Radio Continuum Observations of New Radio Halos and Relics from the NVSS and WENSS Surveys Relic Orientations, Cluster X-Ray Luminosity and Redshift Distributions
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ROSAT PSPC Observations of the Infrared Quasar IRAS 13349
Mon Not R Astron So c Printed August ROSAT PSPC observations of the infrared quasar IRAS evidence for a warm absorb er with internal dust WN Brandt AC Fabian and KA Pounds Institute of Astronomy Madingley Road Cambridge CB HA Internet wnbastcamacuk acfastcamacuk Xray Astronomy Group Department of Physics Astronomy University of Leicester University Road Leicester LE RH Internet kapstarleacuk ABSTRACT We present spatial temp oral and sp ectral analyses of ROSAT Position Sensitive Pro p ortional Counter PSPC observations of the infrared loud quasar IRAS IRAS is the archetypal highlyp olarized radioquiet QSO and has an op ticalinfrared luminosity of erg s We detect variability in the ROSAT count rate by a factor of in ab out one year and there is also evidence for p er cent variability within one week We nd no evidence for large intrinsic cold absorption of soft Xrays These two facts have imp ortant consequences for the scatteringplus transmission mo del of this ob ject which was developed to explain its high wavelength dep endent p olarization and other prop erties The soft Xray variability makes electron scattering of most of the soft Xrays dicult without a very p eculiar scattering mirror The lack of signicant intrinsic cold Xray absorption together with the large observed E B V suggests either a very p eculiar system geometry or more probably absorp tion by warm ionized gas with internal dust There is evidence for an ionized oxygen edge in the Xray sp ectrum IRAS has many prop erties that are similar to those -
Precollimator for X-Ray Telescope (Stray-Light Baffle) Mindrum Precision, Inc Kurt Ponsor Mirror Tech/SBIR Workshop Wednesday, Nov 2017
Mindrum.com Precollimator for X-Ray Telescope (stray-light baffle) Mindrum Precision, Inc Kurt Ponsor Mirror Tech/SBIR Workshop Wednesday, Nov 2017 1 Overview Mindrum.com Precollimator •Past •Present •Future 2 Past Mindrum.com • Space X-Ray Telescopes (XRT) • Basic Structure • Effectiveness • Past Construction 3 Space X-Ray Telescopes Mindrum.com • XMM-Newton 1999 • Chandra 1999 • HETE-2 2000-07 • INTEGRAL 2002 4 ESA/NASA Space X-Ray Telescopes Mindrum.com • Swift 2004 • Suzaku 2005-2015 • AGILE 2007 • NuSTAR 2012 5 NASA/JPL/ASI/JAXA Space X-Ray Telescopes Mindrum.com • Astrosat 2015 • Hitomi (ASTRO-H) 2016-2016 • NICER (ISS) 2017 • HXMT/Insight 慧眼 2017 6 NASA/JPL/CNSA Space X-Ray Telescopes Mindrum.com NASA/JPL-Caltech Harrison, F.A. et al. (2013; ApJ, 770, 103) 7 doi:10.1088/0004-637X/770/2/103 Basic Structure XRT Mindrum.com Grazing Incidence 8 NASA/JPL-Caltech Basic Structure: NuSTAR Mirrors Mindrum.com 9 NASA/JPL-Caltech Basic Structure XRT Mindrum.com • XMM Newton XRT 10 ESA Basic Structure XRT Mindrum.com • XMM-Newton mirrors D. de Chambure, XMM Project (ESTEC)/ESA 11 Basic Structure XRT Mindrum.com • Thermal Precollimator on ROSAT 12 http://www.xray.mpe.mpg.de/ Basic Structure XRT Mindrum.com • AGILE Precollimator 13 http://agile.asdc.asi.it Basic Structure Mindrum.com • Spektr-RG 2018 14 MPE Basic Structure: Stray X-Rays Mindrum.com 15 NASA/JPL-Caltech Basic Structure: Grazing Mindrum.com 16 NASA X-Ray Effectiveness: Straylight Mindrum.com • Correct Reflection • Secondary Only • Backside Reflection • Primary Only 17 X-Ray Effectiveness Mindrum.com • The Crab Nebula by: ROSAT (1990) Chandra 18 S. -
NASA's Goddard Space Flight Center Laboratory for High Energy
1 NASA’s Goddard Space Flight Center Laboratory for High Energy Astrophysics Greenbelt, Maryland 20771 @S0002-7537~99!00301-7# This report covers the period from July 1, 1997 to June 30, Toshiaki Takeshima, Jane Turner, Ken Watanabe, Laura 1998. Whitlock, and Tahir Yaqoob. This Laboratory’s scientific research is directed toward The following investigators are University of Maryland experimental and theoretical research in the areas of X-ray, Scientists: Drs. Keith Arnaud, Manuel Bautista, Wan Chen, gamma-ray, and cosmic-ray astrophysics. The range of inter- Fred Finkbeiner, Keith Gendreau, Una Hwang, Michael Loe- ests of the scientists includes the Sun and the solar system, wenstein, Greg Madejski, F. Scott Porter, Ian Richardson, stellar objects, binary systems, neutron stars, black holes, the Caleb Scharf, Michael Stark, and Azita Valinia. interstellar medium, normal and active galaxies, galaxy clus- Visiting scientists from other institutions: Drs. Vadim ters, cosmic-ray particles, and the extragalactic background Arefiev ~IKI!, Hilary Cane ~U. Tasmania!, Peter Gonthier radiation. Scientists and engineers in the Laboratory also ~Hope College!, Thomas Hams ~U. Seigen!, Donald Kniffen serve the scientific community, including project support ~Hampden-Sydney College!, Benzion Kozlovsky ~U. Tel such as acting as project scientists and providing technical Aviv!, Richard Kroeger ~NRL!, Hideyo Kunieda ~Nagoya assistance to various space missions. Also at any one time, U.!, Eugene Loh ~U. Utah!, Masaki Mori ~Miyagi U.!, Rob- there are typically between twelve and eighteen graduate stu- ert Nemiroff ~Mich. Tech. U.!, Hagai Netzer ~U. Tel Aviv!, dents involved in Ph.D. research work in this Laboratory. Yasushi Ogasaka ~JSPS!, Lev Titarchuk ~George Mason U.!, Currently these are graduate students from Catholic U., Stan- Alan Tylka ~NRL!, Robert Warwick ~U. -
Nustar Observatory Guide
NuSTAR Guest Observer Program NuSTAR Observatory Guide Version 3.2 (June 2016) NuSTAR Science Operations Center, California Institute of Technology, Pasadena, CA NASA Goddard Spaceflight Center, Greenbelt, MD nustar.caltech.edu heasarc.gsfc.nasa.gov/docs/nustar/index.html i Revision History Revision Date Editor Comments D1,2,3 2014-08-01 NuSTAR SOC Initial draft 1.0 2014-08-15 NuSTAR GOF Release for AO-1 Addition of more information about CZT 2.0 2014-10-30 NuSTAR SOC detectors in section 3. 3.0 2015-09-24 NuSTAR SOC Update to section 4 for release of AO-2 Update for NuSTARDAS v1.6.0 release 3.1 2016-05-10 NuSTAR SOC (nusplitsc, Section 5) 3.2 2016-06-15 NuSTAR SOC Adjustment to section 9 ii Table of Contents Revision History ......................................................................................................................................................... ii 1. INTRODUCTION ................................................................................................................................................... 1 1.1 NuSTAR Program Organization ..................................................................................................................................................................................... 1 2. The NuSTAR observatory .................................................................................................................................... 2 2.1 NuSTAR Performance ........................................................................................................................................................................................................ -
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 -
___... -.:: GEOCITIES.Ws
__ __ _____ _____ _____ _____ ____ _ __ / / / / /_ _/ / ___/ /_ _/ / __ ) / _ \ | | / / / /__/ / / / ( ( / / / / / / / /_) / | |/ / / ___ / / / \ \ / / / / / / / _ _/ |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ersion 1.21 By K. Bradley Washburn "The Historian" ______________ | __ | | \| /\ / | | |/_/ / | | |\ \/\ / | | |_\/ \/ | |______________| K. Bradley Washburn HISTORY OF THE FUTURE Page 2 of 2 FOREWARD Relevant Notes WARNING: THIS FILE IS HAZARDOUS TO YOUR PRINTER'S INK SUPPLY!!! [*Story(Time Before:Time Transpired:Time After)] KEY TO ABBREVIATIONS AS--The Amazing Stories AST--Animated Star Trek B5--Babylon 5 BT--The Best of Trek DS9--Deep Space Nine EL--Enterprise Logs ENT--Enterprise LD--The Lives of Dax NE--New Earth NF--New Frontier RPG--Role-Playing Games S.C.E.--Starfleet Corps of Engineers SA--Starfleet Academy SNW--Strange New Worlds sQ--seaQuest ST--Star Trek TNG--The Next Generation TNV--The New Voyages V--Voyager WLB—Gateways: What Lay Beyond Blue italics - Completely canonical. Animated and live-action movies, episodes, and their novelizations. Green italics - Officially canonical. Novels, comics, and graphic novels. Red italics – Marginally canonical. Role-playing material, source books, internet sources. For more notes, see the AFTERWORD K. Bradley Washburn HISTORY OF THE FUTURE Page 3 of 3 TIMELINE circa 13.5 billion years ago * The Big Bang. -
Exep Science Plan Appendix (SPA) (This Document)
ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 1 of 61 Created By: David A. Breda Date Program TDEM System Engineer Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Nick Siegler Date Program Chief Technologist Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology Concurred By: Dr. Gary Blackwood Date Program Manager Exoplanet Exploration Program NASA/Jet Propulsion Laboratory California Institute of Technology EXOPDr.LANET Douglas Hudgins E XPLORATION PROGRAMDate Program Scientist Exoplanet Exploration Program ScienceScience Plan Mission DirectorateAppendix NASA Headquarters Karl Stapelfeldt, Program Chief Scientist Eric Mamajek, Deputy Program Chief Scientist Exoplanet Exploration Program JPL CL#19-0790 JPL Document No: 1735632 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 2 of 61 Approved by: Dr. Gary Blackwood Date Program Manager, Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory Dr. Douglas Hudgins Date Program Scientist Exoplanet Exploration Program Science Mission Directorate NASA Headquarters Created by: Dr. Karl Stapelfeldt Chief Program Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology Dr. Eric Mamajek Deputy Program Chief Scientist Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory California Institute of Technology This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. © 2018 California Institute of Technology. Government sponsorship acknowledged. Exoplanet Exploration Program JPL CL#19-0790 ExEP Science Plan, Rev A JPL D: 1735632 Release Date: February 15, 2019 Page 3 of 61 Table of Contents 1. -
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. -
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. -
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 -
The Norris Survey of the Corona Borealis Supercluster: II. Galaxy
The Norris Survey of the Corona Borealis Supercluster: II. Galaxy Evolution with Redshift and Environment Todd A. Small1 and Wallace L.W. Sargent Palomar Observatory, California Institute of Technology, Pasadena, CA 91125 Electronic mail: [email protected], [email protected] Donald Hamilton Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, Heidelberg D-69117, Germany Electronic mail: [email protected] ABSTRACT We measure the field galaxy luminosity function (LF) as a function of color and redshift from z =0 to z =0.5 using galaxies from the Norris Survey of the Corona Borealis Supercluster. The data set consists of 603 field galaxies with m m 0 < z ≤ 0.5 and spans a wide range in apparent magnitude (14.0 ∼<r ∼< 21.5 ), although our field galaxy LF analysis is limited to 493 galaxies with r ≤ 20.0m. We use the observed g − r colors of the galaxies to compute accurate corrections to the rest BAB and r bands. We find that our local r-band LF, when normalized to counts in high galactic latitude fields, agrees well with the local LF measured in the Las Campanas Redshift Survey. Our BAB-band local LF, however, does not match the bj-band LF from the Stromlo/APM survey, having a normalization 1.6 times higher. We see compelling evidence that the BAB-band field galaxy LF evolves with redshift. The evolution is strongest for arXiv:astro-ph/9705021v1 5 May 1997 the population of star-forming galaxies with [O II] λ3727 rest-frame equivalent widths greater than 10A.˚ The population of red, quiescent galaxies shows no sign of evolution to z = 0.5.