Simulations of the Merging Galaxy Cluster Abell 3376
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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 -
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). -
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 -
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. -
I. Big Bang II. Galaxies and Clusters III. Milky Way Galaxy IV. Stars and Constella Ons 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. -
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. -
![Arxiv:1705.02358V2 [Hep-Ph] 24 Nov 2017](https://docslib.b-cdn.net/cover/8698/arxiv-1705-02358v2-hep-ph-24-nov-2017-1518698.webp)
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. -
The Hubble Catalog of Variables (HCV)? A
Astronomy & Astrophysics manuscript no. hcv c ESO 2019 September 25, 2019 The Hubble Catalog of Variables (HCV)? A. Z. Bonanos1, M. Yang1, K. V. Sokolovsky1; 2; 3, P. Gavras4; 1, D. Hatzidimitriou1; 5, I. Bellas-Velidis1, G. Kakaletris6, D. J. Lennon7; 8, A. Nota9, R. L. White9, B. C. Whitmore9, K. A. Anastasiou5, M. Arévalo4, C. Arviset8, D. Baines10, T. Budavari11, V. Charmandaris12; 13; 1, C. Chatzichristodoulou5, E. Dimas5, J. Durán4, I. Georgantopoulos1, A. Karampelas14; 1, N. Laskaris15; 6, S. Lianou1, A. Livanis5, S. Lubow9, G. Manouras5, M. I. Moretti16; 1, E. Paraskeva1; 5, E. Pouliasis1; 5, A. Rest9; 11, J. Salgado10, P. Sonnentrucker9, Z. T. Spetsieri1; 5, P. Taylor9, and K. Tsinganos5; 1 1 IAASARS, National Observatory of Athens, Penteli 15236, Greece e-mail: [email protected] 2 Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA 3 Sternberg Astronomical Institute, Moscow State University, Universitetskii pr. 13, 119992 Moscow, Russia 4 RHEA Group for ESA-ESAC, Villanueva de la Cañada, 28692 Madrid, Spain 5 Department of Physics, National and Kapodistrian University of Athens, Panepistimiopolis, Zografos 15784, Greece 6 Athena Research and Innovation Center, Marousi 15125, Greece 7 Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain 8 ESA, European Space Astronomy Centre, Villanueva de la Canada, 28692 Madrid, Spain 9 Space Telescope Science Institute, Baltimore, MD 21218, USA 10 Quasar Science Resources for ESA-ESAC, Villanueva de la Cañada, 28692 Madrid, Spain 11 The Johns Hopkins University, Baltimore, MD 21218, USA 12 Institute of Astrophysics, FORTH, Heraklion 71110, Greece 13 Department of Physics, Univ. -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63 -
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. -
Détection Directionnelle De Matière Sombre Avec MIMAC
THÈSE Pour obtenir le grade de DOCTEUR DE L’UNIVERSITÉ DE GRENOBLE Spécialité : Cosmologie et astroparticules Arrêté ministériel : 7 août 2006 Présentée par Quentin Riffard Thèse dirigée par Daniel Santos préparée au sein du Laboratoire de physique subatomique et de cosmologie (LPSC) à l’école doctorale de Physique de Grenoble Détection directionnelle de matière sombre avec MIMAC Thèse soutenue publiquement le Lundi 12 Octobre 2015, devant le jury composé de : Laurent Derome LPSC Grenoble, Président Philippe Di Stefano Queen’s University Kingston, Rapporteur Jacque Dumarchez LPNHE Paris, Examinateur Emmanuel Moulin CEA Saclay, Examinateur Fabrice Piquemal CENBG/LSM Bordeaux/Modane, Rapporteur Daniel Santos LPSC Grenoble, Directeur de thèse Table des matières I Matière sombre non-baryonique : Observations astrophysiques et détec- tion 7 1 Observations astrophysiques et supersymétrie 9 1.1 La matière sombre à différentes échelles. ....................... 10 1.1.1 À l’échelle locale : l’échelle galactique ..................... 10 1.1.2 À l’échelle des amas .............................. 11 1.1.3 A l’échelle cosmologique ............................ 13 1.2 Candidats à la matière sombre non-baryonique ................... 17 1.2.1 Contraintes sur le candidat : la densité relique . 17 1.2.2 Le WIMP, un candidat à la matière sombre non-baryonique . 19 1.3 Physique des particules et matière sombre ...................... 19 1.3.1 La supersymétrie ................................ 19 1.3.2 Le MSSM .................................... 20 1.3.3 Neutralino : un candidat au WIMP ...................... 21 1.4 Stratégies de détection de matière sombre ...................... 22 1.4.1 Détection directe ................................ 22 1.4.2 Détection indirecte ............................... 23 1.4.3 Production de matière sombre ......................... 25 1.5 Conclusions ...................................... -
Morphology and Kinematics of Z ∼ 1 Galaxies As Seen Through Gravitational Telescopes
Universita` degli Studi di Napoli \Federico II" Dipartimento di Fisica \Ettore Pancini" Corso di Laurea in Fisica Anno Accademico 2017/2018 Tesi di Laurea Magistrale Morphology and kinematics of z ∼ 1 galaxies as seen through gravitational telescopes Relatore: Prof. Giovanni Covone Candidato: Maria Vittoria Milo Matricola: N94000352 Se parlassi le lingue degli uomini e degli angeli, ma non avessi amore, sarei un rame risonante o uno squillante cembalo. Se avessi il dono di profezia e conoscessi tutti i misteri e tutta la scienza e avessi tutta la fede in modo da spostare i monti, ma non avessi amore, non sarei nulla. Se distribuissi tutti i miei beni per nutrire i poveri, se dessi il mio corpo a essere arso, e non avessi amore, non mi gioverebbe a niente. (1 Corinzi 13:1-3) ii Abstract Observing high−z galaxies is an hard challenge for astrophysicists. As much we go back in time (and therefore far away in space), the Universe in which we live becomes smaller, denser and hotter. On the other hand, at high redshift, astro- nomical objects result as fainter as smaller to make their detection impossible even for the most powerful today's telescopes. Hence, trying to determine the morphol- ogy of these high−z galaxies and even to characterize their physical properties (such as kinematics) would result just a dream of a crazy astrophysicist. Fortu- nately, Nature offers a way out, allowing us to overcome the obstacle. Telescopes able to observe regions of the Universe never before reached by any human or artificial \eye" already exist! These are galaxy clusters, the largest known grav- itationally bound structures in the Universe.