DOCSLIB.ORG

View Letters, 121, 211302, (2018)

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
View Letters, 121, 211302, (2018) Constraining Dark Matter Properties with Dwarf Galaxies and Galaxy Clusters DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Stacy Yeonchi Kim Graduate Program in Astronomy The Ohio State University 2019 Dissertation Committee: Professor Annika Peter, Advisor Professor David Weinberg Professor Christopher Kochanek Copyright by Stacy Yeonchi Kim 2019 Abstract Dark matter makes up the overwhelming majority of the matter in the Universe. Its complex structure and dynamics play an essential role in the evolution and formation of galaxies, stars, and ultimately, life itself. Although dark matter is a cornerstone of modern cosmology, the fundamental question of its identity remains unknown. Astrophysical studies have yielded many clues: it is likely an exotic new particle that is relatively massive, uncharged, stable to decays, and does not appear to obey any force other than gravity. Despite these hints, its exact particle identity remains elusive, and dark matter candidates abound. In this dissertation, I present the theoretical groundwork I have laid to harness the tremendous statistical power promised by upcoming astronomical surveys to produce robust new constraints on the dark matter model space. In particular, I have derived the strongest constraints to date on two dark matter properties: its ability reproduce the structural hierarchy of the universe down to low mass scales, and whether or not it obeys a new \dark" force that allows dark matter particles to exchange momentum. My work has already ruled out potential dark matter candidates and promises to further constrain the parameter space of others. These results will inform complementary searches by the particle physics community, ii bringing us closer to the identity of the dark matter particle(s), one of the most pressing open questions in cosmology today. iii Dedication To my parents, who sacrificed so much to come to the States, and to raise us, and to Tom, the viscosity to my turbulence. iv Acknowledgments Its been a long six years that I have been here. In those six years, I've met so many wonderful, amazing people that I'm so grateful to have known. I can't adequately express the thanks I have for them, and the role they've played during my graduate career, but here is an attempt at doing so. Firstly, to Annika, a huge thank you. I owe so much of the successes in my graduate school career to you. It hasn't been the easiest journey to get here, but I was encouraged countless times to continue pushing onwards through your enthusiasm, your many emails, and your words of encouragement|which you went out of your way to express. Thank you for your ardent and vocal support for me during conferences, in communications with colleagues, and in the department at OSU. It was through you that I started feeling like astrophysics not just the science, but also a community that I could identify with, and belong to. I hope I can carry forward the example you set in supporting diversity and a healthy work-life balance, in fostering connections, and in advocating for those who may have been overlooked. I will really miss working with you in Columbus. v I am also immensely grateful to the Department of Astronomy at OSU. The collaboration and enthusiasm that pervades the department, from Astro Coffee to one-on-one meetings, was instrumental in my decision to come to OSU, and a highlight of my time at OSU. I am also grateful for the examples of thoughtful leadership I've witnessed during my time here|one that gives not just an ear but also a voice to the concerns of graduate students and other quieter voices, and takes not just the scientific but also the personal welfare of the community seriously. Last but not least, I am grateful for the support Ive received both personally as well as through nominations for university fellowships and departmental graduate student prizes. To my friends at CGSA, thank you for musing over the less quantifiable mysteries of the universe with me, and opening my eyes to the wonders of childrens literature, music education, evolutionary biology, and American political history, among others. Its incredible that our small planet hosts so many fascinating little worlds of knowledge. Your friendships, above all else, have anchored and refreshed me when the demands and exhaustion of debugging, writing (or rather, unending editing), or nonsensical plots had otherwise consumed my life. To Risa and Al Lazaroff, a heartfelt thanks for treating me like family, and showing me a side of Columbus that I would otherwise never have seen. To Sandy and Jeff Ungar, thank you for your warm hospitality, lovely dinners, and Lucy's furry, energetic company. And a huge thanks to Sue and Jeff Dinitz for welcoming vi me into their home with open arms this past year (and before!) on my quasi-monthly visits to Vermont to see Tom. It's clear where Tom gets his compassion, brilliance, gentleness, heart for service, and love for mountains. To my parents, who have sacrificed so much for me and my sister, even before I was born. Thank you for supporting me and never questioning my decision to pursue physics even despite significant struggles as an undergrad. I am so grateful that you guys let me explore my intellectual interests, despite the possibility of uncertain career prospects|a luxury that not all Asian American college students experience! To my sister, my partner in crime for all things nonsensical. For the late-night chats commiserating about the more unglamorous side of graduate school and job applications; geeking out about good design, presentations, and teaching; all the cat pictures; and everything in between. Life always seems to make more sense after chatting with you. I promise I won't be overseas forever! And of course, Tom. When I first came to Columbus, I felt quite lost for a number of reasons. But when I first met you, I felt like I'd found a home for the first time. Thank you for taking a chance on a quiet Asian girl who didn't know the difference between Star Trek and Star Wars and believes units are integral to calculations. And for not just putting up with all the crazy that comes with the job, but also for helping me address the many (and sometimes mundane) quandaries I find myself in with endless compassion, patience, and creativity. Despite the moves, vii and though hundreds|and soon thousands|of miles separate us, I will always know where to find home. viii Vita January 29, 1991 . Born { Suwon, South Korea 2013 . B.S. Physics, California Institute of Technology 2013 { 2014 . University Fellow, The Ohio State University 2014 { 2018 . Graduate Teaching and Research Associate, The Ohio State University 2019 . Presidential Fellow, The Ohio State University Publications Research Publications 1. L. Pei, M. M. Fausnaugh, A. J. Barth, B. M. Peterson, M. C. Bentz, G. De Rosa, K. D. Denney, M. R. Goad, C. S. Kochanek, K. T. Korista, G. A. Kriss, R. W. Pogge, V. N. Bennert, M. Brotherton, K. I. Clubb, E. Dalla Bont`a,A. V. Filippenko, J. E. Greene, C. J. Grier, M. Vestergaard, W. Zheng, S. M. Adams, T. G. Beatty, A. Bigley, J. E. Brown, J. S. Brown, G. Canalizo, J. M. Comerford, C. T. Coker, E. M. Corsini, S. Croft, K. V. Croxall, A. J. Deason, M. Eracleous, O. D. Fox, E. L. Gates, C. B. Henderson, E. Holmbeck, T. W.-S. Holoien, J. J. Jensen, C. A. Johnson, P. L. Kelly, S. Kim, A. King, M. W. Lau, M. Li, C. Lochhaas, Z. Ma, E. R. Manne-Nicholas, J. C. Mauerhan, M. A. Malkan, R. McGurk, L. Morelli, A. Mosquera, D. Mudd, F. Muller Sanchez, M. L. Nguyen, P. Ochner, B. Ou-Yang, A. Pancoast, M. T. Penny, A. Pizzella, R. Poleski, J. Runnoe, B. Scott, J. S. Schimoia, B. J. Shappee, I. Shivvers, G. V. Simonian, A. Siviero, G. Somers, D. J. Stevens, M. A. Strauss, J. Tayar, N. Tejos, T. Treu, J. Van Saders, L. Vican, S. Villanueva Jr., H. Yuk, N. L. Zakamska, W. Zhu, M. D. Anderson, P. Ar´evalo, C. Bazhaw, S. Bisogni, G. A. Borman, M. C. Bottorff, W. N. Brandt, A. A. Breeveld, E. M. Cackett, M. ix T. Carini, D. M. Crenshaw, A. De Lorenzo-C´aceres,M. Dietrich, R. Edelson, N. V. Efimova, J. Ely, P. A. Evans, G. J. Ferland, K. Flatland, N. Gehrels, S. Geier, J. M. Gelbord, D. Grupe, A. Gupta, P. B. Hall, S. Hicks, D. Horenstein, K. Horne, T. Hutchison, M. Im, M. D. Joner, J. Jones, J. Kaastra, S. Kaspi, B. C. Kelly, J. A. Kennea, M. Kim, S. C. Kim, S. A. Klimanov, J. C. Lee, D. C. Leonard, P. Lira, F. MacInnis, S. Mathur, I. M. McHardy, C. Montouri, R. Musso, S. V. Nazarov, H. Netzer, R. P. Norris, J. A. Nousek, D. N. Okhmat, I. Papadakis, J. R. Parks, J.-U. Pott, S. E. Rafter, H.-W. Rix, D. A. Saylor, K. Schn¨ulle,S. G. Sergeev, M. Siegel, A. Skielboe, M. Spencer, D. Starkey, H.-I. Sung, K. G. Teems, C. S. Turner, P. Uttley, C. Villforth, Y. Weiss, J.-H. Woo, H. Yan, S. Young, and Y. Zu, \Space Telescope and Optical Reverberation Mapping Project. V. Optical Spectroscopic Campaign and Emission-line Analysis for NGC 5548", The Astrophysical Journal, 837, 131, (2017) 2. M. M. Fausnaugh, C. J. Grier, M. C. Bentz, K. D. Denney, G. De Rosa, B. M. Peterson, C. S. Kochanek, R. W. Pogge, S.
Load more

Recommended publications
  • Source-Plane Reconstruction of the Giant Gravitational Arc in A2667: a Candidate Wolf–Rayet Galaxy At
    SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1 Shuo Cao, Giovanni Covone, Eric Jullo, Johan Richard, Luca Izzo, Zong-Hong Zhu To cite this version: Shuo Cao, Giovanni Covone, Eric Jullo, Johan Richard, Luca Izzo, et al.. SOURCE-PLANE RE- CONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF– RAYET GALAXY AT z ∼ 1. Astronomical Journal, American Astronomical Society, 2015, 149, pp.8. 10.1088/0004-6256/149/1/3. hal-01109685 HAL Id: hal-01109685 https://hal.archives-ouvertes.fr/hal-01109685 Submitted on 26 Jan 2015 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. The Astronomical Journal, 149:3 (8pp), 2015 January doi:10.1088/0004-6256/149/1/3 C 2015. The American Astronomical Society. All rights reserved. SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1 Shuo Cao1,2, Giovanni Covone2,3, Eric Jullo4, Johan Richard5, Luca Izzo6,7, and Zong-Hong Zhu1 1 Department of Astronomy, Beijing Normal University, 100875 Beijing, China; [email protected] 2 Dipartimento di Scienze Fisiche, Universita` di Napoli “Federico II,” Via Cinthia, I-80126 Napoli, Italy 3 INFN Sez.
    [Show full text]
  • Small-Scale Structure Is It a Valid Motivation?
    Small-scale Structure Is it a valid motivation? Jakub Scholtz IPPP (Durham) Small Scale Structure Problems <—> All the reasons why “CDM is not it” How did we get here? We are gravitationally sensitive to something sourcing T • <latexit sha1_base64="055AcnSYYRkGsBe2aYAe7vH1peg=">AAAB8XicbVDLSgNBEOz1GeMr6tHLYBA8hV0R9Bj04jFCXphdwuxkNhkyM7vMQwhL/sKLB0W8+jfe/BsnyR40saChqOqmuyvOONPG97+9tfWNza3t0k55d2//4LBydNzWqVWEtkjKU9WNsaacSdoyzHDazRTFIua0E4/vZn7niSrNUtk0k4xGAg8lSxjBxkmPzX4eChtKO+1Xqn7NnwOtkqAgVSjQ6Fe+wkFKrKDSEI617gV+ZqIcK8MIp9NyaDXNMBnjIe05KrGgOsrnF0/RuVMGKEmVK2nQXP09kWOh9UTErlNgM9LL3kz8z+tZk9xEOZOZNVSSxaLEcmRSNHsfDZiixPCJI5go5m5FZIQVJsaFVHYhBMsvr5L2ZS3wa8HDVbV+W8RRglM4gwsI4BrqcA8NaAEBCc/wCm+e9l68d+9j0brmFTMn8Afe5w/beZEG</latexit> µ⌫ —> we are fairly certain that DM exists. • An exception is MOND, which has issues of its own. However, the MOND community has been instrumental in pointing out some of the discrepancies with CDM. • But how do we verify the picture? —> NBODY simulations (disclaimer: I have never run a serious body simulation) 2WalterDehnen,JustinI.Read:N-body SimulationsN-body simulations of gravitational dynamics have reached over 106 particles [6], while collisionless calculations can now reach more than 109 particles [7–10]. This disparity reflects the difference in complexity of these rather dissimilar N-body problems. The significant increase in N in the last decade was driven by the usage of parallel computers. In this review, we discuss the state-of-the art software algo- Takerithms N and dark hardware matter improvements
    [Show full text]
  • MC^ 2: Galaxy Imaging and Redshift Analysis of the Merging Cluster CIZA J2242. 8+ 5301
    LLNL-DOC-661846-DRAFT A Preprint typeset using LTEX style emulateapj v. 8/13/10 MC2: GALAXY IMAGING AND REDSHIFT ANALYSIS OF THE MERGING CLUSTER CIZA J2242.8+5301 William A. Dawson1, M. James Jee2, Andra Stroe3, Y. Karen Ng2, Nathan Golovich2, David Wittman2, David Sobral3,4,5, M. Bruggen¨ 6, H. J. A. Rottgering¨ 3, R. J. van Weeren7 (Dated: Draft June 21, 2021) LLNL-DOC-661846-DRAFT ABSTRACT X-ray and radio observations of CIZA J2242.8+5301 suggest that it is a major cluster merger. Despite being well studied in the X-ray, and radio, little has been presented on the cluster structure and dynamics inferred from its galaxy population. We carried out a deep (i< 25) broad band imaging survey of the system with Subaru SuprimeCam (g & i bands) and the Canada France Hawaii Telescope (r band) as well as a comprehensive spectroscopic survey of the cluster area (505 redshifts) using Keck DEIMOS. We use this data to perform a comprehensive galaxy/redshift analysis of the system, which is the first step to a proper understanding the geometry and dynamics of the merger, as well as using the merger to constrain self-interacting dark matter. We find that the system is dominated by two ′+0.7 +0.13 subclusters of comparable richness with a projected separation of6.9 −0.5 (1.3−0.10 Mpc). We find that the north and south subclusters have similar redshifts of z 0.188 with a relative line-of-sight velocity difference of 69 190kms−1. We also find that north and south≈ subclusters have velocity dispersions of +100 −±1 +100 −1 +4.6 14 1160−90 kms and 1080−70 kms , respectively.
    [Show full text]
  • Hst Frontier Fields Preliminary Map Modeling
    HST FRONTIER FIELDS PRELIMINARY MAP MODELING CATs Team (Clusters As Telescopes) Johan Richard (CRAL Lyon), Benjamin Clement (University of Arizona), Mathilde Jauzac (University of KwaZulu-Natal), Eric Jullo (LAM Marseille), Marceau Limousin (LAM, Marseille), Harald Ebeling (IfA, Hawaii), Priyamvada Natarajan (Yale University), Jean-Paul Kneib (EPFL Lausanne) & Eiichi Egami (University of Arizona). RECONSTRUCTION METHODOLOGY Producing a magnification map involves solving the lens equation for light rays originating from distant sources and deflected by the massive foreground cluster. This is ultimately an inversion problem for which several sets of codes and approaches have been developed independently (see recent review by Kneib & Natarajan 2010). Our collaboration uses LENSTOOL1, an algorithm developed collectively by us over the years. LENSTOOL is a hybrid code that combines observational strong- and weak-lensing data to constrain the cluster mass model. The total mass distribution of clusters is assumed to consist of several smooth, large-scale potentials that are modeled either in a parametric form or non-parametrically, along with contributions from many (typically N > 50) individual cluster galaxies that are modeled using physically motivated parametric forms. For lensing clusters a multi-scale approach is optimal, in as much as the constraints resulting from this inversion exercise are derived from a range of scales. Further details of the methodology are outlined in Jullo & Kneib (2009) and have been extended to the weak-lensing regime (Jauzac et al. 2012). At present, the prevailing modeling approach is to assign a small-scale dark-matter clump to each major cluster galaxy and a large-scale dark-matter clump to prominent concentrations of cluster galaxies (Natarajan & Kneib 1997).
    [Show full text]
  • 16Th HEAD Meeting Session Table of Contents
    16th HEAD Meeting Sun Valley, Idaho – August, 2017 Meeting Abstracts Session Table of Contents 99 – Public Talk - Revealing the Hidden, High Energy Sun, 204 – Mid-Career Prize Talk - X-ray Winds from Black Rachel Osten Holes, Jon Miller 100 – Solar/Stellar Compact I 205 – ISM & Galaxies 101 – AGN in Dwarf Galaxies 206 – First Results from NICER: X-ray Astrophysics from 102 – High-Energy and Multiwavelength Polarimetry: the International Space Station Current Status and New Frontiers 300 – Black Holes Across the Mass Spectrum 103 – Missions & Instruments Poster Session 301 – The Future of Spectral-Timing of Compact Objects 104 – First Results from NICER: X-ray Astrophysics from 302 – Synergies with the Millihertz Gravitational Wave the International Space Station Poster Session Universe 105 – Galaxy Clusters and Cosmology Poster Session 303 – Dissertation Prize Talk - Stellar Death by Black 106 – AGN Poster Session Hole: How Tidal Disruption Events Unveil the High 107 – ISM & Galaxies Poster Session Energy Universe, Eric Coughlin 108 – Stellar Compact Poster Session 304 – Missions & Instruments 109 – Black Holes, Neutron Stars and ULX Sources Poster 305 – SNR/GRB/Gravitational Waves Session 306 – Cosmic Ray Feedback: From Supernova Remnants 110 – Supernovae and Particle Acceleration Poster Session to Galaxy Clusters 111 – Electromagnetic & Gravitational Transients Poster 307 – Diagnosing Astrophysics of Collisional Plasmas - A Session Joint HEAD/LAD Session 112 – Physics of Hot Plasmas Poster Session 400 – Solar/Stellar Compact II 113
    [Show full text]
  • Arxiv:1801.05235V1 [Astro-Ph.CO] 16 Jan 2018
    YITP-18-04 KUNS-2714 RUP-18-2 Primordial Black Holes - Perspectives in Gravitational Wave Astronomy - Misao Sasakia, Teruaki Suyamab, Takahiro Tanakac;a, and Shuichiro Yokoyamad;e a Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan b Research Center for the Early Universe (RESCEU), Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan c Department of Physics, Kyoto University, Kyoto 606-8502, Japan d Department of Physics, Rikkyo University, Tokyo 171-8501, Japan e Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan Abstract This is a review article on the primordial black holes (PBHs), with particular focus on 15 the massive ones (& 10 g) which have not evaporated by the present epoch by the Hawking radiation. By the detections of gravitational waves by LIGO, we have gained a completely novel tool to observationally search for PBHs complementary to the electromagnetic waves. Based on the perspective that gravitational-wave astronomy will make a significant progress in the next decades, a purpose of this article is to give a comprehensive review covering a wide range of topics on PBHs. After discussing PBH formation as well as several inflation models leading to PBH production, we summarize various existing and future observational constraints. We then present topics on formation of PBH binaries, gravitational waves from PBH binaries, various observational tests of PBHs by using gravitational waves. arXiv:1801.05235v1 [astro-ph.CO] 16 Jan 2018 1 Contents 1 Introduction 4 2 Formation of PBHs 6 2.1 Basis of primordial black holes formation in the early Universe .
    [Show full text]
  • MASS and LIGHT of ABELL 370: a STRONG and WEAK LENSING ANALYSIS ABSTRACT We Present a New Gravitational Lens Model of the Hubble
    Draft version October 15, 2018 Preprint typeset using LATEX style emulateapj v. 01/23/15 MASS AND LIGHT OF ABELL 370: A STRONG AND WEAK LENSING ANALYSIS V. Strait1, M. Bradacˇ1, A. Hoag1, K.-H. Huang1, T. Treu2, X. Wang2,4, R. Amorin6,7, M. Castellano5, A. Fontana5, B.-C. Lemaux1, E. Merlin5, K.B. Schmidt3, T. Schrabback8, A. Tomczack1, M. Trenti9,10, and B. Vulcani9,11 1Physics Department, University of California, Davis, CA 95616, USA 2Department of Physics and Astronomy, UCLA, Los Angeles, CA, 90095-1547, USA 3Leibniz-Institut f¨urAstrophysik Postdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 4Department of Physics, University of California, Santa Barbara, CA, 93106-9530, USA 5INAF - Osservatorio Astronomico di Roma Via Frascati 33 - 00040 Monte Porzio Catone, 00040 Rome, Italy 6Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, CB3 0HE, Cambridge, UK 7Kavli Institute for Cosmology, University of Cambridge, Madingley Rd., CB3 0HA, Cambridge, UK 8Argelander-Institut f¨urAstronomie, Auf dem H¨ugel71, D-53121 Bonn, Germany 9School of Physics, University of Melbourne, Parkville, Victoria, Australia 10ARC Centre of Excellence fot All Sky Astrophysics in 3 Dimensions (ASTRO 3D) and 11INAF - Astronomical Observatory of Padora, 35122 Padova, Italy Draft version October 15, 2018 ABSTRACT We present a new gravitational lens model of the Hubble Frontier Fields cluster Abell 370 (z = 0:375) using imaging and spectroscopy from Hubble Space Telescope and ground-based spectroscopy. We combine constraints from a catalog of 909 weakly lensed galaxies and 39 multiply-imaged sources comprised of 114 multiple images, including a system of multiply-imaged candidates at z = 7:84 ± 0:02, to obtain a best-fit mass distribution using the cluster lens modeling code Strong and Weak Lensing United.
    [Show full text]
  • I. Big Bang II. Galaxies and Clusters III. Milky Way Galaxy IV. Stars and ConstellaOns I
    The Big Bang and the Structure of the Universe I. Big Bang II. Galaxies and Clusters III. Milky Way Galaxy IV. Stars and Constellaons I. The Big Bang and the Origin of the Universe The Big Bang is the prevailing theory for the formaon of our universe. The theory states that the Universe was in a high density state and then began to expand. The state of the Universe before the expansion is commonly referred to as a singularity (a locaon or state where the properes used to measure gravitaonal field become infinite). The best determinaon of when the Universe inially began to expand (inflaon) is 13.77 billion years ago. NASA/WMAP This is a common arst concepon of the expansion and evoluon (in me and space) of the Universe. NASA / WMAP Science Team This image shows the cosmic microwave background radiaon in our Universe – “echo” of the Big Bang. This is the oldest light in the Universe. In the microwave poron of the electromagnec spectrum, this corresponds to a temperature of ~2.7K and is the same in all direcons. The temperature is color coded and varies by only ±0.0002K. This radiaon represents the thermal radiaon le over from the period aer the Big Bang when normal maer formed. One consequence of the expanding Universe and the immense distances is that the further an object, the further back in me you are viewing. Since light travels at a finite speed, the distance to an object indicates how far back in me you are viewing. For example, it is easy to view the Andromeda galaxy form Earth.
    [Show full text]
  • Globular Cluster Systems in Brightest Cluster Galaxies
    GLOBULAR CLUSTER SYSTEMS IN BRIGHTEST CLUSTER GALAXIES. III. BEYOND BIMODALITY Item Type Article Authors Harris, William E.; Ciccone, Stephanie M.; Eadie, Gwendolyn M.; Gnedin, Oleg Y.; Geisler, D.; Rothberg, B.; Bailin, Jeremy Citation GLOBULAR CLUSTER SYSTEMS IN BRIGHTEST CLUSTER GALAXIES. III. BEYOND BIMODALITY 2017, 835 (1):101 The Astrophysical Journal DOI 10.3847/1538-4357/835/1/101 Publisher IOP PUBLISHING LTD Journal The Astrophysical Journal Rights © 2017. The American Astronomical Society. All rights reserved. Download date 04/10/2021 03:48:29 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/622870 The Astrophysical Journal, 835:101 (21pp), 2017 January 20 doi:10.3847/1538-4357/835/1/101 © 2017. The American Astronomical Society. All rights reserved. GLOBULAR CLUSTER SYSTEMS IN BRIGHTEST CLUSTER GALAXIES. III. BEYOND BIMODALITY William E. Harris1, Stephanie M. Ciccone1, Gwendolyn M. Eadie1, Oleg Y. Gnedin2, Douglas Geisler3, Barry Rothberg4, and Jeremy Bailin5 1 Department of Physics & Astronomy, McMaster University, Hamilton, ON, Canada; [email protected], [email protected], [email protected] 2 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA; [email protected] 3 Departamento de Astronomiá, Universidad de Concepción, Casilla 160-C, Concepción, Chile; [email protected] 4 LBT Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA; [email protected] 5 Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487-0324, USA; [email protected] Received 2016 September 13; revised 2016 November 7; accepted 2016 November 21; published 2017 January 20 ABSTRACT We present new deep photometry of the rich globular cluster (GC) systems around the Brightest Cluster Galaxies UGC 9799 (Abell 2052) and UGC 10143 (Abell 2147),obtainedwiththeHubble Space Telescope (HST) ACS and WFC3 cameras.
    [Show full text]
  • Arxiv:1705.02358V2 [Hep-Ph] 24 Nov 2017
    Dark Matter Self-interactions and Small Scale Structure Sean Tulin1, ∗ and Hai-Bo Yu2, y 1Department of Physics and Astronomy, York University, Toronto, Ontario M3J 1P3, Canada 2Department of Physics and Astronomy, University of California, Riverside, California 92521, USA (Dated: November 28, 2017) Abstract We review theories of dark matter (DM) beyond the collisionless paradigm, known as self-interacting dark matter (SIDM), and their observable implications for astrophysical structure in the Universe. Self- interactions are motivated, in part, due to the potential to explain long-standing (and more recent) small scale structure observations that are in tension with collisionless cold DM (CDM) predictions. Simple particle physics models for SIDM can provide a universal explanation for these observations across a wide range of mass scales spanning dwarf galaxies, low and high surface brightness spiral galaxies, and clusters of galaxies. At the same time, SIDM leaves intact the success of ΛCDM cosmology on large scales. This report covers the following topics: (1) small scale structure issues, including the core-cusp problem, the diversity problem for rotation curves, the missing satellites problem, and the too-big-to-fail problem, as well as recent progress in hydrodynamical simulations of galaxy formation; (2) N-body simulations for SIDM, including implications for density profiles, halo shapes, substructure, and the interplay between baryons and self- interactions; (3) semi-analytic Jeans-based methods that provide a complementary approach for connecting particle models with observations; (4) merging systems, such as cluster mergers (e.g., the Bullet Cluster) and minor infalls, along with recent simulation results for mergers; (5) particle physics models, including light mediator models and composite DM models; and (6) complementary probes for SIDM, including indirect and direct detection experiments, particle collider searches, and cosmological observations.
    [Show full text]
  • Annual Report ESO Staff Papers 2018
    ESO Staff Publications (2018) Peer-reviewed publications by ESO scientists The ESO Library maintains the ESO Telescope Bibliography (telbib) and is responsible for providing paper-based statistics. Publications in refereed journals based on ESO data (2018) can be retrieved through telbib: ESO data papers 2018. Access to the database for the years 1996 to present as well as an overview of publication statistics are available via http://telbib.eso.org and from the "Basic ESO Publication Statistics" document. Papers that use data from non-ESO telescopes or observations obtained with hosted telescopes are not included. The list below includes papers that are (co-)authored by ESO authors, with or without use of ESO data. It is ordered alphabetically by first ESO-affiliated author. Gravity Collaboration, Abuter, R., Amorim, A., Bauböck, M., Shajib, A.J., Treu, T. & Agnello, A., 2018, Improving time- Berger, J.P., Bonnet, H., Brandner, W., Clénet, Y., delay cosmography with spatially resolved kinematics, Coudé Du Foresto, V., de Zeeuw, P.T., et al. , 2018, MNRAS, 473, 210 [ADS] Detection of orbital motions near the last stable circular Treu, T., Agnello, A., Baumer, M.A., Birrer, S., Buckley-Geer, orbit of the massive black hole SgrA*, A&A, 618, L10 E.J., Courbin, F., Kim, Y.J., Lin, H., Marshall, P.J., Nord, [ADS] B., et al. , 2018, The STRong lensing Insights into the Gravity Collaboration, Abuter, R., Amorim, A., Anugu, N., Dark Energy Survey (STRIDES) 2016 follow-up Bauböck, M., Benisty, M., Berger, J.P., Blind, N., campaign - I. Overview and classification of candidates Bonnet, H., Brandner, W., et al.
    [Show full text]
  • INTERPRETING HIGH RESOLUTION SUNYAEV ZEL'dovich EFFECT MEASUREMENTS with MUSTANG Charles Romero Fort Collins, CO B.A., Univers
    INTERPRETING HIGH RESOLUTION SUNYAEV ZEL’DOVICH EFFECT MEASUREMENTS WITH MUSTANG Charles Romero Fort Collins, CO B.A., University of Colorado, 2009 M.S., University of Virginia, 2011 A Dissertation Presented to the Graduate Faculty of the University of Virginia in Candidacy for the Degree of Doctor of Philosophy Department of Astronomy University of Virginia August, 2015 Brian Mason Craig Sarazin Mark Whittle Mike Skrutskie Barry Condron c Copyright by ° Charles Romero All rights reserved August, 2015 ii Acknowledgements There are many people I must thank for inspiring and supporting my path towards a graduate degree in astronomy. Certainly somewhere in elementary school, between the science classes and fairs, my interest in science took formation. Thus, I wish to thanks all the science teachers and volunteers whom I have encountered who have taught me that science is cool, fun, interesting, and ever growing. I thank my advisor, Brian Mason, for introducing me to the Sunyaev Zel’dovich effect and means of observing it. Brian has been an excellent advisor for me; he has pushed me when I needed motivation and given my space when I needed some time off. To my collaborators, I am grateful for the collegiality and willingness to answer any questions (simple or otherwise) I may have had. To those at the astronomy de- partment at the University of Virginia, I am thankful for the opportunities presented and the guidance offered. Of course, my family: Henry, Paolo, and Marian Romero have encouraged me from the start (from my earliest interests in science) through graduate school and have been more supportive than I could have asked of them to be.
    [Show full text]