Simulating the Cooling Flow of Cool-Core Clusters Yuan Li Advisor: Greg Bryan Department of Astronomy, Columbia University July 2011.

Slides:



Advertisements
Similar presentations
AGN Feedback at the Parsec Scale Feng Yuan Shanghai Astronomical Observatory, CAS with: F. G. Xie (SHAO) J. P. Ostriker (Princeton University) M. Li (SHAO)
Advertisements

arvard.edu/phot o/2007/m51/. Confronting Stellar Feedback Simulations with Observations of Hot Gas in Elliptical Galaxies Q. Daniel Wang,
GALAXIES IN DIFFERENT ENVIRONMENTS: VOIDS TO CLUSTERS:  Simulations will require to model full physics:  Cooling, heating, star formation feedbacks…
X-Ray Measurements of the Mass of M87 D. Fabricant, M. Lecar, and P. Gorenstein Astrophysical Journal, 241: , 15 October 1980 Image:
Entropy in the ICM Institute for Computational Cosmology University of Durham Michael Balogh.
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.
Theoretical Perspectives Amr El-Zant Canadian Institute for Theoretical Astrophysics.
The Regulation of Star Formation by AGN Feedback D AVID R AFFERTY (Penn State / Ohio U.) Collaborators: Brian McNamara (Waterloo) and Paul Nulsen (CfA)
HOT TIMES FOR COOLING FLOWS Mateusz Ruszkowski. Cooling flow cluster Non-cooling flow cluster gas radiates X-rays & loses pressure support against gravity.
Prospects and Problems of Using Galaxy Clusters for Precision Cosmology Jack Burns Center for Astrophysics and Space Astronomy University of Colorado,
Radio galaxies in the Chandra Era, Boston, July 2008 Shock heating in the group atmosphere of the radio galaxy B A Nazirah Jetha 1, Martin Hardcastle.
Simon Portegies Zwart (Univ. Amsterdam with 2 GRAPE-6 boards)
Magnetic Jets and Lobes in Cosmological MHD Hui Li Los Alamos National Laboratory NSF/DOE Center for Magnetic Self-Organization (CMSO) Collaborators: H.
How Do Supermassive Black Holes Get Starved? Q. D. Wang, Z. Y. Li, S.-K. Tang University of Massachusetts B. Wakker University of Wisconsin.
Numerical Modeling of Hierarchical Galaxy Formation Cole, S. et al. 2000, MNRAS 319, Adam Trotter December 4, 2007 Astronomy 704, UNC-Chapel Hill,
Cosmological N-body simulations of structure formation Jürg Diemand, Ben Moore and Joachim Stadel, University of Zurich.
Krakow 2010 Galactic magnetic fields: MRI or SN-driven dynamo? Detlef Elstner Oliver Gressel Natali Dziourkevich Alfio Bonanno Günther Rüdiger.
Cosmological MHD Hui Li Collaborators: S. Li, M. Nakamura, S. Diehl, B. Oshea, P. Kronberg, S. Colgate (LANL) H. Xu, M. Norman (UCSD), R. Cen (Princeton)
Galaxy Clusters Perseus Cluster in X-rays. Why study clusters? Clusters are the largest virialized objects in the Universe. Cosmology: tail of density.
PRESIDENCY UNIVERSITY
THE STRUCTURE OF COLD DARK MATTER HALOS J. Navarro, C. Frenk, S. White 2097 citations to NFW paper to date.
Estimate* the Total Mechanical Feedback Energy in Massive Clusters Bill Mathews & Fulai Guo University of California, Santa Cruz *~ ±15-20% version 2.
A Critical Role for Viscosity in the Radio Mode AGN Feedback Cycle Paul Nulsen Harvard-Smithsonian Center for Astrophysics 2014 July 9X-ray View of Galaxy.
The Physics of the ICM core: Conduction, the HBI, and cold filaments Chris Reynolds (UMd) with… Mark Avara (UMd) Steve Balbus (Oxford) Tamara Bogdanovic.
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,
Cosmological formation of elliptical galaxies * Thorsten Naab & Jeremiah P. Ostriker (Munich, Princeton) T.Naab (USM), P. Johannson (USM), J.P. Ostriker.
SEARCHING FOR COOLING FLOWS… Silvia Caffi IASF/CNR Sez. Milano.
J. Cuadra – Accretion of Stellar Winds in the Galactic Centre – IAU General Assembly – Prague – p. 1 Accretion of Stellar Winds in the Galactic Centre.
Subgrid models of active galactic nuclei in clusters of galaxies Paul Matthew Sutter Paul M. Ricker Univ. of Illinois at Urbana-Champaign Frontiers in.
AGN Feedback Heating in Clusters of Galaxies
1 Does AGN “Feedback” in Galaxy Clusters Work? Dave De Young NOAO Girdwood AK May 2007.
Studying AGN feedback in nearby X-ray groups and clusters Electra Panagoulia Institute of Astronomy, Cambridge, UK With: Andy Fabian Jeremy Sanders Julie.
Equal- and unequal-mass mergers of disk and elliptical galaxies with black holes Peter Johansson University Observatory Munich 8 th Sino-German workshop.
THE CORES OF TWO GALAXY GROUPS: WHAT ARE THEY TEACHING US ? FABIO GASTALDELLO UNIBO & UC IRVINE D. BUOTE UCI W. MATHEWS UCSC F. BRIGHENTI UNIBO S. ETTORI.
The Environments of Galaxies: from Kiloparsecs to Megaparsecs August 2004 Cool Cores in Galaxy Groups Ewan O’Sullivan Harvard-Smithsonian Center for Astrophysics.
The Main Mode of Galaxy/Star Formation? Avishai Dekel, HU Jerusalem Leiden, September 2008 HU Flow Team Birnboim, Freundlich, Goerdt, Neistein, Zinger.
Entropy Generation in the ICM Institute for Computational Cosmology University of Durham Michael Balogh.
Hot gas in galaxy pairs Olga Melnyk. It is known that the dark matter is concentrated in individual haloes of galaxies and is located in the volume of.
MASS AND ENTROPY PROFILES OF X-RAY BRIGHT RELAXED GROUPS FABIO GASTALDELLO UC IRVINE & BOLOGNA D. BUOTE P. HUMPHREY L. ZAPPACOSTA J. BULLOCK W. MATHEWS.
Stellar Feedback Effects on Galaxy Formation Filippo Sigward Università di Firenze Dipartimento di Astronomia e Scienza dello Spazio Japan – Italy Joint.
GH2005 Gas Dynamics in Clusters II Craig Sarazin Dept. of Astronomy University of Virginia A85 Chandra (X-ray) Cluster Merger Simulation.
Renaissance: Formation of the first light sources in the Universe after the Dark Ages Justin Vandenbroucke, UC Berkeley Physics 290H, February 12, 2008.
The Fate of the X-Ray Emitting Gas in the Early-Type Galaxy NGC 5044
Simulating the SZ Sky Predictions for Upcoming Sunyaev-Zel’dovich Effect Galaxy Cluster Surveys Eric J. Hallman CASA, University of Colorado 16 February,
AGN Outflows: Observations Doron Chelouche (IAS) The Physics of AGN Flows as Revealed by Observations Doron Chelouche* Institute for Advanced Study, Princeton.
Deep Chandra observation of WARPJ at z=1: an evolved cool-core cluster at high-z (and a bonus…) P. Tozzi, M.Nonino (INAF-TS), P. Rosati (ESO),
Feedback Observations and Simulations of Elliptical Galaxies –Daniel Wang, Shikui Tang, Yu Lu, Houjun Mo (UMASS) –Mordecai Mac-Low (AMNH) –Ryan Joung (Princeton)
Energy Balance in Clusters of Galaxies Patrick M. Motl & Jack O. Burns Center for Astrophysics and Space Astronomy University of Colorado at Boulder X-ray.
1 Suparna Roychowdhury Groups of galaxies in nearby universe, Santiago, Chile, december, 2005 Astronomy Group, Raman Research Institute Bangalore,
RGS observations of cool gas in cluster cores Jeremy Sanders Institute of Astronomy University of Cambridge A.C. Fabian, J. Peterson, S.W. Allen, R.G.
The cold component of cluster accretion Yuval Birnboim Jerusalem 2011.
The influence of baryons on the matter distribution and shape of dark matter halos Weipeng Lin ， Yipeng Jing （ Shanghai Astronomical Observatory ， CAS.
What determines the gas content of galaxies?. Galaxy formation - a reminder of the puzzle The fraction of baryons that are “cold” (stars+cold gas) is.
Jet Interactions with the Hot Atmospheres of Clusters & Galaxies B.R. McNamara University of Waterloo Girdwood, Alaska May 23, 2007 L. Birzan, P.E.J. Nulsen,
What the Formation of the First Stars Left in its Wake.
Lyman Alpha Spheres from the First Stars observed in 21 cm Xuelei Chen (Beijing) Jordi Miralda Escudé (IEEC, Barcelona).
JEREMY S. RITTER, MILOS MILOSAVLJEVIC, AND VOLKER BROMM Population III Stars HII Regions Supernovae Discussion The University of Texas at Austin LEFT:
KASI Galaxy Evolution Journal Club A Massive Protocluster of Galaxies at a Redshift of z ~ P. L. Capak et al. 2011, Nature, in press (arXive: )
Capturing inflows and outflows requires 3D. Enrichment is biased. The first stars were formed in dark matter minihalos around redshift z ≈ 20. In order.
G.W. Pratt, Ringberg, 26/10/2005 Structure and scaling of nearby clusters of galaxies – in X-rays Gabriel W. Pratt, MPE Garching, Germany.
Preventing Star and Galaxy Formation Michael Balogh Department of Physics and Astronomy University of Waterloo.
Radiative Feedback by the First Stars Dan Whalen, T-2, LANL Whalen et al 2008, ApJ, 679, 925 Hueckstadt & Whalen, ApJ, in prep.
Thermal Energy & Heat.
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 ?!
On the Cusp of the Dark Matter Sergey Mashchenko Hugh Couchman James Wadsley McMaster University ( Nature 3/8/06; Science 29/11/07 )
Cooling, AGN Feedback and Star Formation in Simulated Cool-Core Galaxy Clusters Yuan Li University of Michigan Collaborators: Greg L. Bryan (Columbia)
Towards Realistic Modeling of Massive Star Clusters Oleg Gnedin (University of Michigan) graduate student Hui Li.
The First Stars in the Universe: Formation and Feedback
Presentation transcript:

Simulating the Cooling Flow of Cool-Core Clusters Yuan Li Advisor: Greg Bryan Department of Astronomy, Columbia University July 2011

The Cooling Flow Problem In Cool-Core Clusters: t cool << Hubble Time Steady state => Cooling flow 100s M sun /yr >> SFR => Heating sources: AGN

How cold gas cools out of the flow: local or global? The amount of cold gas produced The rate of gas accretion on to a central SMBH The lack of cool gas observed in X-rays The impact of other processes (thermal conduction, Type Ia SN heating, etc) on the cooling instability Will focus on heating in later work Key Questions:

Simulation Setup Enzo, an Adaptive Mesh Refinement (AMR) code: Mpc to pc scale (smallest cell: 2pc) 3D, spherical symmetric + rotation An Isolated Cluster at z = 1 Comoving box size = 16 Mpc/h NFW Dark Matter + BCG + SMBH + gas Initial gas density and temperature: observations of Perseus Cluster Initial pressure: HSE Initial velocity: Gaussian random velocity + rotation No feedback (yet)

Results: Density Temperature and Pressure

Compressional Heating / CoolingRotational Support

Results: Time-scales

16.6 kpc Projection-z t=296 Myr

330 pc Projection-z t=296 Myr

330 pc Projection-x t=296 Myr

Results: The Amount of Cool Gas Compared to Observations

Results: Estimated AGN Feedback

Results: Impact of Resolution

Conclusion A global cooling catastrophe occurs first at a transition radius of about 50 pc from the SMBH The temperature profile remains remarkably flat as the cluster core cools There is a distinct lack of gas below a few keV Local thermal instabilities do not grow outside the transition radius Thermal conduction and Type Ia SN heating are not important The final result is sensitive to the presence of the BCG and the resolution of the simulation Next step: including feedback

Results: Gas Inflow Velocity

Classic Cooling Flow

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2024 SlidePlayer.com. Inc. All rights reserved.