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JWST Science Requirements Document

JWST-RQMT-002558 Revision

James Webb Space Telescope Project

Science Requirements Document

December 3, 2004
JWST GSFC CMO
March 11, 2005

RELEASED

Goddard Space Flight Center Greenbelt, Maryland
National Aeronautics and Space Administration

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JWST Science Requirements Document

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CM FOREWORD

This document is a James Webb Space Telescope (JWST) Project Configuration Management (CM)-controlled document. Changes to this document require prior approval of the JWST Project Manager. Proposed changes shall be submitted to the JWST CM Office (CMO), along with supportive material justifying the proposed change. Changes to this document will be made by complete revision. Questions or comments concerning this document should be addressed to: JWST Configuration Manager JWST Configuration Management Office Mail Stop 443 Goddard Space Flight Center Greenbelt, Maryland 20771

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JWST Science Requirements Document
Signature Page Prepared by: Original signed by Dr. John Mather JWST Senior Project Scientist NASA/GSFC 685 __3/8/2005__ Date

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Approved by:

Original signed by Phil Sabelhaus JWST Project Manager NASA/GSFC 443

__3/8/2005__ Date

Concurred by:

Original signed by __3/11/2005__ Eric Smith Date JWST Program Scientist Universe Division, Science Mission Directorate NASA Headquarters

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JWST Science Requirements Document
JAMES WEBB SPACE TELESCOPE PROJECT DOCUMENT CHANGE RECORD
REV LEVEL DESCRIPTION OF CHANGE

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Sheet: 1 of 1

APPROVED BY

DATE APPROVED

Initial

Release per JWST-CCR-000209

J. Decker

2/18/2005

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JWST Science Requirements Document
List of TBDs/TBRs
Item No. 1 Location Section 8.18 Summary SR-31, When requested the Observatory shall track targets which exhibit any angular velocity in the range of 30 mas/s over a total motion 30 arcsec with respect to the guide star (TBR). SR-22, Add to ISIM (TBD) SR-40, Add to ISIM (TBD) SR-23, Add to ISIM (TBD)

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Ind./Org. P. Sabelhaus/GSFC

Due Date 5/31/2005

2 3 4

Appendix B Appendix B Appendix B

Pam Sullivan/GSFC Pam Sullivan/GSFC Pam Sullivan/GSFC

5/9/2005 5/9/2005 5/9/2005

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JWST Science Requirements Document TABLE OF CONTENTS Section 1.0 2.0

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Page

PURPOSE AND SCOPE ............................................................................................... 1-1 SCIENTIFIC INTRODUCTION ................................................................................. 2-1 2.1 The End of the Dark Ages: First Light and Reionization .................................... 2-1 2.2 The Assembly of Galaxies ................................................................................... 2-2 2.3 The Birth of Stars and Protoplanetary Systems ................................................... 2-3 2.4 Planetary Systems and the Origins of Life .......................................................... 2-3 THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION.......... 3-1 3.1 Impact on Science ................................................................................................ 3-1 3.1.1 General Understanding ............................................................................ 3-3 3.1.2 Major Open Questions ............................................................................. 3-4 3.1.3 Specific Objectives .................................................................................. 3-5 3.2 Previous Investigations ........................................................................................ 3-6 3.2.1 Observational Foundation ........................................................................ 3-6 3.2.2 Theoretical Predictions ............................................................................ 3-9 3.3 Measurements Required from JWST ................................................................. 3-11 3.3.1 Detection of First Luminous Objects at Very High Redshifts ............... 3-11 3.3.2 Establishing when Reionization Occurred and Identifying the Reionizers3-13 3.4 Summary ............................................................................................................ 3-16 THE ASSEMBLY OF GALAXIES.............................................................................. 4-1 4.1 Impact on Science ................................................................................................ 4-1 4.2 Previous Investigations ........................................................................................ 4-2 4.3 Measurements required from JWST .................................................................... 4-4 4.3.1 Where were Stars in the Hubble Sequence Galaxies Formed, When did Luminous Quiescent Galaxies Appear, and How does this Process Depend on the Environment? ................................................................................ 4-4 4.3.2 Where and When are the Heavy Elements Produced and to What Extent do Galaxies Exchange Material with the Intergalactic Medium? ............ 4-6 4.3.3 When and How are the Global Scaling Relations for Galaxies Established?4-7 4.3.4 Do Luminous Galaxies Form through the Hierarchical Assembly of Dark Matter Halos? ........................................................................................... 4-8 4.3.5 What are the Redshifts and Power Sources of the High Redshift Ultra Luminous Infrared Galaxies? ................................................................... 4-9 4.3.6 What is the Relation Between the Evolution of Galaxies and the Growth and Development of Black Holes in Their Nuclei? ............................... 4-10 4.4 Summary ............................................................................................................ 4-11 THE BIRTH OF STARS AND PROTOPLANETARY SYSTEMS ......................... 5-1 5.1 How do Protostellar Clouds Collapse? ................................................................ 5-2 5.1.1 Scientific Rationale .................................................................................. 5-2 5.1.2 Key JWST Observations .......................................................................... 5-5

3.0

4.0

5.0

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JWST Science Requirements Document 5.2

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6.0

7.0

What is The Early Evolution of Protostars? ........................................................ 5-6 5.2.1 Scientific Rationale .................................................................................. 5-6 5.2.2 Key JWST Observations .......................................................................... 5-8 5.3 How do massive stars form and affect their Environment? ................................. 5-8 5.3.1 Scientific Rationale .................................................................................. 5-8 5.3.2 Key JWST Observations ........................................................................ 5-10 5.4 What is the Initial Mass Function at sub-stellar Masses? .................................. 5-12 5.4.1 Scientific Rationale ................................................................................ 5-12 5.4.2 Key JWST Observations ........................................................................ 5-14 5.5 How do Protoplanetary Systems form? ............................................................. 5-16 5.5.1 Scientific Rationale ................................................................................ 5-16 5.5.2 Key JWST Observations ........................................................................ 5-18 5.6 What are the life cycles of gas and dust? ........................................................... 5-18 5.6.1 Scientific Rationale ................................................................................ 5-18 5.6.2 Key JWST Observations ........................................................................ 5-20 5.7 Summary ............................................................................................................ 5-22 PLANETARY SYSTEMS AND THE ORIGINS OF LIFE....................................... 6-1 6.1 Origins of Planetary Systems ............................................................................... 6-1 6.1.1 Questions.................................................................................................. 6-1 6.1.2 Observations ............................................................................................ 6-4 6.1.3 Observatory Capabilities........................................................................ 6-11 6.2 Early Evolution of Planetary Systems ............................................................... 6-12 6.2.1 Questions................................................................................................ 6-12 6.2.2 Observations .......................................................................................... 6-13 6.2.3 Observatory Capabilities........................................................................ 6-15 6.3 Transition to Life ............................................................................................... 6-16 6.3.1 Questions................................................................................................ 6-16 6.3.2 Observations .......................................................................................... 6-17 6.4 Summary ............................................................................................................ 6-18 REQUIREMENTS RATIONALE ............................................................................... 7-1 7.1 Wavelength range ................................................................................................ 7-1 7.2 Imaging and Coronagraphy.................................................................................. 7-1 7.3 Spectroscopy ........................................................................................................ 7-2 7.4 Near-Infrared Camera .......................................................................................... 7-2 7.5 Near-Infrared Spectrograph ................................................................................. 7-2 7.6 Mid-Infrared Instrument ...................................................................................... 7-2 7.7 Tunable Filters ..................................................................................................... 7-3 7.8 Minimum Collecting Area ................................................................................... 7-3 7.9 Image Quality....................................................................................................... 7-3 7.9.1 Strehl Ratio .............................................................................................. 7-3 7.9.2 Encircled Energy...................................................................................... 7-3 7.9.3 Point-Spread Function Symmetry ............................................................ 7-4 7.9.4 Point-Spread Function Stability ............................................................... 7-4 7.10 Sensitivity ............................................................................................................ 7-4

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JWST Science Requirements Document 7.11

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8.0

Stray light ............................................................................................................. 7-5 7.11.1 Diffuse Stray Light .................................................................................. 7-5 7.11.2 Local Stray Light and Dynamic Range .................................................... 7-5 7.12 Long Exposures ................................................................................................... 7-6 7.13 Photometric Accuracy and Calibration ................................................................ 7-6 7.14 Field of View ....................................................................................................... 7-7 7.15 Angular Resolution .............................................................................................. 7-7 7.16 Pointing Accuracy................................................................................................ 7-7 7.17 Field of Regard .................................................................................................... 7-8 7.18 Moving Object Tracking ...................................................................................... 7-8 7.19 Mission Lifetime .................................................................................................. 7-9 7.20 Observing Efficiency ........................................................................................... 7-9 7.21 Data Rate.............................................................................................................. 7-9 7.22 Targets of Opportunity......................................................................................... 7-9 7.23 Public Access ..................................................................................................... 7-10 SCIENCE REQUIREMENTS ...................................................................................... 8-1 8.1 Wavelength Range ............................................................................................... 8-2 8.2 Imaging and Coronagraphy.................................................................................. 8-2 8.3 Spectroscopy ........................................................................................................ 8-2 8.4 Near-Infrared Camera .......................................................................................... 8-3 8.5 Near-Infrared Spectrograph ................................................................................. 8-3 8.6 Mid-Infrared Instrument ...................................................................................... 8-3 8.7 Medium and Narrow-band Imaging..................................................................... 8-3 8.8 Primary Mirror Area ............................................................................................ 8-3 8.9 Image Quality....................................................................................................... 8-4 8.9.1 Strehl Ratio .............................................................................................. 8-4 8.9.2 Encircled Energy...................................................................................... 8-4 8.9.3 Point Spread Function Symmetry ............................................................ 8-4 8.9.4 Point Spread Function Stability ............................................................... 8-4 8.10 Sensitivity ............................................................................................................ 8-4 8.11 Stray Light ........................................................................................................... 8-5 8.11.1 Diffuse Stray Light .................................................................................. 8-5 8.11.2 Local Stray Light ..................................................................................... 8-5 8.12 Long Exposures ................................................................................................... 8-5 8.13 Photometric Accuracy and Calibration ................................................................ 8-6 8.14 Field of View ....................................................................................................... 8-6 8.15 Angular Resolution .............................................................................................. 8-6 8.16 Pointing Accuracy................................................................................................ 8-6 8.17 Field of Regard .................................................................................................... 8-6 8.18 Moving Object Tracking ...................................................................................... 8-7 8.19 Mission Lifetime .................................................................................................. 8-7 8.20 Observing Efficiency ........................................................................................... 8-7 8.21 Data Rate.............................................................................................................. 8-7 8.22 Targets of Opportunity......................................................................................... 8-7

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JWST Science Requirements Document 8.23

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Public Access ....................................................................................................... 8-8

APPENDIX A: ABBREVIATIONS AND ACRONYMS ..................................................... A-1 APPENDIX B: SCIENCE TO MISSION REQUIREMENT TRACEABILITY SUMMARY ................................................................................................................................B-1

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JWST Science Requirements Document FIGURES Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure Figure 3-1. 3-2. 3-3. 3-4. 4-1. 4-2. 4-3. 5-1. 5-2. 5-3. 5-4. 5-5. 5-6. 5-7. 5-8. 6-1. 6-2. 6-3. 6-4. 6-5. 6-6. 6-7. 6-8. 6-9.

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Page Schematic view of cosmic history............................................................................ 3-2 Cumulative galaxy counts for z ~ 6 ......................................................................... 3-4 The Hubble Ultra Deep Field ................................................................................... 3-8 SEDs of Type II Supernovae at Maximum Light .................................................. 3-13 Analysis of HST Images .......................................................................................... 4-5 Spectrum of a galaxy at z~0.5 ................................................................................... 4-7 ISO Circinus Spectrum .......................................................................................... 4-10 How a Single, Isolated, Low-Mass Star and its Planetary System are Formed ...... 5-2 The Low-Mass Dark Cloud Barnard 68 ................................................................... 5-4 Azimuthally Averaged Radial Dust Column Density Profile for B68..................... 5-5 The Spectral Energy Distribution of the Prototypical Class 0 Protostar .................. 5-7 The M 16 Elephant Trunks .................................................................................... 5-10 Color-Magnitude Diagram for the Orion Trapezium Cluster ................................ 5-13 Young Circumstellar Disks in Orion...................................................................... 5-17 Mid-Infrared Spectra of Young Stars and Circumstellar Disks ............................. 5-19 Comets and Circumstellar Disks .............................................................................. 6-3 Detectability of Extra-Solar Giant Planets and Brown Dwarfs ............................... 6-5 Spectra of the Closest T-dwarfs .............................................................................. 6-6 Detectability of a Jovian-sized Exoplanet ................................................................ 6-7 Guide to Spectral Features in Extrasolar Giant Planets ........................................... 6-8 Seeing the Effect of Planets on Dust Disks .............................................................. 6-9 Models and Observations of a Dusty Disk............................................................. 6-11 Simulated KBO Spectrum ...................................................................................... 6-14 Sensitivity of MIRI for KBOs ................................................................................ 6-15

TABLES Table Table Table Table Table 3-1. 3-2. 4-1. 4-2. JWST Measurements Required Capabilities JWST Measurements Required Capabilities for for for for the the the the End of the Dark Ages End of the Dark Ages Assembly of Galaxies Assembly of Galaxies Page Theme ................................... Theme ................................... Theme ................................... Theme .................................. 3-16 3-17 4-12 4-13

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JWST Science Requirements Document Table Table Table Table Table Table Table Table 5-1. 5-2. 5-3. 6-1. 6-2. 6-3. 8-1. 8-2.

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Predicted Fluxes for Sub-Stellar Objects ................................................................ 5-15 JWST Measurements for the Birth of Stars Theme................................................. 5-22 Required Capabilities for the Birth of Stars Theme ................................................ 5-23 Model Fluxes of Bound Giant Planets....................................................................... 6-4 JWST Measurements for the Planetary Systems Theme ......................................... 6-18 Required Capabilities for the Planetary Systems Theme ........................................ 6-19 Required Sensitivity Values ...................................................................................... 8-5 Required Calibration Accuracies ............................................................................... 8-6

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JWST Science Requirements Document 1.0 PURPOSE AND SCOPE

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The purpose of this document is to define the scientific objectives and requirements of the James Webb Space Telescope (JWST) Project. JWST will be a large, cold, infrared-optimized space telescope designed to enable fundamental breakthroughs in our understanding of the formation and evolution of galaxies, stars, and planetary systems. This document provides detail for the Level 1 requirements which form part of the JWST Program Plan controlled at the National Aeronautics and Space Administration (NASA) Headquarters. It was written by the JWST Science Working Group under the direction of the JWST Senior Project Scientist, and is controlled by the JWST Project. It provides the rationale for the requirements contained in the Mission Requirements Document (MRD). If there is a conflict between this document and the MRD, the MRD requirement prevails. This document takes precedence over the instrument Science Rationale and Analysis documents (SRAs) which are controlled by the instrument science teams. The Near-Infrared Camera (NIRCam) SRA is controlled by the NIRCam Investigation Definition Team. The Mid-Infrared Instrument (MIRI) SRA is controlled by the MIRI Science Team. The Fine Guidance SensorTunable Filter (FGS-TF) SRA is controlled by the Canadian Space Agency (CSA). The NearInfrared Spectrograph (NIRSpec) SRA is controlled by the European Space Agency (ESA). We base these requirements on current theoretical understanding, interpretation of Hubble Space Telescope (HST) observations, and results from studies using ground-based and other spacebased facilities. Many classes of targets for JWST have never been observed before, so the scientific requirements are necessarily derived from theoretical predictions and extrapolations from known objects. In these cases we outline the basis of the predictions and derive the needed observatory capabilities to verify them. At the time of writing, the Spitzer Space Telescope has recently been launched, and promises great advances in all of the scientific areas outlined in this document. We expect that results from Spitzer, additional results from HST, and other advances in theory and observation will further refine the observational plans for JWST. The science requirements in this document define the required measurement capabilities of the telescope, but they do not require that particular observations be made. A mission which provides these capabilities will support a wide variety of astrophysical investigations. JWST is a facility-class mission, and most of the observing time will be allocated to investigators from the international astronomical community through competitively selected proposals. This document supersedes previous editions developed by the Ad-Hoc Science Working Group (ASWG) and the Interim Science Working Group (ISWG). In particular, it supersedes the Design Reference Mission (DRM) document, spreadsheets, and computer programs, which were developed by the ASWG and ISWG as examples of observing programs. JWST is consistent with the scientific program for a "Large Infrared-Optimized Space Telescope", described in the report "HST and Beyond," (Dressler 1996), and the program for the "Next Generation Space Telescope", which was given top priority by the National Academy of Sciences survey "Astronomy and Astrophysics in the New Millennium" (McKee & Taylor, 2001). 1-1
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JWST Science Requirements Document 2.0 SCIENTIFIC INTRODUCTION

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The scientific objectives of the JWST fall into four themes: 1. The End of the Dark Ages: First Light and Reionization 2. The Assembly of Galaxies 3. The Birth of Stars and Protoplanetary Systems 4. Planetary Systems and the Origins of Life These themes require observations specified in the JWST Program Plan Mission Success Criteria (Level 1 Baseline Science Requirements), quoted here: "4.1.1.1 Measure the space density of galaxies to a 2 µm flux density limit of 1.0 x 10-34 W m-2 Hz-1 via imagery within the 0.6 to 27 µm spectral band to enable the determination of how this density varies as a function of their age and evolutionary state. 4.1.1.2 Measure the spectra of at least 2500 galaxies with spectral resolutions of approximately 100 (over 0.6 to 5 µm) and 1000 (over 1 to 5 µm) and to a 2 µm emission line flux limit of 5.2x10-22 W m-2 to enable determination of their redshift, metallicity, star formation rate, and ionization state of the intergalactic medium. 4.1.1.3 Measure the physical and chemical properties of young stellar objects, circumstellar debris disks, extra-solar giant planets, and Solar System objects via spectroscopy, and imagery within the 0.6 to 27 µm spectral band to enable determination of how planetary systems form and evolve." 2.1 THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION

Theory and observation have given us a simple picture of the early Universe. The Big Bang produced (in decreasing order of present mass-energy density): dark energy (the cosmic acceleration force), dark matter, hydrogen, helium, cosmic microwave and neutrino background radiation, and trace quantities of lithium, beryllium, and boron. As the Universe expanded and cooled, hydrogen molecules formed, enabling the formation of the first individual stars. The Universe has expanded by a factor of about 20 since that time, the mean density was about 8000 times greater than it is now, and the age was about 180 million years. According to theory, these first stars were 30 to 300 times as massive as the Sun and millions of times as bright, burning for only a few million years before meeting a violent end. Each one produced either a core-collapse supernova (type II) or a black hole. The supernovae enriched the surrounding gas with the chemical elements produced in their interiors, and future generations of stars contained these heavier elements. The black holes started to swallow gas and other stars to become mini-quasars, growing and merging to become the huge black holes now found at the centers of nearly all massive galaxies. The supernovae and the mini-quasars should be observable by the JWST. Both might also be sources of gamma ray bursts and gravity wave bursts that could be discovered by other observatories and then observed by JWST. 2-1
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JWST Science Requirements Document

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Some time after the appearance of the first sources of light, hydrogen in the intergalactic medium was reionized. Results from the Wilkinson Microwave Anisotropy Probe (WMAP) combined with data from the Sloan Digital Sky Survey show that this reionization occurred at two or more epochs, perhaps with a complex history. Although there are indications that galaxies produced the majority of the ultraviolet radiation which caused the reionization, the contribution of quasars could be significant. JWST must address several key questions: · · · What are the first galaxies? When and how did reionization occur? What sources caused reionization?

To find the first galaxies, JWST must make ultra-deep near-infrared surveys of the Universe, and follow-up with low-resolution spectroscopy and mid-infrared photometry. To study reionization, high resolution near-infrared spectroscopy is required. 2.2 THE ASSEMBLY OF GALAXIES

Galaxies are the basic building blocks of the Universe. Theory and observation show that galaxies are assembled through a process of the hierarchical merging of dark matter concentrations. Small objects formed first, and were drawn together to form larger ones. This dynamical build-up of massive systems is accompanied by chemical evolution, as the gas and dust within the galaxies are processed through successive generations of stars. The interaction of these luminous components with the invisible dark matter produces the beautiful appearance and diverse properties of present-day galaxies. This process is still occurring today, as the Magellanic Clouds fall into the Milky Way, and as the Andromeda Nebula heads toward the Milky Way for a future collision. Galaxies have been observed back to times about one billion years after the Big Bang. While most of these early galaxies are smaller and more