progress in Modeling of Galaxy Formation. Oleg Gnedin (University of Michigan)
Recent Progress in Modeling of Galaxy Formation Oleg Gnedin (University of Michigan) In current simulations, galaxies look like this: 10 kpc Disk galaxy at z=3: stars, molecular gas, atomic gas (Zemp,
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
Massive black hole formation in cosmological simulations
Institut d Astrophysique de Paris IAP - France Massive black hole formation in cosmological simulations Mélanie HABOUZIT Marta Volonteri In collaboration with Yohan Dubois Muhammed Latif Outline Project:
MAURIZIO SALARIS AGB STARS STRUCTURE 2 nd dredge up only for masses above ~4 M Early AGB Thermal pulses M=2.0M Z=0.02 Weiss & Ferguson (2009) HOT BOTTOM BURNING The minimum mass for HBB decreases with
Dust Formation History with Galaxy Evolution
Dust Formation History with Galaxy Evolution Tsutomu T. TAKEUCHI Division of Particle and Astrophysical Science, Nagoya University, Japan ESTEC, 14 Nov., 2014, the Netherlands 1. Introduction What are
How environment shapes galaxy evolution: the satellite galaxies' perspective
How environment shapes galaxy evolution: the satellite galaxies' perspective Anna Pasquali Astronomisches Rechen Institut, Zentrum für Astronomie der Universität Heidelberg NGC 4651 Why do we care? At
Nucleosynthesis in heliumenriched
Nucleosynthesis in heliumenriched stars Amanda Karakas With Anna Marino and David Nataf Outline 1. The effect of helium enrichment on the evolution and nucleosynthesis of lowmetallicity AGB models 2. The
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
Dust production by various types of supernovae
Dust production by various types of supernovae Takaya Nozawa ( 野沢貴也 ) IPMU, University of Tokyo, Kashiwa, Japan Collaborators: T. Kozasa (Hokkaido Univ.), N. Tominaga (Konan Univ.) K. Maeda, M. Tanaka,
A Zoo of Ancient Stellar Relics in our Galactic Halo
A Zoo of Ancient Stellar Relics in our Galactic Halo Simon W. Campbell1,2 1) GAA, Dept. Fisica i Enginyeria Nuclear, Universitat Politecnica de Catalunya 2) CSPA, Australia (Centre for Stellar and Planetary
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
arxiv:astro-ph/ v2 28 Apr 2005
Mon. Not. R. Astron. Soc. 000, 1 8 (2004) Printed 2 February 2008 (MN LATEX style file v1.4) Early chemical enrichment of the universe and the role of very massive pop III stars arxiv:astro-ph/0502487v2
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
The evolution of supernova progenitors
The evolution of supernova progenitors NuGrid (p,n) (γ,α) (n,α) (α,γ) (γ,p) (n,p) Samuel Jones University of Victoria In collaboration with: R. Hirschi (Keele U), K. Nomoto (Kavli IPMU), F. Herwig (UVic),
A synthetic model of the gravitational wave background from evolving binary compact objects
A synthetic model of the gravitational wave background from evolving binary compact objects Irina Dvorkin, Jean-Philippe Uzan, Elisabeth Vangioni, Joe Silk (Institut d Astrophysique de Paris) [arxiv:1607.06818]
Environment and the Formation of Globular Cluster Systems
Environment and the Formation of Globular Cluster Systems Eric Peng Peking University, Dept of Astronomy Kavli Institute for Astronomy and Astrophysics Peking University (PKU) in Beijing, China China s
Simulations of First Star Formation
Simulations of First Star Formation Michael L. Norman (UCSD) Brian O Shea (LANL) 1 Formation of the first stars: current paradigm (Abel et al. 2002, Bromm et al. 2002,Yoshida et al. 2006) DM halos of M~10
The Pop III/II Transition
The First Stars and Galaxies: Challenges for the Next Decade March 8-11, 2010 Austin, Texas The Pop III/II Transition Raffaella Schneider INAF/Osservatorio Astrofisico di Arcetri What are the minimal conditions
Chemo-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
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
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:
Supernova feedback in the smallest Milky Way satellites
Supernova feedback in the smallest Milky Way satellites Donatella Romano INAF Osservatorio Astronomico di Bologna Collaborators: F. Calura, C. G. Few, A. D Ercole Scientific Rationale: Our view of the
The Trieste galaxy formation group
The Trieste galaxy formation group P. Monaco, F. Fontanot, G. De Lucia, G. Murante, S. Borgani, G. Granato, L. Silva Semi-analytic models (De Lucia, Fontanot, Monaco + Xie, Zoldan) Hydro simulations of
The Illustris simulation: a new look at galaxy black hole co-evolution. Debora Sijacki IoA & KICC Cambridge
The Illustris simulation: a new look at galaxy black hole co-evolution Debora Sijacki IoA & KICC Cambridge LSS conference July 23 2015 Cosmological simulations of galaxy and structure formation Hierarchical
Impact of Type Ia Supernova Ejecta on Binary Companions
Impact of Type Ia Supernova Ejecta on Binary Companions Speaker: Kuo-Chuan Pan (ASTR) Charm++ Workshop, April 18, 2011 1 [Dept. of Astronomy] Advisor: Prof. Paul Ricker Collaborator: Prof. Ronald Taam
Supernovae as sources of interstellar dust
Supernovae as sources of interstellar dust Takaya Nozawa (IPMU, University of Tokyo) Collaborators; T. Kozasa, A. Habe (Hokkaido Univ.), M. Tanaka, K. Maeda, K. Nomoto (IPMU) N. Tominaga (Konan Univ.),
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
Identifying Progenitors of Stripped-Envelope Supernovae
Identifying Progenitors of Stripped-Envelope Supernovae Gastón Folatelli Instituto de Astrofísica de La Plata (IALP), CONICET, Argentina Aug 11th, 2016 Collaborators: S. Van Dyk, H. Kuncarayakti, K. Maeda,
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
Growing and merging massive black holes
Growing and merging massive black holes Marta Volonteri Institut d Astrophysique de Paris S. Cielo (IAP) R. Bieri (MPA) Y. Dubois (IAP) M. Habouzit (Flatiron Institute) T. Hartwig (IAP) H. Pfister (IAP)
Optical/IR Counterparts of GW Signals (NS-NS and BH-NS mergers)
Optical/IR Counterparts of GW Signals (NS-NS and BH-NS mergers) Chris Belczynski 1,2 1 Warsaw University Observatory 2 University of Texas, Brownsville Theoretical Rate Estimates (MOSTLY NS-NS MERGERS:
PUSHing CORE-COLLAPSE SUPERNOVAE TO EXPLOSIONS IN SPHERICAL SYMMETRY
PUSHing CORE-COLLAPSE SUPERNOVAE TO EXPLOSIONS IN SPHERICAL SYMMETRY Fifty-One Ergs Oregon State June 2017 Ebinger In collaboration with: Sanjana Sinha Carla Fröhlich Albino Perego Matthias Hempel Outline
Supernova and Star Formation Rates
Supernova and Star Formation Rates Enrico Cappellaro Istituto Nazionale di Astrofisica Osservatorio Astronomico di Padova SN vs. SF rates Kennicutt 1998 SFR vs. galaxy color from evolutionary synthesis
arxiv: v1 [astro-ph] 28 Nov 2008
![arxiv: v1 [astro-ph] 28 Nov 2008](/thumbs/83/87224443.jpg "arxiv: v1 [astro-ph] 28 Nov 2008")
arxiv:0811.4648v1 [astro-ph] 28 Nov 2008 Nucleosynthesis Calculations from Core-Collapse Supernovae, Patrick Young ac, Michael Bennett ad, Steven Diehl abe, Falk Herwig adg, Raphael Hirschi ad, Aimee Hungerford
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
The First Black Holes and. their Host Galaxies. John Wise
The First Black Holes and John Wise Chao Shi (GT), Pengfei Chen (UCSD), Ayçin Aykutalp (GT), Tom Abel (Stanford), Peter Johansson (Helsinki), Michael Norman (UCSD), Brian O Shea (MSU), John Regan (Helsinki),
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
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
Structure and Evolution of Massive Stars (and of the less massive ones also...) Ana Palacios, LUPM / Université de Montpellier
Structure and Evolution of Massive Stars (and of the less massive ones also...) Ana Palacios, LUPM / Université de Montpellier The Hertzsprung Russell diagram New reduction fo Hipparcos Catalog The evolutionary
Globular cluster formation with multiple stellar populations: self-enrichment in fractal massive molecular clouds
Advance Access publication 2017 April 27 doi:10.1093/mnras/stx982 Globular cluster formation with multiple stellar populations: self-enrichment in fractal massive molecular clouds Kenji Bekki ICRAR M468
PATRICIA 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
CONSTRAINING THE FINAL FATES OF MASSIVE STARS BY OXYGEN AND IRON ENRICHMENT HISTORY IN THE GALAXY
Draft version December 7, 2017 Preprint typeset using L A TEX style AASTeX6 v. 1.0 CONSTRAINING THE FINAL FATES OF MASSIVE STARS BY OXYGEN AND IRON ENRICHMENT HISTORY IN THE GALAXY AKIHIRO SUZUKI 1 and
The first phases of life of stars in Globular Clusters: an example of the problems of modern stellar structure computation
Mem. S.A.It. Suppl. Vol. 3, 64 c SAIt 2003 Memorie della Supplementi The first phases of life of stars in Globular Clusters: an example of the problems of modern stellar structure computation Francesca
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:
arxiv:astro-ph/ v1 31 Jul 1998
Cosmic Star Formation from the Milky Way and its Satellites arxiv:astro-ph/973v1 31 Jul 199 F.D.A. Hartwick Department of Physics and Astronomy, University of Victoria, Victoria, BC, Canada, VW 3P Abstract.
GALACTIC Al 1.8 MeV GAMMA-RAY SURVEYS WITH INTEGRAL
Proceedings of the 3rd Galileo Xu Guangqi Meeting International Journal of Modern Physics: Conference Series Vol. 23 (2013) 48 53 c World Scientific Publishing Company DOI: 10.1142/S2010194513011069 GALACTIC
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
What Doesn t Quench Galaxy Formation?
What Doesn t Quench Galaxy Formation? Phil Hopkins Dusan Keres, Claude Faucher-Giguere, Jose Onorbe, Freeke van de Voort, Sasha Muratov, Xiangcheng Ma, Lena Murchikova, Norm Murray, Eliot Quataert, James
Spectrum of the Supernova Relic Neutrino Background
Spectrum of the Supernova Relic Neutrino Background Ken ichiro Nakazato (Tokyo University of Science) Numazu Workshop 2015, Sep. 1, 2015 Outline 1. Introduction Neutrino signal from supernovae Supernova
Ultra High Energy Cosmic Rays. UHECRs from Mildly Relativistic Supernovae
Ultra High Energy Cosmic Rays from Mildly Relativistic Supernovae Tata Institute of Fundamental Research Mumbai, India March 13, 2012 Outline UHECRS Chakraborti, Ray, Soderberg, Loeb, Chandra 2011 Nature
The Monash Chemical Yields Project
The Monash Chemical Yields Project Carolyn Doherty (Konkoly Observatory) George Angelou Simon W. Campbell Ross Church Thomas Constantino Sergio Cristallo Pilar Gil Pons Amanda Karakas John Lattanzio Maria
Correlations between stellar dynamics and metallicity in the discs
Correlations between stellar dynamics and metallicity in the discs Semi-analytic chemodynamical model of the Milky Way Jan Rybizki (Supervisor: Andreas Just) Astronomisches Rechen-Institut - Zentrum für
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
Lecture 11: Ages and Metalicities from Observations. A Quick Review. Multiple Ages of stars in Omega Cen. Star Formation History.
Ages from main-sequence turn-off stars Lecture 11: Main sequence lifetime: Ages and Metalicities from Observations R diagram lifetime = fuel / burning rate MV *1 M ' L ' MS = 7 10 9 ) ) M. ( L. ( A Quick
Stellar Dynamics and Structure of Galaxies
Stellar Dynamics and Structure of Galaxies. Spherically symmetric objects Vasily Belokurov vasily@ast.cam.ac.uk Institute of Astronomy Lent Term 2016 1 / 21 Outline I 1 2 Globular of galaxies 2 / 21 Why
The Old Stellar Population Studies with Subaru Young-Wook Lee Yonsei Univ., Seoul, Korea
(Some humble suggestions for) The Old Stellar Population Studies with Subaru Young-Wook Lee Yonsei Univ., Seoul, Korea 1. Globular cluster Dwarf galaxy Connection (Some) Globular clusters show multiple
Overview. Metals in the Intergalactic Medium at z 6: Pop III Stars or Normal Star-Forming Galaxies? p.2/26
p.1/26 Overview Metals in the Intergalactic Medium at z 6: Pop III Stars or Normal Star-Forming Galaxies? p.2/26 Overview Metals in the Intergalactic Medium at z 6: Pop III Stars or Normal Star-Forming
Galactic Winds in Starburst Irregular Galaxies
Chemical Enrichment of Intracluster and Intergalactic Medium ASP Conference Series, Vol. **VOLUME**, 2001 Francesca Matteucci and Roberto Fusco-Femiano Eds. Galactic Winds in Starburst Irregular Galaxies
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
The impact of stellar rotation on the CNO abundance patterns in the Milky Way at low metallicities
The impact of stellar rotation on the CNO abundance patterns in the Milky Way at low metallicities Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I - 34131 Trieste, Italia E-mail: Christina.Chiappini@obs.unige.ch
The First Stars and their Impact on Cosmology
The First Stars and their Impact on Cosmology V. Bromm University of Texas, Austin, TX 78712, USA Within variants of the cold dark matter model of cosmological structure formation, the first sources of
Part two of a year-long introduction to astrophysics:
ASTR 3830 Astrophysics 2 - Galactic and Extragalactic Phil Armitage office: JILA tower A909 email: pja@jilau1.colorado.edu Spitzer Space telescope image of M81 Part two of a year-long introduction to astrophysics:
AGN Feedback In an Isolated Elliptical Galaxy
AGN Feedback In an Isolated Elliptical Galaxy Feng Yuan Shanghai Astronomical Observatory, CAS Collaborators: Zhaoming Gan (SHAO) Jerry Ostriker (Princeton) Luca Ciotti (Bologna) Greg Novak (Paris) 2014.9.10;
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)
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
GALACTIC CHEMICAL EVOLUTION N. Prantzos (Institut d Astrophysique de Paris)
GALACTIC CHEMICAL EVOLUTION N. Prantzos (Institut d Astrophysique de Paris) I) INTRODUCTION TO GALACTIC CHEMICAL EVOLUTION II) III) A CASE STUDY: THE SOLAR NEIGHBORHOOD THE MILKY WAY HALO: FROM C TO Zn
Feedback 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
Deriving stellar masses from SDSS
Deriving stellar masses from SDSS Reference: Bruzual and Charlot 2003MNRAS.344.1000B Kauffmann et al. 2003MNRAS.341.33 Salim et al. 2007ApJS..173..267S Bell et al. 2003ApJS..149..289B Outline! Basic idea!
Chapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
Globular Clusters: a chemical roadmap between anomalies and homogeneity ALESSIO MUCCIARELLI
Globular Clusters: a chemical roadmap between anomalies and homogeneity ALESSIO MUCCIARELLI Physics & Astronomy Department University of Bologna (Italy) !.5(year.project.!.Advanced(Research(Grant(funded.by.the.European.Research.Council.(ERC).!.PI:.Francesco.R..Ferraro.(Dip..of.Physics.&.Astronomy..Bologna.University).!.AIM:.to#understand#the#complex#interplay#between#dynamics#&#stellar#evolu7on#!.HOW:.using.globular#clusters#as.cosmic.laboratories.and.....Blue#Straggler#Stars#
Observations of galaxy evolution. Pieter van Dokkum
Observations of galaxy evolution Pieter van Dokkum Overview Broad topic! Split in three conceptually-different parts: ç ç low redshift high redshift 1. Census: what is out there? N (z, L, Mstars, Mdark,
The Giant Branches. Stellar evolution of RGB and AGB stars. Importance, features, uncertainties
The Giant Branches Stellar evolution of RGB and AGB stars Importance, features, uncertainties Achim Weiss (Max-Planck-Institut für Astrophysik, Garching) M5 (Rosenberg et al. 2000) Giant Branches MACHO
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
Einführung in die Astronomie II
Einführung in die Astronomie II Teil 10 Peter Hauschildt yeti@hs.uni-hamburg.de Hamburger Sternwarte Gojenbergsweg 112 21029 Hamburg 15. Juni 2017 1 / 47 Overview part 10 Death of stars AGB stars PNe SNe
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
HST & 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),
r-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
Origin and Evolution of Disk Galaxy Scaling Relations
Origin and Evolution of Disk Galaxy Scaling Relations Aaron A. Dutton (CITA National Fellow, University of Victoria) Collaborators: Frank C. van den Bosch (Utah), Avishai Dekel (HU Jerusalem), + DEEP2
Studying stars in M31 GCs using NIRI and GNIRS
Studying stars in M31 GCs using NIRI and GNIRS Ricardo Schiavon Gemini Observatory GSM 2012 San Francisco July 19, 2012 Collaborators Andy Stephens (Gemini) Nelson Caldwell (SAO) Matthew Shetrone (HET)