IAU Information Bulletin No. 78
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The X-Ray Imaging Polarimetry Explorer
Call for a Medium-size mission opportunity in ESA‟s Science Programme for a launch in 2025 (M4) XXIIPPEE The X-ray Imaging Polarimetry Explorer Lead Proposer: Paolo Soffitta (INAF-IAPS, Italy) Contents 1. Executive summary ................................................................................................................................................ 3 2. Science case ........................................................................................................................................................... 5 3. Scientific requirements ........................................................................................................................................ 15 4. Proposed scientific instruments............................................................................................................................ 20 5. Proposed mission configuration and profile ........................................................................................................ 35 6. Management scheme ............................................................................................................................................ 45 7. Costing ................................................................................................................................................................. 50 8. Annex ................................................................................................................................................................... 52 Page 1 XIPE is proposed -
Nova Report 2006-2007
NOVA REPORTNOVA 2006 - 2007 NOVA REPORT 2006-2007 Illustration on the front cover The cover image shows a composite image of the supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. The red and green colors in the image are obtained from a million second observation of Cas A with the Chandra X-ray Observatory. The blue image is obtained with the Very Large Array at a wavelength of 21.7 cm. The emission is caused by very high energy electrons swirling around in a magnetic field. The red image is based on the ratio of line emission of Si XIII over Mg XI, which brings out the bi-polar, jet-like, structure. The green image is the Si XIII line emission itself, showing that most X-ray emission comes from a shell of stellar debris. Faintly visible in green in the center is a point-like source, which is presumably the neutron star, created just prior to the supernova explosion. Image credits: Creation/compilation: Jacco Vink. The data were obtained from: NASA Chandra X-ray observatory and Very Large Array (downloaded from Astronomy Digital Image Library http://adil.ncsa.uiuc. edu). Related scientific publications: Hwang, Vink, et al., 2004, Astrophys. J. 615, L117; Helder and Vink, 2008, Astrophys. J. in press. -
Globular Clusters and Galactic Nuclei
Scuola di Dottorato “Vito Volterra” Dottorato di Ricerca in Astronomia– XXIV ciclo Globular Clusters and Galactic Nuclei Thesis submitted to obtain the degree of Doctor of Philosophy (“Dottore di Ricerca”) in Astronomy by Alessandra Mastrobuono Battisti Program Coordinator Thesis Advisor Prof. Roberto Capuzzo Dolcetta Prof. Roberto Capuzzo Dolcetta Anno Accademico 2010-2011 ii Abstract Dynamical evolution plays a key role in shaping the current properties of star clus- ters and star cluster systems. We present the study of stellar dynamics both from a theoretical and numerical point of view. In particular we investigate this topic on different astrophysical scales, from the study of the orbital evolution and the mutual interaction of GCs in the Galactic central region to the evolution of GCs in the larger scale galactic potential. Globular Clusters (GCs), very old and massive star clusters, are ideal objects to explore many aspects of stellar dynamics and to investigate the dynamical and evolutionary mechanisms of their host galaxy. Almost every surveyed galaxy of sufficiently large mass has an associated group of GCs, i.e. a Globular Cluster System (GCS). The first part of this Thesis is devoted to the study of the evolution of GCSs in elliptical galaxies. Basing on the hypothesis that the GCS and stellar halo in a galaxy were born at the same time and, so, with the same density distribution, a logical consequence is that the presently observed difference may be due to evolution of the GCS. Actually, in this scenario, GCSs evolve due to various mechanisms, among which dynamical friction and tidal interaction with the galactic field are the most important. -
Max-Planck-Institut Für Extraterrestrische
The X-ray Universe 2011, Berlin Max-Planck-Institut für extraterrestrische Physik Download this poster here: http://www.xray.mpe.mpg.de/~hbrunner/Berlin2011Poster.pdf eROSITA: all-sky survey data reduction, source characterization, and X-ray catalogue creation Hermann Brunner1, Thomas Boller1, Marcella Brusa1, Fabrizia Guglielmetti1, Georg Lamer2, Jan Robrade3, Christian Schmid4, Nico Cappelluti5, Francesco Pace6, Mauro Roncarelli7 1Max-Planck-Institut für extraterrestrische Physik, Garching, 2Leibniz-Institut für Astrophysik, Potsdam, 3Hamburger Sternwarte, 4Dr. Karl Remeis-Sternwarte und ECAP, 5INAF-Osservatorio Astronomico di Bologna, 6Zentrum für Astronomie der Universität Heidelberg, 7Dipartimento di Astronomico, Università di Bologna eROSITA on SRG All-sky survey sensitivity eROSITA (extended Roentgen Survey with an Imaging Telescope Array) is the primary instrument on the Russian Spektrum-Roentgen-Gamma (SRG) mission, scheduled for launch in 2013. eROSITA consists of Effective area on axis 15´Background off-axis 30´off-axis seven Wolter-I telescope modules, each of which is equipped with 54 mirror shells with an outer diameter of 36 cm and a fast frame-store pn-CCD, resulting in a field-of-view (1o diameter) averaged PSF of 25´´-30´´ 1 keV HEW (on-axis: 15´´ HEW) and an effective area of 1500 cm2 at 1.5 keV. eROSITA/SRG will perform a four year long all-sky survey, to be followed be several years of pointed observations (Predehl et al. 2010). More info on eROSITA: http://www.mpe.mpg.de/erosita/ 4 keV eROSITA orbit and scanning strategy 7 keV Orbit: eROSITA/SRG will be placed in an Averaged all-sky survey PSF (examples) L2 orbit with a semi-major axis of about 1 million km and an orbital period of about 6 months. -
Exploring the Sky with Erosita
Exploring the X-ray Sky with eROSITA for the eROSITA Team Observatories and mission timelines Basic Scientific Idea …. to extend the ROSAT all-sky survey up to 12 keV with an XMM type sensitivity Historical Development Spectrum-XG Jet-X, SODART, etc. ROSAT 1990-1998 First X-ray all-sky survey with an imaging telescope Negotiations between Roskosmos and ESA ABRIXAS 1999 on a "new" Spectrum-XG mission (2005) To extend the all-sky survey towards higher energies Agreement between Roskosmos and DLR (2007) ROSITA 2002 Spectrum-RG ABRIXAS science on the eROSITA International Space Station Dark Energy 105 Clusters of Galaxies extended ROentgen Survey with an Imaging Telescope Array Mission scenario & Instrument specification • 3 month calibration & science verification phase • 4 yrs all-sky survey (8 sky coverages) • 2.7 yrs pointed observations • Energy range 0.2 - 12 keV • FOV: 1 degree • All-sky survey sensitivity ~ 6 x10-14 erg cm-2 s-1 ~ (10 – 30) x ROSAT • Deep survey field(s) (~100 sqdeg) with 5×10-15 erg cm-2 s-1 • Temporal resolution ~ 50 ms • Energy resolution ~ 130 ev @ 6 keV / 80 ev @ 1.5 keV • Angular resolution ~ 15” (20” survey) eROSITA status: completely approved and funded Mr. Putin gets informed about Dark Energy... Signature of the "Detailed Agreement" (Reichle, Wörner, Perminov) 50:50 data share between Ru / Germany HERCULES BOOTES URSA MAIOR DRACO URSA MINOR LEO CEPHEUS VIRGO CASSIOPEIA CYGNUS AURIGA AQUILA GEMINI PERSEUS ANDROMEDA SCORPIUS PEGASUS SAGITTARIUS CENTAURUS TAURUS ORION VELA CRUX CANIS MAIOR AQUARIUS CARINA HEMISPHAERA ORIENTALIS HEMISPHAERA OCCIDENTALIS Actual definition depends on mission planning eROSITA: Launch date …. -
The X-Ray Background and the ROSAT Deep Surveys
THE X–RAY BACKGROUND AND THE ROSAT DEEP SURVEYS G. HASINGER Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany E-mail : [email protected] G. ZAMORANI Osservatorio Astronomico, Via Zamboni 33, Bologna, 40126, Italy E-mail: [email protected] In this article we review the measurements and understanding of the X-ray back- ground (XRB), discovered by Giacconi and collaborators 35 years ago. We start from the early history and the debate whether the XRB is due to a single, homo- geneous physical process or to the summed emission of discrete sources, which was finally settled by COBE and ROSAT. We then describe in detail the progress from ROSAT deep surveys and optical identifications of the faint X-ray source popula- tion. In particular we discuss the role of active galactic nuclei (AGNs) as dominant contributors for the XRB, and argue that so far there is no need to postulate a hypothesized new population of X-ray sources. The recent advances in the under- standing of X-ray spectra of AGN is reviewed and a population synthesis model, based on the unified AGN schemes, is presented. This model is so far the most promising to explain all observational constraints. Future sensitive X-ray surveys in the harder X-ray band will be able to unambiguously test this picture. 1 Introduction It is a heavy responsibility for us, as it would be for everybody else, to write a paper on the X–ray Deep Surveys and the X–ray background (XRB) for this book, in honour of Riccardo Giacconi. -
Towards a New Generation Axion Helioscope
Towards a new generation axion helioscope Igor G Irastorza Universidad de Zaragoza International Conference onParticle Physics IstambulIstambul,, Turkey,Turkey, June 2020--25th25th 2011 Outline TlkTalk bdbased on JCAP 06 (2011) 013 OutlineOutline:: – Axions: motivation,motivation, theorytheory,, cosmologycosmology.. – Solar axions & the axion helioscopppe concept ––PreviousPrevioushelioscopes & CAST ––TechnicalTechnicalprospects for a new helioscope – Sensitivity prospects ––ConclusionsConclusions ICPP, Istambul, June 2011 Igor G. Irastorza / Universidad de 2 Zaragoza AXION motivation Strong CP problem: why strong interactions seem not to violate CP? – CP violating term in QCD is not forbidden . But neutron electric dipole moment not observed. Natural answer if Peccei-Quinn mechanism exist. – New U(1) gl lob al symmet ry spontlbktaneously broken. As a result, new pseudoscalar, neutral and very light particle is predicted, the axion. It couples to the photon in every model. PRIMAKOFF EFFECT ICPP, Istambul, June 2011 Igor G. Irastorza / Universidad de 3 Zaragoza AXION motivation: Cosmology Axions are produced in the earlyyy Universe by a number of processes: – Axion realignment – Decay of axion strings NONNON--RELATIVISTICRELATIVISTIC – Decay of axion walls (COLD) AXIONS In general, Range of axion masses of 10--66 ––1010--33 eV are of interest for the axionto be the (main component of the) CDM. – Thermal production RELATIVISTIC (HOT) AXIONS In order to have substantial relativistic axiondensity, the axion mass must be close to 1 eV.eV. (ma >1.02 eV gives densities too much in excess to be compatible with latest CMB data) Hannestad et al, JCAP 0804 (2008) 019 [0803.1585 (astro-ph)] ICPP, Istambul, June 2011 Igor G. Irastorza / Universidad de 4 Zaragoza Solar Axions SlSolar axi ons prod uced db by ph otonoton--toto-- axion conversion of the solar plasma photons Solar axion flux [van Bibber PRD 39 (89)] [CAST JCAP 04(2007)010] Solar physics + Primakoff effect Only one unknown parameter ga ICPP, Istambul, June 2011 Igor G. -
[Astro-Ph.IM] 5 Nov 2017 INTEGRAL Nodrt Rgesi Hsfil,T Sals Hc R H Technolog Universe
Noname manuscript No. (will be inserted by the editor) Hard X–ray/Soft gamma–ray experiments and missions: overview and prospects Erica Cavallari · Filippo Frontera Received: date / Accepted: date Abstract Starting from 1960s, a great number of missions and experiments have been performed for the study of the high–energy sky. This review gives a wide vision of the most important space missions and balloon experiments that have operated in the 10–600 keV band, a crucial window for the study of the most energetic and violent phenomena in the Universe. Thus it is important to take the stock of the achievements to better establish what we have still to do with future missions in order to progress in this field, to establish which are the technologies required to solve the still open issues and to extend our knowledge of the Universe. Keywords high-energy astrophysics · hard X-ray astronomy · space missions · balloon experiments 1 Introduction It is recognized that hard X–ray/soft gamma–ray astronomy (10–600 keV) is a crucial window for the study of the most energetic and violent events in the Universe. An increasing number of missions devoted to observations in this band or including instruments specifically devoted to perform hard X–ray observations have been performed (e.g., BeppoSAX , Rossi XTE) or are still operational (e.g., INTEGRAL, Swift, Fermi). Actually in the remote past this was only considered an ancillary energy band. The bands which were considered key for astrophysical observations were the 2–10 keV band, also dubbed classic en- ergy band, and the soft X–ray band (≤ 2 keV). -
SIMULTANEOUS Nustar/CHANDRA OBSERVATIONS of the BURSTING PULSAR GRO J1744-28 DURING ITS THIRD REACTIVATION
SIMULTANEOUS NuSTAR/CHANDRA OBSERVATIONS OF THE BURSTING PULSAR GRO J1744-28 DURING ITS THIRD REACTIVATION The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Younes, G., C. Kouveliotou, B. W. Grefenstette, J. A. Tomsick, A. Tennant, M. H. Finger, F. Fürst, et al. “SIMULTANEOUS NuSTAR/ CHANDRA OBSERVATIONS OF THE BURSTING PULSAR GRO J1744-28 DURING ITS THIRD REACTIVATION.” The Astrophysical Journal 804, no. 1 (April 29, 2015): 43. © 2015 The American Astronomical Society As Published http://dx.doi.org/10.1088/0004-637x/804/1/43 Publisher IOP Publishing Version Final published version Citable link http://hdl.handle.net/1721.1/98366 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal, 804:43 (16pp), 2015 May 1 doi:10.1088/0004-637X/804/1/43 © 2015. The American Astronomical Society. All rights reserved. SIMULTANEOUS NuSTAR/CHANDRA OBSERVATIONS OF THE BURSTING PULSAR GRO J1744-28 DURING ITS THIRD REACTIVATION G. Younes1,2, C. Kouveliotou3,2, B. W. Grefenstette4, J. A. Tomsick5, A. Tennant3,2, M. H. Finger1,2, F. Fürst4, K. Pottschmidt6,7, V. Bhalerao8, S. E. Boggs5, L. Boirin9, D. Chakrabarty10, F. E. Christensen11, W. W. Craig5,12, N. Degenaar13, A. C. Fabian14, P. Gandhi15,E.Göğüş16, C. J. Hailey17, F. A. Harrison4, J. A. Kennea18, J. M. Miller11, D. Stern19, and W. W. Zhang20 1 Universities Space Research Association, -
PLANETARIAN Journal of the International Planetarium Society Vol
PLANETARIAN Journal of the International Planetarium Society Vol. 26, No.4, December 1997 Articles 6 Planetarium Mystique-Our Secret Weapon ..... Jon A. Marshall 12 Astronomy Link Update ........................................... Jim Manning 18 Invitations to IPS 2002 ............................................................. hosts 22 Minutes of the 1972 Council Meeting ............... Lee Ann Hennig Features 27 Computer Corner: Moontool & Jupiter's Moons ...... Ken Wilson 29 Regional Roundup ..................................................... Lars Broman 32 Book Reviews ............................................................ April S. Whitt 38 Planetarium Memories ................................... Kenneth E. Perkins 40 Mobile News Network ............................................. Sue Reynolds 43 Forum: NASA & Public Education ............................ Steve Tidey 47 Gibbous Gazette .................................................. Christine Shupla 50 What's New ................................................................ Jim Manning 53 Opening the Dome: Spirit of Dome .. Jon U. Bell/Carrie Meyers 56 President's Message ............................................. Thomas Kraupe 59 Planetechnica: Computer Imaging Basics ... Richard McColman 66 Jane's Corner ............................................................. Jane Hastings Seeing Is Believing! (Ps EDi'i[ZEe,arlums For further information contact Pearl Reilly: 1-800 .. 726-8805 I NSTRLJrvl fax: 1-504-764-7665 Planetarium Division email: [email protected] -
Erosita Extended Roentgen Survey with an Imaging Telescope Array
eROSITA extended ROentgen Survey with an Imaging Telescope Array Vadim Burwitz for the eROSITA Team: PI: Peter Predehl Co-Is: Hans Böhringer, Ulrich Briel, Hermann Brunner, Evgeniy Churazov, Michael Freyberg, Peter Friedrich, Günther Hasinger, Eckhard Kendziorra, Dieter Lutz, Norbert Meidinger, Mikhail Pavlinsky, Andrea Santangelo, Jürgen Schmitt, Axel Schwope, Matthias Steinmetz, Lothar Strüder, Rashid Sunyaev, Jörn Wilms System Engineer: Josef Eder Product Assurance: H. Bräuninger, M. Hengmith Electronics Engineering: W. Bornemann, O. Hälker, S. Hermann, W. Kink, S. Müller, O. Hans Mechanical Engineering: H. Huber, Chr. Rohé, L. Tiedemann, R. Schreib, B. Mican, K. Lehmann, H. Eibl, F. Huber, R. Sandmair, P. Straube, H. Kestler, F. Soller, J. Liebhart Mirror System, PANTER: P. Friedrich, W. Burkert, M. Freyberg, B. Budau, E. Pfeffermann, V. Burwitz + students CliThlEiiCooling, Thermal Engineering: MFüM. Fürmetz + stu dents CCD-Camera: N. Meidinger, R. Hartmann, G. Schächner, J. Elbs, S. Ebermayer Attitude: A. Schwope Calibration, Analysis: G. Hartner, U. Briel, K. Dennerl, R. Andritschke, Chr. Tenzer Laboratory, PUMA, Tests: M. Vongehr, R. Gaida, K. Dittrich, F. Schrey Ground Software, Simulation: H. Brunner,,pp, N. Cappelluti, G. Lamer, M. Mühlegg gg,,yer, J. Wilms, I. Kreykenbohm , Chr. Schmid Mission Planning: J. Schmitt, J. Robrade Institutes: Industry: Max-Planck-Institut für extraterrestrische Physik, Garching/D Media Lario/I Mirrors, Mandrels Space Research Institute IKI, Moscow/Ru Kayser-Threde/D Mirror Mechanics Univ. Tübingen/D Carl Zeiss/D Mirror Mandrels Univ. Hamburg/D Invent/D Telescope Structure Univ. Erlangen-Nürnberg/D pnSensor/D CCDs Astroppyhysikalisches Institut Potsdam/D EHP/B Cooling Max-Planck-Institut für Astrophysik/D RUAG/A Mechanisms, MLI .. -
Women of Goddard: Careers in Science, Technology, Engineering, and Mathematics
Women of Goddard: Careers in Science, Technology, Engineering, and Mathematics Engineering, Technology, Careers in Science, of Goddard: Women National Aeronautics and Space Administration Goddard of Parkinson, Millar, Thaller Millar, Parkinson, Careers in Science Technology Engineering & Mathematics Women www.nasa.gov Women of Goddard NASA’s Goddard Space Flight Center IV&V, WV Goddard Institute for Space Studies, Greenbelt, Maryland, Main Campus Wallops Flight Facility, Virginia New York City Testing and Integration Facility, Greenbelt Home of Super Computing and Data Storage, Greenbelt GSFC’s new Sciences and Exploration Building, Greenbelt Women of Goddard: Careers in Science, Technology, Engineering, and Mathematics Editors: Claire L. Parkinson, Pamela S. Millar, and Michelle Thaller Graphics and Layout: Jay S. Friedlander In Association with: The Maryland Women’s Heritage Center (MWHC) NASA Goddard Space Flight Center, Greenbelt, Maryland, July 2011 Women of Goddard Careers in Foreword Science A century ago women in the United States could be schoolteachers and nurses but were largely excluded from the vast majority of other jobs that could Technology be classified as Science, Technology, Engineering, or Mathematics (STEM careers). Some inroads were fortuitously made during World Wars I and II, when because of Engineering the number of men engaged in fighting overseas it became essential that women fill in on jobs of all types on the home front. However, many of these inroads Mathematics were lost after the wars ended and the men