Optical 3D-Spectroscopy for Astronomy

Inbunden, Engelska, 2017

Av Roland Bacon, Guy Monnet, Observatoire de Lyon) Bacon, Roland (CNRS

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Over the last 50 years, a variety of techniques have been developed to add a third dimension to regular imaging, with an extended spectrum associated to every imaging pixel. Dubbed 3D spectroscopy from its data format, it is now widely used in the astrophysical domain, but also inter alia for atmospheric sciences and remote sensing purposes.This is the first book to comprehensively tackle these new capabilities. It starts with the fundamentals of spectroscopic instruments, in particular their potentials and limits. It then reviews the various known 3D techniques, with particular emphasis on pinpointing their different `ecological? niches. Putative users are finally led through the whole observing process, from observation planning to the extensive ? and crucial - phase of data reduction.This book overall goal is to give the non-specialist enough hands-on knowledge to learn fast how to properly use and produce meaningful data when using such a 3D capability.

Produktinformation

Utgivningsdatum2017-04-12
Mått173 x 249 x 20 mm
Vikt703 g
FormatInbunden
SpråkEngelska
Antal sidor296
FörlagWiley-VCH Verlag GmbH
ISBN9783527412020

Tillhör följande kategorier

Astronomi inom Naturvetenskap och teknik
Fysik inom Naturvetenskap och teknik

Roland Bacon is astrophysicist, directeur de recherche au CNRS and former director of the Lyon Observatory (1994-2004). He has played a pioneering role in the development of integral field spectroscopy as leader of 4 major and innovative instruments for ground based telescope: TIGER and OASIS at the 3.6m Canada France Hawaii telescope, SAURON at the 4.2m William Herschel telescope and MUSE at the 8m ESO Very Large Telescope. His main research field is extragalactic astronomy. He is the owner since 2014 of an advanced grant from the European Research Commission. Guy Monnet is an astrophysicist, with 50-year experience of developing astronomical instrumentation, on the ground and in space, mostly with a 3D spectroscopic flavor. Successively, he was director of the Marseilles Observatory, Lyon Observatory and the Canada France Hawaii Telescope Corporation. He then took the position of Head of Instrumentation at the European Southern Observatory (1995-2009) and the Australian Astrophysical Observatory (2010-2011). His main scientific domain is the dynamics of stars and ionized gas in galaxies.

Foreword xiAcknowledgments xiiiThe Emergence of 3D Spectroscopy in Astronomy 1Scientific Rationale 13D History 43D Technology 9Part I 3D Instrumentation 111 The Spectroscopic Toolbox 131.1 Introduction 131.1.1 Geometrical Optics # 101 131.1.2 Etendue Conservation 151.2 Basic Spectroscopic Principles 181.2.1 The Spectroscopic Case 181.3 Scanning Filters 201.3.1 Introduction 201.3.2 Interference Filters 221.3.3 Fabry–Pérot Filter 241.4 Dispersers 251.4.1 Prisms 251.4.2 Grating Principle 271.4.3 The Grating Spectrograph 281.4.4 Grating Species 291.4.5 Grating Etendue 301.4.6 Conclusion 311.5 2D Detectors 311.5.1 Introduction 311.5.2 The Photographic Plate 321.5.3 2D Optical Detectors 321.5.4 2D Infrared Arrays 351.5.5 Conclusion 351.6 Optics and Coatings 361.6.1 Introduction to Optics 361.6.2 Optical Computation 371.6.3 Optical Fabrication 401.6.4 Anti-Reflection Coatings 421.6.5 High Reflectivity Coatings 431.6.6 Conclusions 441.7 Mechanics, Cryogenics and Electronics 451.7.1 Mechanical Design 451.7.2 Alignments 481.7.3 Cryogenics 481.7.4 Electronics and Control System 491.8 Management, Timeline, and Cost 501.9 Conclusion 522 Multiobject Spectroscopy 612.1 Introduction 612.1.1 MOS History: The Pioneers 612.1.2 MOS History: The Digital Age 622.1.3 MOS Flavors 622.2 Slitless Based Multi-Object Spectroscopy 622.2.1 Slitless Spectroscopy Concept 622.2.2 Slitless Spectroscopic Systems 642.3 Multislit-Based Multiobject Spectroscopy 642.3.1 Multislit Concept 642.3.2 Multislit Holders 662.3.3 Multislit Systems 692.3.4 Multislit Instruments 702.4 Fiber-Based Multiobject Spectroscopy 702.4.1 Multifiber Concept 702.4.2 Positioning Systems 712.4.3 Fiber-Based Spectrograph 752.4.4 Fiber Systems Performance 752.4.5 Present Multifiber Facilities 762.4.6 Conclusion 773 Scanning Imaging Spectroscopy 813.1 Introduction 813.2 Scanning Long-Slit Spectroscopy 813.2.1 The Scanning Long-Slit Spectroscopy Concept 813.2.2 Astronomical Use 823.3 Scanning Fabry–Pérot Spectroscopy 833.3.1 Introduction 833.3.2 Fixed Fabry–Pérot Concept 833.3.3 Scanning Fabry–Pérot 853.4 Scanning Fourier Transform Spectroscopy 883.4.1 Fourier Transform Spectrometer 883.4.2 Fourier Transform Spectrograph 903.5 Conclusion: Comparing the Different Scanning Flavors 914 Integral Field Spectroscopy 954.1 Introduction 954.2 Lenslet-Based Integral Field Spectrometer 954.3 Fiber-Based Integral Field Spectrometer 1024.3.1 The Fiber-Based IFS Concept 1024.3.2 The Fiber-Based IFS Development 1034.3.3 Conclusion 1034.4 Slicer-Based Integral Field Spectrograph 1044.4.1 Introduction 1044.4.2 Integral Field Spectroscopy from Space 1074.5 Conclusion: Comparing the Different IFS Flavors 1085 Recent Trends in Integral Field Spectroscopy 1155.1 Introduction 1155.2 High-Contrast Integral Field Spectrometer 1155.2.1 Exoplanet Detection 1155.2.2 High-Contrast Integral Field Spectrometer 1165.3 Wide-Field Integral Field Spectroscopy 1175.3.1 The Rationale for Wide-Field Integral Field Spectroscopy 1175.3.2 Current Wide-Field Projects 1175.3.3 Wide-Field Systems 3D Format 1195.4 An Example: Autopsy of the MUSE Wide-Field Instrument 1205.4.1 MUSE Concept 1205.4.2 MUSE Approach 1205.4.3 MUSE Conclusions 1225.4.4 Validity of the Multi-instrument Approach 1235.5 Deployable Multiobject Integral Field Spectroscopy 1235.5.1 Concept 1235.5.2 The First Deployable Integral Field Units System 1245.5.3 Near Infra-Red Deployable Integral Field Units 1245.5.4 Deployable Multi-Integral Field Systems: Conclusion 1266 Comparing the Various 3D Techniques 1296.1 Introduction 1296.2 3D Spectroscopy Grasp Invariant Principle 1296.3 3-D Techniques Practical Differences 1306.3.1 Packing Efficiency 1306.3.2 Observational Efficiency 1316.4 A Tentative Rating 1337 Future Trends in 3D Spectroscopy 1377.1 3D Instrumentation for the ELTs 1377.2 Photonics-Based Spectrograph 1387.2.1 OH Suppression Filter 1387.2.2 Photonics Dispersers 1417.2.3 Photonics Fourier Transform Spectrometer 1417.2.4 Analysis 1427.3 Quest for the Grail: Toward 3D Detectors? 1447.3.1 Introduction 1447.3.2 Photon-Counting 3D Detectors 1447.3.3 Integrating 3D Detector 1457.4 Conclusion 1467.5 For Further Reading 146Part II Using 3D Spectroscopy 1518 Data Properties 1538.1 Introduction 1538.2 Data Sampling and Resolution 1538.2.1 Spatial Sampling and Resolution 1548.2.2 Spectral Sampling and Resolution 1558.3 Noise Properties 1589 Impact of Atmosphere 1679.1 Introduction 1679.2 Basic Seeing Principles 1689.2.1 What is Astronomical Seeing? 1689.2.2 Seeing Properties 1709.3 Seeing-Limited Observations 1729.3.1 Seeing Impact on 3D Instruments 1729.4 Adaptive Optics Corrected Observations 1739.4.1 The Need for Overcoming Atmospheric Turbulence 1739.4.2 Adaptive Optics Correction Principle 1739.4.3 Adaptive Optics Components 1769.4.4 Adaptive Optics: The Optical Domain Curse 1789.4.5 Addressing the Lack of Reference Stars 1799.4.6 Addressing the Small Field Limitation 1829.4.7 Large Field Partial AO Correction 1839.4.8 AO-Based Scanning Interferometers 1849.4.9 AO-Based Slit Spectrographs 1859.4.10 AO-Based Integral Field Spectrographs 1859.4.11 AO-Based Near-IR Multiobject Integral Field Spectrographs 1879.4.12 Deriving AO-Corrected Point-Spread Functions 1889.4.13 Conclusion 1889.4.14 For Further Reading 1899.5 Other Atmosphere Impacts 1899.5.1 Atmospheric Extinction 1899.5.2 Atmospheric Refraction 1899.5.3 Night Sky Emission 1919.6 Space-Based Observations 1929.6.1 The Case for Space-Based Observations 1929.6.2 Why all Telescopes are not Space Telescopes 1939.7 Conclusion 19410 Data Gathering 19910.1 Introduction 19910.2 Planning Observations 19910.3 Estimating Observing Time 20010.4 Observing Strategy 20410.5 At the Telescope 20610.6 Conclusion 20911 Data Reduction 21311.1 Introduction 21311.2 Basics 21411.3 Specific Cases 21611.3.1 Slitless Multiobject Spectrograph 21611.3.2 Scanning Fabry–Pérot Spectrograph 21611.3.3 Scanning Fourier Transform Spectrograph 21711.3.4 Getting Noise Variance Estimation 21711.3.5 Minimizing Systematics 21811.4 Data Reduction Example: The MUSE Scheme 21911.4.1 Detector Calibration 22111.4.2 Flat-Field Calibrations and Trace Mask 22211.4.3 Wavelength Calibrations 22411.4.4 Geometrical Calibration 22511.4.5 Basic Science Extraction and Pixel Tables 22611.4.6 Differential Atmospheric Correction 22611.4.7 Sky Subtraction 22811.4.8 Spectrophotometric and Astrometric Calibrations 22911.4.9 Data-Cube Creation 23211.4.10 Data Quality 23311.5 Conclusion 23612 Data Analysis 23712.1 Introduction 23712.2 Handling Data Cubes 23712.2.1 The Spectral View 23812.2.2 The Spatial View 23912.2.3 The 3D View 23912.3 Viewing Data Cubes 24012.4 Conclusion 24112.5 Further Reading 24313 Conclusions 24513.1 Conclusions 24513.2 General-Use Instruments 24513.3 Team-Use Instruments 25013.4 The Bumpy Road to Success 251References 253Index 269