Feedback in Galaxy Clusters

Size: px
Start display at page:

Download "Feedback in Galaxy Clusters"

Transcription

1 Feedback in Galaxy Clusters Brian Morsony University of Maryland 1

2 Not talking about Galaxy-scale feedback Local accretion disk feedback 2

3 Outline Galaxy cluster properties Cooling flows the need for feedback Feedback candidates AGN feedback Conduction instabilities AGN and conduction 3

4 Galaxy Cluster Properties Massive, Solar masses total Close to cosmological baryon fraction, 85-90% dark matter 10-30% of baryons in stars Most baryons (70-90%) in hot ICM gas Gas is pressure supported 4

5 Cluster Example - Perseus 5 Ken Crawford

6 Cluster Example - Perseus a 6 Fabian et al. 2011

7 Cooling Flows For some clusters, cooling time of gas in center less than age of universe See X-ray temperature decreasing towards the cluster center Cool-core cluster 7

8 Cool-core vs. non-cool core a 8 Fabian et al 2009

9 Cool-core vs. non-cool core 9 Sanderson et al. 2006

10 Cool-core vs. non-cool core 10 Cavagnolo et al. 2009

11 Cooling Flows Gas in cool-core cluster should continue to cool Pressure decreases, hot gas will flow in to replace it - Cooling flow Should be either Lots of cold gas in cluster center Lots of stars and star formation 11

12 Need for feedback Cooling flows are not seen Cluster have a large elliptical central galaxy M Sun of stars Form stars/year Have some (10 10 M Sun ) cold gas Should have: M Sun of stars or gas Form stars/year 12

13 Filaments in Perseus 13 C. Conselice

14 Filaments in Perseus 14 Fabian et al. 2008

15 Feedback What does feedback mean to me? Need a heat source Powerful enough to balance cooling Able to maintain cool core Knows how much cooling is going on and adjust its self Fairly stable on long time scales 15

16 Example: Thermostat Metal contracts, triggers a switch Heat source turns on, gets warm Metal expands, turns heat off Room cools, repeat Heater needs to be powerful enough, but not too powerful 16

17 Feedback Candidates Supernova Gravitational heating Dynamical friction / sloshing AGN Conduction 17

18 Supernova Gas cools -> gas forms stars -> stars make SN -> SN drive winds and heat gas Very important in galaxy-scale feedback Cluster are a very deep potential Stars are a small fraction of baryons Not enough energy 18

19 Gravitational heating and Dynamical friction / sloshing 19 Gravitational heating As galaxies fall into cluster, gas is stripped Gas has excess potential energy, converted to heat Dynamical friction / sloshing As galaxies or sub-clusters move through the cluster, they create tides Tidal energy dissipated as heat Gas displaced from dark matter potential, sloshing releases energy

20 Sloshing Abell Blanton et al. 2011

21 Gravitational heating and Dynamical friction / sloshing These are sources of heat, not feedback Galaxy infall or cluster mergers don t know about gas cooling rate Should see some cluster catastrophically cooling 21

22 AGN Jets Cool gas falls in, accretes onto SMBH Accretion powers AGN jets Kinetic energy of jets injected into cluster core Jets heat gas, shut off cooling Accretion rate deceases, shuts of jets 22

23 AGN Jets 23 Perseus Cluster X-ray Image Multiple X-ray cavities Sound waves extending out from cluster center

24 AGN Jets Inner cavities filled with radio emission Radio bubbles 24

25 AGN jet advantages They exists, ~all cool core clusters have X- ray cavities Have a clear feedback loop Have (maybe) enough energy to balance cooling 25

26 AGN jet problems 26 Jets are not isotropic is energy well distributed? How is jet energy converted into heat? Shocks? Mixing? Gravitational uplift? Cosmic rays? Do they really produce enough energy to balance cooling?

27 AGN Jets in hydrostatic cluster Morsony et al

28 AGN Jets in realistic cluster Morsony et al

29 Conduction Hot gas in outer cluster has lots of energy compared to cooling gas in core If you can tap into that, can stop cooling Spitzer conduction time is short compared to cooling time But, clusters are (weakly) magnetized 29

30 Conduction Conduction is anisotropic, along field lines Effectiveness depends on field structure For a tangled magnetic field, conduction suppressed by 100+, not effective For radial field, conduction not suppressed, effective For azimuthal field, conduction suppressed, not effective 30

31 Magnetic field structure 31 Thermal instabilities alter field structure Clusters are stable to convection in absence of magnetic fields In outer cluster, magnetic fields lead to magnetothermal instability (MTI), create turbulence In inner cluster, heat flux-driven buoyancy instability (HBI), creates stable azimuthal field

32 MTI Magnetic field structure HBI 32 McCourt et al. 2011

33 Conduction field structure From Karen Yang Preliminary 33

34 AGN Jets + Conduction Jets have magnetic fields Partially aligned with jet Jets are long, ~100 kpc Could create connection for conduction to happen Jets generate turbulence Could disrupt HBI fields (more conduction) Create tangled fields (less conduction) 34

35 AGN Jets From Karen Yang Preliminary 35

36 AGN Jets + Conduction From Karen Yang Preliminary 36

37 AGN vs. AGN + Conduction From Karen Yang Hot mode w/o conduction Hot mode with conduction 37

38 Summary Feedback is needed in galaxy clusters Type of feedback uncertain AGN accretion is an important part, either: Direct feedback from jet energy Indirect feedback from impact on conduction Quasar mode feedback? Other heating may also contribute 38

39 39

Hydra A (x-ray) Perseus ` (optical)

Hydra A (x-ray) Perseus ` (optical) The Biermann Lectures: Adventures in Theoretical Astrophysics I: The Physics of Galaxy Cluster Plasmas Eliot Quataert (UC Berkeley) w/ Mike McCourt, Ian Parrish, Prateek Sharma Perseus ` (optical) Hydra

More information

Molecular gas & AGN feedback in brightest cluster galaxies

Molecular gas & AGN feedback in brightest cluster galaxies Molecular gas & AGN feedback in brightest cluster galaxies Helen Russell Brian McNamara Alastair Edge Robert Main Adrian Vantyghem Francoise Combes Andy Fabian Philippe Salomé Outline Introduction Radiative

More information

Enrico Fermi School Varenna Cool Cores and Mergers in Clusters Lecture 3

Enrico Fermi School Varenna Cool Cores and Mergers in Clusters Lecture 3 Enrico Fermi School Varenna Cool Cores and Mergers in Clusters Lecture 3 Craig Sarazin Dept. of Astronomy University of Virginia A85 Chandra (X-ray) Cluster Merger Simulation Cool Cores in Clusters Central

More information

Driving hot and cold gas flows with AGN feedback in galaxy clusters Credit: ESO

Driving hot and cold gas flows with AGN feedback in galaxy clusters Credit: ESO Driving hot and cold gas flows with AGN feedback in galaxy clusters Credit: ESO Helen Russell (Cambridge) Brian McNamara (Waterloo), Andy Fabian (Cambridge), Paul Nulsen (CfA), Michael McDonald (MIT),

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

New Forms of Convection in Galaxy Cluster Plasmas (i.e., how do galaxy clusters boil?)

New Forms of Convection in Galaxy Cluster Plasmas (i.e., how do galaxy clusters boil?) New Forms of Convection in Galaxy Cluster Plasmas (i.e., how do galaxy clusters boil?) Eliot Quataert (UC Berkeley) Hydra A w/ Chandra in collaboration with Ian Parrish Prateek Sharma Overview Hot Plasma

More information

Feedback from growth of supermassive black holes

Feedback from growth of supermassive black holes Research Collection Other Conference Item Feedback from growth of supermassive black holes Author(s): Begelman, Mitchell C.; Ruszkowksi, Mateusz Publication Date: 2003 Permanent Link: https://doi.org/10.3929/ethz-a-004585094

More information

Galaxy Activity in Semi Analytical Models. Fabio Fontanot (INAF OATs) Ljubljana 05/04/11

Galaxy Activity in Semi Analytical Models. Fabio Fontanot (INAF OATs) Ljubljana 05/04/11 Galaxy Activity in Semi Analytical Models Fabio Fontanot (INAF OATs) Ljubljana 05/04/11 Part I: Theoretical background 1. Baryonic gas falls in the gravitational potential of Dark Matter Halos 2. Baryonic

More information

Massive molecular gas flows and AGN feedback in galaxy clusters

Massive molecular gas flows and AGN feedback in galaxy clusters Massive molecular gas flows and AGN feedback in galaxy clusters CO(3-2) Helen Russell (Cambridge) Brian McNamara (Waterloo), Andy Fabian (Cambridge), Paul Nulsen (CfA), Michael McDonald (MIT), Alastair

More information

Heat Transport and Buoyancy Instabilities in Astrophysical Plasmas. Eliot Quataert (UC Berkeley)

Heat Transport and Buoyancy Instabilities in Astrophysical Plasmas. Eliot Quataert (UC Berkeley) Heat Transport and Buoyancy Instabilities in Astrophysical Plasmas Eliot Quataert (UC Berkeley) Galaxy Cluster Hydra A w/ Chandra Surface of the Sun ~ 1 Million light-years Overview Microscopic Energy

More information

Chapter 11 The Formation and Structure of Stars

Chapter 11 The Formation and Structure of Stars Chapter 11 The Formation and Structure of Stars Guidepost The last chapter introduced you to the gas and dust between the stars that are raw material for new stars. Here you will begin putting together

More information

Observational Evidence of AGN Feedback

Observational Evidence of AGN Feedback 10 de maio de 2012 Sumário Introduction AGN winds Galaxy outflows From the peak to the late evolution of AGN and quasars Mergers or secular evolution? The AGN feedback The interaction process between the

More information

the self-regulated agn feedback loop: chaotic cold accretion

the self-regulated agn feedback loop: chaotic cold accretion the self-regulated agn feedback loop: chaotic cold accretion Massimo Gaspari Max Planck Institute for Astrophysics the self-regulated agn feedback loop: raining onto black holes Massimo Gaspari Max Planck

More information

AGN/Galaxy Co-Evolution. Fabio Fontanot (HITS)

AGN/Galaxy Co-Evolution. Fabio Fontanot (HITS) AGN/Galaxy Co-Evolution Fabio Fontanot (HITS) 21/11/2012 AGN activity in theoretical models of galaxy formation Represents a viable solution for a number of long-standing theoretical problems Properties

More information

The AGN Jet Model of the Fermi Bubbles

The AGN Jet Model of the Fermi Bubbles The AGN Jet Model of the Fermi Bubbles Fulai Guo Shanghai Astronomical Observatory IAU 322 Symposium, Palm Cove, July 18-22, 2016 1 The All-sky Fermi View at E >10 GeV The Fermi bubbles! (NASA image based

More information

Part two of a year-long introduction to astrophysics:

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:

More information

AGN Feedback In an Isolated Elliptical Galaxy

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;

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

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

The Radio/X-ray Interaction in Abell 2029

The Radio/X-ray Interaction in Abell 2029 The Radio/X-ray Interaction in Abell 2029 Tracy Clarke (Univ. of Virginia) Collaborators: Craig Sarazin (UVa), Elizabeth Blanton (UVa) Abell 2029: Background z = 0.0767, D=320 Mpc, scale = 1.44 kpc/ typically

More information

Clusters: Observations

Clusters: Observations Clusters: Observations Last time we talked about some of the context of clusters, and why observations of them have importance to cosmological issues. Some of the reasons why clusters are useful probes

More information

Part 2. Hot gas halos and SMBHs in optically faint ellipticals. Part 3. After Chandra?

Part 2. Hot gas halos and SMBHs in optically faint ellipticals. Part 3. After Chandra? Hot gas and AGN Feedback in Nearby Groups and Galaxies Part 1. Cool cores and outbursts from supermassive black holes in clusters, groups and normal galaxies Part 2. Hot gas halos and SMBHs in optically

More information

Chapter 17. Active Galaxies and Supermassive Black Holes

Chapter 17. Active Galaxies and Supermassive Black Holes Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study

More information

AST242 LECTURE NOTES PART 7

AST242 LECTURE NOTES PART 7 AST242 LECTURE NOTES PART 7 Contents 1. HII regions and Ionization Fronts 1 1.1. The Strömgren Sphere 2 1.2. Early Evolution 3 1.3. Achieving Pressure equilibrium 3 1.4. Jump conditions on an ionization

More information

Galaxy groups: X-ray scaling relations, cool cores and radio AGN

Galaxy groups: X-ray scaling relations, cool cores and radio AGN Galaxy groups: X-ray scaling relations, cool cores and radio AGN Ming Sun (UVA) (M. Voit, W. Forman, P. Nulsen, M. Donahue, C. Jones, A. Vikhlinin, C. Sarazin ) Outline: 1) Scaling relations and baryon

More information

AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation!

AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation! AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation! Bring pencil #2 with eraser No use of calculator or any electronic device during the exam We provide the scantrons

More information

The X-Ray Universe. The X-Ray Universe

The X-Ray Universe. The X-Ray Universe The X-Ray Universe The X-Ray Universe Potsdam University Dr. Lidia Oskinova Wintersemester 2013-2014 lida@astro.physik.uni-potsdam.de astro.physik.uni-potsdam.de/~lida/x-ray.html Chandra X-ray, HST optical,

More information

Cold Clouds in Cool Cores

Cold Clouds in Cool Cores Becky Canning NGC 1275, Perseus Cluster Cold Clouds in Cool Cores 1 Snowcluster 2015 Cold Clouds in Cool Cores Excitation mechanisms of the multi-phase cool/cold gas Why should we care? Heard that X-ray

More information

AGN in hierarchical galaxy formation models

AGN in hierarchical galaxy formation models AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Physics of Galactic Nuclei, Ringberg Castle, June 18, 2009 Outline Brief introduction

More information

AGN Feedback in the Hot Halo of NGC 4649

AGN Feedback in the Hot Halo of NGC 4649 AGN Feedback in the Hot Halo of NGC 4649 A. Paggi1 G. Fabbiano1, D.-W. Kim1, S. Pellegrini2, F. Civano3, J. Strader4 and B. Luo5 Harvard-Smithsonian Center for Astrophysics; 2Department of Astronomy, University

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

COSMIC-RAY DRIVEN MAGNETIC FIELD DYNAMO IN GALAXIES

COSMIC-RAY DRIVEN MAGNETIC FIELD DYNAMO IN GALAXIES COSMIC-RAY DRIVEN MAGNETIC FIELD DYNAMO IN GALAXIES Michał Hanasz, Centre for Astronomy Nicolaus Copernicus University, Toruń MAGNETIC FIELDS IN SPIRAL GALAXIES - RADIO OBSERVATIONS M51 NGC891 A. Fletcher

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

Star systems like our Milky Way. Galaxies

Star systems like our Milky Way. Galaxies Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in

More information

Astro-2: History of the Universe

Astro-2: History of the Universe Astro-2: History of the Universe Lecture 13; May 30 2013 Previously on astro-2 Energy and mass are equivalent through Einstein s equation and can be converted into each other (pair production and annihilations)

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

THE GALACTIC CORONA. In honor of. Jerry Ostriker. on his 80 th birthday. Chris McKee Princeton 5/13/2017. with Yakov Faerman Amiel Sternberg

THE GALACTIC CORONA. In honor of. Jerry Ostriker. on his 80 th birthday. Chris McKee Princeton 5/13/2017. with Yakov Faerman Amiel Sternberg THE GALACTIC CORONA In honor of Jerry Ostriker on his 80 th birthday Chris McKee Princeton 5/13/2017 with Yakov Faerman Amiel Sternberg A collaboration that began over 40 years ago and resulted in a lifelong

More information

A Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA

A Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA M87 A Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA interactions galore; stripping at work, M87 outburst Low Eddington ratio accretion (like other normal

More information

Gasflows in Galaxy Clusters

Gasflows in Galaxy Clusters Gasflows in Galaxy Clusters Brian McNamara University of Waterloo Perimeter Ins7tute for Theore7cal Physics, Canada H. Russell, C.J. Ma, A. Vantyghem, C. Kirkpatrick, R. Main P. Nulsen, A. Edge, A., Fabian,

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

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

Outline. Walls, Filaments, Voids. Cosmic epochs. Jeans length I. Jeans length II. Cosmology AS7009, 2008 Lecture 10. λ =

Outline. Walls, Filaments, Voids. Cosmic epochs. Jeans length I. Jeans length II. Cosmology AS7009, 2008 Lecture 10. λ = Cosmology AS7009, 2008 Lecture 10 Outline Structure formation Jeans length, Jeans mass Structure formation with and without dark matter Cold versus hot dark matter Dissipation The matter power spectrum

More information

Accretion Disks. Review: Stellar Remnats. Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath 2/25/10. Review: Creating Stellar Remnants

Accretion Disks. Review: Stellar Remnats. Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath 2/25/10. Review: Creating Stellar Remnants Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath Review: Creating Stellar Remnants Binaries may be destroyed in white dwarf supernova Binaries be converted into black holes Review: Stellar

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

Uri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 2008

Uri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 2008 Uri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 008 Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 008 Relaxed, cool

More information

the ICM Power Spectrum:

the ICM Power Spectrum: the ICM Power Spectrum: probing the gas physics of galaxy clusters Massimo Gaspari Max Planck Institute for Astrophysics Collaborators: E. Churazov, D. Nagai, E. Lau, I. Zhuravleva, R. Sunyaev Power Spectrum

More information

Chapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo

Chapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo Chapter 19 Galaxies Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past halo disk bulge Barred Spiral Galaxy: Has a bar of stars across the bulge Spiral Galaxy 1

More information

Feedback flows of gas, energy and momentum in and out of galaxies

Feedback flows of gas, energy and momentum in and out of galaxies Feedback flows of gas, energy and momentum in and out of galaxies Matthijs H.D. van der Wiel March 10 th 2005 a part of the course Formation and Evolution of Galaxies Feedback accretion outflow Feedback

More information

Active Galactic Nuclei

Active Galactic Nuclei Active Galactic Nuclei Prof. Jeff Kenney Class 18 June 20, 2018 the first quasar discovered 3C273 (1963) very bright point source (the quasar ) jet the first quasar discovered 3C273 (1963) very bright

More information

Energy Balance in Clusters of Galaxies. Patrick M. Motl & Jack O. Burns Center for Astrophysics and Space Astronomy University of Colorado at Boulder

Energy Balance in Clusters of Galaxies. Patrick M. Motl & Jack O. Burns Center for Astrophysics and Space Astronomy University of Colorado at Boulder 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 and Radio Connections, February 6th, 2004 With

More information

The Superbubble Power Problem: Overview and Recent Developments. S. Oey

The Superbubble Power Problem: Overview and Recent Developments. S. Oey The Superbubble Power Problem: Overview and Recent Developments S. Oey It has been known for decades that superbubbles generated by massive star winds and supernovae are smaller than expected based on

More information

Galactic Scale Winds. Elizabeth Harper-Clark, Mubdi Rahman, Brice Ménard, Eve Lee, Eliot Quataert, Phil Hopkins,Todd Thompson

Galactic Scale Winds. Elizabeth Harper-Clark, Mubdi Rahman, Brice Ménard, Eve Lee, Eliot Quataert, Phil Hopkins,Todd Thompson Galactic Scale Winds Elizabeth Harper-Clark, Mubdi Rahman, Brice Ménard, Eve Lee, Eliot Quataert, Phil Hopkins,Todd Thompson Phenomenology Weiner, Koo: we see winds in most high z star forming galaxies

More information

Chapter 21 Galaxy Evolution. How do we observe the life histories of galaxies?

Chapter 21 Galaxy Evolution. How do we observe the life histories of galaxies? Chapter 21 Galaxy Evolution How do we observe the life histories of galaxies? Deep observations show us very distant galaxies as they were much earlier in time (old light from young galaxies). 1 Observing

More information

Gravitational heating, clumps, overheating. Yuval Birnboim (Harvard Smithsonian Center for Astrophysics) Avishai Dekel (Hebrew University)

Gravitational heating, clumps, overheating. Yuval Birnboim (Harvard Smithsonian Center for Astrophysics) Avishai Dekel (Hebrew University) Gravitational heating, clumps, overheating Yuval Birnboim (Harvard Smithsonian Center for Astrophysics) Avishai Dekel (Hebrew University) Basic idea: Cooling flow Clusters need additional energy to reduce

More information

Luminous radio-loud AGN: triggering and (positive?) feedback

Luminous radio-loud AGN: triggering and (positive?) feedback Luminous radio-loud AGN: triggering and (positive?) feedback Clive Tadhunter University of Sheffield ASA, ESA, NRAO Collaborators: C. Ramos Almeida, D. Dicken," R. Morganti,T. Oosterloo, " R. Oonk, M.

More information

Dynamics of hot gas in Galaxies, Groups, & Clusters

Dynamics of hot gas in Galaxies, Groups, & Clusters Dynamics of hot gas in Galaxies, Groups, & Clusters Bill Mathews Colleagues: Fabrizio Brighenti (Bologna) David Buote (UC Irvine) X-ray images of groups and clusters of galaxies Conventional cooling flows

More information

Why study plasma astrophysics?

Why study plasma astrophysics? Why study plasma astrophysics? Nick Murphy and Xuening Bai Harvard-Smithsonian Center for Astrophysics Astronomy 253: Plasma Astrophysics January 25, 2016 Today s plan Definition of a plasma Plasma astrophysics:

More information

Selected Topics in Plasma Astrophysics

Selected Topics in Plasma Astrophysics Selected Topics in Plasma Astrophysics Range of Astrophysical Plasmas and Relevant Techniques Stellar Winds (Lecture I) Thermal, Radiation, and Magneto-Rotational Driven Winds Connections to Other Areas

More information

Snowballs in hell! X-ray galactic coronae in galaxy! clusters and the need for sub-arcsecond resolution! Simona Giacintucci (NRL)!

Snowballs in hell! X-ray galactic coronae in galaxy! clusters and the need for sub-arcsecond resolution! Simona Giacintucci (NRL)! Snowballs in hell X-ray galactic coronae in galaxy clusters and the need for sub-arcsecond resolution Simona Giacintucci (NRL) M. Markevitch (GSFC), T. Clarke (NRL), E. Richards (NRC-NRL) X-ray Skies with

More information

(Astro)Physics 343 Lecture # 12: active galactic nuclei

(Astro)Physics 343 Lecture # 12: active galactic nuclei (Astro)Physics 343 Lecture # 12: active galactic nuclei Schedule for this week Monday & Tuesday 4/21 22: ad hoc office hours for Lab # 5 (you can use the computer in my office if necessary; Sections A

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

Topics for Today s Class

Topics for Today s Class Foundations of Astronomy 13e Seeds Chapter 11 Formation of Stars and Structure of Stars Topics for Today s Class 1. Making Stars from the Interstellar Medium 2. Evidence of Star Formation: The Orion Nebula

More information

Formation of z~6 Quasars from Hierarchical Galaxy Mergers

Formation of z~6 Quasars from Hierarchical Galaxy Mergers Formation of z~6 Quasars from Hierarchical Galaxy Mergers Yuexing Li et al Presentation by: William Gray Definitions and Jargon QUASAR stands for QUASI-stellAR radio source Extremely bright and active

More information

The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

The Monster Roars: AGN Feedback & Co-Evolution with Galaxies The Monster Roars: AGN Feedback & Co-Evolution with Galaxies Philip Hopkins Ø (Nearly?) Every massive galaxy hosts a supermassive black hole Ø Mass accreted in ~couple bright quasar phase(s) (Soltan, Salucci+,

More information

Powering the Universe with Supermassive Black Holes. Steve Ehlert and Paul Simeon

Powering the Universe with Supermassive Black Holes. Steve Ehlert and Paul Simeon Powering the Universe with Supermassive Black Holes Steve Ehlert and Paul Simeon Overview Introduction to Galactic Nuclei Galactic Nuclear Activity Input and output energies. The aftermath of AGN flares.

More information

AST 101 Introduction to Astronomy: Stars & Galaxies

AST 101 Introduction to Astronomy: Stars & Galaxies AST 101 Introduction to Astronomy: Stars & Galaxies The H-R Diagram review So far: Stars on Main Sequence (MS) Next: - Pre MS (Star Birth) - Post MS: Giants, Super Giants, White dwarfs Star Birth We start

More information

Astrofysikaliska Dynamiska Processer

Astrofysikaliska Dynamiska Processer Astrofysikaliska Dynamiska Processer VT 2008 Susanne Höfner hoefner@astro.uu.se Aims of this Course - understanding the role and nature of dynamical processes in astrophysical contexts and how to study

More information

AC Fabian, M. Cappi, J Sanders. Cosmic Feedback from AGN

AC Fabian, M. Cappi, J Sanders. Cosmic Feedback from AGN AC Fabian, M. Cappi, J Sanders Cosmic Feedback from AGN AC Fabian, M Cappi, J Sanders, S Heinz, E Churazov, B McNamara, J Croston, D Worrall, F Humphrey, F Tombesi, J Reeves, M Giustini, P O Brien, T Reiprich

More information

Black Holes and Active Galactic Nuclei

Black Holes and Active Galactic Nuclei Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently

More information

Embedded Spiral Patterns in the massive galaxy cluster Abell 1835

Embedded Spiral Patterns in the massive galaxy cluster Abell 1835 2017/06/08 X-ray Universe @ Rome Embedded Spiral Patterns in the massive galaxy cluster Abell 1835 Shutaro Ueda (ISAS/JAXA), Tetsu Kitayama (Toho University), Tadayasu Dotani (ISAS/JAXA, SOKENDAI) This

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

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

Cosmic ray feedback in hydrodynamical simulations. simulations of galaxy and structure formation

Cosmic ray feedback in hydrodynamical simulations. simulations of galaxy and structure formation Cosmic ray feedback in hydrodynamical simulations of galaxy and structure formation Canadian Institute for Theoretical Astrophysics, Toronto April, 13 26 / Workshop Dark halos, UBC Vancouver Outline 1

More information

AGN feedback and the connection to triggering

AGN feedback and the connection to triggering AGN feedback and the connection to triggering Ryan C. Hickox Dartmouth College The Triggering Mechanisms for Active Galactic Nuclei Lorentz Center, Leiden 26 July 2013 Illustration courtesy NASA Outline

More information

The First Stars. Simone Ferraro Princeton University. Sept 25, 2012

The First Stars. Simone Ferraro Princeton University. Sept 25, 2012 The First Stars Simone Ferraro Princeton University Sept 25, 2012 Outline Star forming minihalos at high z Cooling physics and chemistry Gravitational Collapse and formation of protostar Magnetic fields

More information

Chapter 16 Lecture. The Cosmic Perspective Seventh Edition. Star Birth Pearson Education, Inc.

Chapter 16 Lecture. The Cosmic Perspective Seventh Edition. Star Birth Pearson Education, Inc. Chapter 16 Lecture The Cosmic Perspective Seventh Edition Star Birth 2014 Pearson Education, Inc. Star Birth The dust and gas between the star in our galaxy is referred to as the Interstellar medium (ISM).

More information

X- ray surface brightness fluctuations and turbulence in galaxy clusters. Jeremy Sanders. Andy Fabian. Sanders & Fabian 2011, MNRAS, submitted

X- ray surface brightness fluctuations and turbulence in galaxy clusters. Jeremy Sanders. Andy Fabian. Sanders & Fabian 2011, MNRAS, submitted X- ray surface brightness fluctuations and turbulence in galaxy clusters Jeremy Sanders Andy Fabian Sanders & Fabian 2011, MNRAS, submitted Simulations predict that in galaxy clusters turbulent energy

More information

Other Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies

Other Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at

More information

Chapter 21 Galaxy Evolution. Agenda

Chapter 21 Galaxy Evolution. Agenda Chapter 21 Galaxy Evolution Agenda Announce: Test in one week Part 2 in 2.5 weeks Spring Break in 3 weeks Online quizzes & tutorial are now on assignment list Final Exam questions Revisit Are we significant

More information

Clusters of galaxies and the large scale structure of the universe. Gastão B. Lima Neto IAG/USP

Clusters of galaxies and the large scale structure of the universe. Gastão B. Lima Neto IAG/USP Clusters of galaxies and the large scale structure of the universe Gastão B. Lima Neto IAG/USP IWARA, Maresias 10/2009 Our story begins... William Herschel recognizes the clustering of nebulae and their

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

A100H Exploring the Universe: Quasars, Dark Matter, Dark Energy. Martin D. Weinberg UMass Astronomy

A100H Exploring the Universe: Quasars, Dark Matter, Dark Energy. Martin D. Weinberg UMass Astronomy A100H Exploring the :, Dark Matter, Dark Energy Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 19, 2016 Read: Chaps 20, 21 04/19/16 slide 1 BH in Final Exam: Friday 29 Apr at

More information

11/6/18. Today in Our Galaxy (Chap 19)

11/6/18. Today in Our Galaxy (Chap 19) ASTR 1040: Stars & Galaxies Prof. Juri Toomre TAs: Ryan Horton, Loren Matilsky Lecture 21 Tues 6 Nov 2018 zeus.colorado.edu/astr1040-toomre Edge-on spiral galaxy NGG 4013 Today in Our Galaxy (Chap 19)

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

Galaxy Evolution & Black-Hole Growth (review)

Galaxy Evolution & Black-Hole Growth (review) Galaxy Evolution & Black-Hole Growth (review) Avishai Dekel The Hebrew University of Jerusalem & UCSC Delivered by Fangzhou Jiang Dali, China, November 2018 See also Claude-Andre s talk and Joel s talk

More information

Chapter 11 The Formation of Stars

Chapter 11 The Formation of Stars Chapter 11 The Formation of Stars A World of Dust The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful objects in the sky.

More information

The Hot Gaseous Halos of Spiral Galaxies. Joel Bregman, Matthew Miller, Edmund Hodges Kluck, Michael Anderson, XinyuDai

The Hot Gaseous Halos of Spiral Galaxies. Joel Bregman, Matthew Miller, Edmund Hodges Kluck, Michael Anderson, XinyuDai The Hot Gaseous Halos of Spiral Galaxies Joel Bregman, Matthew Miller, Edmund Hodges Kluck, Michael Anderson, XinyuDai Hot Galaxy Halos and Missing Baryons Dai et al. (2010) Rich clusters have nearly all

More information

ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014

ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014 ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools

More information

Recent Progress in Modeling of Galaxy Formation. Oleg Gnedin (University of Michigan)

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,

More information

The Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)

The Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley) The Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? The Best Evidence for a BH: M 3.6 10 6 M (M = mass of sun) It s s close! only ~ 10 55 Planck Lengths

More information

Astronomy 1 Fall 2016

Astronomy 1 Fall 2016 Astronomy 1 Fall 2016 Lecture11; November 1, 2016 Previously on Astro-1 Introduction to stars Measuring distances Inverse square law: luminosity vs brightness Colors and spectral types, the H-R diagram

More information

Chapter 23: Dark Matter, Dark Energy & Future of the Universe. Galactic rotation curves

Chapter 23: Dark Matter, Dark Energy & Future of the Universe. Galactic rotation curves Chapter 23: Dark Matter, Dark Energy & Future of the Universe Galactic rotation curves Orbital speed as a function of distance from the center: rotation_of_spiral_galaxy.htm Use Kepler s Third Law to get

More information

ASTR 200 : Lecture 25. Galaxies: internal and cluster dynamics

ASTR 200 : Lecture 25. Galaxies: internal and cluster dynamics ASTR 200 : Lecture 25 Galaxies: internal and cluster dynamics 1 Galaxy interactions Isolated galaxies are often spirals One can find small galaxy `groups' (like the Local group) with only a few large spiral

More information

Building the Red Sequence

Building the Red Sequence Building the Red Sequence Jared Gabor University of Arizona Romeel Davé, Kristian Finlator, and Ben Oppenheimer See arxiv 1012.3166 Building the Red Sequence Jared Gabor University of Arizona Romeel Davé,

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

What Doesn t Quench Galaxy Formation?

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

More information

Dark Energy: Measuring the Invisible with X-Ray Telescopes

Dark Energy: Measuring the Invisible with X-Ray Telescopes Black holes, Galactic Dark Center Matter and Galactic Center Dark Energy: Measuring the Invisible with X-Ray Telescopes Christine Jones Before 1930 -- only optical observations of the sky Intro Before

More information

Black Holes in the Early Universe Accretion and Feedback

Black Holes in the Early Universe Accretion and Feedback 1 1 Black Holes in the Early Universe Accretion and Feedback 1 1 Black Holes in the Early Universe Accretion and Feedback Geoff Bicknell & Alex Wagner Australian National University 1 1 High redshift radio

More information

Observations of diffuse radio emission in cool-core clusters

Observations of diffuse radio emission in cool-core clusters Observations of diffuse radio emission in cool-core clusters Simona Giacintucci U.S. Naval Research Laboratory Maxim Markevitch (GSFC), Tracy Clarke (NRL), Tiziana Venturi (INAF-IRA), Rossella Cassano

More information

How do Black Holes Get Their Gas?

How do Black Holes Get Their Gas? How do Black Holes Get Their Gas? Philip Hopkins Eliot Quataert, Lars Hernquist, T. J. Cox, Kevin Bundy, Jackson DeBuhr, Volker Springel, Dusan Keres, Gordon Richards, Josh Younger, Desika Narayanan, Paul

More information