William I. Fine

Theoretical Physics Institute

ICM 2016

Physics of the Intracluster Medium: Theory & Computation

Image credits: NRAO, F. Owen et al (2014), G. Taylor (2008); NASA, ESA, A. Fabian et al (2005), Taylor et al, E. Blanton et al (2011); & MSI F. Vazza et al (2016)

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

T A B PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP L E August 22 - 24, 2016 O F

TABLE OF CONTENTS Program...........................................................................................2 Workshop Banquet info...........................................................6 & 29 Wireless Information.......................................................................9 Abstracts.........................................................................................10 Participant List...............................................................................23 Talk Uploading Instructions...........................................................25 Poster Titles....................................................................................26 Maps Workshop Banquet Location................................................29



Additional Locations............................................................30



Dining Guide........................................................................31



William I. Fine Theoretical Physics Institute School of Physics & Astronomy University of Minnesota 116 Church Street SE Minneapolis, MN 55455

Phone: (612) 624-7366 Fax: (612) 626-8606 [email protected] www.ftpi.umn.edu

C O N T E N T S

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

Welcome to the 4th “Physics of the Intracluster Medium: Theory & Computation” workshop We are very pleased to announce the 4th “Physics of the Intracluster Medium: Theory and Computation” workshop hosted by the William I. Fine Theoretical Physics Institute at the University of Minnesota, Twin Cities and co-sponsored by the Michigan Center for Theoretical Physics in Ann Arbor and the Niels Bohr International Academy in Copenhagen. The event will take place August 22-24, 2016 in Minneapolis. The workshop will bring together researchers who share overlapping interests in the physics and dynamics of ICMs. Expected topics include such issues as shocks, cold fronts and turbulence in the ICM; the evolution, amplification and consequences of ICM magnetic fields; non-thermal particles, their generation and emissions; the coupling between AGN outflows and the ICM; microphysical, plasma processes and their roles in ICMs. Participation is by invitation only. We welcome participation of graduate students. Please contact us with any questions by email at ICM2016 (at) physics.umn.edu. Scientific Organizing Committee: Tom Jones, University of Minnesota Yong Qian, University of Minnesota Gus Evrard, University of Michigan Mateusz Ruszkowski, University of Michigan Martin Pessah, Niels Bohr Institute

http://www.ftpi.umn.edu/workshops/2016-2017/ICM2016/index.html

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016



8:45 AM

MONDAY, AUGUST 22ND

The West Bank Office Building, Room 142 Registration West Bank Office Building, Room 142 1300 2nd Street S Minneapolis, MN 55455

8:55 AM Welcome and Opening Remarks Tom Jones University of Minnesota 9:00 AM New Kid on the Block: Kinematic Sunyaev-Zel’dovich Effect Daisuke Nagai Yale University 9:25 AM Viscosity, Conduction, Convection, and Dynamo in a Weakly Collisional Magnetized Plasma Matthew Kunz Princeton University 9:50 AM New High-order Methods using Gaussian Processes for CFD Dongwook Lee University of California, Santa Cruz 10:15 AM

COFFEE BREAK

10:35 AM Rest-Frame UV Spectroscopy of Hot Gas in the Centers of Cool Core Brightest Cluster Galaxies Megan Donahue Michigan State University 11:00 AM

Cluster kinematics in the post-Hitomi era Sebastian Heinz University of Wisconsin - Madison

11:25 AM

Poster abstracts Nine Poster Abstracts (~5 min per)

12:10 PM

Discussion Session I

12:30 PM

LUNCH BREAK Lunch is on your own. Please refer to the dining guide in the back of this booklet.

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P R O G R A M

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

MONDAY, AUGUST 22ND

The West Bank Office Building, Room 142

2:00 PM

Flow dynamics in galaxy clusters Elke Roediger University of Hull

2:25 PM Simulating the ICM As Seen Through the Next Generation of X-ray Telescopes John ZuHone Massachusetts Institute of Technology 2:50 PM Deep Chandra observations as probes of detailed ICM physics Norbert Werner Stanford University 3:15 PM

COFFEE BREAK

3:35 PM Microphysics of ICM from X-ray images: effective equation of state, turbulence, heating Irina Zhuravleva Stanford University 4:00 PM Witnessing the growth of the nearest galaxy cluster Aurora Simionescu ISAS – Japan Aerospace Exploration Agency 4:25 PM High-resolution micro-calorimeter X-ray spectroscopy of the core of the Perseus Cluster of galaxies Hitomi Collaboration 4:50 PM

Discussion Session II

5:20 PM

Workshop Ends for the Day

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

TUESDAY, AUGUST 23RD

The West Bank Office Building, Room 142

9:00 AM Insights on non-thermal phenomena in the ICM from radio observations Annalisa Bonafede University Hamburg 9:25 AM Merging clusters as physics laboratories - first results from LOFAR Marcus Brüggen University Hamburg 9:50 AM The challenge of turbulence in galaxy clusters: physics and particle acceleration Gianfranco Brunetti IRA-INAF, Bologna 10:15 AM

COFFEE BREAK

10:35 AM The Role of Turbulence in Accelerating Cosmic Rays and Amplifying B-fields in the ICM Peng Oh University of California, Santa Barbara 11:00 AM Cosmic Ray Propagation in High Beta Plasmas Ellen Zweibel University of Wisconsin - Madison 11:25 PM

Superdiffusion and Streaming and Acceleration of Cosmic rays Alex Lazarian University of Wisconsin, Madison

11:50 PM

Discussion Session I

12:20 PM

LUNCH BREAK Lunch is on your own. Please refer to the dining guide in the back of this booklet.

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P R O G R A M

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

TUESDAY, AUGUST 23RD

The West Bank Office Building, Room 142

2:00 PM Is cosmic ray heating relevant in cool core clusters? Christoph Pfrommer Heidelberg Institute for Theoretical Studies 2:25 PM

Role of cosmic ray heating in the ICM Mateusz Ruszkowski University of Michigan

2:50 PM

Shock Waves in the Outskirt of Galaxy Clusters Dongsu Ryu Ulsan National Institute of Technology

3:15 PM

COFFEE BREAK

3:35 PM Cluster outskirts as a gateway to the physics of particle acceleration and magnetogenesis Franco Vazza University of Hamburg 4:00 PM Re-acceleration Model for Radio Relics in Galaxy Clusters Hyesung Kang Pusan National University 4:25 PM New Models of the Sausage Relic Julius Donnert University of Minnesota 4:50 PM

Discussion Session II

5:20 PM

Workshop Ends for the Day

6:00 PM

Banquet for ICM workshop participants

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

TUESDAY, AUGUST 23RD

Workshop Banquet VIC’S

201 SE Main St Minneapolis, MN 55414 6:00 PM



Leave Hotel to walk to banquet dinner (30 minute walk)



OR

Board bus at workshop hotel at 6:10 pm. Bus will leave the hotel at 6:20 pm to drop off at Vic’s for dinner

6:30 PM

Social Hour

7:15 PM



Dinner

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P R O G R A M

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

WEDNESDAY, AUGUST 24TH

The West Bank Office Building, Room 142 8:45 AM Shattering cold gas into tiny cloudlets Mike McCourt University of California, Santa Barbara 9:10 AM Metal Mixing in the Presence of a Magnetic Field Evan Scannapieco Arizona State University 9:35 AM On Helium Mixing in Quasi-global Simulations of the Intra-Cluster Medium Martin Pessah Niels Bohr Institute 10:00 AM

COFFEE BREAK

10:20 AM Jet-Lobe Morphology Under the Cluster Weather: Inferences on ICM Dynamics and Jet Composition Hui Li Los Alamos National Laboratory 10:45 AM Properties of the ICM of Galaxy Cluster from hydrodynamical simulations with AGN feedback Elena Rasia University of Michigan 11:10 PM How AGN Jets Heat the Intracluster Medium – Insights from Simulations Karen Yang University of Maryland 11:35 PM

Discussion Session I

12:05 PM

LUNCH BREAK Lunch is on your own. Please refer to the dining guide in the back of this booklet.

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

WEDNESDAY, AUGUST 24TH

The West Bank Office Building, Room 142 1:35 PM Heating in Simulated Galaxy Clusters with Momentum-driven AGN Feedback Yuan Li Columbia University 2:00 PM Thermal Instability in Low Entropy Gas Lifted behind Buoyantly-Rising X-ray Bubbles Brian McNamara University of Waterloo 2:25 PM Nonlinear thermal instability in the radio mode feedback cycle Paul Nulsen Center for Astrophysics, Harvard-Smithsonian 2:50 PM

COFFEE BREAK

3:10 PM Triggering and delivery methods for AGN feedback Brian O’Shea Michigan State University 3:35 PM The Black-Hole Feedback Valve Mark Voit Michigan State University 4:00 PM Simulations of AGN jet feedback in galaxy clusters: heating and cooling cycles Prateek Sharma Indian Institute of Science, Bangalore 4:25 PM

Discussion Session II

5:00 PM

Workshop Closing

Thank you for your participation!

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P R O G R A M

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

WIRELESS ACCESS Please see workshop staff for a secure Wi-Fi connection username and password

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

ABSTRACTS (alphabetical by speaker)

Insights on non-thermal phenomena in the ICM from radio observations Radio observations provide the best tool to understand the physics and the evolution of the non-thermal component n the Intra-cluster Medium. In particular, they probe(re)acceleration processes due to shocks and turbulence, allowing one to explore turbulence and low Mach number shock acceleration. In this talk, I will present the main discoveries done in the past years thanks to the advent of low frequency observatories (LOFAR and GMRT). ANNALISA BONEFEDE University of Hamburg Merging clusters as physics laboratories - first results from LOFAR Merging galaxy clusters are interesting to study (i) particle acceleration, (ii) magnetic fields, (iii) self-interacting Dark Matter and (iv) galaxy evolution. I will report on recent observational and theoretical progress in understanding radio relics. Finally, I will present recent results from the Low Frequency Array (LOFAR) MARCUS BRÜGGEN University of Hamburg The challenge of turbulence in galaxy clusters: physics and particle acceleration Non-thermal phenomena in galaxy clusters suggest that a fraction of the energy that is associated with large-scale motions in the intra-cluster-medium (ICM) is channeled into electromagnetic fluctuations on small scales. This poses fundamental questions about the microphysics of the ICM: presumably a plasma that is weakly collisional, stirred and unstable. I will discuss relevant points of the physics of turbulence in the ICM and focus on the mechanisms of particle acceleration mediated by turbulence in the ICM. Observational consequences on cluster-scale radio emission and on the high energy emission from galaxy clusters are discussed. GIANFRANCO BRUNETTI IRA-INAF, Bologna

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

Rest-Frame UV Spectroscopy of Hot Gas in the Centers of Cool Core Brightest Cluster Galaxies We will present new Hubble Space Telescope COS and STIS spectroscopy of the central knots in the Brightest Cluster Galaxy in the CLASH cluster RXJ1532.9+3021. X-ray observations show this cluster hosts a radio AGN that has excavated large holes in the X-ray intracluster medium. The X-ray gas in the core of this cluster is extremely luminous. Although the star formation visible in the cluster is higher than that of many starburst galaxies (> 100 solar masses per year, estimated from FIR and UV -based SFRs), the AGN appears to preventing a far higher rate of star formation. We place very strong limits on the rate of gas cooling from intermediate gas temperatures (~1 million K) using UV spectroscopy. The UV spectra from the center of this BCG bear a strong resemblance to that of the most extreme Lyman Break galaxies at z~3, including significant UV continuum and absorption line features from recently formed hot stars and Lyman alpha emission and Lyman beta absorption consistent with winds driven by hot stars. We will discuss the implications of the state of this system in context with the handful of other active BCGs that have spectroscopy at similar rest wavelengths. MEGAN DONAHUE Michigan State University New Models of the Sausage Relic We will present a novel theoretical model for the sausage relic. Given a favorable set of parameters, we show that the steeping in the relic can be explained by a turbulent Dynamo acting behind the shock. We also present a set of idealized simulations of the sausage cluster. Given recent constrains of the cluster mass and mass ratio from weak lensing estimates, our simulations allow us to constrain the Mach number in the relic. JULIUS DONNERT University of Minnesota Cluster kinematics in the post-Hitomi era SEBASTIAN HEINZ University of Wisconsin - Madison Re-acceleration Model for Radio Relics in Galaxy Clusters Radio relics are diffuse radio sources found in the outskirts of galaxy clusters and they are

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

thought to trace synchrotron-emitting electrons accelerated via diffusive shock acceleration (DSA) at merger-driven shocks. For some radio relics, the shock Mach number inferred from the radio spectral index is often larger than that estimated from the discontinuities in X-ray observations. Here we study the re-acceleration model in which a weak shock encounters the intracluster plasma with a pre-existing population of relativistic electrons. Toward this end, we perform DSA simulations of spherical shocks with the parameters relevant for cluster radio relics and calculate the ensuing radio synchrotron emission from re-accelerated electrons. We demonstrate that the re-accelerated electron spectrum depends on the shape of the preshock electron spectrum, so the shock Mach number cannot be estimated directly from radio spectral index. Moreover, this scenario alleviates the problems regarding low acceleration efficiency of weak shocks and low frequency of merging clusters with detected radio relics. HYESUNG KANG Pusan National University Viscosity, Conduction, Convection, and Dynamo in a Weakly Collisional Magnetized Plasma I will report on recent advances in our understanding of stability, transport, and magneticfield amplification in weakly collisional magnetized plasmas, such as the intracluster medium of galaxy clusters. These include: (1) the linear properties of the magnetothermal instability in a collisionless plasma; (2) the regulation of viscous transport by ion-Larmor-scale kinetic instabilities; (3) the efficacy of heat conduction in the presence of ion-Larmor-scale magnetic mirrors; and (4) turbulent dynamo in a collisionless plasma. All of these subjects are connected by a deceivingly simple question: what is the evolution of a plasma in which the long-wavelength (“fluid”) and small-wavelength (“kinetic”) scales are simultaneously driven unstable by the same free-energy source? MATTHEW KUNZ Princeton University Superdiffusion and Streaming and Acceleration of Cosmic rays I shall relate the modern understanding of MHD turbulence with the basic processes of cosmic ray propagation and acceleration. First of all, I shall show that on the scales less than the turbulence injection scale, which is approximately 100 pc for the Milky Way, cosmic rays undergo super diffusion in the direction perpendicular to the mean galactic magnetic field. Then I will show how turbulence damping of the streaming instability depends on the regime of turbulence, e.g. strong Alfvenic or weak Alfvenic turbulence, and what are the astrophysical

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

consequences of this instability. In particular, I shall show that the in the Galactic halo the weak turbulence and not strong turbulence is responsible for the damping of the streaming instability. Finally, I shall discuss how these two processes affect cosmic ray acceleration in shocks. ALEX LAZARIAN University Wisconsin - Madison New High-order Methods using Gaussian Processes for CFD We present an entirely new class of high-order numerical algorithms for computational fluid dynamics. The new method is based on the Gaussian Processes (GP) modeling that generalizes the Gaussian probability distribution. Our approach is to adapt the idea of the GP prediction technique which utilizes the covariance kernel functions, and use it to reconstruct a highorder approximations for computational simulations. We propose the GP high-order method as a new numerical high-order formulation, alternative to the conventional polynomial-based approaches. We will show that the GP method is shown to be much faster in both convergence and performance rates than the popular choices of polynomial-based high-order methods such as PPM, WENO-5, and WENO-Z. DONGWOOK LEE University of California, Santa Cruz Jet-Lobe Morphology Under the Cluster Weather: Inferences on ICM Dynamics and Jet Composition Jets and lobes in the ICM are expected to be affected by their galaxy cluster environment and indeed observations often reveal distortions in jet-lobe morphologies. We present 3D MHD modeling of these systems and study the physical processes that might be occurring. We will discuss several findings: 1) jet survival is non-trivial and it can place strong constraints on the jet composition; 2) jet distortions can be used to infer the ICM conditions, its motion and energetics. Implications for inferring AGN feedback in the ICM will also be discussed. HUI LI Los Alamos National Laboratory Heating in Simulated Galaxy Clusters with Momentum-driven AGN Feedback AGN feedback is widely considered the major heating source to prevent a classical cooling flow in the center of galaxy clusters. Numerical simulations have shown that momentum-driven AGN feedback can suppress cooling successfully and reproduce cluster properties generally in good

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

agreement with the observations. However, exactly how the jet is coupled to the intra-cluster medium is still unclear. In this work, we study how much heating comes from shock waves, and how much from turbulent dissipation in a simulation where cooling is balanced by AGN feedback. We also examine how the importance of different heating processes changes as a function of time, distance to the center, and the thermal properties of the gas. YUAN LI Columbia University Shattering cold gas into tiny cloudlets Absorption studies of galaxies and galaxy clusters at high-redshift have unexpectedly found that their halos are also full of cold gas, in addition to the theoretically-predicted virialized plasma. These observations typically indicate a relatively modest total fraction of cold gas (~10^{-4}% by volume), yet find it in essentially every sightline through the galaxy. I will show that cold gas clouds are prone to “shattering” into tiny fragments, and that the resulting small clouds naturally reproduce the large area-covering fractions and small volume-filling fractions inferred from observations. This same effect enhances the drag force coupling the dynamics of cold and hot gasses; I will also discuss potential applications to entrainment of cold gas in galaxy winds, and the possibility of using cold gas to constrain the kinematics of the hot ICM. MIKE MCCOURT University of California, Santa Barbara Thermal Instability in Low Entropy Gas Lifted behind Buoyantly-Rising X-ray Bubbles Precipitation models indicate that cooling instabilities form when the ratio of cooling time to free-fall in hot atmospheres surrounding massive galaxies falls below ~10, i.e., t_c/t_ff < 10. We show that this criterion is rarely met in central galaxies and is a statistically weaker indicator of cooling instabilities than cooling time alone. Hot atmospheres apparently do not experience large swings in gas density and cooling time in response to powerful AGN outbursts, which is an essential aspect of precipitation models. Based primarily on new ALMA observations, we show instead that molecular gas likely forms from low entropy gas caught in the updraft of rising X-ray bubbles. We suggest that thermal instabilities ensue when the ratio of the cooling time to the infall time of gas lifted to high altitudes falls below unity, i.e., t_c/t_I ~ 1.

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

BRIAN MCNAMARA University of Waterloo New Kid on the Block: Kinematic Sunyaev-Zel’dovich Effect In recent years, the kinematic Sunyaev-Zel’dovich (kSZ) effect measurements of galaxy cluster peculiar velocities have emerged as a new promising probe of cosmology and fundamental physics. However, the power of kSZ cosmology is fundamentally limited by an uncertainty the optical depth of galaxy clusters, which depends sensitively on still poorly understood astrophysical processes, such as star formation and feedback from supernovae and active galactic nuclei on the hot X-ray emitting intracluster medium. I will describe the current state of affairs on our understanding of the optical depth of galaxy clusters from both simulations and observations and discuss a roadmap for the use of kSZ effect (and other cluster-based techniques) as a precision cosmological probe in the era of large-scale CMB and galaxy surveys. DAISUKE NAGAI Yale University Nonlinear thermal instability in the radio mode feedback cycle Substantial masses of cold gas found at the centers of cool core clusters are widely believed to be produced by thermally unstable cooling of the hot intracluster medium. A small part of the cold gas can power the radio jets that prevent much greater quantities of gas from cooling, sustaining a radio mode feedback cycle. I will argue that nonlinear hydrodynamic processes play a critical role in the onset of thermally unstable cooling, helping to define the necessary conditions for thermal instability. I will also show that uplift by radio lobes is a likely mechanism for driving this nonlinear thermal instability. PAUL NULSEN Center for Astrophysics, Harvard-Smithsonian The Role of Turbulence in Accelerating Cosmic Rays and Amplifying B-fields in the ICM I address the role of turbulence in accelerating cosmic rays in cluster radio halos, and whether matching the observations requires fine tuning. I also consider how turbulence induced by shockclump interactions amplify B-fields, and implications for radio relics. PENG OH University of California, Santa Barbara

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

Triggering and delivery methods for AGN feedback In this talk I present a comparison of several common sub-grid implementations of AGN feedback, focusing on the effects of different triggering mechanisms and the differences between thermal and kinetic feedback (although we also attempt to assess the importance of physical resolution and some AGN jet properties as well). Our main result is that pure thermal feedback that is centrally injected behaves differently from feedback with even a small kinetic component. We do not see large differences between implementations of different triggering mechanisms, as long as the spatial resolution is sufficiently high, probably because all of the implementations tested here trigger strong AGN feedback under similar conditions. Our simulations confirm that AGN can regulate the thermal state of cool-core galaxy clusters and maintain the core in a state that is marginally susceptible to thermal instability and precipitation. BRIAN O’SHEA Michigan State University On Helium Mixing in Quasi-global Simulations of the Intra-Cluster Medium The assumption of a spatially uniform helium distribution in the intra-cluster medium can lead to biases in the estimates of key cluster parameters if composition gradients are present. The helium concentration profile in galaxy clusters is unfortunately not observable directly. Current models addressing the putative sedimentation are one-dimensional and parametrize the presence of magnetic fields in a crude way, ignoring the weakly-collisional, magnetized nature of the medium. When these effects are considered, a wide variety of instabilities can play an important role in the plasma dynamics. We have recently developed the local, linear theory of these instabilities and addressed their non-linear development with a modified version of Athena. In this talk, I will present a semi-global approach that we use to simulate the mixing of helium as induced by generalizations of the heat-flux driven buoyancy instability (HBI) and the magneto-thermal instability (MTI), which feed off thermal and composition gradients. In the inner region of the ICM, mixing can occur on few Gyrs, after which the average magnetic field inclination angle is $\sim 45^{\circ}$ resulting in an averaged Spitzer-parameter higher by about 20\% than the value obtained in homogeneous simulations. In the cluster outskirts the instabilities are rather inefficient, due to the shallow gradients. This suggests that compositions gradients in cluster cores might be shallower than one-dimensional models predict. MARTIN PESSAH Niels Bohr Institute

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

Is cosmic ray heating relevant in cool core clusters? The absence of large cooling flows in cool core clusters appears to require self-regulated energy feedback by active galactic nuclei (AGNs) but the exact heating mechanism has not yet been identified. Here, we analyse whether a combination of cosmic-ray (CR) heating that is provided by the AGN and thermal conduction can offset radiative cooling. Using a large sample of about 40 cool core clusters, we determine steady state solutions of the hydrodynamic equations that are coupled to an evolution equation for the CRs. We find stable solutions that match the observed density and temperature profiles for all our clusters well. Radiative cooling is balanced by CR heating in the cluster centres and by thermal conduction on larger scales, thus demonstrating the relevance of both heating mechanisms. Our mass deposition rates vary by three orders of magnitude and are linearly correlated to the observed star formation rates. Clusters with large mass deposition rates show larger cooling radii and require a larger radial extent of the CR injection function. However, the resulting radio-synchrotron and gamma-ray emission of clusters that are hosting radio mini halos is in conflict with observational data suggesting that these clusters cannot be stably heated by CRs. Most interestingly, this inability of supplying sufficient heat to the cooling cluster gas is reflected in the thermodynamic profiles of these cool cores: clusters with radio mini halos are characterised by the largest cooling radii, star formation and mass deposition rates in our sample and thus signal the presence of a higher cooling activity. On the contrary, clusters without radio mini halos show little signs of cooling and appear to be stably heated. This diversity of cool cores for the first time demonstrates evidence for a heating-cooling cycle in cool cores with potentially CR heating from AGNs as the underlying physical source of heat. Contributors:C.Pfrommer, S. Jacob (HITS Heidelberg)C. Pfrommer, HITS Heidelberg, [email protected] S. Jacob, HITS Heidelberg, [email protected] CHRISTOPH PFROMMER Heidelberg Institute for Theoretical Studies Properties of the ICM of Galaxy Cluster from hydrodynamical simulations with AGN feedback Powerful phenomena determine the energy of Galaxy Clusters from sub-pc scales to Mpc distances. Via high-resolution, cosmological and hydrodynamical simulations we studied how the main properties of the ICM (entropy, temperature, pressure, and metallicity) are influences by the presence of the central AGN. We will report on the evolution of profiles and scaling relation between global quantities including luminosity and total mass. Special focus will be given to the metallicity profile. ELENA RASIA University of Michigan

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

Flow dynamics in galaxy clusters Gas stripping of elliptical galaxies in clusters is accompanied by a wealth of fluid dynamics features, including an upstream contact discontinuity between the galactic gas and the cluster ICM, the upstream bow shock, Kelvin-Helmholz-instabilities at the sides of the galactic atmosphere, the galaxy’s gas tail and its wake along its orbit through the ICM. The prominence of each of these features is modified by additional aspects or processes, e.g., the stage of the stripping process, the ellipticity of the galaxy’s potential, transport coefficients in the ICM, or simultaneous AGN activity. I will compare our recent simulations with deep X-ray observations of several galaxies. ELKE ROEDIGER University of Hull Role of cosmic ray heating in the ICM I will briefly discuss preliminary results from the simulations of black hole jet feedback in cool cores of galaxy clusters including the effects of cosmic rays (CR). I will argue that CR diffusion/ streaming out of the AGN-inflated lobes, followed by the heating of the intracluster medium (ICM) via the CR streaming instability, may be an important mechanism responsible for the thermalization of the AGN energy in the ICM. I will also argue that the streaming instability may be a viable mechanism responsible for powering of the Halpha-emitting filaments in clusters. MATEUSZ RUSZKOWSKI University of Michigan Shock Waves in the Outskirt of Galaxy Clusters Galaxy clusters are continuously disturbed by major and minor mergers of clumps and gas infall along filaments of the WHIM. Such activities induce shock waves, which are observed as radio relics and X-ray shocks in cluster outskirts. In this talk, we discuss the properties of shocks that form in sample galaxy clusters from simulations of the large-scale structure of the universe, with a special emphasis on their temporal evolution. We present the radio and X-ray manifestations of simulated shocks, and compare them with observed characteristics of radio relics and X-ray shocks. DONGSU RYU Ulsan National Institute of Technology

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

Metal Mixing in the Presence of a Magnetic Field Random motions are essential to the mixing of entrained fluids, and they are also capable of amplifying weak initial magnetic fields by small-scale dynamo action. I will describe a systematic study of mixing in magnetized media as a function of magnetic Prandtl number and Mach number. Using three-dimensional magnetohydrodynamic simulations that include a scalar concentration field, I show that metallicity gradients are always strongly biased perpendicular to the direction of the magnetic field. This is true both early on, when the magnetic field strength is negligible, and at late times, when the field is strong enough to back-react on the flow. I describe the origin of this anticorrelation and its consequences for modeling metal mixing in the intracluster medium and in other environments. EVAN SCANNAPIECO Arizona State University Simulations of AGN jet feedback in galaxy clusters: heating and cooling cycles I will present results from hydrodynamic simulations of AGN jets interacting with the intracluster medium (ICM). Cold gas condensation (triggered by local thermal instability) and a sudden increase in feedback heating result in overheating of the ICM. Such overheating prevents further cooling and accretion of gas onto the central black hole. In absence of heating the core slowly cools again, restarting the heating cycle. Feedback heating driven by cold gas condensation leads to a large scatter between jet power, cold gas mass, core entropy, etc. I will highlight the importance of angular momentum of cold gas in closing the feedback heating loop. I will compare the kinematics of cold gas in our simulations with the ALMA observations of cold gas in cluster cores. PRATEEK SHARMA Indian Institute of Science, Bangalore Witnessing the growth of the nearest galaxy cluster We present results from the last Suzaku Key Project dedicated to cluster outskirts studies, namely a mosaic of 60 pointings exploring the Virgo Cluster from its centre out to beyond the virial radius along 4 different directions. We discuss the thermodynamical properties in the intracluster medium of this dynamically young system, focusing on departures from hydrodynamic equilibrium and from the expected baseline pressure and entropy profiles. Moreover, we present measurements of the chemical composition of the ICM at large radii and discuss the implication of these results for the chemical enrichment history in the Universe. AURORA SIMIONESCU

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

ISAS – Japan Aerospace Exploration Agency Cluster outskirts as a gateway to the physics of particle acceleration and magnetogenesis Cluster outskirts are expected to be the region where there is maximum conversion of infall gas kinetic energy into the thermal/non-thermal energy components. of the intracluster medium. In this talk I will present recent studies targeting the interplay of turbulence, shocks, magnetic fields and particle acceleration in galaxy cluster outskirts. Using high-resolution grid simulations with the ENZO code, I will discuss how simulations and available observations of non-thermal emissions can constrain, both, the acceleration efficiency of particles at shocks and the origin of extragalactic magnetic fields. FRANCO VAZZA University of Hamburg The Black-Hole Feedback Valve Feedback from a central supermassive black hole is an essential component of galaxy evolution models. Without it, those models cannot obtain massive galaxies and galaxy clusters with the observed properties. However, the black-hole feedback mechanism remains mysterious. Somehow, accretion of matter onto the central black hole of a massive galaxy becomes precisely tuned so that it regulates radiative cooling and condensation of gas in a volume many orders of magnitude larger than the black-hole’s gravitational zone of influence. I will discuss how the required coupling can arise through condensation and precipitation of cold clouds out of a galaxy’s circumgalactic medium, through a mechanism in which the ambient entropy gradient acts as a valve that regulates black-hole feedback. MARK VOIT Michigan State University Deep Chandra observations as probes of detailed ICM physics The spectacular, sub-arcsecond imaging capabilities of the Chandra X-ray Observatory will remain unsurpassed for at least the next 20 years, and deep observations with this instrument still provide opportunities for breakthroughs in our understanding of the microphysics of the hot plasma. I will present new results from deep Chandra observations of the Virgo cold front and the Ophiuchus Cluster, which allow us to place constraints on the effective conductivity and viscosity of the ICM. The deep 500 ks observation of the Virgo cold front reveals intriguing quasi-linear features that may be due to the amplification of magnetic fields by gas sloshing in wide layers below the cold front. The core of the Ophiuchus Cluster lacks strong AGN activity, which may be due to bulk of the cooling taking place offset from the central

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

supermassive black hole. The observed unchecked cooling where a largely dormant AGN is offset from the cooling flow solidifies the idea that AGN play a key role in maintaining the cooling/ heating balance in cluster cores. NORBERT WERNER Stanford University How AGN Jets Heat the Intracluster Medium – Insights from Simulations Feedback from active galactic nuclei (AGN) is believed to prevent catastrophic cooling in galaxy clusters. However, how the feedback energy is transformed into heat, and how the AGN jets heat the intracluster medium (ICM) isotropically, still remain elusive. Since recent simulations based on cold gas accretion and momentum-driven jet feedback have shown remarkable successes reproducing properties of the cool cores (CCs), we use such simulations to gain insights into the mechanisms and distributions of AGN heating. In this talk, I will present our findings on the relative importance of shock heating, mixing with the hot thermal gas within bubbles, and turbulent dissipation. I will also show how the thermal balance is established within the entire CC despite the fact that AGN jets preferentially dump the heat near the jet axis. KAREN YANG University of Maryland Microphysics of ICM from X-ray images: effective equation of state, turbulence, heating The only Hitomi direct velocity measurement in the core of the Perseus cluster showed a surprising consistency with the indirect velocity measurements from the analysis of gas fluctuations imprinted in the high-resolution X-ray images provided by Chandra. This result motivates to extend the analysis of fluctuations on a sample of galaxy clusters, which I will present during the meeting. In particular, I will discuss the effective equation of state of ICM fluctuations, velocity measurements on a range of spatial scales, down to small, microphysical scales, and will address the role of gas motions in the ICM heating. I will emphasize the main assumptions of the analysis, which should be studied numerically in future. IRINA ZHURAVLEVA Stanford University Simulating the ICM As Seen Through the Next Generation of X-ray Telescopes The next generation of X-ray telescopes will have higher effective area and higher spectral resolution. Though we have a number of years to go before Athena and the hoped-for X-ray

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

Surveyor, theorists and simulators can approach the questions that these next great observatories will be able to answer about the structure of the intracluster medium today. I will show using synthetic observations of simulated galaxy clusters the power of high spectral resolution to resolve the kinematical properties of the ICM, as well as the benefits of increased effective area. I will close my talk with a brief presentation of a new initiative to make the data from simulations of galaxy cluster mergers more accessible to the broader community of cluster researchers, for closer comparisons with existing observations and for making predictions for new ones. JOHN ZUHONE Massachusetts Institute of Technology

Cosmic Ray Propagation in High Beta Plasmas Cosmic ray propagation in galaxy clusters is important for understanding nonthermal emission (or its absence) from these systems, and for understanding the energetics of AGN and starforming galaxies. We discuss work in progress on the driving and damping of the cosmic ray streaming instability under the high beta conditions prevailing in cluster plasmas, and the implications for cosmic ray propagation and confinement. ELLEN ZWEIBEL University of Wisconsin - Madison

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A B S T R A C T S

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

WORKSHOP PARTICIPANT LIST CAMILLE AVESTRUZ University of Chicago [email protected] THOMAS BERLOK Niels Bohr Institute [email protected] ANNALISA BONAFEDE Hamburg University Hamburger sternwarte [email protected] MARCUS BRÜGGEN University of Hamburg [email protected] GIANFRANCO BRUNETTI INAF- Istituto di Radioastronomia [email protected] YI-HAO CHEN University of Wisconsin Madison [email protected] MEGAN DONAHUE Michigan State University [email protected] JULIUS DONNERT University of Minnesota [email protected] AUGUST EVRARD University of Michigan [email protected]

PHILIPP GRETE Max-Planck-Institute Sonnensystemforschung [email protected]

DONGWOOK LEE University of California, Santa Cruz [email protected]

SHAUL HANANY University of Minnesota [email protected]

YUAN LI University of Michigan [email protected]

SEBASTIAN HEINZ University of Wisconsin Madison [email protected]

HUI LI Los Alamos National Laboratory [email protected]

SUOQING JI University of California, Santa Barbara [email protected] TOM JONES University of Minnesota [email protected] HYESUNG KANG Pusan National University [email protected] MATTHEW KUNZ Princeton University [email protected] MEHDI LAMEE University of Minnesota [email protected] ALEX LAZARIAN University of Wisconsin Madison [email protected]

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MICHAEL MCCOURT University of California, Santa Barbara [email protected] BRIAN MCNAMARA University of Waterloo [email protected] PETER MENDYGRAL Cray Inc. [email protected] DAISUKE NAGAI Yale University [email protected] CHRIS NOLTING University of Minnesota [email protected] PAUL NULSEN Harvard-Smithsonian Center for Astrophysics [email protected]

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

BRIAN O’NEILL University of Minnesota [email protected]

LAWRENCE RUDNICK University of Minnesota [email protected]

QIAN WANG University of Maryland [email protected]

BRIAN O’SHEA Michigan State University [email protected]

MATEUSZ RUSZKOWSKI University of Michigan [email protected]

GANDHARI WATTAL University of Wisconsin-Madison [email protected]

S. PENG OH University of California, Santa Barbara [email protected]

MICHAEL RUTKOWSKI University of Minnesota [email protected]

NORBERT WERNER Stanford University [email protected]

DONGSU RYU Ulsan National Institute of Technology [email protected]

LILIYA WILLIAMS University of Minnesota [email protected]

MARTIN PESSAH Niels Bohr Institute [email protected] CHRISTOPH PFROMMER Heidelberg Institute for Theoretical Studies [email protected] YONG-ZHONG QIAN University of Minnesota [email protected] ELENA RASIA INAF-OATs / University of Michigan [email protected] GARETH ROBERG-CLARK UMD College Park [email protected] ELKE ROEDIGER E.A. Milne Centre for Astrophysics, University of Hull [email protected]

EVAN SCANNAPIECO Arizona State University [email protected]

ZEWEI XIONG University of Minnesota, Twin Cities [email protected]

PRATEEK SHARMA Department of Physics [email protected]

HSIANG-YI KAREN YANG University of Maryland [email protected]

AURORA SIMIONESCU ISAS/JAXA [email protected]

IRINA ZHURAVLEVA KIPAC, Stanford University [email protected]

FRANCO VAZZA JOHN ZUHONE Hamburg University Harvard-Smithsonian Center for [email protected] Astrophysics [email protected] MARK VOIT Michigan State University ELLEN ZWEIBEL [email protected] University of Wisconsin-Madison [email protected]

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

INSTRUCTIONS FOR UPLOADING TALKS TO THE WORKSHOP FOLDER Please submit a PDF of your talk slides by Friday, August 30, 2016 to be included in the conference web archive. Please include your name in the file name. 1. Use the following link to access the folder: 2016_ICMworkshop:

https://netfiles.umn.edu/xythoswfs/webview/_xy-17948881_1 2. Drop files into the folder or right click and select “upload file” select file and click “open”.

All submitted talks will be archived online for general access at the University of Minnesota’s Digital Conservancy. By submitting your talk slides you are agreeing to the Digital Conservancy’s Copyright policy. For policy details see the website at: http://conservancy.umn.edu Please note that there will be a delay between your upload and final posting on the workshop website. Once all talks have been submitted, participants will be notified by email. As always, any questions may be addressed to [email protected].



***If you are having problems uploading your PDF please email your talk to the workshop email address [email protected]***

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

POSTER TITLES & ABSTRACTS Stirred, not Clumped: the Evolution of Temperature Profiles in the Outskirts of Galaxy Clusters Camille Avestruz University of Chicago X-ray measurements of the intracluster medium (ICM) suggest that temperature profiles at large radii deviate from selfsimilar evolution. Using a mass-limited sample of galaxy clusters from cosmological hydrodynamical simulations, we show that the departure from self-similarity is due to physical processes that are driven by mergers and accretion. The dominant contribution comes from the evolution of non-thermal gas motions that have not yet thermalized (stirring). The evolution of accreting cool, dense gas substructures that bias the average temperature low (clumping), is subdominant. We can mitigate departures from self-similarity with a careful choice of halo overdensity definition that scales out the accretion dependence. These results highlight the importance of understanding non-thermal gas motions in the ICM and the use of galaxy clusters as cosmological probes.

Local Simulations of Instabilities Driven by Composition Gradients in the ICM Thomas Berlok Niels Bohr Institute Weakly collisional and magnetised atmospheres that are stratified in composition and temperature have been shown to be unstable even though the entropy increases with height - with possible consequences for the dynamics of the intracluster medium in galaxy clusters. We have modified the MHD code Athena in order to study atmospheres with a non-uniform composition. On this poster we present the first simulations of the instabilities that are driven by gradients in composition. We find that the instabilities saturate by mixing of the composition and rearrangement of the magnetic field. For simplicity, we have only considered isothermal atmospheres within a local approximation. These assumptions are relaxed in the talk by Martin Pessah.

Subgrid-scale closures for MHD turbulence Philipp Grete Max-Planck-Institute Large eddy simulations (LES) are a powerful method to reduce the billions degrees-of-freedom in numerical simulations of astrophysical MHD turbulence to a tractable number. This is achieved by simulating only the largest and intermediate scales directly, and employing a subgrid-scale model for the smallest scales. Formally this procedure introduces new, unclosed terms in the MHD equations, which encode the interaction of small-scale unresolved motions with both the small and large scales. We present a new nonlinear model that explicitly captures compressibility. This model is systematically tested a priori from the subsonic (Ms = 0.2) to the supersonic (Ms = 20) regime of isothermal, homogeneous, isotropic turbulence. Furthermore, we compare it against a set of traditional models including eddy-viscosity type models and models based on the scalesimilarity hypothesis. We find that the new nonlinear model outperforms the traditional ones in all tests conducted including the representation of the energy flux along the turbulent cascade.

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

POSTER TITLES & ABSTRACTS The Impact of Magnetic Fields on Thermal Instability Suoqing Ji University of California, Santa Barbara Multiphase gas structure is ubiquitous in our universe which exists in both galaxy clusters and galaxy halos. Recent results from COS (Cosmic Origins Spectrograph) suggest that large quantities of cold gas with temperature of a few 10^4 K are found in so called circumgalactic medium (CGM), which extends up to galactic virial radius (~ 100 kpc). However, the origin and stability of such cold gas still remains unclear. In this presented ongoing work, we explore thermal instability as a possible mechanism, and find that the existence of magnetic fields can significantly enhance thermal instability and modify the structure of multiphase gas (even for very weak fields), which is applicable for both ICM and CGM.

jMCMC: Decoding centres of galaxy clusters Kiran Lakhchaura Tarun Deep Saini Prateek Sharma Indian Institute of Science, Bangalore, India We have developed a method based on a free-form model for the projected X-ray emission of a cluster. Our model involves 2N parameters (n, T) for N spherical shells, and is jointly forward fitted to the X-ray data by constructing a Bayesian posterior probability distribution, sampled using Markov Chain Monte Carlo (MCMC). Our method is an improvement over the usual deprojection due to joint fitting and careful consideration of covariance of parameters. We compare our results from a sample of 17 clusters with the much larger samples of Cavagnolo et al. 2009 and Panagoulia et al. 2014. We find that while most cluster cores show constant entropy cores, there are a few in which power-law entropy profiles in the core are allowed. Associated paper: http://adsabs.harvard.edu/abs/2016MNRAS.460.2625L

Shocked Radio Jets: Emerging Complex Structures Chris Nolting University of Minnesota

Rise of the Phoenix: Simulations of Shocking Fossil Radio Plasma Brian O’Neill University of Minnesota Fossil clouds of mildly relativistic electrons from Active Galactic Nuclei (AGN) may contribute to the brightness of diffuse

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

radio sources associated with cluster shocks. To explore this, we have simulated shocks of different strengths running over an evolved narrow-angle tailed radio galaxy (NAT). A NAT is formed from bipolar AGN jets being blown into tails by a strong, perpendicular cross-wind. We evolve the NAT with a continuous AGN source for hundreds of Myr allowing the structure to grow several hundred kpc in length. In our canonical scenarios the AGN shuts off around the time a planar shock front, traveling with shock normal parallel to the jet axis, first encounters the nearest tail. This setup allows us to test the theory behind the formation of so-called radio phoenix sources, as well as investigate the possibility that large, aged clouds of relativistic electrons act as seed particles of certain exceptionally bright, Mpc-scale giant radio relics.

Suppression of Electron Thermal Conduction in the ICM Gareth Roberg-Clark UMD College Park We study the thermal conductivity of electrons in an ICM-like collisionless plasma via kinetic theory, employing both Particle-In-Cell (PIC) numerical simulations and analytic calculations. We solve an initial value problem in which electrons are given a large heat flux parallel to an initially uniform magnetic field and are allowed to relax to a final state. A plasma instability develops that generates turbulence, which then effectively scatters electrons and strongly suppresses the parallel heat conduction. The results suggest that thermal conductivity may be reduced significantly from the nominal Spitzer value in the ICM.

P O S T E R S

Shock front and radio halo in Abell 520 Qian Wang University of Maryland

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

WORKSHOP DINNER VIC’S RESTAURANT

201 SE Main St, Minneapolis, MN 55414 6:30 pm Social Hour 7:15 pm Workshop Dinner

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A link to step-by-step walking directions are on the ICM workshop “Program” tab Under “Directions from West Bank Office Building” click and select “Step-by-step directions” OR You may board the bus outside the workshop hotel at 6:10 pm and the bus will leave approximatly 6:20 pm to drop off at Vic’s.

https://www.google.com/maps/d/edit?mid=18G8LaT9CDxYpRKmrqjJwDO3mqNY

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

ADDITIONAL LOCATIONS A. FTPI and workshop location West Bank Office Building - 1300 S 2nd St, Minneapolis B. Workshop Hotel Courtyard Minneapolis Downtown - 1500 S Washington Ave, Minneapolis C. Workshop banquet location - Vic’s Restaurant 201 SE Main St, Minneapolis

M A P S

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

WEST BANK DINING GUIDE

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WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

PHYSICS OF THE INTRACLUSTER MEDIUM: THEORY & COMPUTATION WORKSHOP August 22 - 24, 2016

THANK YOU FOR YOUR PARTICIPATION!!!

T



he William I. Fine Theoretical Physics Institute (FTPI) was established in 1987 as part of the School of Physics and Astronomy at the University of Minnesota, with the goal of conducting research in theoretical physics at a worldclass level.

The most important function of FTPI is to produce exciting and sound theoretical physics that will have an impact on physics as a whole. To this end the Institute provides a meeting place for theorists from around the globe to exchange and develop ideas. FTPI sponsors short-term workshops and longer-term programs, as well as hosting visiting scholars for long-term stays. Through these and other outreach programs, the Institute serves to advance theoretical physics and to further develop its links to other science and engineering research disciplines, industrial research initiatives, and other academic sectors. For more information please visit our website at www.ftpi.umn.edu

The University of Minnesota is an equal opportunity educator and employer. This publication/material is available in alternative formats upon request. Direct requests to Meghan Murray, FTPI in the School of Physics and Astronomy, [email protected], 612-624-8367. Printed on recycled and recyclable paper with at least 10% postconsumer material.