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Studying the evolution of the hot universe with the X-ray evolving universe spectroscopy mission – XEUS
Authors:A N Parmar  G Hasinger  M Arnaud  X Barcons  D Barret  H Bhringer  A Blanchard  M Cappi  A Comastri  T Courvoisier  A C Fabian  F Fiore  I Georgantopoulos  P Grandi  R Griffiths  A Hornstrup  N Kawai  K Koyama  K Makishima  G Malaguti  K O Mason  C Motch  M Mendez  T Ohashi  F Paerels  L Piro  T Ponman  J Schmitt  S Sciortino  G Trinchieri  M van der Klis  M Ward
Institution:a Research and Scientific Support Department of ESA, ESTEC, Keplerlaan 1, 2200 AG, Noordwijk, The Netherlands;b MPE für Extraterrische Physik, Giessenbachstrasse, Garching-bei-München, D-85741, Germany;c CEA/DSM/DAPNIA/SAP CEN-Saclay, Orme des Merisiers, Gif-sur-Yvette, F 91191, France;d Instituto de Fisica de Cantabria (CSIC-UC), Avenida Los Castros, Santander, 39005, Spain;e CESR-CNRS/UPS, 9 Avenue du Colonel Roche, 31029, Toulouse, France;f Observatoire Astronomique de Strasbourg, 11 Rue de l'Universitat, F-67000, Strasbourg, France;g IASF-CNR Bologna, Via Gobetti 101, I-40129, Bologna, Italy;h INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127, Bologna, Italy;i Observatoire de Geneve, Chemin des Maillettes, Sauverny, CH-1290, Switzerland;j Insitute of Astronomy, Madingley Road, Cambridge, CB3 0HA, United Kingdom;k INAF – Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio Catone, I-00040, Italy;l IA & A, National Observatory of Athens, I. Metaxa & B. Pavlou, Palaia Penteli, GR-15236, Greece;m IASF-CNR Roma, via del Fosso del Cavaliere, 0133, Roma, Italy;n Carnegie Mellon University, Wean Hall, 5000 Forbes Avenue, Pittsburgh, PA 15213-3890, USA;o Danish Space Research Institute, Juliane Maries Vej30, Copenhagen, DK-2100, Denmark;p Cosmic Radiation Laboratory, (RIKEN), 2-1 Hirosawa, Wako, Saitama, 351-0198, Japan;q Department of Physics, Kyoto University, Kitashirakawa-Oiwke-Cho, Sayto, Kyoto 606-8502, Japan;r Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113, Japan;s Mullard Space Science Laboratory, University College London, Holmbury St. Mary, RH5 6NT, UK;t Space Research Organization Netherlands, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands;u Department of Physics, Tokyo Metropolitan University, 1-1 Minamiosawa Hachioji, Tokyo 192-0397, Japan;v Columbia Astrophysics Laboratory, University of Columbia, 550 West 120th Street, NY 10027, USA;w Department of Space Research, University of Birmingham, Edgbaston, B15 2TT, UK;x Universität Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, Hamburg, D-21029, Germany;y INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, Parlermo, Italy;z INAF – Osservatorio Astronomico di Brera, via Brera 28, 20121, Brera, Italy;aa Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam, The Netherlands;bb X-ray Astronomy Group, University of Leicester, University Road, Leicester, LE1 7RH, UK
Abstract:Europe is one of the major partners building the International Space Station (ISS) and European industry, together with ESA, is responsible for many station components including the Columbus Orbital Facility, the Automated Transport Vehicle, two connecting modules and the European Robotic Arm. Together with this impressive list of contributions there is a strong desire within the ESA Member States to benefit from this investment by utilizing the unique capabilities of the ISS to perform world-class science. XEUS is one of the astronomical applications being studied by ESA to utilize the capabilities of the ISS. XEUS will be a long-term X-ray observatory with an initial mirror area of 6 m2 at 1 keV that will be expanded to 30 m2 following a visit to the ISS. The 1 keV spatial resolution is expected to be 2–5″ half-energy-width. XEUS will consist of separate detector and mirror spacecraft (MSC) aligned by active control to provide a focal length of 50 m. A new detector spacecraft, complete with the next generation of instruments, will also be added after visiting the ISS. The limiting 0.1–2.5 keV sensitivity will then be 4 × 10−18 erg cm−2 s−1, around 200 times better than XMM-Newton, allowing XEUS to study the properties of the hot baryons and dark matter at high redshift.
Keywords:XEUS  X-ray observatory  Astronomy  Hot baryons  Dark matter
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