Download or read book AGN Feedback Heating in Clusters of Galaxies written by Fulai Guo and published by . This book was released on 2008 with total page 254 pages. Available in PDF, EPUB and Kindle. Book excerpt: Recent observations show that the cooling flows in the central regions of galaxy clusters are highly suppressed. Observed active galactic nucleus (AGN)-induced cavities/bubbles are a leading candidate for suppressing cooling. Motivated by observational signatures of a non-thermal particle population in these bubbles and the surrounding intracluster medium (ICM), we first propose a new model of AGN heating, in which the ICM is efficiently heated by cosmic-rays, which are injected into the ICM through diffusion or the shredding of the bubbles by Rayleigh-Taylor or Kelvin-Helmholtz instabilities. We include thermal conduction as well. Using numerical simulations, we show that the cooling catastrophe is efficiently suppressed. The cluster quickly relaxes to a quasi-equilibrium state with a highly reduced accretion rate and temperature and density profiles which match observations. Unlike the conduction-only case, no fine-tuning of the Spitzer conduction suppression factor f is needed. The cosmic ray pressure Pc/Pg & lsim;0.1 and1Pc & lsim;0. 1rg is well within observational bounds.

Download or read book Heating versus Cooling in Galaxies and Clusters of Galaxies written by Hans Böhringer and published by Springer Science & Business Media. This book was released on 2007-09-27 with total page 453 pages. Available in PDF, EPUB and Kindle. Book excerpt: This volume documents recent developments that have advanced our understanding of the heating and cooling mechanisms in galaxies and galaxy clusters. Chapters detail results from multi-wavelength observations and advances in numerical hydrodynamical simulations. An additional section covers new research findings on feedback and self-regulatory mechanisms during cosmic structure formation in general and in galaxy formation in particular.

Download or read book AGN Feedback in Galaxy Formation written by Vincenzo Antonuccio-Delogu and published by Cambridge University Press. This book was released on 2010-10-28 with total page 219 pages. Available in PDF, EPUB and Kindle. Book excerpt: During the past decade, convincing evidence has been accumulated concerning the effect of active galactic nuclei (AGN) activity on the internal and external environment of their host galaxies. Featuring contributions from well-respected researchers in the field, and bringing together work by specialists in both galaxy formation and AGN, this volume addresses a number of key questions about AGN feedback in the context of galaxy formation. The topics covered include downsizing and star-formation time scales in massive elliptical galaxies, the connection between the epochs of supermassive black hole growth and galaxy formation and the question of whether AGN and star formation coexist. Authors also discuss key challenging computational problems, including jet-interstellar/intergalactic medium interactions, and both jet- and merging-induced star formation. Suitable for researchers and graduate students in astrophysics, this volume reflects the engaging and lively discussions taking place in this emerging field of research.

Download or read book Regulation of Star Formation Amidst Heating and Cooling in Galaxies and Galaxy Clusters written by Sravani Vaddi and published by . This book was released on 2016 with total page 342 pages. Available in PDF, EPUB and Kindle. Book excerpt: "Galaxy clusters are the largest gravitationally bound systems in the Universe and often host the largest galaxies (known as the brightest cluster galaxies (BCG)) at its centers. These BCG’s are embedded in hot 1-10 keV X-ray gas. A subset of galaxy clusters known as cool-core clusters show sharply peaked X-ray emission and high central densities, demonstrating cooling of the surrounding halo gas in timescales much shorter than a Hubble time. These observations led to the development of a simple cooling flow model. In the absence of an external heating process, a cooling flow model predicts that the hot intracluster medium gas in these dense cores would hydrostatically cool, generating cooling flows in the center of the cluster. This cooled gas will eventually collapse to form stars and contribute to the bulk of galaxy mass. The rates of star formation actually observed in the clusters however are far less than predicted by the cooling flow model, suggesting a non-gravitational heating source. Active galactic nuclei (AGN), galaxies hosting a supermassive black hole that ejects outflows via accretion, is currently the leading heating mechanism (referred to as AGN feedback) explaining the observed deficit in the star formation rates. AGN feedback also offers an elegant explanation to the observed black hole and galaxy co- evolution. Much of the evidence for AGN feedback has been obtained from studies focussed on galaxy clusters and luminous massive systems with little evidence that it occurs in more typical systems in the local universe. Our research investigates this less explored area to address the importance of AGN heating in the regulation of star formation in typical early type galaxies in the local universe. We selected a sample of 200+ early type, low redshift galaxies and carried out a multiple wavelength study using archival observed in the UV, IR and radio. Our results suggest that early type galaxies in the current epoch are rarely powerful AGN and AGN feedback is constrained to be low in our sample of low redshift, typical early type galaxies. Although heating from the AGN is powerful enough to suppress the cooling of the hot gas, it does not completely offset gas cooling at all times and substantial cooler gas exists in the cores of some galaxy clusters (cool-core clusters), the gas properties of which are not explained by AGN heating models alone. The second part of our research focuses on unravelling the mystery of the unknown heating source regulating star formation in galaxy clusters. We have obtained deep FUV spectroscopy using the HST cosmic origins spectrograph of two cool-core clusters A2597 and Zw3146. FUV spectral lines provide the much needed diagnostics capable of discriminating between various heating models, which was difficult with the standard optical line diagnostics. We investigate several heating/ionization mechanisms namely stellar photoionization, AGN photoionization, and shock heating. We use pre-run Mappings III photoionization code results to model the ionizing radiation field. In general, we notice that there is no one single model that provides a satisfactory explanation for the ionization state of gas. How- ever, we show that stellar and AGN photoionization alone are not enough to ionize the nebula in A2597 and speculate that, shock heating is the likely ionizing source."--Abstract.

Download or read book AGN Feedback in Cool Core Galaxy Clusters written by Yuan Li and published by . This book was released on 2014 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: Jet heating elevates the gas entropy and cooling time, halting clump formation. The cold gas that is not accreted onto the SMBH settles into a rotating disk. In the last few Gyr, the ICM cools onto the disk directly while the innermost region of the disk continues to accrete onto the SMBH, powering the AGN jets to achieve a thermal balance. The mass cooling rate averaged over 7 Gyr is &sim 30 solarmass/yr, an order of magnitude lower than the classic cooling flow value (which we obtain in runs without the AGN). Owing to its self-regulating mechanism, AGN feedback can successfully balance cooling with a wide range of model parameters. Besides suppressing cooling, our model produces cold structures in early stages (up to &sim 2 Gyr) that are in good agreement with the observations. However, the long-lived massive cold disk is unrealistic, suggesting that additional physical processes are still needed. Our recent investigation shows that star formation may play an important role.

Download or read book Clusters of Galaxies Beyond the Thermal View written by Jelle Kaastra and published by Springer Science & Business Media. This book was released on 2008-05-01 with total page 418 pages. Available in PDF, EPUB and Kindle. Book excerpt: The existence of soft excess emission originating from clusters of galaxies, de ned as em- sion detected below 1 keV in excess over the usual thermal emission from hot intracluster gas (hereafter the ICM) has been claimed since 1996. Soft excesses are particularly - portant to detect because they may (at least partly) be due to thermal emission from the Warm-Hot Intergalactic Medium, where as much as half of the baryons of the Universe could be. They are therefore of fundamental cosmological importance. Soft excess emission has been observed (and has also given rise to controversy) in a number of clusters, mainly raising the following questions: (1) Do clusters really show a soft excess? (2) If so, from what spatial region(s) of the cluster does the soft excess or- inate? (3) Is this excess emission thermal, originating from warm-hot intergalactic gas (at 6 temperatures of?10 K), or non-thermal, in which case several emission mechanisms have been proposed. Interestingly, some of the non-thermal mechanisms suggested to account for soft excess emission can also explain the hard X-ray emission detected in some clusters, for example by RXTE and BeppoSAX (also see Petrosian et al. 2008—Chap. 10, this issue; Rephaeli et al. 2008—Chap. 5, this issue).

Download or read book How Active Galactic Nucleus Feedback and Metal Cooling Shape Cluster Entropy Profiles written by and published by . This book was released on with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: Observed clusters of galaxies essentially come in two flavours: non-cool-core clusters characterized by an isothermal temperature profile and a central entropy floor, and cool-core clusters where temperature and entropy in the central region are increasing with radius. Using cosmological resimulations of a galaxy cluster, we study the evolution of its intracluster medium (ICM) gas properties, and through them we assess the effect of different (subgrid) modelling of the physical processes at play, namely gas cooling, star formation, feedback from supernovae and active galactic nuclei (AGNs). More specifically, we show that AGN feedback plays a major role in the pre-heating of the protocluster as it prevents a high concentration of mass from collecting in the centre of the future galaxy cluster at early times. However, AGN activity during the cluster's later evolution is also required to regulate the mass flow into its core and prevent runaway star formation in the central galaxy. Whereas the energy deposited by supernovae alone is insufficient to prevent an overcooling catastrophe, supernovae are responsible for spreading a large amount of metals at high redshift, enhancing the cooling efficiency of the ICM gas. As the AGN energy release depends on the accretion rate of gas on to its central black hole engine, the AGNs respond to this supernova-enhanced gas accretion by injecting more energy into the surrounding gas, and as a result increase the amount of early pre-heating. We demonstrate that the interaction between an AGN jet and the ICM gas that regulates the growth of the AGN's black hole can naturally produce cool-core clusters if we neglect metals. However, as soon as metals are allowed to contribute to the radiative cooling, only the non-cool-core solution is produced

Download or read book Active Galactic Nuclei written by Volker Beckmann and published by John Wiley & Sons. This book was released on 2013-08-29 with total page 390 pages. Available in PDF, EPUB and Kindle. Book excerpt: Active Galactic Nuclei This AGN textbook gives an overview on the current knowledge of the Active Galacitc Nuclei phenomenon. The spectral energy distribution will be discussed, pointing out what can be observed in different wavebands. The different physical models are presented together with formula important for the understanding of AGN physics. Furthermore, the authors discuss the AGN with respect to its environment, host galaxy, feedback in galaxies and in clusters of galaxies, variability, etc. and finally the cosmological evolution of the AGN phenomenon. This book includes phenomena based on new results in the X-Ray and gamma-ray domain from new telescopes such as Chandra, XMM-Newton, the Fermi Gamma-Ray Space Telescope, and the VHE regime not mentioned so far in AGN books. Those and other new developments as well as simulations of AGN merging events and formations, enabled through latest super-computing capabilities. From the contents: The observational picture of AGN Radiative processes The central engine AGN types and unification AGN through the electromagnetic spectrum AGN variability Environment Quasars and cosmology Formation, evolution and the ultimate fate of AGN What we do not know (yet)

Download or read book The Relationship Between Active Galactic Nuclei and Metal enriched Outflows in Galaxy Clusters written by Charles Kirkpatrick and published by . This book was released on 2012 with total page 141 pages. Available in PDF, EPUB and Kindle. Book excerpt: Clusters of galaxies are host to powerful Active Galactic Nuclei (AGN) that greatly affect the thermal history of clusters. By keeping X-ray emitting gas from cooling, massive, run away star formation does not occur in the brightest cluster galaxy (BCG). This is achieved through radio jets displacing large quantities of metal-rich gas and carving out cavities in the intracluster medium (ICM). This metal-rich gas was originally formed within the BCG and ejected through type Ia supernovae. The current distribution of the ejecta suggests an extra source of energy has spread the material far out into the ICM. Currently, it is unclear what mechanisms are responsible. In this thesis, I present evidence, in the form of X-ray imaging and spectra, that establishes a link between AGN and the observed distribution of metal-rich gas. First, the BCG in the Abell 1664 cluster is unusually blue and is forming stars at a rate of ~23 solar masses per year. The BCG is located within 5 kpc of the X-ray peak, where the cooling time of 3.5x10^8 yr and entropy of 10.4 keV cm^2 are consistent with other star-forming BCGs in cooling flow clusters. The cooling rate in this region is roughly consistent with the star formation rate, suggesting that the hot gas is condensing onto the BCG. We use the scaling relations of Birzan et al. (2008) to show that the AGN is underpowered compared to the central X-ray cooling luminosity by roughly a factor of three. We suggest that A1664 is experiencing rapid cooling and star formation during a low-state of an AGN feedback cycle that regulates the rates of cooling and star formation. Modeling the emission as a single temperature plasma, we find that the metallicity peaks 100 kpc from the X-ray center, resulting in a central metallicity dip. However, a multi-temperature cooling flow model improves the fit to the X-ray emission and is able to recover the expected, centrally-peaked metallicity profile. Next, using deep Chandra observations of the Hydra A galaxy cluster, we examine the metallicity structure near the central galaxy and along its powerful radio source. We show that the metallicity of the ICM is enhanced by up to 0.2 dex along the radio jets and lobes compared to the metallicity of the undisturbed gas. The enhancements extend from a radius of 20 kpc from the central galaxy to a distance of ~120 kpc. We estimate the total iron mass that has been transported out of the central galaxy to be between 2E7 and 7E7 solar masses which represents 10% - 30% of the iron mass within the central galaxy. The energy required to lift this gas is roughly 1% to 5% of the total energetic output of the AGN. Evidently, Hydra A's powerful radio source is able to redistribute metal-enriched, low entropy gas throughout the core of the galaxy cluster. The short re-enrichment timescale

Download or read book Thermal Properties of the Gas in Early type Galaxies and Galaxy Clusters written by Rachel L.S. Frisbie and published by . This book was released on 2020 with total page 220 pages. Available in PDF, EPUB and Kindle. Book excerpt: Most of the baryons, or "normal" matter, found in galaxies and galaxy clusters are found in the hot, X-ray emitting gas known as the circumgalactic medium (CGM) or intracluster medium (ICM). The hot gas traces the gravitational potential well and is affected by both thermal and gravitational processes, so we use observations of the hot gas to explore changes across the galaxy or cluster's radius. Heating and cooling in the central regions of galaxies and clusters is primarily driven by feedback processes, including Active Galactic Nuclei (AGNs) and Type Ia supernovae. We can use X-ray observations of the hot gas to understand its thermal history and how the various feedback mechanisms affect the gas at small and large radii. Furthermore, we use X-ray gas properties (temperature, density, entropy, concentration, centroid shift, and power ratios) to characterize galaxies and clusters, understand their evolution, and classify them in meaningful ways. The combination of observations along with theoretical models and simulations explored in this thesis provides key insight into understanding how feedback processes affect the hot gas.I begin by presenting gas property results for a uniformly reduced sample of 348 galaxy clusters and show how those results can be used to characterize the sample and for further galaxy cluster science. I will then turn my focus to early-type galaxies for the remainder of this work. I examine a sample of 12 nearby early-type galaxies with powerful radio sources and find that IC 4296 exhibits unusually low central entropy as previously observed in NGC 4261. We also find some evidence that the minimum of the ratio between the cooling time and free-fall time, if it occurs at the galaxy center, may indicate the presence of a powerful radio source. Finally, I examine the galactic atmospheres of a sample of 49 early-type galaxies. I will show that the equilibrium pressure and density radial profiles for single- and multiphase galaxies agree with the Voit et al. (2020) theoretical model. I also find evidence for a correlation between the central velocity dispersion and entropy profile slope of the galaxies in the sample that agrees with the theoretical model.

Download or read book Probing the Physics of AGN Feedback with High Resolution X ray Spectroscopy written by Anna Maria Ogorzalek and published by . This book was released on 2019 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: Active galactic nuclei (AGN) significantly impact the evolution of their host galaxies, as they can prevent star formation by either expelling large fractions of gas with wide-angle outflows, or by heating up the halo gas with jets. However, how the AGN energy is transferred to the galaxy in either of these feedback modes is still not known. My dissertation research involves novel applications of modern inference techniques to high resolution X-ray spectra in order to gain new insights into the physical processes behind AGN feedback. First, our improved Bayesian framework for the self-consistent modelling of deep spectra from nearby AGN with X-ray detected outflows is introduced. For the first time we are able to perform robust model selection, while keeping all of the parameter space open. We applied our approach to a new, deep Chandra High Energy Transmission Grating observation of the Seyfert-1 galaxy NGC 4051, where we successfully mapped multiple absorbing components moving at a few 1000 km/s. We obtained one of the tightest outflow density constraints to date, thereby measuring the wind's impact on the galaxy. Second, our unprecedented measurements of the gas turbulent velocities in the cores of 13 nearby giant elliptical galaxies are presented. These new constraints were obtained by statistically combining resonant scattering and direct line broadening, studied with deep XMM-Newton Reflection Grating Spectrometer observations. This allowed us to explore the precise nature of the hot gas motions in massive galaxies and constrain models of AGN feedback in these objects. Then, a successful application of our resonant scattering analysis to the first X-ray microcalorimeter observation, the Hitomi Perseus Cluster spectrum, is discussed. This analysis allowed us to place constraints on the hot gas turbulence in a galaxy cluster that are independent of direct line width measurements. This technique can also provide unique clues to the three dimensional structure of the gas velocity field when statistical uncertainties are minimized. Both of the presented analyses will naturally extend to new data sets from the upcoming high spectral resolution X-ray missions, such as XRISM, ATHENA, Arcus, and Lynx.

Download or read book Feedback Regulated Star Formation in Cool Core Clusters of Galaxies written by Grant Russell Tremblay and published by . This book was released on 2011 with total page 440 pages. Available in PDF, EPUB and Kindle. Book excerpt: "The classical 'cooling flow' model historically associated with 'cool core' clusters of galaxies fails in the absence of an external, non-gravitational heating mechanism needed to offset catastrophic radiative losses of the X-ray bright intracluster medium (ICM). Numerous proposed solutions exist, including feedback from active galactic nuclei (AGN), which may elegantly calibrate fundamental relationships such as the coupled co-evolution of black holes and the stellar component of their host galaxies. AGN feedback cannot completely offset cooling at all times, however, as the brightest cluster galaxies (BCGs) in cool core clusters harbor extensive warm (~104 K) and cold (10

Download or read book The Co evolution of Galaxies and Their Surrounding Environments in Massive Galaxy Clusters written by Steven Ehlert and published by . This book was released on 2013 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: A key yet poorly understood component to galaxy evolution models is the influence of the local environment, and is a particularly important aspect to understanding the evolution in galaxy clusters. Galaxy clusters are not only host to significant overdensities of galaxies, but these galaxies are embedded in a hot, diffuse Intracluster Medium (ICM). The ICM has long been observed to have important and lasting impacts on the properties of their constituent galaxies, which are commonly attributed to a number of unique astrophysical processes such as the stripping of galaxy gas by the ICM due to ram pressure and repeated tidal interactions. The galaxies in turn have also been observed to play an important role in the evolution of the ICM, especially near the centers of galaxy clusters where powerful outbursts from Active Galactic Nuclei (AGN) can provide a quasi-steady source of heating to the surrounding ICM, a process known as AGN feedback. Although great progress has been made in recent years to understand the connection between galaxies and the ICM, the precise influence of the ICM on cluster galaxies and the astrophysical processes that drive galaxy evolution in clusters are still subject to important uncertainties. It is clear from the data, however, that the predictions of the simplest models of ram pressure stripping, tidal encounters, and AGN feedback are inconsistent with observations; in particular observations taken with the modern generation of X-ray telescopes such as Chandra and XMM-Newton. These telescopes, with their superb angular resolution, large collecting areas, and wide fields of view, have revolutionized our understanding of galaxies in clusters, in particular for AGN. In this thesis, I will present a series of results regarding the nature of ram pressure stripping, harassment, and AGN feedback in cluster member galaxies driven primarily by X-ray observations. These results include multiwavelength observations of one of the most extreme cases of AGN feedback currently known, a mosaic of galaxies in the nearby Virgo Cluster which are all undergoing different variants of ramp pressure stripping, and the first set of results from one of the largest X-ray AGN surveys ever undertaken with Chandra. All of these results suggest an intricate choreography between the gas reservoirs initially hosted by galaxies and the surrounding ICM, with tests that investigate length scales ranging from 10 kpc to 1 Mpc.

Download or read book Multi wavelength Studies of AGN Feedback and Non thermal Emission in Galaxy Clusters and Groups written by Thomas Pasini and published by . This book was released on 2022 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt:

Download or read book Unveiling the Origin of Filamentary Structures Around Central Galaxies in Groups and Clusters written by Valeria Olivares and published by . This book was released on 2020 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: The classical cooling-flow' model fails in the absence of an external non-gravitational heating mechanism needed to offset catastrophic radiative cooling in the intracluster medium (ICM) of galaxy clusters. Feedback from an active galactic nuclei (AGN) contributes to offset the cooling through bubbles inflated by radio jets launched from massive black holes. However, it cannot completely offset the cooling, as the brightest cluster galaxies (BCGs) harbors extended warm and cold gas reservoirs of gas, whose physical nature remains unknown. The aim of this thesis is to understand the life-cycle of gas in the presence of radio-mechanical AGN-feedback by studying the filamentary network surrounding nearby Brightest Cluster Galaxies and Brightest Group Galaxies (BGGs). We present 15 galaxy clusters and 18 galaxy groups to investigate the origin and physical state of these gaseous filaments. By combining ALMA, MUSE observations, and archive optical textit{Hubble Space Telescope}, X-ray textit{Chandra}, radio VLA, GMRT observations, we have assembled a comprehensive picture of these enigmatic filaments.BCGs reveal extended networks, 10--60~kpc, of Halpha filaments as a consequence of residual cooling from the hot ICM. ALMA observations show clumpy, massive, molecular filaments, preferentially located beneath the radio bubbles inflated by the AGN. The optical nebula is certainly tracing the warm envelopes of cold molecular filaments. Surprisingly, the radial profile of the Halpha/CO flux ratio is roughly constant for most of the objects, revealing that cold gas could be present in the faintest filaments detected in Halpha, and indicating that a local process must be responsible for the excitation mechanism of the gas. To investigate where the cold gas condensed out from the ICM, we compare the radial extent of the filaments with predictions from numerical simulations. We found that the filaments are always inside the low-entropy region, and where the ratio of the cooling time over the free-fall time is minimum, and similarly, where the ratio of the cooling time to the eddy-turnover time is approximately unity. This may be consistent with theoretical predictions, which argue that cold gas might condense from the cooling of the ICM via the top-down cascade through thermal instabilities. Finally, we found that the velocity of the molecular gas is below the escape velocity of the BCG, indicating that cold clouds must then fall back onto the black hole, feeding the central engine, where the cycle starts again.By extending the sample, including 18 galaxy groups, we explore an intermediate-mass range between individual galaxies and massive clusters, offering an exciting avenue to study the life-cycle of gas and the effect of AGN-feedback. Our MUSE observations reveal ionized gas distributed on principally within filamentary structures, 3--14~kpc, but massive rotating disks and rings are also identified, in comparison to galaxy clusters where the filaments are ubiquitous. The exaltation of gas appears to be dominated by LINERS; though, star-formation is identified within the clumpy rings. Spatial and kinematic information of the molecular phase is required to understand the evolutionary scenario of gas cycling entirely. Our NOEMA observations of a disk source reveal that these two temperature phases are cospatial and comoving, which might hint a common origin.Significant progress has been made in the understanding of the origin of the filamentary structures in galaxy clusters and groups by increasing the size of the sample. However, many questions remain in the inkwell. Future high-spatial and spectral resolution facilities, such as Athena satellite, will yield a more complete view of the nature of the gas.

Download or read book AGN Feedback and Delivery Methods for Simulations of Cool core Galaxy Clusters written by Gregory Robert Meece and published by . This book was released on 2016 with total page 193 pages. Available in PDF, EPUB and Kindle. Book excerpt:

Download or read book Numerical Simulations of Plasmas in Galaxy Clusters written by Forrest Wolfgang Glines and published by . This book was released on 2022 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: As the largest gravitationally bound objects in the universe, galaxy clusters are a unique probe of large scale cosmological structure. Determining the distribution of galaxy clusters and their virial masses may be key to constraining properties of dark energy and dark matter. Since 84%of a typical galaxy cluster's mass is comprised of non-radiating dark matter, however, determining the virial mass of galaxy clusters depends on inference from the radiating baryonic matter. 84%of this baryonic matter is contained in the intracluster medium (ICM)-a hot, diffuse, magnetized plasma permeating the galaxy cluster. While the baryonic matter is the only emitter of observable electromagnetic emissions from galaxy clusters, the complex behavior of the ICM as a turbulent magnetized plasma makes constraining the virial mass of the cluster with observable signatures difficult. Numerical simulations are essential tools for advancing understanding of the ICM and for tying galaxy cluster observables to virial masses. The goal of this dissertation is to explore and enable simulations of galaxy clusters and magnetized plasmas via a number of different avenues.I first explore self-regulation of feedback from active galactic nuclei (AGN) preventing over-cooling in cool-core (CC) clusters-galaxy clusters with anomalously high central thermal emission which should cool on shorter timescales than they persist. In the idealized galaxy cluster simulations with a thermal abstraction of AGN feedback, we find that the thermal-only heating kernels we test are unable to offset cooling while maintaining a realistic structure, suggesting exploration of more complex AGN feedback mechanisms such as those including magnetic fields and turbulence.We then explore how kinetic and magnetic energy thermalizes in the ICM by studying decaying magnetized turbulence with simulations of the magnetized compressible Taylor-Green vortex. Using a shell-to-shell energy transfer analysis, we find that the magnetic fields facilitate a significant amount of the energy flux that is not seen in hydrodynamic turbulence. Although the full cascade will not be directly captured in ICM simulations for the foreseeable future, higher resolution simulations enabled by larger computational resources can diminish such effects.Different novel many-core architectures have emerged in recent years on the way toward larger supercomputers in the exascale era. Performance portability is required to prevent repeated nontrivial refactoring of a code for different architectures. To address the need for a performance portable magnetohydrodynamics (MHD) code, we combined Athena++, an existing MHD CPU code, with Kokkos, a performance portable framework, into K-Athena to allow efficient simulations on multiple architectures using a single codebase. K-Athena has also inspired the Parthenon performance portable adaptive mesh refinement (AMR) framework. Using this framework, we developed the performance portable AMR MHD code AthenaPK.Galaxy clusters contain significant magnetic fields, although their origin and role is still under investigation. Numerical modeling is essential for the inference of their properties. One aspect is whether magnetic AGN feedback models can self-regulate. I present work-in-progress simulations with AthenaPK of magnetized galaxy clusters slated for exascale supercomputers later this year.With the higher resolutions enabled by exascale systems, galaxy cluster simulations with relativistic jet velocities will be possible. Robust methods for relativistic plasmas will be needed. With this goal, I present a discontinuous-Galerkin (DG) method for relativistic hydrodynamics. We include an exploration of different methods to recover the primitive variables from conserved variables, a new operator for enforcing a physically permissible conserved state, and numerous tests of the method. This method has been used at Sandia National Laboratories to study terrestrial plasmas and will inform relativistic MHD methods for AthenaPK.Finally, I cover the future directions of the work in this dissertation, including the many codes enabled by Parthenon, additions to the magnetized galaxy cluster simulations with AthenaPK, and the large body of projects at Los Alamos National Laboratory to explore binary black hole mergers embedded within AGN accretion disks as a possible formation channel of the massive black holes observed by LIGO. The work in this dissertation to develop performance portable plasma simulations will enable ground-breaking simulations for years to come.