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High-energy astrophysics I Introduction to high-energy astrophysics II Detectors for X-ray and gamma-rays Stéphane Paltani With lots of help from Marc Audard! Slide origin…and courtesy Several slides are original, i.e., created by Marc Audard for this course Many are, however, taken (or adapted) from presentations made by others Figures were also borrowed from the web Sources have been identified as much as possible and apologize for missing credits 2 Overview High-energy astrophysics, a short overview Detectors for the X-ray regime Proportional counter Microchannel plate CCDs: from optical to X-rays Calorimeters Superconducting tunnel junctions Detectors for the gamma-ray regime Interactions of gamma-ray photons with matter Gas-filled detectors Scintillators (organic/inorganic) Solid-state detectors Compton telescope Pair production telescope TeV astronomy 3 High-energy astrophysics Here focused on X-ray and gamma-ray energies Energetic photons from about 0.1 keV (123 Å) to several tens of keV for X-rays, MeV-GeV in gamma-rays Energetic processes: inverse Compton diffusion, synchrotron, cyclotron, collisional plasma, photoionized plasma, bremsstrahlung Common study of degenerate, compact objects (neutron stars, black holes, white dwarfs), but also non-degenerate objects (hot plasma, magnetic activity, wind shocks) 4 The atmosphere Need to go outside the atmosphere! Rockets and satellites Alternatively, use the atmosphere for detection (>10 GeV) 5 The starting point Aerobee Rocket was launched to observe X-rays from the Moon Discovery by Giacconi et al. 1962, 2002 Nobel Prize Sco X-1 was identified in 1966 The image is from a later rocket flight in 1967 6 High Energy Astrophysics: the early days Adapted7 from Palumbo, Urbino 08 High Energy Astrophysics: the days of maturity Adapted8 from Palumbo, Urbino 08 High Energy Astrophysics: the golden days + Agile 2007 Fermi 2008 NuSTAR 2012 Adapted9 from Palumbo, Urbino 08 High Energy Astrophysics: the present and future Athena ? SVOM SpektrumRG Polar ASTRO-H Astrosat Fermi Agile Suzaku Swift INTEGRAL XMM Chandra RXTE 2000 2005 2010 2015 2020 2025 2030 10 SAS-1 (Uhuru) 12-12-1970 to 03-1973 2-20 keV, 2 PC Fourth UHURU Catalog: 339 X-ray sources detected: binaries, SNR, Seyfert galaxies and cluster of galaxies First comprehensive and uniform All-sky survey Adapted11 from Palumbo, Urbino 08 COS-B, Aug 1975 – Apr 1982, 20 MeV – 1GeV Adapted12 from Palumbo, Urbino 08 HEAO-1, Aug 1977 – Jan 1979, 0.2 keV, 10 MeV 13 Adapted14 from Palumbo, Urbino 08 Adapted15 from Palumbo, Urbino 08 HEAO-2, later renamed Einstein photo Perkin-Elmer Corp. First X-ray telescope to produce images 12 November 1978 April 1981 16 Adapted from Palumbo, Urbino 08 17 EXOSAT ESA launch: 26 may 1983 End 9 april 1986 Very eccentric: orbit duration 90 h Energy range: 0.05-2 keV & 1-50keV 18 Adapted from Palumbo, Urbino 08 19 20 Blackbody emission 21 22 Bremsstrahlung (free-free), free-bound and bound bound emission 23 24 25 Compton scattering and inverse Compton scattering Inverse Compton scattering 26 Fluorescence 27 SIGMA aboard GRANAT: The precursor First space coded mask telescope in operation from 1990 to 1997 Energy range: 35 keV - 1.3 MeV Source location accuracy: 30” - 5’ 28 Adapted from Palumbo, Urbino 08 It works! observation deconvolution transmission 29 Adapted from Palumbo, Urbino 08 ROSAT : The Roentgen Satellite Lifetime : 1 June 1990 - 12 February 1999 Energy Range : X-ray 0.1 - 2.5 keV , EUV 62-206 eV 30 Adapted from Palumbo, Urbino 08 >150,000 objects 31 32 Adapted33 from Palumbo, Urbino 08 34 XMM-Newton European Photon Imaging Cameras MOS Reflection Grating Arrays EPIC pn Reflection Grating Spectrometers 35 Mirror Module Optical Monitor 36 Audard et al. (2001) 37 38 COSMOS feld 39 40 Chandra 41 Chandra X-Ray Observatory Tycho's Supernova Remnant CXC Chandra X-Ray Observatory Cassiopeia A CXC Chandra X-Ray Observatory Crab Nebula CXC Chandra X-Ray Observatory Perseus Cluster CXC Chandra X-Ray Observatory Centaurus A CXC.
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