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 d l e f
S O M S O
38 C 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