Tutorial Guide to X-ray and Gamma-ray Astronomy (eBook, PDF)
Data Reduction and Analysis
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Tutorial Guide to X-ray and Gamma-ray Astronomy (eBook, PDF)
Data Reduction and Analysis
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This book provides a comprehensive introduction to X-ray and gamma-ray astronomy. The first part discusses the basic theoretical and observational topics related to black hole astrophysics; the optics and the detectors employed in X-ray and gamma-ray astronomy; and past, present, and future X-ray and gamma-ray missions. The second part then describes data reduction and analysis, the statistics used in X-ray and gamma-ray astronomy, and demonstrates how to write a successful proposal and a scientific paper. Data reduction in connection with specific X-ray and gamma-ray missions is covered in…mehr
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This book provides a comprehensive introduction to X-ray and gamma-ray astronomy. The first part discusses the basic theoretical and observational topics related to black hole astrophysics; the optics and the detectors employed in X-ray and gamma-ray astronomy; and past, present, and future X-ray and gamma-ray missions. The second part then describes data reduction and analysis, the statistics used in X-ray and gamma-ray astronomy, and demonstrates how to write a successful proposal and a scientific paper. Data reduction in connection with specific X-ray and gamma-ray missions is covered in the appendices. Presenting the state of the art in X-ray and gamma-ray astronomy, this is both a valuable textbook for students and an important reference resource for researchers in the field.
Produktdetails
- Produktdetails
- Verlag: Springer Singapore
- Erscheinungstermin: 30. Juli 2020
- Englisch
- ISBN-13: 9789811563379
- Artikelnr.: 59899319
- Verlag: Springer Singapore
- Erscheinungstermin: 30. Juli 2020
- Englisch
- ISBN-13: 9789811563379
- Artikelnr.: 59899319
Cosimo Bambi is Xie Xide Junior Chair Professor at the Department of Physics at Fudan University (China). He received his Ph.D. from Ferrara University (Italy) in 2007 and was a postdoc at Wayne State University (Michigan), IPMU at The University of Tokyo (Japan), and at LMU Munich (Germany). He moved to Fudan University at the end of 2012 under the Thousand Young Talents Program. His research interests cover several areas in gravity, cosmology, and high-energy astrophysics. He has published more than 100 papers on refereed journals as first or corresponding author, has over 3,500 citations, and his h-index is 36. He has authored three books, and edited one volume (in ASSL) with Springer.
Preface Contents 1. The High Energy Window 1.1 Some fundamental concepts 2. Emission processes in Active Galactic Nuclei [Bambi, Grandi, Torresi,…] 2.1 Thermal processes: 2.1.1 Optically thick and geometrically thin disk 2.1.2 Hot corona: x-ray production by Thermal Comptonization 2.1.3 X-ray reprocessing: iron line and Compton hump 2.1.4 ADAF 2.2 Non thermal Processes 2.1 Synchrotron radiation 2.2 Inverse Compton 2.3 SSC 2.4 Hadronic cascade 3. AGN as a high energy laboratory [Grandi, Torresi,…] 3.1 AGN: why do we study them? 3.2 Spectral energy Distribution 3.2.1 Radio quiet AGN 3.2.1.1 Accretion disk and soft excess 3.2.1.2 Iron line and reflection 3.2.1.3 Warm absorber and winds 3.2.2 Radio Loud AGN 3.2.2.1 Core 3.2.2.2 Jets on kpc scales 3.2.2.3 Radio lobes 3.3 Classification of AGN 3.3.1 Optical classification 3.3.2 Radio classification 3.3.3 Doppler Boosting 3.4 Radio Quiet - Radio Loud AGN 3.4.1 Radio Loudness 3.4.2 Tomography of an AGN 3.5 Unification of accreting black holes through all mass scales 4. How to detect X-rays and gamma-rays from space: optics and detectors [Bulgarelli, Fioretti] 4.1 Matter and radiation interaction 4.1.1 Photoelectric effect 4.1.2 Compton effect 4.1.3 Pair production 4.2 Fundamental Concepts 4.2.1 Quantum efficiency 4.2.2 Effective Area 4.2.3 Energy redistribution 4.2.4 Sensitivity 4.2.5 Spatial Resolution 4.2.6 Angular Resolution 4.3 Detectors 4.3.1 Scintillator (including scintillators for gamma-ray astronomy) 4.3.2 Microchannel Plate 4.3.3 CdTe 4.3.4 CZT 4.3.5 CCD 4.3.6 Spark chambers 4.3.7 Silicon strip detectors 4.3.8 Calorimeters 4.4 Mirror and focussing of photons 4.4.1 Collimated System 4.4.2 Focussing System 4.5 Monte Carlo Simulations of X-ray and Gamma-ray Telescope 4.5.1 Toolkits and frameworks 4.5.2 Space radiation environment 4.5.3 Spacecraft and payload mass modeling 4.5.4 Analysis pipeline for the residual background evaluation 5 Past, present, and future X-ray and gamma-ray missions [Bulgarelli, Guainazzi, Pollock, …] 5.1 The discovery of astrophysical X-ray sources 5.2 The initial surveys 5.3 The first observatories 5.3.1 Explorer-11 5.3.2 OSO-3 5.3.3 SAS-2 5.3.4 COS-B 5.3.5 Einstein 5.3.6 EXOSAT 5.3.7 CGRO (A general introduction here to provide the big view: more details in 5.8.2 and 5.9.2) 5.4 Imaging proportional counters 5.4.1 The ROSAT PSPC 5.4.2 The ROSAT All Sky Survey (RASS) 5.4.3 The broad-band perspective 5.4.3.1 BeppoSAX 5.4.3.2 Astrosat 5.4.3.3 HXMT 5.4.4 High-resolution timing 5.5 X-ray CCD astrophysics 5.5.1 Spectroscopic imaging of thermal plasmas 5.5.1.2 SNRs 5.5.1.3 Galaxies 5.5.1.4 Galaxy clusters 5.5.2 Surveys and the XRB 5.5.3 Serendipitous source catalogs 5.5.3.1 The Chandra Source Catalog 5.5.3.2 The XMM-Newton EPIC Source Catalog 5.5.3.3 The XMM-Newton Slew Catalog 5.5.3.4 The Swift XRT catalogs 5.6 The path towards hard X-ray focusing 5.6.1 The BeppoSAX/PDS 5.6.2 Suzaku 5.6.3 NuSTAR: the focusing revolution 5.7 High-resolution spectroscopy 5.7.1 Gratings versus calorimeters 5.7.2 Diagnostics of intergalactic plasmas 5.7.3 Where are the missing baryons? 5.7.4 Accreting black holes 5.8 Compton telescopes 5.8.1 General principles 5.8.2 CGRO/COMPTEL 5.9 Pair-tracking telescopes 5.9.1 General principles 5.9.2 Early phase: SAS-II, COS-B, CGRO/EGRET [spark chamber + calorimeter + anticoincidence shield: SAS-II (1972, 20 MeV - 300 MeV), COS-B (1975-82, 30 MeV - 3 GeV), CGRO/EGRET (1991-2000, 20 MeV - 30 GeV)] 5.9.3 - Silicon Trackers: AGILE and Fermi [silicon-strip detectors + calorimeter + anticoincidence shield: AGILE/GRID (2007-now, 30 MeV - 50 GeV) and Fermi/LAT (2008-now, 30 MeV - 300 GeV)] 5.10 The Future 5.10.1 eRosita 5.10.2 XARM 5.10.3 eXTP 5.10.4 Einstein Probe 5.10.5 Athena 5.10.6 Lynx 5.10.7 X-ray interferometry 5.10.8 eASTROGAM and Compair 6 From raw data to scientific products: images, light curves and spectra [Giommi, Grandi, Pollock, Torresi] 6.1 How to get raw data 6.1.1 Writing a successful proposal 6.1.2 Exploiting public archives 6.1.3 Open Universe 6.2 Building a clean event file 6.2.1 Data Calibration 6.2.2 Data Screening 6.3 Extracting Scientific Products 6.3.1 Images 6.3.2 Light curves 6.3.3 Spectra 7 Statistics [Pollock, Bulgarelli] 7.1 Basic concepts 7.2 Probability distribution 7.3 Chi2 statistics 7.4 Cash statistics 7.5 F-test 7.6 Likelihood function 7.7 Wilks’s Theorem and Test statistic 7.8 Maximimum likelihood estimation and test statistics for gamma-ray data analysis 8 Data analysis (tutorials in the appendices) [Guainazzi, Pollock, …] 8.1 Spatial study: exploring a sky image 8.1.1 Is the source there? 8.1.2 Is the source extended? 8.1.3 Multiwavelength approach to identify different x-ray emitting regions 8.2 Temporal Study: bulding a light curve 8.2.1 Checking source flux variations 8.2.2 Variability time scale as measure of the x-ray source extension 8.2.3 Temporal domain analysis 8.2.4 Cross-correlation and time lags 8.3 Spectral analysis 8.3.1 Selection of the source and background regions 8.3.2 Ancillary and response matrices 8.3.3 Model fitting 8.3.4 Parameter uncertainties 8.4 Likelihood analysis for gamma-ray data 8.4.1 Data selection 8.4.2 Model selection 8.4.3 Model fitting 8.4.4 Source detection and localization 8.4.5 Time-series analysis with Likelihood 9. How to put your data analysis and interpretation into a scientific paper Appendices A.1 Tutorial guide for X-ray data analysis [Mission(s) TBD] A.2 Tutorial guide for AGILE A.3 Tutorial guide for Fermi
PrefaceContents1. The High Energy Window1.1 Some fundamental concepts2. Emission processes in Active Galactic Nuclei [Bambi, Grandi, Torresi,...]2.1 Thermal processes:2.1.1 Optically thick and geometrically thin disk2.1.2 Hot corona: x-ray production by Thermal Comptonization2.1.3 X-ray reprocessing: iron line and Compton hump2.1.4 ADAF2.2 Non thermal Processes2.1 Synchrotron radiation2.2 Inverse Compton2.3 SSC2.4 Hadronic cascade3. AGN as a high energy laboratory [Grandi, Torresi,...]3.1 AGN: why do we study them?3.2 Spectral energy Distribution3.2.1 Radio quiet AGN3.2.1.1 Accretion disk and soft excess3.2.1.2 Iron line and reflection3.2.1.3 Warm absorber and winds3.2.2 Radio Loud AGN3.2.2.1 Core3.2.2.2 Jets on kpc scales3.2.2.3 Radio lobes3.3 Classification of AGN3.3.1 Optical classification3.3.2 Radio classification3.3.3 Doppler Boosting3.4 Radio Quiet - Radio Loud AGN3.4.1 Radio Loudness3.4.2 Tomography of an AGN3.5 Unification of accreting black holes through all mass scales4. How to detect X-rays and gamma-rays from space: optics and detectors [Bulgarelli,Fioretti]4.1 Matter and radiation interaction4.1.1 Photoelectric effect4.1.2 Compton effect4.1.3 Pair production4.2 Fundamental Concepts4.2.1 Quantum efficiency4.2.2 Effective Area4.2.3 Energy redistribution4.2.4 Sensitivity4.2.5 Spatial Resolution4.2.6 Angular Resolution4.3 Detectors4.3.1 Scintillator (including scintillators for gamma-ray astronomy)4.3.2 Microchannel Plate4.3.3 CdTe4.3.4 CZT4.3.5 CCD4.3.6 Spark chambers4.3.7 Silicon strip detectors4.3.8 Calorimeters4.4 Mirror and focussing of photons4.4.1 Collimated System4.4.2 Focussing System4.5 Monte Carlo Simulations of X-ray and Gamma-ray Telescope4.5.1 Toolkits and frameworks4.5.2 Space radiation environment4.5.3 Spacecraft and payload mass modeling4.5.4 Analysis pipeline for the residual background evaluation5 Past, present, and future X-ray and gamma-ray missions [Bulgarelli, Guainazzi,Pollock, ...]5.1 The discovery of astrophysical X-ray sources5.2 The initial surveys5.3 The first observatories5.3.1 Explorer-115.3.2 OSO-35.3.3 SAS-25.3.4 COS-B5.3.5 Einstein5.3.6 EXOSAT5.3.7 CGRO (A general introduction here to provide the big view: moredetails in 5.8.2 and 5.9.2)5.4 Imaging proportional counters5.4.1 The ROSAT PSPC5.4.2 The ROSAT All Sky Survey (RASS)5.4.3 The broad-band perspective5.4.3.1 BeppoSAX5.4.3.2 Astrosat5.4.3.3 HXMT5.4.4 High-resolution timing5.5 X-ray CCD astrophysics5.5.1 Spectroscopic imaging of thermal plasmas5.5.1.2 SNRs5.5.1.3 Galaxies5.5.1.4 Galaxy clusters5.5.2 Surveys and the XRB5.5.3 Serendipitous source catalogs5.5.3.1 The Chandra Source Catalog5.5.3.2 The XMM-Newton EPIC Source Catalog5.5.3.3 The XMM-Newton Slew Catalog5.5.3.4 The Swift XRT catalogs5.6 The path towards hard X-ray focusing5.6.1 The BeppoSAX/PDS5.6.2 Suzaku5.6.3 NuSTAR: the focusing revolution5.7 High-resolution spectroscopy5.7.1 Gratings versus calorimeters5.7.2 Diagnostics of intergalactic plasmas5.7.3 Where are the missing baryons?5.7.4 Accreting black holes5.8 Compton telescopes5.8.1 General principles5.8.2 CGRO/COMPTEL5.9 Pair-tracking telescopes5.9.1 General principles5.9.2 Early phase: SAS-II, COS-B, CGRO/EGRET [spark chamber +calorimeter + anticoincidence shield: SAS-II (1972, 20 MeV - 300 MeV),COS-B (1975-82, 30 MeV - 3 GeV), CGRO/EGRET (1991-2000, 20 MeV - 30GeV)]5.9.3 - Silicon Trackers: AGILE and Fermi [silicon-strip detectors +calorimeter + anticoincidence shield: AGILE/GRID (2007-now, 30 MeV - 50GeV) and Fermi/LAT (2008-now, 30 MeV - 300 GeV)]5.10 The Future5.10.1 eRosita5.10.2 XARM5.10.3 eXTP5.10.4 Einstein Probe5.10.5 Athena5.10.6 Lynx5.10.7 X-ray interferometry5.10.8 eASTROGAM and Compair6 From raw data to scientific products: images, light curves and spectra [Giommi, Grandi,Pollock, Torresi]6.1 How to get raw data6.1.1 Writing a successful proposal6.1.2 Exploiting public archives6.1.3 Open Universe6.2 Building a clean event file6.2.1 Data Calibration6.2.2 Data Screening6.3 Extracting Scientific Products6.3.1 Images6.3.2 Light curves6.3.3 Spectra7 Statistics [Pollock, Bulgarelli]7.1 Basic concepts7.2 Probability distribution7.3 Chi2 statistics7.4 Cash statistics7.5 F-test7.6 Likelihood function7.7 Wilks's Theorem and Test statistic7.8 Maximimum likelihood estimation and test statistics for gamma-ray dataanalysis8 Data analysis (tutorials in the appendices) [Guainazzi, Pollock, ...]8.1 Spatial study: exploring a sky image8.1.1 Is the source there?8.1.2 Is the source extended?8.1.3 Multiwavelength approach to identify different x-ray emitting regions8.2 Temporal Study: bulding a light curve8.2.1 Checking source flux variations8.2.2 Variability time scale as measure of the x-ray source extension8.2.3 Temporal domain analysis8.2.4 Cross-correlation and time lags8.3 Spectral analysis8.3.1 Selection of the source and background regions8.3.2 Ancillary and response matrices8.3.3 Model fitting8.3.4 Parameter uncertainties8.4 Likelihood analysis for gamma-ray data8.4.1 Data selection8.4.2 Model selection8.4.3 Model fitting8.4.4 Source detection and localization8.4.5 Time-series analysis with Likelihood9. How to put your data analysis and interpretation into a scientific paperAppendicesA.1 Tutorial guide for X-ray data analysis [Mission(s) TBD]A.2 Tutorial guide for AGILEA.3 Tutorial guide for Fermi
Preface Contents 1. The High Energy Window 1.1 Some fundamental concepts 2. Emission processes in Active Galactic Nuclei [Bambi, Grandi, Torresi,…] 2.1 Thermal processes: 2.1.1 Optically thick and geometrically thin disk 2.1.2 Hot corona: x-ray production by Thermal Comptonization 2.1.3 X-ray reprocessing: iron line and Compton hump 2.1.4 ADAF 2.2 Non thermal Processes 2.1 Synchrotron radiation 2.2 Inverse Compton 2.3 SSC 2.4 Hadronic cascade 3. AGN as a high energy laboratory [Grandi, Torresi,…] 3.1 AGN: why do we study them? 3.2 Spectral energy Distribution 3.2.1 Radio quiet AGN 3.2.1.1 Accretion disk and soft excess 3.2.1.2 Iron line and reflection 3.2.1.3 Warm absorber and winds 3.2.2 Radio Loud AGN 3.2.2.1 Core 3.2.2.2 Jets on kpc scales 3.2.2.3 Radio lobes 3.3 Classification of AGN 3.3.1 Optical classification 3.3.2 Radio classification 3.3.3 Doppler Boosting 3.4 Radio Quiet - Radio Loud AGN 3.4.1 Radio Loudness 3.4.2 Tomography of an AGN 3.5 Unification of accreting black holes through all mass scales 4. How to detect X-rays and gamma-rays from space: optics and detectors [Bulgarelli, Fioretti] 4.1 Matter and radiation interaction 4.1.1 Photoelectric effect 4.1.2 Compton effect 4.1.3 Pair production 4.2 Fundamental Concepts 4.2.1 Quantum efficiency 4.2.2 Effective Area 4.2.3 Energy redistribution 4.2.4 Sensitivity 4.2.5 Spatial Resolution 4.2.6 Angular Resolution 4.3 Detectors 4.3.1 Scintillator (including scintillators for gamma-ray astronomy) 4.3.2 Microchannel Plate 4.3.3 CdTe 4.3.4 CZT 4.3.5 CCD 4.3.6 Spark chambers 4.3.7 Silicon strip detectors 4.3.8 Calorimeters 4.4 Mirror and focussing of photons 4.4.1 Collimated System 4.4.2 Focussing System 4.5 Monte Carlo Simulations of X-ray and Gamma-ray Telescope 4.5.1 Toolkits and frameworks 4.5.2 Space radiation environment 4.5.3 Spacecraft and payload mass modeling 4.5.4 Analysis pipeline for the residual background evaluation 5 Past, present, and future X-ray and gamma-ray missions [Bulgarelli, Guainazzi, Pollock, …] 5.1 The discovery of astrophysical X-ray sources 5.2 The initial surveys 5.3 The first observatories 5.3.1 Explorer-11 5.3.2 OSO-3 5.3.3 SAS-2 5.3.4 COS-B 5.3.5 Einstein 5.3.6 EXOSAT 5.3.7 CGRO (A general introduction here to provide the big view: more details in 5.8.2 and 5.9.2) 5.4 Imaging proportional counters 5.4.1 The ROSAT PSPC 5.4.2 The ROSAT All Sky Survey (RASS) 5.4.3 The broad-band perspective 5.4.3.1 BeppoSAX 5.4.3.2 Astrosat 5.4.3.3 HXMT 5.4.4 High-resolution timing 5.5 X-ray CCD astrophysics 5.5.1 Spectroscopic imaging of thermal plasmas 5.5.1.2 SNRs 5.5.1.3 Galaxies 5.5.1.4 Galaxy clusters 5.5.2 Surveys and the XRB 5.5.3 Serendipitous source catalogs 5.5.3.1 The Chandra Source Catalog 5.5.3.2 The XMM-Newton EPIC Source Catalog 5.5.3.3 The XMM-Newton Slew Catalog 5.5.3.4 The Swift XRT catalogs 5.6 The path towards hard X-ray focusing 5.6.1 The BeppoSAX/PDS 5.6.2 Suzaku 5.6.3 NuSTAR: the focusing revolution 5.7 High-resolution spectroscopy 5.7.1 Gratings versus calorimeters 5.7.2 Diagnostics of intergalactic plasmas 5.7.3 Where are the missing baryons? 5.7.4 Accreting black holes 5.8 Compton telescopes 5.8.1 General principles 5.8.2 CGRO/COMPTEL 5.9 Pair-tracking telescopes 5.9.1 General principles 5.9.2 Early phase: SAS-II, COS-B, CGRO/EGRET [spark chamber + calorimeter + anticoincidence shield: SAS-II (1972, 20 MeV - 300 MeV), COS-B (1975-82, 30 MeV - 3 GeV), CGRO/EGRET (1991-2000, 20 MeV - 30 GeV)] 5.9.3 - Silicon Trackers: AGILE and Fermi [silicon-strip detectors + calorimeter + anticoincidence shield: AGILE/GRID (2007-now, 30 MeV - 50 GeV) and Fermi/LAT (2008-now, 30 MeV - 300 GeV)] 5.10 The Future 5.10.1 eRosita 5.10.2 XARM 5.10.3 eXTP 5.10.4 Einstein Probe 5.10.5 Athena 5.10.6 Lynx 5.10.7 X-ray interferometry 5.10.8 eASTROGAM and Compair 6 From raw data to scientific products: images, light curves and spectra [Giommi, Grandi, Pollock, Torresi] 6.1 How to get raw data 6.1.1 Writing a successful proposal 6.1.2 Exploiting public archives 6.1.3 Open Universe 6.2 Building a clean event file 6.2.1 Data Calibration 6.2.2 Data Screening 6.3 Extracting Scientific Products 6.3.1 Images 6.3.2 Light curves 6.3.3 Spectra 7 Statistics [Pollock, Bulgarelli] 7.1 Basic concepts 7.2 Probability distribution 7.3 Chi2 statistics 7.4 Cash statistics 7.5 F-test 7.6 Likelihood function 7.7 Wilks’s Theorem and Test statistic 7.8 Maximimum likelihood estimation and test statistics for gamma-ray data analysis 8 Data analysis (tutorials in the appendices) [Guainazzi, Pollock, …] 8.1 Spatial study: exploring a sky image 8.1.1 Is the source there? 8.1.2 Is the source extended? 8.1.3 Multiwavelength approach to identify different x-ray emitting regions 8.2 Temporal Study: bulding a light curve 8.2.1 Checking source flux variations 8.2.2 Variability time scale as measure of the x-ray source extension 8.2.3 Temporal domain analysis 8.2.4 Cross-correlation and time lags 8.3 Spectral analysis 8.3.1 Selection of the source and background regions 8.3.2 Ancillary and response matrices 8.3.3 Model fitting 8.3.4 Parameter uncertainties 8.4 Likelihood analysis for gamma-ray data 8.4.1 Data selection 8.4.2 Model selection 8.4.3 Model fitting 8.4.4 Source detection and localization 8.4.5 Time-series analysis with Likelihood 9. How to put your data analysis and interpretation into a scientific paper Appendices A.1 Tutorial guide for X-ray data analysis [Mission(s) TBD] A.2 Tutorial guide for AGILE A.3 Tutorial guide for Fermi
PrefaceContents1. The High Energy Window1.1 Some fundamental concepts2. Emission processes in Active Galactic Nuclei [Bambi, Grandi, Torresi,...]2.1 Thermal processes:2.1.1 Optically thick and geometrically thin disk2.1.2 Hot corona: x-ray production by Thermal Comptonization2.1.3 X-ray reprocessing: iron line and Compton hump2.1.4 ADAF2.2 Non thermal Processes2.1 Synchrotron radiation2.2 Inverse Compton2.3 SSC2.4 Hadronic cascade3. AGN as a high energy laboratory [Grandi, Torresi,...]3.1 AGN: why do we study them?3.2 Spectral energy Distribution3.2.1 Radio quiet AGN3.2.1.1 Accretion disk and soft excess3.2.1.2 Iron line and reflection3.2.1.3 Warm absorber and winds3.2.2 Radio Loud AGN3.2.2.1 Core3.2.2.2 Jets on kpc scales3.2.2.3 Radio lobes3.3 Classification of AGN3.3.1 Optical classification3.3.2 Radio classification3.3.3 Doppler Boosting3.4 Radio Quiet - Radio Loud AGN3.4.1 Radio Loudness3.4.2 Tomography of an AGN3.5 Unification of accreting black holes through all mass scales4. How to detect X-rays and gamma-rays from space: optics and detectors [Bulgarelli,Fioretti]4.1 Matter and radiation interaction4.1.1 Photoelectric effect4.1.2 Compton effect4.1.3 Pair production4.2 Fundamental Concepts4.2.1 Quantum efficiency4.2.2 Effective Area4.2.3 Energy redistribution4.2.4 Sensitivity4.2.5 Spatial Resolution4.2.6 Angular Resolution4.3 Detectors4.3.1 Scintillator (including scintillators for gamma-ray astronomy)4.3.2 Microchannel Plate4.3.3 CdTe4.3.4 CZT4.3.5 CCD4.3.6 Spark chambers4.3.7 Silicon strip detectors4.3.8 Calorimeters4.4 Mirror and focussing of photons4.4.1 Collimated System4.4.2 Focussing System4.5 Monte Carlo Simulations of X-ray and Gamma-ray Telescope4.5.1 Toolkits and frameworks4.5.2 Space radiation environment4.5.3 Spacecraft and payload mass modeling4.5.4 Analysis pipeline for the residual background evaluation5 Past, present, and future X-ray and gamma-ray missions [Bulgarelli, Guainazzi,Pollock, ...]5.1 The discovery of astrophysical X-ray sources5.2 The initial surveys5.3 The first observatories5.3.1 Explorer-115.3.2 OSO-35.3.3 SAS-25.3.4 COS-B5.3.5 Einstein5.3.6 EXOSAT5.3.7 CGRO (A general introduction here to provide the big view: moredetails in 5.8.2 and 5.9.2)5.4 Imaging proportional counters5.4.1 The ROSAT PSPC5.4.2 The ROSAT All Sky Survey (RASS)5.4.3 The broad-band perspective5.4.3.1 BeppoSAX5.4.3.2 Astrosat5.4.3.3 HXMT5.4.4 High-resolution timing5.5 X-ray CCD astrophysics5.5.1 Spectroscopic imaging of thermal plasmas5.5.1.2 SNRs5.5.1.3 Galaxies5.5.1.4 Galaxy clusters5.5.2 Surveys and the XRB5.5.3 Serendipitous source catalogs5.5.3.1 The Chandra Source Catalog5.5.3.2 The XMM-Newton EPIC Source Catalog5.5.3.3 The XMM-Newton Slew Catalog5.5.3.4 The Swift XRT catalogs5.6 The path towards hard X-ray focusing5.6.1 The BeppoSAX/PDS5.6.2 Suzaku5.6.3 NuSTAR: the focusing revolution5.7 High-resolution spectroscopy5.7.1 Gratings versus calorimeters5.7.2 Diagnostics of intergalactic plasmas5.7.3 Where are the missing baryons?5.7.4 Accreting black holes5.8 Compton telescopes5.8.1 General principles5.8.2 CGRO/COMPTEL5.9 Pair-tracking telescopes5.9.1 General principles5.9.2 Early phase: SAS-II, COS-B, CGRO/EGRET [spark chamber +calorimeter + anticoincidence shield: SAS-II (1972, 20 MeV - 300 MeV),COS-B (1975-82, 30 MeV - 3 GeV), CGRO/EGRET (1991-2000, 20 MeV - 30GeV)]5.9.3 - Silicon Trackers: AGILE and Fermi [silicon-strip detectors +calorimeter + anticoincidence shield: AGILE/GRID (2007-now, 30 MeV - 50GeV) and Fermi/LAT (2008-now, 30 MeV - 300 GeV)]5.10 The Future5.10.1 eRosita5.10.2 XARM5.10.3 eXTP5.10.4 Einstein Probe5.10.5 Athena5.10.6 Lynx5.10.7 X-ray interferometry5.10.8 eASTROGAM and Compair6 From raw data to scientific products: images, light curves and spectra [Giommi, Grandi,Pollock, Torresi]6.1 How to get raw data6.1.1 Writing a successful proposal6.1.2 Exploiting public archives6.1.3 Open Universe6.2 Building a clean event file6.2.1 Data Calibration6.2.2 Data Screening6.3 Extracting Scientific Products6.3.1 Images6.3.2 Light curves6.3.3 Spectra7 Statistics [Pollock, Bulgarelli]7.1 Basic concepts7.2 Probability distribution7.3 Chi2 statistics7.4 Cash statistics7.5 F-test7.6 Likelihood function7.7 Wilks's Theorem and Test statistic7.8 Maximimum likelihood estimation and test statistics for gamma-ray dataanalysis8 Data analysis (tutorials in the appendices) [Guainazzi, Pollock, ...]8.1 Spatial study: exploring a sky image8.1.1 Is the source there?8.1.2 Is the source extended?8.1.3 Multiwavelength approach to identify different x-ray emitting regions8.2 Temporal Study: bulding a light curve8.2.1 Checking source flux variations8.2.2 Variability time scale as measure of the x-ray source extension8.2.3 Temporal domain analysis8.2.4 Cross-correlation and time lags8.3 Spectral analysis8.3.1 Selection of the source and background regions8.3.2 Ancillary and response matrices8.3.3 Model fitting8.3.4 Parameter uncertainties8.4 Likelihood analysis for gamma-ray data8.4.1 Data selection8.4.2 Model selection8.4.3 Model fitting8.4.4 Source detection and localization8.4.5 Time-series analysis with Likelihood9. How to put your data analysis and interpretation into a scientific paperAppendicesA.1 Tutorial guide for X-ray data analysis [Mission(s) TBD]A.2 Tutorial guide for AGILEA.3 Tutorial guide for Fermi