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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. -
GMRT 610 Mhz Observations of Galaxy Clusters in the ACT Equatorial Sample
MNRAS 000,1{26 (2018) Preprint 20 March 2019 Compiled using MNRAS LATEX style file v3.0 GMRT 610 MHz observations of galaxy clusters in the ACT equatorial sample Kenda Knowles,1? Andrew J. Baker,2 J. Richard Bond,3 Patricio A. Gallardo,4 Neeraj Gupta,5 Matt Hilton,1 John P. Hughes,2 Huib Intema,6 Carlos H. L´opez- Caraballo,7;8 Kavilan Moodley,1 Benjamin L. Schmitt,9 Jonathan Sievers,10 Crist´obal Sif´on,4;11 Edward Wollack,12 1Astrophysics & Cosmology Research Unit, School of Mathematics, Statistics & Computer Science, University of KwaZulu-Natal, Durban, 3690, South Africa 2Department of Physics and Astronomy, Rutgers, The State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019, USA 3Canadian Institute for Theoretical Astrophysics, 60 St. George Street, University of Toronto, Toronto, ON, M5S 3H8, Canada 4Department of Physics, Cornell University, Ithaca, NY USA 5IUCAA, Post Bag 4, Ganeshkhind, Pune 411007, India 6Leiden Observatory, Leiden University, PO Box 9513, NL2300 RA Leiden, Netherlands 7Instituto de Astrof´ısica and Centro de Astro-Ingenier´ıa, Facultad de F´ısica, Pontificia Universidad Cat´olica de Chile, Av. Vicu~na Mackenna 4860, 7820436 Macul, Santiago, Chile 8Departamento de Matem´aticas, Universidad de La Serena, Av. Juan Cisternas 1200, La Serena, Chile 9Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104, USA 10Astrophysics & Cosmology Research Unit, School of Chemistry & Physics, University of KwaZulu-Natal, Durban, 3690, South Africa 11Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ 08544, USA 12NASA/Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA Accepted XXX. -
Cosmic Evolution Through Uv Surveys (Cetus) Final Report
COSMIC EVOLUTION THROUGH UV SURVEYS (CETUS) FINAL REPORT Thematic Activity: Project (probe mission concept) Program: Electromagnetic observations from space Authors of Final Report: Jonathan Arenberg, Northrop Grumman Corporation Sally Heap, Univ. of Maryland, [email protected] Tony Hull, Univ. of New Mexico Steve Kendrick, Kendrick Aerospace Consulting LLC Bob Woodruff, Woodruff Consulting Scientific Contributors: Maarten Baes, Rachel Bezanson, Luciana Bianchi, David Bowen, Brad Cenko, Yi-Kuan Chiang, Rachel Cochrane, Mike Corcoran, Paul Crowther, Simon Driver, Bill Danchi, Eli Dwek, Brian Fleming, Kevin France, Pradip Gatkine, Suvi Gezari, Lea Hagen, Chris Hayward, Matthew Hayes, Tim Heckman, Edmund Hodges-Kluck, Alexander Kutyrev, Thierry Lanz, John MacKenty, Steve McCandliss, Harvey Moseley, Coralie Neiner, Goren Östlin, Camilla Pacifici, Marc Rafelski, Bernie Rauscher, Jane Rigby, Ian Roederer, David Spergel, Dan Stark, Alexander Szalay, Bryan Terrazas, Jonathan Trump, Arjun van der Wel, Sylvain Veilleux, Kate Whitaker, Isak Wold, Rosemary Wyse Technical Contributors: Jim Burge, Kelly Dodson, Chip Eckles, Brian Fleming, Jamie Kennea, Gerry Lemson, John MacKenty, Steve McCandliss, Greg Mehle, Shouleh Nikzad, Trent Newswander, Lloyd Purves, Manuel Quijada, Ossy Siegmund, Dave Sheikh, Phil Stahl, Ani Thakar, John Vallerga, Marty Valente, the Goddard IDC/MDL. September 2019 Cosmic Evolution Through UV Surveys (CETUS) TABLE OF CONTENTS INTRODUCTION TO CETUS ................................................................................................................ -
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 -
Where Are the Missing Baryons in Clusters?
1 Where Are the Missing Baryons in Clusters? Bilhuda Rasheed Adviser: Dr. Neta Bahcall Submitted in partial fulfillment of the requirements for the degree of Bachelor of Arts Department of Astrophysical Sciences Princeton University May 2010 I hereby declare that I am the sole author of this thesis. I authorize Princeton University to lend this thesis to other institutions or individuals for the purpose of scholarly research. Bilhuda Rasheed I further authorize Princeton University to reproduce this thesis by photocopying or by other means, in total or in part, at the request of other institutions or individuals for the purpose of scholarly research. Bilhuda Rasheed Abstract We address previous claims that the baryon fraction in clusters is significantly below the cosmic value of the baryon fraction as determined from WMAP 7-year results. We use X-ray and SZ observations to determine the slope of the gas density profile to R200. This is shallower than the slope of total mass density (NFW) profile. We use the gas density slope to extrapolate the X-ray observations of gas fraction at R500 to the virial radius (R100). The gas fraction increases beyond R500 for all cluster masses. We add the stellar fraction as determined from COSMOS and 2MASS samples, with ICL contributing 10% to the stellar fraction. For massive clusters 14 (M500 ∼ 7 × 10 M ), the baryon fraction reaches the cosmic baryon fraction at Rvir± 20%. Poorer clusters and groups typically reach 75–85% of the cosmic baryon fraction at the virial radius. We compare these results with simulations which take into account gravitational shock-heating, star formation, heating from SNe and AGN, and energy transfer from dark matter. -
8603517.PDF (12.42Mb)
Umversify Microfilins International 1.0 12.5 12.0 LI 1.8 1.25 1.4 1.6 MICROCOPY RESOLUTION TEST CHART NATIONAL BUREAU OF STANDARDS STANDARD REFERENCE MATERIAL 1010a (ANSI and ISO TEST CHART No. 2) University Microfilms Inc. 300 N. Zeeb Road, Ann Arbor, MI 48106 INFORMATION TO USERS This reproduction was made from a copy of a manuscript sent to us for publication and microfilming. While the most advanced technology has been used to pho tograph and reproduce this manuscript, the quality of the reproduction is heavily dependent upon the quality of the material submitted. Pages in any manuscript may have indistinct print. In all cases the best available copy has been filmed. The following explanation of techniques is provided to help clarify notations which may appear on this reproduction. 1. Manuscripts may not always be complete. When it is not possible to obtain missing pages, a note appears to indicate this. 2. When copyrighted materials are removed from the manuscript, a note ap pears to indicate this. 3. Oversize materials (maps, drawings, and charts) are photographed by sec tioning the original, beginning at the upper left hand comer and continu ing from left to right in equal sections with small overlaps. Each oversize page is also filmed as one exposure and is available, for an additional charge, as a standard 35mm slide or in black and white paper format.* 4. Most photographs reproduce acceptably on positive microfilm or micro fiche but lack clarify on xerographic copies made from the microfilm. For an additional charge, all photographs are available in black and white standard 35mm slide format. -
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. -
List of Reserved Targets Sent to GRANTECAN for the Exploitation of the MEGARA Guaranteed Time at GTC
List of Reserved Targets sent to GRANTECAN for the exploitation of the MEGARA Guaranteed Time at GTC List of Reserved Targets sent to GRANTECAN for the exploitation of the MEGARA Guaranteed Time at GTC List of Reserved Targets sent to GRANTECAN for the exploitation of the MEGARA Guaranteed Time at GTC INDEX 1. MEGADES – MEGARA GALAXY DISKS EVOLUTION SURVEY: S4G .................. 3 2. MEGADES – MEGARA GALAXY DISKS EVOLUTION SURVEY: M33 ............... 11 3. SPECTROSCOPIC STUDY OF COMPACT STELLAR CLUSTERS AND THEIR SURROUNDINGS IN NEARBY GALAXIES ........................................................................ 12 4. THE CHEMICAL COMPOSITION OF PHOTOIONIZED NEBULAE¡ERROR! MARCADOR NO DEFINIDO. 5. CHROMOSPHERIC ACTIVITY AND AGE OF SOLAR ANALOGS IN OPEN CLUSTERS ................................................................ ¡ERROR! MARCADOR NO DEFINIDO. 6. STUDY OF STELLAR POPULATIONS AND GAS PROPERTIES IN STAR FORMING GALAXIES ............................................................................................................ 14 7. DISSECTING Z∼2-3 HEII-EMITTERS: SPECTRAL TEMPLATES FOR THE SOURCES OF THE COSMIC DAWN ................................................................................... 16 8. CHEMODYNAMICS OF METAL-POOR EXTREME EMISSION LINE GALAXIES AT INTERMEDIATE Z ...................................................................................... 18 9. CONSTRAINING WOLF-RAYET STARS IN EXTREMELY METAL-POOR GALAXIES ................................................................................................................................ -
407 a Abell Galaxy Cluster S 373 (AGC S 373) , 351–353 Achromat
Index A Barnard 72 , 210–211 Abell Galaxy Cluster S 373 (AGC S 373) , Barnard, E.E. , 5, 389 351–353 Barnard’s loop , 5–8 Achromat , 365 Barred-ring spiral galaxy , 235 Adaptive optics (AO) , 377, 378 Barred spiral galaxy , 146, 263, 295, 345, 354 AGC S 373. See Abell Galaxy Cluster Bean Nebulae , 303–305 S 373 (AGC S 373) Bernes 145 , 132, 138, 139 Alnitak , 11 Bernes 157 , 224–226 Alpha Centauri , 129, 151 Beta Centauri , 134, 156 Angular diameter , 364 Beta Chamaeleontis , 269, 275 Antares , 129, 169, 195, 230 Beta Crucis , 137 Anteater Nebula , 184, 222–226 Beta Orionis , 18 Antennae galaxies , 114–115 Bias frames , 393, 398 Antlia , 104, 108, 116 Binning , 391, 392, 398, 404 Apochromat , 365 Black Arrow Cluster , 73, 93, 94 Apus , 240, 248 Blue Straggler Cluster , 169, 170 Aquarius , 339, 342 Bok, B. , 151 Ara , 163, 169, 181, 230 Bok Globules , 98, 216, 269 Arcminutes (arcmins) , 288, 383, 384 Box Nebula , 132, 147, 149 Arcseconds (arcsecs) , 364, 370, 371, 397 Bug Nebula , 184, 190, 192 Arditti, D. , 382 Butterfl y Cluster , 184, 204–205 Arp 245 , 105–106 Bypass (VSNR) , 34, 38, 42–44 AstroArt , 396, 406 Autoguider , 370, 371, 376, 377, 388, 389, 396 Autoguiding , 370, 376–378, 380, 388, 389 C Caldwell Catalogue , 241 Calibration frames , 392–394, 396, B 398–399 B 257 , 198 Camera cool down , 386–387 Barnard 33 , 11–14 Campbell, C.T. , 151 Barnard 47 , 195–197 Canes Venatici , 357 Barnard 51 , 195–197 Canis Major , 4, 17, 21 S. Chadwick and I. Cooper, Imaging the Southern Sky: An Amateur Astronomer’s Guide, 407 Patrick Moore’s Practical -
The Argonne Leadership Computing Facility Scott Parker Argonne and the Blue Gene
The Argonne Leadership Computing Facility Scott Parker Argonne and the Blue Gene . 2005: – Argonne accepts 1 rack (1024 nodes) of Blue Gene/L (5.6 TF) . 2006: – Argonne Leadership Computing Facility (ALCF) created . 2008: – ALCF accepts 40 racks (160k nodes) of Blue Gene/P (557 TF) . 2009: – ALCF approved for 10 petaflop system to be delivered in 2012 . 2012 – 10 PF Mira Blue Gene/Q hardware delivered to ALCF . 2013: – Mira in production 2 ALCF Systems . Mira – BG/Q system – 49,152 nodes / 786,432 cores – 768 TB of memory – Peak flop rate: 10 PF – Linpack flop rate: 8.6 PF (#5 Top 500) . Cetus & Vesta (T&D) - BG/Q systems – 4K & 2k nodes / 64k & 32k cores – 64 TB & 32 TB of memory – 820 TF & 410 TF peak flop rate . Tukey – Nvidia system – 100 nodes / 1600 x86 cores/ 200 M2070 GPUs – 6.4 TB x86 memory / 1.2 TB GPU memory – Peak flop rate: 220 TF . Storage – 30 PB capacity, 240 GB/s bw (GPFS) – Storage upgrade planned in 2015 3 ALCF Systems (16) DDN 12Ke couplets – Scratch – 28 PB (raw), 240 GB/s Mira Infiniband 48 racks/768K cores 10 PF I/O Switch Switch (3) DDN 12Ke couplets – Home – 1.8 PB (raw), 45 GB/s Cetus (Dev) 4 rack/64K cores Complex I/O 820 TF Tape Library – 16 PB (raw) Tukey (Viz) 100 nodes/1600 cores 200 NVIDIA GPUs 220 TF Networks – 100Gb (via ESnet, internet2 UltraScienceNet, ) IB Switch (1) DDN 12Ke – 600 TB (raw), 15 GB/s Vesta (Dev) 2 racks/32K cores I/O 410 TF 4 Blue Gene DNA . -
WASP-26B: a 1-Jupiter-Mass Planet Around an Early-G-Type Star B
A&A 520, A56 (2010) Astronomy DOI: 10.1051/0004-6361/201014705 & c ESO 2010 Astrophysics WASP-26b: a 1-Jupiter-mass planet around an early-G-type star B. Smalley1,D.R.Anderson1, A. Collier Cameron2, M. Gillon3,4, C. Hellier1,T.A.Lister5,P.F.L.Maxted1, D. Queloz4,A.H.M.J.Triaud4,R.G.West6,S.J.Bentley1,B.Enoch2,F.Pepe4, D. L. Pollacco7, D. Segransan4,A.M.S.Smith1, J. Southworth1,S.Udry4,P.J.Wheatley8,P.L.Wood1, and J. Bento8 1 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK e-mail: [email protected] 2 School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK 3 Institut d’Astrophysique et de Géophysique, Université de Liège, 17 Allée du 6 Août, Bât. B5C, Liège 1, Belgium 4 Observatoire de Genève, Université de Genève, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland 5 Las Cumbres Observatory, 6740 Cortona Dr. Suite 102, Santa Barbara, CA 93117, USA 6 Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK 7 Astrophysics Research Centre, School of Mathematics & Physics, Queen’s University, University Road, Belfast, BT7 1NN, UK 8 Department of Physics, University of Warwick, Coventry CV4 7AL, UK Received 1 April 2010 / Accepted 24 June 2010 ABSTRACT We report the discovery of WASP-26b, a moderately over-sized Jupiter-mass exoplanet transiting its 11.3-mag early-G-type host star (1SWASP J001824.70-151602.3; TYC 5839-876-1) every 2.7566 days. A simultaneous fit to transit photometry and radial-velocity measurements yields a planetary mass of 1.02 ± 0.03 MJup and radius of 1.32 ± 0.08 RJup. -
Bo\" Otes IV: a New Milky Way Satellite Discovered in the Subaru Hyper
Publ. Astron. Soc. Japan (2014) 00(0), 1–13 1 doi: 10.1093/pasj/xxx000 Bootes¨ IV: A New Milky Way Satellite Discovered in the Subaru Hyper Suprime-Cam Survey and Implications for the Missing Satellite Problem Daisuke Homma1, Masashi Chiba2, Yutaka Komiyama1,3, Masayuki Tanaka1, Sakurako Okamoto1,7, Mikito Tanaka4, Miho N. Ishigaki5,2, Kohei Hayashi6, Nobuo Arimoto7,10, Scott G. Carlsten8, Robert H. Lupton8, Michael A. Strauss8, Satoshi Miyazaki1,3, Gabriel Torrealba9, Shiang-Yu Wang9, and Hitoshi Murayama5 1National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan 2Astronomical Institute, Tohoku University, Aoba-ku, Sendai 980-8578, Japan 3The Graduate University for Advanced Studies, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan 4Department of Advanced Sciences, Faculty of Science and Engineering, Hosei University, 184-8584 Tokyo, Japan 5Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan 6ICRR, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan 7Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, HI 96720, USA 8Princeton University Observatory, Peyton Hall, Princeton, NJ 08544, USA 9Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, 10617, Taiwan 10Astronomy Program, Department of Physics and Astronomy, Seoul National University, 599 Gwanak-ro, Gwanak-gu, Seoul, 151-742, Korea ∗E-mail: [email protected] Received hreception datei; Accepted hacception datei Abstract We report on the discovery of a new Milky Way (MW) satellite in Bootes¨ based on data from the on-going Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP).