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The Hot Atmospheres of X-Shaped Radio Galaxies

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The Hot Atmospheres of X-Shaped Radio Galaxies Abstract Title of Dissertation: The Hot Atmospheres of X-Shaped Radio Galaxies Edmund Hodges-Kluck, Doctor of Philosophy, 2011 Dissertation directed by: Professor Christopher Reynolds Department of Astronomy We present an observational and numerical study of X-shaped radio galaxies, a subset of the double-lobed radio galaxies with a second set of lobes or “wings.” These sources have been proposed as the “smoking gun” of supermassive black hole mergers, in which case the secondary lobes would be fossil remnants following a black hole spin-flip jet reorientation. However, they may instead originate in the interplay between giant radio lobes and their hot plasma environments, since radio lobes can be considered as bubbles of light fluid in the heavier intracluster medium. Circumstantial evidence from studies of the host galaxies at optical wavelengths indicates that this may indeed be the case, leading to two important questions we attempt to answer in this work: (1) Does it appear that X-shaped radio galaxies are aware of their environments? (2) Can radio galaxies respond to their environments in such a way as to form X-shaped morphology? We use radio, optical, and X-ray imaging data to investigate the first question, finding that, in general, X-shaped sources have jets co-aligned with the major axes of their hot (X-ray emitting) atmospheres and wings co-aligned with their minor axes. However, in at least one case (where the jet clearly does not follow this trend), a deep X-ray observation suggests that rapid reorientation of the jet axis is the best explanation. Moreover, despite the trend we discover, the hydrodynamic models of wing formation have significant theoretical problems. Thus, the second major component of this thesis is concerned with using hy- drodynamical simulations to determine whether X-shaped radio galaxies can be produced in response to asymmetries in the atmosphere. We inject jets as light fluids into a model cluster or galactic atmosphere previously in hydrostatic equi- librium, thereby forming bubbles similar to those observed in radio galaxies. Since we inject the jet along the major axis of an asymmetric atmosphere, distortions to the canonical double-lobed radio galaxy result from different responses to the local pressure gradient. With a significantly anisotropic atmosphere and a powerful but decaying jet, we find that X-shaped morphology indeed results for reasonable jet and cluster parameters. However, it is unclear whether our simulated mechanism would be effectual in nature because of the high degree of anisotropy required and the differences between some observed wings and our model wings. We make a number of predictions which we would expect to be observed in the future if the hydrodynamic model is at work. The Hot Atmospheres of X-Shaped Radio Galaxies by Edmund Hodges-Kluck Dissertation submitted to the Faculty of the Graduate School of the University of Maryland at College Park in partial fulfillment of the requirements for the degree of Doctor of Philosophy 2011 Advisory Committee: Professor Christopher Reynolds, chair Doctor Teddy Cheung Professor Kara Hoffman Professor Richard Mushotzky Professor Sylvain Veilleux c Edmund Hodges-Kluck 2011 Preface The contents of this thesis have been published in a series of three articles in The Astrophysical Journal. Brief supplementary material excluded from these articles for brevity has been included here when necessary for clarity. The bibliographic information of the published portions of this thesis follows: • The Chandra View of Nearby X-shaped Radio Galaxies (Chapter 2) Hodges-Kluck, E., Reynolds, C. S., Cheung, C. C. & Miller, M. C. 2010, ApJ, 710, 1205 • A Deep Chandra Observation of the X-shaped Radio Galaxy 4C +00.58: A Candidate for Merger-induced Reorientation? (Chapter 3) Hodges-Kluck, E., Reynolds, C. S., Miller, M. C. & Cheung, C. C. 2010, ApJL, 717, 37 • Hydrodynamic Simulations of Radio Galaxies: Winged and X-shaped Sources (Chapter 4) Hodges-Kluck, E. & Reynolds, C. S. 2011, ApJ, 733, 58 The entirety of this work has been supervised by Prof. Christopher Reynolds and has been divided evenly between observational X-ray, optical, and radio studies and hydrodynamic simulations. Committee members Profs. Richard Mushotzky and Sylvain Veilleux bring substantial expertise in X-ray astronomy, active galactic nuclei, and the environments of galaxies. Dr. Teddy Cheung is intimately involved in discerning the origin of X-shaped radio galaxies and provides substantial expertise in radio astronomy, radio galaxies, and high energy astrophysics. ii To Scott Paine, who had faith in me on Cerro Sairecabur. iii Acknowledgements My deepest gratitude is to my advisor, Chris Reynolds, for three years of guidance, assistance, and friendship. Chris is an exceptional scien- tist possessed of a remarkable clarity of explanation, and a wonderful resource for any aspiring astronomer. I am very fortunate to have had the chance to work with him, and look forward to continued collabora- tion. As a graduate student, it is easy to take an R.A. for granted, so I am especially grateful for all the work he has done to secure funding, data, and a postdoctoral position, and for the chance to visit Hawaii and Japan. I also owe a debt of gratitude to my previous advisors: Andy Harris, su- pervisor of the Second Year Project that won’t end, and Alex Brown and Tom Ayres at Colorado who introduced me to astrophysics. Andy has been a continual source of encouragement and guidance, and it has been through working with him over the past five years that I have learned the most about designing and carrying out an original astrophysical ex- periment from start to finish. Thanks to Andy, I can claim the coveted iv title of “multiwavelength observer.” To Alex, thanks for talking to me virtually every day through my first exposure to real astronomy. Of course, I have not solely worked with my past advisors. I am indebted to Teddy Cheung for his careful attention to my work and motivating this dissertation, Marc Pound for his introduction to reducing CARMA data and ongoing participation in the Galactic Center project, and Cole Miller for his back-to-basics approach to work. Thanks to Richard Mushotzky for frequently providing a broader perspective on my interests. I have learned a great deal about how to be an effective astronomer from you all. None of this work would be possible without the instrumentation and software built to do the science. I extend my thanks to the Chandra, VLA, SDSS, and CARMA teams, to the developers of ZEUS, and to John Vernaleo for working the bugs out of much of the code I use. I would be remiss if I did not also acknowledge the important role the de- partment administration has played in my life here, albeit usually behind the scenes. Thanks especially to Adrienne Newman and Susan Lehr for looking out for me, and to MaryAnn Phillips for guarding the sanctity of our work environment. Virtually all of the interactions I’ve had at the University of Maryland have been positive, and for the culture of the department I am grateful. I would like to acknowledge the UMD grad students who make coming to work a pleasure: BAZ, DSJ-H, SRS, MJK, MED, KHP, HG, SK, MAM, DRP, RIH-C, MJA, and AML. Thanks for the many little adventures, trips to the Union, and late-night goofing around. v Thanks as well to friends outside of the campus. In particular, my church family and small group has made me feel at home in metro DC, and I thank Kevin Offner and the grads in InterVarsity for years of friendship. Thanks again to Ann Wion for friendship and hospitality, and to Helen McComas for the gift of so much furniture when I first arrived. Last but certainly not least, I would like to thank my family for years of love and support. To my parents, who impressed upon me the im- portance of finding work you can love and working at it, thank you. To Stefan, thanks for putting up with me over the years, and for many fond childhood memories. Finally, to Jana, I can’t express how grateful I am to you and for you. Knowing you has been one of the great joys of my life. vi Contents List of Tables x List of Figures xi 1 Introduction 1 1.1 Radio Galaxies . 2 1.2 Radio Galaxy Morphology . 5 1.3 Active Galactic Nuclei . 12 1.4 The Hot Atmospheres of Radio Galaxies & Radio-Mode Feedback . 18 1.5 X-shaped Radio Galaxies . 24 1.6 Relevant Astronomical Instrumentation . 32 1.6.1 Chandra X-ray Observatory . 32 1.6.2 The Very Large Array & Radio Interferometry . 35 1.7 Dissertation Outline . 38 2 The Chandra View of Nearby X-shaped Radio Galaxies 41 2.1 Introduction . 41 2.2 Chandra Observations . 45 2.2.1 Preliminary Target Selection . 47 2.2.2 Data Reduction . 49 2.2.3 Spectral Extraction . 56 2.2.4 Detection of Diffuse Gas . 60 2.2.5 Radio & Optical Maps . 71 2.3 Thermal Atmosphere Properties . 73 2.3.1 Ellipse Fitting . 74 2.3.2 Optical—X-ray Correlation . 81 2.3.3 X-ray—Radio Correlation . 85 2.4 Properties of the Central Engine . 93 2.5 Discussion & Summary . 95 vii 3 A Deep Chandra Observation of the X-shaped Radio Galaxy 4C +00.58 98 3.1 Introduction . 98 3.2 Observations . 99 3.3 Results . 102 3.3.1 Hot Atmosphere . 102 3.3.2 Wings . 104 3.3.3 Nucleus and Jet . 105 3.4 Wing Formation Models . 108 3.5 Context and Summary . 111 4 Hydrodynamic Models of Radio Galaxy Morphology: Winged and X-shaped Sources 112 4.1 Introduction .
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