Provisional Scientific Programme
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Arxiv:1903.02002V1 [Astro-Ph.GA] 5 Mar 2019
Draft version March 7, 2019 Typeset using LATEX twocolumn style in AASTeX62 RELICS: Reionization Lensing Cluster Survey Dan Coe,1 Brett Salmon,1 Maruˇsa Bradacˇ,2 Larry D. Bradley,1 Keren Sharon,3 Adi Zitrin,4 Ana Acebron,4 Catherine Cerny,5 Nathalia´ Cibirka,4 Victoria Strait,2 Rachel Paterno-Mahler,3 Guillaume Mahler,3 Roberto J. Avila,1 Sara Ogaz,1 Kuang-Han Huang,2 Debora Pelliccia,2, 6 Daniel P. Stark,7 Ramesh Mainali,7 Pascal A. Oesch,8 Michele Trenti,9, 10 Daniela Carrasco,9 William A. Dawson,11 Steven A. Rodney,12 Louis-Gregory Strolger,1 Adam G. Riess,1 Christine Jones,13 Brenda L. Frye,7 Nicole G. Czakon,14 Keiichi Umetsu,14 Benedetta Vulcani,15 Or Graur,13, 16, 17 Saurabh W. Jha,18 Melissa L. Graham,19 Alberto Molino,20, 21 Mario Nonino,22 Jens Hjorth,23 Jonatan Selsing,24, 25 Lise Christensen,23 Shotaro Kikuchihara,26, 27 Masami Ouchi,26, 28 Masamune Oguri,29, 30, 28 Brian Welch,31 Brian C. Lemaux,2 Felipe Andrade-Santos,13 Austin T. Hoag,2 Traci L. Johnson,32 Avery Peterson,32 Matthew Past,32 Carter Fox,3 Irene Agulli,4 Rachael Livermore,9, 10 Russell E. Ryan,1 Daniel Lam,33 Irene Sendra-Server,34 Sune Toft,24, 25 Lorenzo Lovisari,13 and Yuanyuan Su13 1Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 2Department of Physics, University of California, Davis, CA 95616, USA 3Department of Astronomy, University of Michigan, 1085 South University Ave, Ann Arbor, MI 48109, USA 4Physics Department, Ben-Gurion University of the Negev, P.O. -
Radio Observations of the Merging Galaxy Cluster Abell 520 D
A&A 622, A20 (2019) Astronomy https://doi.org/10.1051/0004-6361/201833900 & c ESO 2019 Astrophysics LOFAR Surveys: a new window on the Universe Special issue Radio observations of the merging galaxy cluster Abell 520 D. N. Hoang1, T. W. Shimwell2,1, R. J. van Weeren1, G. Brunetti3, H. J. A. Röttgering1, F. Andrade-Santos4, A. Botteon3,5, M. Brüggen6, R. Cassano3, A. Drabent7, F. de Gasperin6, M. Hoeft7, H. T. Intema1, D. A. Rafferty6, A. Shweta8, and A. Stroe9 1 Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, The Netherlands e-mail: [email protected] 2 Netherlands Institute for Radio Astronomy (ASTRON), PO Box 2, 7990 AA Dwingeloo, The Netherlands 3 INAF-Istituto di Radioastronomia, via P. Gobetti 101, 40129 Bologna, Italy 4 Harvard-Smithsonian for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 5 Dipartimento di Fisica e Astronomia, Università di Bologna, via P. Gobetti 93/2, 40129 Bologna, Italy 6 Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany 7 Thüringer Landessternwarte, Sternwarte 5, 07778 Tautenburg, Germany 8 Indian Institute of Science Education and Research (IISER), Pune, India 9 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany Received 18 July 2018 / Accepted 10 September 2018 ABSTRACT Context. Extended synchrotron radio sources are often observed in merging galaxy clusters. Studies of the extended emission help us to understand the mechanisms in which the radio emitting particles gain their relativistic energies. Aims. We examine the possible acceleration mechanisms of the relativistic particles that are responsible for the extended radio emis- sion in the merging galaxy cluster Abell 520. -
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. -
Spectral Index Maps of the Radio Halos in Abell 665 and Abell 2163
A&A 423, 111–119 (2004) Astronomy DOI: 10.1051/0004-6361:20040316 & c ESO 2004 Astrophysics Spectral index maps of the radio halos in Abell 665 and Abell 2163 L. Feretti1,E.Orr`u1,G.Brunetti1, G. Giovannini1,2, N. Kassim3, and G. Setti1,2 1 Istituto di Radioastronomia – CNR, via P. Gobetti 101, 40129 Bologna, Italy e-mail: [email protected] 2 Dipartimento di Astronomia, Univ. Bologna, via Ranzani 1, 40127 Bologna, Italy 3 Naval Research Laboratory, Code 7213, Washington DC 20375, USA Received 23 February 2004 / Accepted 14 April 2004 Abstract. New radio data at 330 MHz are presented for the rich clusters Abell 665 and Abell 2163, whose radio emission is characterized by the presence of a radio halo. These images allowed us to derive the spectral properties of the two clusters α1.4 = . under study. The integrated spectra of these halos between 0.3 GHz and 1.4 GHz are moderately steep: 0.3 1 04 and α1.4 = . 0.3 1 18, for A665 and A2163, respectively. The spectral index maps, produced with an angular resolution of the order of ∼1, show features of the spectral index (flattening and patches), which are indication of a complex shape of the radiating electron spectrum, and are therefore in support of electron reacceleration models. Regions of flatter spectrum are found to be related to the recent merger activity in these clusters. This is the first strong confirmation that the cluster merger supplies energy to the radio halo. In the undisturbed cluster regions, the spectrum steepens with the distance from the cluster center. -
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. -
Physical Properties of the X-Ray Gas As a Dynamical Diagnosis for Galaxy
MNRAS 000, 1–24 (2019) Preprint 7 February 2019 Compiled using MNRAS LATEX style file v3.0 Physical properties of the X-ray gas as a dynamical diagnosis for galaxy clusters T. F. Lagan´a,1⋆ F. Durret2 and P. A. A. Lopes3 1NAT, Universidade Cruzeiro do Sul, Rua Galv˜ao Bueno, 868, CEP:01506-000, S˜ao Paulo-SP, Brazil 2 Sorbonne Universit´e, CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis Bd Arago, F-75014 Paris, France. 3 Observat´orio do Valongo, Universidade Federal do Rio de Janeiro, Ladeira do Pedro Antˆonio 43, Rio de Janeiro, RJ, 20080-090, Brazil Accepted 2018 December 19. Received 2018 December 17; in original form 2018 November 29. ABSTRACT We analysed XMM-Newton EPIC data for 53 galaxy clusters. Through 2D spec- tral maps, we provide the most detailed and extended view of the spatial distribution of temperature (kT), pressure (P), entropy (S) and metallicity (Z) of galaxy clusters to date with the aim of correlating the dynamical state of the system to six cool-core diagnoses from the literature. With the objective of building 2D maps and resolving structures in kT, P, S and Z, we divide the data in small regions from which spectra can be extracted. Our analysis shows that when clusters are spherically symmetric the cool-cores (CC) are preserved, the systems are relaxed with little signs of perturbation, and most of the CC criteria agree. The disturbed clusters are elongated, show clear signs of interaction in the 2D maps, and most do not have a cool-core. -
Dark Matter and Background Light
Dark Matter and Background Light J.M. Overduin Gravity Probe B, Hansen Experimental Physics Laboratory, Stanford University, Stanford, California, U.S.A. 94305-4085 and P.S. Wesson Department of Physics, University of Waterloo, Ontario, Canada N2L 3G1 Abstract Progress in observational cosmology over the past five years has established that the Universe is dominated dynamically by dark matter and dark energy. Both these new and apparently independent forms of matter-energy have properties that are inconsistent with anything in the existing standard model of particle physics, and it appears that the latter must be extended. We review what is known about dark matter and energy from their impact on the light of the night sky. Most of the candidates that have been proposed so far are not perfectly black, but decay into or otherwise interact with photons in characteristic ways that can be accurately modelled and compared with observational data. We show how experimental limits on the intensity of cosmic background radiation in the microwave, infrared, optical, arXiv:astro-ph/0407207v1 10 Jul 2004 ultraviolet, x-ray and γ-ray bands put strong limits on decaying vacuum energy, light axions, neutrinos, unstable weakly-interacting massive particles (WIMPs) and objects like black holes. Our conclusion is that the dark matter is most likely to be WIMPs if conventional cosmology holds; or higher-dimensional sources if spacetime needs to be extended. Key words: Cosmology, Background radiation, Dark matter, Black holes, Higher-dimensional field theory PACS: 98.80.-k, 98.70.Vc, 95.35.+d, 04.70.Dy, 04.50.+h Email addresses: [email protected] (J.M. -
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 -
Dr. Daniel Ryan Wik | Curriculum Vitae
Dr. Daniel Ryan Wik | Curriculum Vitae 201 James Fletcher Bldg. | 115 S. 1400 E. | Salt Lake City, UT 84112-0830 (801) 585-5832 | [email protected] | http://www.astro.utah.edu/~wik PDF version of CV: http://www.astro.utah.edu/~wik/cv.pdf Research Interests and Experience Dr. Wik’s research includes investigations of inverse Compton scattering in galaxy clusters and starburst galaxies, the effects of cluster mergers on intracluster gas and their cosmological implications, the X-ray binary populations of galaxies, dark matter searches, and the X-ray background. He is an observational X-ray astronomer with extensive experience carrying out observatory data calibration and analysis tool development, who also has some background in computer simulations and instrumentation. Research Positions • 2017-present: Assistant Professor, University of Utah • 2013-2017: Assistant Research Scientist, Johns Hopkins University, at NASA/GSFC • 2010-13: NASA Postdoctoral Position (NPP) Fellow at Goddard Space Flight Center Education • 2010: Ph.D. Astronomy, University of Virginia (UVa), Charlottesville, VA – Dissertation Title: “Inverse Compton Scattering in Galaxy Clusters” – Advisor: Craig Sarazin • 2006: M.Sc. Astronomy, University of Virginia, Charlottesville, VA • 2003: B.Sc. Astrophysics (Minor: Mathematics), Ohio University, Athens, OH Awards and Honors • 2019: Students’ Choice Award for the best Undergraduate Seminar (Spring) • 2017: NASA Special Act Team Award for the GSFC Hitomi Science Team • 2017: NASA RHG Exceptional Achievement for Science -
Evolution of the Near-Infrared Luminosity Function in Rich Galaxy
Evolution of the near-infrared luminosity function in rich galaxy clusters Neil Trentham Institute of Astronomy, University of Cambridge Madingley Road, Cambridge CB3 0HA and Bahram Mobasher Astrophysics Group, Imperial College Blackett Laboratory, Prince Consort Road, London SW7 2BZ Submitted to MNRAS arXiv:astro-ph/9805282v1 21 May 1998 ABSTRACT We present the K-band (2.2 µ) luminosity functions of the X-ray luminous clusters MS1054−0321 (z = 0.823), MS0451−0305 (z = 0.55), Abell 963 (z = 0.206), Abell 665 (z = 0.182) and Abell 1795 (z = 0.063) down to absolute magnitudes MK = −20. Our measurements probe fainter absolute magnitudes than do any previous studies of the near- infrared luminosity function of clusters. All the clusters are found to have similar luminosity functions within the errors, when the galaxy populations are evolved to redshift z = 0. It is known that the most massive bound systems in the Universe at all redshifts are X-ray luminous clusters. Therefore, assuming that the clusters in our sample correspond to a single population seen at different redshifts, the results here imply that not only had the stars in present-day ellipticals in rich clusters formed by z =0.8, but that they existed in as luminous galaxies then as they do today. Addtionally, the clusters have K-band luminosity functions which appear to be con- sistent with the K-band field luminosity function in the range −24 < MK < −22, although the uncertainties in both the field and cluster samples are large. Key words: galaxies : clusters: luminosity function – infrared: galaxies – galaxies: clusters: individual: MS1054-0321, MS0451-0305, Abell 963, Abell 665, Abell 1795 –2– 1 INTRODUCTION Recent observations of rich clusters of galaxies and their galaxy populations have revealed a number of interesting results: (i) Three X-ray luminous clusters at redshifts z ∼ 0.8 have been discovered in the ROSAT North Ecliptic Pole (NEP) survey (Gioia & Luppino 1994, Henry et al. -
The Intracluster Magnetic Field Power Spectrum in Abell
Astronomy & Astrophysics manuscript no. paper c ESO 2018 October 30, 2018 The intracluster magnetic field power spectrum in Abell 665 V. Vacca1, M. Murgia2,3, F. Govoni2, L. Feretti3, G. Giovannini3,4, E. Orr`u5, and A. Bonafede3,4 1 Dipartimento di Fisica, Universit`adegli studi di Cagliari, Cittadella Universitaria, I–09042 Monserrato (CA), Italy 2 INAF - Osservatorio Astronomico di Cagliari, Poggio dei Pini, Strada 54, I–09012 Capoterra (CA), Italy 3 INAF - Istituto di Radioastronomia, Via Gobetti 101, I–40129 Bologna, Italy 4 Dipartimento di Astronomia, Univ. Bologna, Via Ranzani 1, I–40127 Bologna, Italy 5 Institute for Astro and Particle Physics, University of Innsbruck, Technikerstr. 25, 6020 Innsbruck, Austria − Received MM DD, YY; accepted MM DD, YY ABSTRACT Aims. The goal of this work is to investigate the power spectrum of the magnetic field associated with the giant radio halo in the galaxy cluster A665. Methods. For this, we present new deep Very Large Array total intensity and polarization observations at 1.4 GHz. We simulated Gaussian random three-dimensional turbulent magnetic field models to reproduce the observed radio halo emission. By comparing observed and synthetic radio halo images we constrained the strength and structure of the intracluster magnetic field. We assumed that the magnetic field power spectrum is a power law with a Kolmogorov index and we imposed a local equipartition of energy density between relativistic particles and field. Results. Under these assumptions, we find that the radio halo emission in A665 is consistent with a central magnetic field strength of about 1.3 µG. To explain the azimuthally averaged radio brightness profile, the magnetic field energy density should decrease following the thermal gas density, leading to an averaged magnetic field strength over the central 1 Mpc3 of about 0.75 µG. -
X-Ray Spectroscopy of Cooling Clusters
X-ray Spectroscopy of Cooling Clusters J. R. Peterson a,1 & A. C. Fabian b,2 aKavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, PO Box 20450, Stanford, CA 94309, USA bInstitute of Astronomy (IoA), Cambridge University, Madingley Road, Cambridge CB3 0HA, UK Abstract We review the X-ray spectra of the cores of clusters of galaxies. Recent high resolu- tion X-ray spectroscopic observations have demonstrated a severe deficit of emission at the lowest X-ray temperatures as compared to that expected from simple radia- tive cooling models. The same observations have provided compelling evidence that the gas in the cores is cooling below half the maximum temperature. We review these results, discuss physical models of cooling clusters, and describe the X-ray instrumentation and analysis techniques used to make these observations. We dis- cuss several viable mechanisms designed to cancel or distort the expected process of X-ray cluster cooling. arXiv:astro-ph/0512549v1 21 Dec 2005 1 JRP E-mail: [email protected] 2 ACF E-mail: [email protected] Preprint submitted to Elsevier Preprint 5 February 2008 Contents 1 Introduction 4 2 Clusters of Galaxies 5 3 Physics of the Intracluster Medium 7 3.1 X-ray Emission from Collisional Plasmas 7 3.2 Magneto-hydrodynamics 15 3.3 Cooling flows 18 4 X-ray Instrumentation and Observational Techniques 24 4.1 X-ray Telescopes and their Relevance to Clusters 24 4.2 Analysis Techniques 26 5 X-ray Spectra of Cooling Clusters 28 5.1 Early Work on Imaging Observations 28 5.2