DOCSLIB.ORG

Dark Matter in Galaxy Clusters: Shape, Projection, and Environment

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Dark Matter in Galaxy Clusters: Shape, Projection, and Environment Dark Matter in Galaxy Clusters: Shape, Projection, and Environment A Thesis Submitted to the Faculty of Drexel University by Austen M. Groener in partial fulfillment of the requirements for the degree of Doctor of Philosophy September 2015 c Copyright 2015 Austen M. Groener. ii Dedications I dedicate this thesis to my family, and to my wife, who supported me unconditionally throughout my career as a scientist. iii Acknowledgments I have many people to thank for making this work a possibility. Firstly, I would like to thank my advisor, Dr. David Goldberg. His guidance, support, and most of all his patience provided the framework for which I was able to build my work from. I would also like to thank my dissertation committee members, Dr. Michael Vogeley, Dr. Gordon Richards, Dr. Luis Cruz, and Dr. Andrew Hicks, for their constructive criticism and support of my research. I would also like to acknowledge fellow graduate students for their assistance and support. A special thanks to Justin Bird, Markus Rexroth, Frank Jones, Crystal Moorman, and Vishal Kasliwal for allowing me to bounce ideas off of them, which was a truly important but time consuming process. iv Table of Contents List of Tables ........................................... vi List of Figures .......................................... vii Abstract .............................................. ix 1. Introduction .......................................... 1 1.1 The Radial Density Profile.................................. 2 1.2 Cluster Scaling Relations .................................. 5 1.3 Clusters and Environment.................................. 7 1.4 Outline ............................................ 11 2. Cluster Shape and Orientation .............................. 12 2.1 Introduction.......................................... 12 2.2 Triaxial Projections...................................... 14 2.3 Sample and Methods..................................... 15 2.3.1 Simulation Sample .................................... 15 2.3.2 Methods.......................................... 18 2.3.3 Non-Virialized Halos................................... 19 2.4 Results............................................. 21 2.5 Summary and Conclusions.................................. 28 2.6 Future Work ......................................... 37 3. The Observed c-M Relation ................................ 38 3.1 Introduction.......................................... 38 3.2 Reconstruction Techniques.................................. 41 3.2.1 Weak Lensing (WL) ................................... 41 3.2.2 Strong Lensing (SL) ................................... 42 3.2.3 Weak+Strong Lensing (WL+SL)............................ 43 v 3.2.4 X-ray............................................ 43 3.2.5 Line-of-sight Velocity Dispersion (LOSVD)....................... 44 3.2.6 The Caustic Method (CM)................................ 44 3.2.7 Hybrid Techniques .................................... 45 3.3 The Sample.......................................... 45 3.3.1 Normalization Procedure................................. 48 3.4 The Observed c-M Relation................................. 51 3.5 Projection and Shape .................................... 56 3.6 Conclusions And Discussions ................................ 61 4. Clusters And The LSS Environment ........................... 66 4.1 Introduction.......................................... 66 4.2 Data.............................................. 67 4.3 Galaxies Around Clusters .................................. 70 4.3.1 Quantifying Structure .................................. 71 4.4 Results And Future Work.................................. 74 5. Conclusions ........................................... 79 Bibliography ............................................ 82 Appendix A: Analytical Projection of Prolate Spheroidal Halos . 90 Appendix B: Lensing Cosmology Correction ....................... 92 Appendix C: Full Observational Dataset .......................... 94 Vita .................................................. 127 vi List of Tables 2.1 Prolate Spheroidal Geometry................................. 15 2.2 Cluster Halo Geometry .................................... 23 2.3 Concentration Enhancements................................. 30 3.1 Population Overview...................................... 47 3.2 Best-Fit Concentration-Mass Relation Parameters ..................... 54 C.1 Cluster concentrations and masses .............................. 96 C.2 A Summary of The References ................................ 123 vii List of Figures 1.1 X-ray Gas in Abell 383 .................................... 2 1.2 The NFW Profile........................................ 3 1.3 c-M Relations: Then and Now ................................ 8 1.4 Cluster Formation ....................................... 9 1.5 Bolshoi Simulation....................................... 10 2.1 Analytical concentration and shape relations......................... 16 2.2 The MultiDark MDR1 Mass Function............................. 17 2.3 Examples of Virialized and Non-Virialized Halos ...................... 20 2.4 The Virial β Parameter .................................... 22 2.5 Low Mass Shape Results.................................... 24 2.6 Medium Mass Shape Results ................................. 25 2.7 High Mass Shape Results ................................... 26 2.8 MDR1 Intrinsic Concentration Parameters.......................... 27 2.9 The Intrinsic MDR1 c-M Relation .............................. 29 2.10 Low Mass Concentration Enhancements........................... 31 2.11 Medium Mass Concentration Enhancements......................... 32 2.12 A Summary of The Change in Shape for the Low Mass Sample.............. 33 2.13 Low Mass Isodensity Alignment................................ 34 2.14 Medium Mass Isodensity Alignment ............................. 35 2.15 High Mass Isodensity Alignment ............................... 36 3.1 Cluster Population Overview ................................. 48 3.2 Concentration/Mass Cosmology Correction ......................... 49 3.3 The Normalized Data ..................................... 52 3.4 Observed c-M Fits....................................... 55 viii 3.5 CLASH Comparison...................................... 56 3.6 The Full c-M Relation..................................... 58 3.7 Lensing Relations and MDR1 Halos ............................. 59 3.8 Comparison of Theory with Observations .......................... 60 3.9 WL and WL+SL Cluster Measurements........................... 61 3.10 X-ray and WL Cluster Measurements ............................ 62 3.11 CM and LOSVD Cluster Measurements........................... 62 4.1 The SDSS DR10 Footprint .................................. 67 4.2 The Galaxy Sample Defined.................................. 68 4.3 Galaxy Clusters In SDSS ................................... 69 4.4 Selecting Galaxies Around Clusters.............................. 72 m 4.5 Mass - Al Correlation..................................... 76 m 4.6 Concentration - Al Correlation................................ 77 m 4.7 Redshift Scaled Concentration - Al Correlation ...................... 78 LIST OF FIGURES LIST OF FIGURES ix Abstract Dark Matter in Galaxy Clusters: Shape, Projection, and Environment Austen M. Groener Dr. David Goldberg We explore the intrinsic distribution of dark matter within galaxy clusters, by combining insights from the largest N-body simulations as well as the largest observational dataset of its kind. Firstly, we study the intrinsic shape and alignment of isodensities of galaxy cluster halos extracted from the MultiDark MDR1 cosmological simulation. We find that the simulated halos are extremely prolate on small scales and increasingly spherical on larger ones. Due to this trend, analytical projection along the line of sight produces an overestimate of the concentration index as a decreasing function of radius, which we quantify by using both the intrinsic distribution of 3D concentrations (c200) and isodensity shape on weak and strong lensing scales. We find this difference to be ∼ 18% (∼ 9%) for low (medium) mass cluster halos with intrinsically low concentrations (c200 = 1 − 3), while we find virtually no difference for halos with intrinsically high concentrations. Isodensities are found to be fairly well-aligned throughout the entirety of the radial scale of each halo population. However, major axes of individual halos have been found to deviate by as much as ∼ 30◦. We also present a value-added catalog of our analysis results, which we have made publicly available to download. Following that, we then turn to observational measurements galaxy clusters. Scaling relations of clusters have made them particularly important cosmological probes of structure formation. In this work, we present a comprehensive study of the relation between two profile observables, con- centration (cvir) and mass (Mvir). We have collected the largest known sample of measurements from the literature which make use of one or more of the following reconstruction techniques: Weak gravitational lensing (WL), strong gravitational lensing (SL), Weak+Strong Lensing (WL+SL), the Caustic Method (CM), Line-of-sight Velocity Dispersion (LOSVD), and X-ray. We find that the concentration-mass (c-M) relation is highly variable depending upon the reconstruction technique used. We also find concentrations derived from dark matter only simulations (at approximately 14 Mvir ∼ 10 M ) to be inconsistent with the WL and WL+SL relations at
Load more

Recommended publications
  • Clusters of Galaxies…
    Budapest University, MTA-Eötvös François Mernier …and the surprisesoftheir spectacularhotatmospheres Clusters ofgalaxies… K complex ) ⇤ Fe ) α [email protected] - Wallon Super - Wallon [email protected] Fe XXVI (Ly (/ Fe XXIV) L complex ) ) (incl. Ne) α α ) Fe ) ) α ) α α ) ) ) ) α ⇥ ) ) ) α α α α α α Si XIV (Ly Mg XII (Ly Ni XXVII / XXVIII Fe XXV (He S XVI (Ly O VIII (Ly Si XIII (He S XV (He Ca XIX (He Ca XX (Ly Fe XXV (He Cr XXIII (He Ar XVII (He Ar XVIII (Ly Mn XXIV (He Ca XIX / XX Yo u are h ere ! 1 km = 103 m Yo u are h ere ! (somewhere behind…) 107 m Yo u are h ere ! (and this is the Moon) 109 m ≃3.3 light seconds Yo u are h ere ! 1012 m ≃55.5 light minutes 1013 m 1014 m Yo u are h ere ! ≃4 light days 1013 m Yo u are h ere ! 1014 m 1017 m ≃10.6 light years 1021 m Yo u are h ere ! ≃106 000 light years 1 million ly Yo u are h ere ! The Local Group Andromeda (M31) 1 million ly Yo u are h ere ! The Local Group Triangulum (M33) 1 million ly Yo u are h ere ! The Local Group 10 millions ly The Virgo Supercluster Virgo cluster 10 millions ly The Virgo Supercluster M87 Virgo cluster 10 millions ly The Virgo Supercluster 2dFGRS Survey The large scale structure of the universe Abell 2199 (429 000 000 light years) Abell 2029 (1.1 billion light years) Abell 2029 (1.1 billion light years) Abell 1689 Abell 1689 (2.2 billion light years) Les amas de galaxies 53 Light emits at optical “colors”… …but also in infrared, radio, …and X-ray! Light emits at optical “colors”… …but also in infrared, radio, …and X-ray! Light emits at optical “colors”…
    [Show full text]
  • Hot Interstellar Matter in Elliptical Galaxies
    Hot Interstellar Matter in Elliptical Galaxies For further volumes: http://www.springer.com/series/5664 Astrophysics and Space Science Library EDITORIAL BOARD Chairman W. B. BURTON, National Radio Astronomy Observatory, Charlottesville, Virginia, U.S.A. ([email protected]); University of Leiden, The Netherlands ([email protected]) F. BERTOLA, University of Padua, Italy J. P. CASSINELLI, University of Wisconsin, Madison, U.S.A. C. J. CESARSKY, Commission for Atomic Energy, Saclay, France P. EHRENFREUND, Leiden University, The Netherlands O. ENGVOLD, University of Oslo, Norway A. HECK, Strasbourg Astronomical Observatory, France E. P. J. VAN DEN HEUVEL, University of Amsterdam, The Netherlands V. M. KASPI, McGill University, Montreal, Canada J. M. E. KUIJPERS, University of Nijmegen, The Netherlands H. VAN DER LAAN, University of Utrecht, The Netherlands P. G. MURDIN, Institute of Astronomy, Cambridge, UK F. PACINI, Istituto Astronomia Arcetri, Firenze, Italy V. RADHAKRISHNAN, Raman Research Institute, Bangalore, India B . V. S O M OV, Astronomical Institute, Moscow State University, Russia R. A. SUNYAEV, Space Research Institute, Moscow, Russia Dong-Woo Kim Silvia Pellegrini Editors Hot Interstellar Matter in Elliptical Galaxies 123 Editors Dong-Woo Kim Harvard Smithsonian Center for Astrophysics Garden Street 60 02138 Cambridge Massachusetts USA [email protected] Silvia Pellegrini Dipartimento di Astronomia Universita` di Bologna Via Ranzani 1 40127 Bologna Italy [email protected] Cover figure: Chandra image of NGC 7619. From Kim et al. (2008). Reproduced by permission of the AAS. ISSN 0067-0057 ISBN 978-1-4614-0579-5 e-ISBN 978-1-4614-0580-1 DOI 10.1007/978-1-4614-0580-1 Springer Heidelberg Dordrecht London New York Library of Congress Control Number: 2011938147 c Springer Science+Business Media, LLC 2012 This work is subject to copyright.
    [Show full text]
  • INVESTIGATING ACTIVE GALACTIC NUCLEI with LOW FREQUENCY RADIO OBSERVATIONS By
    INVESTIGATING ACTIVE GALACTIC NUCLEI WITH LOW FREQUENCY RADIO OBSERVATIONS by MATTHEW LAZELL A thesis submitted to The University of Birmingham for the degree of DOCTOR OF PHILOSOPHY School of Physics & Astronomy College of Engineering and Physical Sciences The University of Birmingham March 2015 University of Birmingham Research Archive e-theses repository This unpublished thesis/dissertation is copyright of the author and/or third parties. The intellectual property rights of the author or third parties in respect of this work are as defined by The Copyright Designs and Patents Act 1988 or as modified by any successor legislation. Any use made of information contained in this thesis/dissertation must be in accordance with that legislation and must be properly acknowledged. Further distribution or reproduction in any format is prohibited without the permission of the copyright holder. Abstract Low frequency radio astronomy allows us to look at some of the fainter and older synchrotron emission from the relativistic plasma associated with active galactic nuclei in galaxies and clusters. In this thesis, we use the Giant Metrewave Radio Telescope to explore the impact that active galactic nuclei have on their surroundings. We present deep, high quality, 150–610 MHz radio observations for a sample of fifteen predominantly cool-core galaxy clusters. We in- vestigate a selection of these in detail, uncovering interesting radio features and using our multi-frequency data to derive various radio properties. For well-known clusters such as MS0735, our low noise images enable us to see in improved detail the radio lobes working against the intracluster medium, whilst deriving the energies and timescales of this event.
    [Show full text]
  • Provisional Scientific Programme
    Galaxy Clusters as Giant Cosmic Laboratories – Programme Monday, 21 May 2012 09:00 Registration 09:50 Schartel: Opening Remarks Session I Dynamical and Thermal Structure of Galaxy Clusters and their ICM Chair: Birzan 10:00 Sanders: The thermal and dynamical state of cluster cores 10:30 Ohashi: X-ray study of clusters at the outer edge and beyond 10:45 Eckert: The gas distribution in galaxy cluster outer regions 11:00 Molendi: Extending measures of the ICM to the outskirts: facts, myths and puzzles 11:15 Sato: Temperature, entropy, and mass profiles to the virial radius of galaxy clusters with Suzaku 11:30- Coffee Break & Poster Viewing 12:00 Session II Dynamical and Thermal Structure of Galaxy Clusters and their ICM Chair: Altieri Cluster Mass Determination 12:00 Ettori: Cluster mass profiles from X-ray observations: present constraints and limitations 12:30 Russell: Shock fronts, electron-ion equilibration and ICM transport processes in the merging cluster Abell 2146 12:45 ZuHone: Probing the Microphysics of the Intracluster Medium with Cold Fronts in the ICM 13:00 Rossetti: Challenging the merging/sloshing cold front paradigm with a new XMM observation of A2142 13:15 Nevalainen: Bulk motion measurements in clusters of galaxies using XMM-Newton and ATHENA 13:30- Lunch 15:00 Session III Dynamical and Thermal Structure of Galaxy Clusters and their ICM Chair: de Grandi Cluster Mass Determination 15:00 Mahdavi: Multiwavelength Constraints on Scaling Relations and Substructure in a Sample of 50 Clusters of Galaxies 15:30 Pratt: Galaxy cluster
    [Show full text]
  • 18.465, Revised Again December 6, 2012 Truncation, the Lynden-Bell Estimator, and Galaxy Data
    18.465, Revised again December 6, 2012 Truncation, the Lynden-Bell estimator, and galaxy data 1. Definitions Suppose there are i.i.d. pairs (Xk,Yk) of variables for k = 1, ..., N where N is unknown to the observer. Within each pair, Xk and Yk are independent positive real variables with distributions F and G respec- tively. In the “truncation” or “left truncation” model, the specific restric- tion is that the pair of values (Xk,Yk) is observed if and only if Yk Xk. Moreover, the index k is not observed. One wants to estimate F≤. Suppose then that we observe (xj, yj), j = 1, ..., n, so that we observe a value of n and know about N at first that N n. Recall the survival function corresponding to F , S(x) 1 F (x),≥ ≡ − 2. The Lynden-Bell estimator Let ξi for i = 1, ..., m be the distinct values of xj. What is called the Lynden-Bell estimator of S(x) is ri (1) Sn(x)= 1 µ − nCn(ξi)¶ ξYi≤x b where ri is the number of j n such that xj = ξi and ≤ n 1 C (s)= 1 . n n {yj <s≤xj } Xj=1 These formulas are as given by Woodroofe (1985, (8)) and Chen et al. (1995, (1)), originating with Lynden-Bell (1971). 3. Absolute and apparent magnitudes for astronomical objects Magnitudes were first assigned in ancient times to stars, with the brightest being assigned first magnitude, a next-brightest category sec- ond magnitude, and so on to the faintest stars visible to the naked eye under good conditions, 6th magnitude.
    [Show full text]
  • Constraining Gas Motions in the Intra-Cluster Medium
    Noname manuscript No. (will be inserted by the editor) Constraining Gas Motions in the Intra-Cluster Medium Aurora Simionescu · John ZuHone · Irina Zhuravleva · Eugene Churazov · Massimo Gaspari · Daisuke Nagai · Norbert Werner · Elke Roediger · Rebecca Canning · Dominique Eckert · Liyi Gu · Frits Paerels Received: date / Accepted: date Aurora Simionescu SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands; E-mail: [email protected] Institute of Space and Astronautical Science (ISAS), JAXA, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa, 252-5210, Japan John ZuHone Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA Irina Zhuravleva Department of Astronomy & Astrophysics, University of Chicago, 5640 S Ellis Ave, Chicago, IL 60637, USA Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305-4085, USA Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305-4085, USA Eugene Churazov Max Planck Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, D-85741 Garching, Germany Space Research Institute (IKI), Profsoyuznaya 84/32, Moscow 117997, Russia Massimo Gaspari Einstein and Spitzer Fellow, Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544-1001, USA Daisuke Nagai Department of Physics, Yale University, PO Box 208101, New Haven, CT, USA Yale Center for Astronomy and Astrophysics, PO Box 208101, New Haven, CT, USA Norbert Werner MTA-E¨otv¨osLor´andUniversity Lend¨uletHot Universe Research Group, H-1117 P´azm´any P´eters´eta´ny1/A, Budapest, Hungary Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk Univer- sity, Kotl´arsk´a2, Brno, 61137, Czech Republic School of Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima 739-8526, arXiv:1902.00024v1 [astro-ph.CO] 31 Jan 2019 Japan 2 Aurora Simionescu et al.
    [Show full text]
  • Jet-Induced Star Formation in 3C 285 and Minkowski's Object⋆
    A&A 574, A34 (2015) Astronomy DOI: 10.1051/0004-6361/201424932 & c ESO 2015 Astrophysics Jet-induced star formation in 3C 285 and Minkowski’s Object? Q. Salomé, P. Salomé, and F. Combes LERMA, Observatoire de Paris, CNRS UMR 8112, 61 avenue de l’Observatoire, 75014 Paris, France e-mail: [email protected] Received 5 September 2014 / Accepted 6 November 2014 ABSTRACT How efficiently star formation proceeds in galaxies is still an open question. Recent studies suggest that active galactic nucleus (AGN) can regulate the gas accretion and thus slow down star formation (negative feedback). However, evidence of AGN positive feedback has also been observed in a few radio galaxies (e.g. Centaurus A, Minkowski’s Object, 3C 285, and the higher redshift 4C 41.17). Here we present CO observations of 3C 285 and Minkowski’s Object, which are examples of jet-induced star formation. A spot (named 3C 285/09.6 in the present paper) aligned with the 3C 285 radio jet at a projected distance of ∼70 kpc from the galaxy centre shows star formation that is detected in optical emission. Minkowski’s Object is located along the jet of NGC 541 and also shows star formation. Knowing the distribution of molecular gas along the jets is a way to study the physical processes at play in the AGN interaction with the intergalactic medium. We observed CO lines in 3C 285, NGC 541, 3C 285/09.6, and Minkowski’s Object with the IRAM 30 m telescope. In the central galaxies, the spectra present a double-horn profile, typical of a rotation pattern, from which we are able to estimate the molecular gas density profile of the galaxy.
    [Show full text]
  • Chapter 1 the PHYSICS of CLUSTER MERGERS
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server To appear in Merging Processes in Clusters of Galaxies, edited by L. Feretti, I. M. Gioia, and G. Giovannini (Dordrecht: Kluwer), in press (2001) Chapter 1 THE PHYSICS OF CLUSTER MERGERS Craig L. Sarazin Department of Astronomy University of Virginia [email protected] Abstract Clusters of galaxies generally form by the gravitational merger of smaller clusters and groups. Major cluster mergers are the most energetic events in the Universe since the Big Bang. Some of the basic physical proper- ties of mergers will be discussed, with an emphasis on simple analytic arguments rather than numerical simulations. Semi-analytic estimates of merger rates are reviewed, and a simple treatment of the kinematics of binary mergers is given. Mergers drive shocks into the intracluster medium, and these shocks heat the gas and should also accelerate non- thermal relativistic particles. X-ray observations of shocks can be used to determine the geometry and kinematics of the merger. Many clus- ters contain cooling flow cores; the hydrodynamical interactions of these cores with the hotter, less dense gas during mergers are discussed. As a result of particle acceleration in shocks, clusters of galaxies should con- tain very large populations of relativistic electrons and ions. Electrons 2 with Lorentz factors γ 300 (energies E = γmec 150 MeV) are expected to be particularly∼ common. Observations and∼ models for the radio, extreme ultraviolet, hard X-ray, and gamma-ray emission from nonthermal particles accelerated in these mergers are described.
    [Show full text]
  • Arxiv:0807.2573V1 [Astro-Ph] 16 Jul 2008 Oy 1-03 Japan
    Draft version November 1, 2018 A Preprint typeset using LTEX style emulateapj v. 08/13/06 STRANGE FILAMENTARY STRUCTURES (“FIREBALLS”) AROUND A MERGER GALAXY IN THE COMA CLUSTER OF GALAXIES1 Michitoshi Yoshida2, Masafumi Yagi3, Yutaka Komiyama3,4, Hisanori Furusawa4, Nobunari Kashikawa3, Yusei Koyama5, Hitomi Yamanoi3,6, Takashi Hattori4 and Sadanori Okamura5,7 Draft version November 1, 2018 ABSTRACT We found an unusual complex of narrow blue filaments, bright blue knots, and Hα-emitting filaments and clouds, which morphologically resembled a complex of “fireballs,” extending up to 80 kpc south from an E+A galaxy RB199 in the Coma cluster. The galaxy has a highly disturbed morphology indicative of a galaxy–galaxy merger remnant. The narrow blue filaments extend in straight shapes toward the south from the galaxy, and several bright blue knots are located at the southern ends of the filaments. The RC band absolute magnitudes, half light radii and estimated masses of the 6−7 bright knots are ∼ −12 −−13 mag, ∼ 200 − 300 pc and ∼ 10 M⊙, respectively. Long, narrow Hα-emitting filaments are connected at the south edge of the knots. The average color of the fireballs is B − RC ≈ 0.5, which is bluer than RB199 (B − R = 0.99), suggesting that most of the stars in the fireballs were formed within several times 108 yr. The narrow blue filaments exhibit almost no Hα emission. Strong Hα and UV emission appear in the bright knots. These characteristics indicate that star formation recently ceased in the blue filaments and now continues in the bright knots. The gas stripped by some mechanism from the disk of RB199 may be traveling in the intergalactic space, forming stars left along its trajectory.
    [Show full text]
  • X-Ray Jets Aneta Siemiginowska
    Chandra News Issue 21 Spring 2014 Published by the Chandra X-ray Center (CXC) X-ray Jets Aneta Siemiginowska The Active Galaxy 4C+29.30 Credit: X-ray: NASA/CXC/SAO/A.Siemiginowska et al; Optical: NASA/STScI; Radio: NSF/NRAO/VLA Contents X-ray Jets HETG 3 Aneta Siemiginowska 18 David Huenemoerder (for the HETG team) 10 Project Scientist’s Report 20 LETG Martin Weisskopf Jeremy Drake 11 Project Manager’s Report 23 Chandra Calibration Roger Brissenden Larry David Message of Thanks to Useful Web Addresses 12 Harvey Tananbaum 23 The Chandra Team Belinda Wilkes Appointed as CIAO 4.6 13 Director of the CXC 24 Antonella Fruscione, for the CIAO Team Of Programs and Papers: Einstein Postdoctoral Fellowship 13 Making the Chandra Connection 29 Program Sherry Winkelman & Arnold Rots Andrea Prestwich Chandra Related Meetings Cycle 14 Peer Review Results 14 and Important Dates 30 Belinda Wilkes ACIS Chandra Users’ Committee 14 Paul Plucinsky, Royce Buehler, 34 Membership List Gregg Germain, & Richard Edgar HRC CXC 2013 Science Press 15 Ralph Kraft, Hans Moritz Guenther 35 Releases (SAO), and Wolfgang Pietsch (MPE) Megan Watzke The Chandra Newsletter appears once a year and is edited by Paul J. Green, with editorial assistance and layout by Evan Tingle. We welcome contributions from readers. Comments on the newsletter, or corrections and additions to the hardcopy mailing list should be sent to: [email protected]. Spring, 2014 3 X-ray Jets many unanswered questions, including the nature of relativistic jets, jet energetics, particle content, parti- Aneta Siemiginowska cle acceleration and emission processes. Both statis- tical studies of large samples of jets across the entire The first recorded observation of an extragalac- electromagnetic spectrum and deep broad-band imag- tic jet was made almost a century ago.
    [Show full text]
  • And Ecclesiastical Cosmology
    GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc.
    [Show full text]
  • 121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
    221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S.
    [Show full text]