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The James Webb telescope is the largest telescope ever built and should yield significant information for science.

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James Webb telescope introduction presentation


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    1. THE JAMES WEBB SPACE TELESCOPE A BRIEF INTRODUCTION

    2. JAMES WEBB Webb was formerly known as the “Next Generation Space Telescope” (NGST); it was renamed in Sept 2002 after a former NASA administrator, James Webb.

    3. WEBB IS AN INTERNATIONAL COLLABORATION National Aeronautics and Space Administration

    4. WEBB IS AN INTERNATIONAL COLLABORATION + National Aeronautics and Space Administration European Space Agency

    5. WEBB IS AN INTERNATIONAL COLLABORATION + + National Aeronautics and Space Administration European Space Agency Canadian Space Agency

    6. WEBB IS AN INTERNATIONAL COLLABORATION + + National Aeronautics and Space Administration European Space Agency Canadian Space Agency Managing The Development Effort Main Industrial Partner Operates Webb After Launch

    7. THE JAMES WEBB SPACE TELESCOPE

    8. THE JAMES WEBB SPACE TELESCOPE Infrared

    9. THE JAMES WEBB SPACE TELESCOPE Infrared 6.5 meter primary mirror

    10. THE JAMES WEBB SPACE TELESCOPE Infrared 6.5 meter primary mirror Hubble’s primary mirror

    11. THE JAMES WEBB SPACE TELESCOPE Infrared 6.5 meter primary mirror Hubble’s primary mirror 2018 launch date

    12. HOW BIG IS WEBB? HUBBLE

    13. HOW BIG IS WEBB? HUBBLE TRACTOR- TRAILER

    14. HOW BIG IS WEBB? WEBB HUBBLE TRACTOR- TRAILER

    15. HOW BIG IS WEBB? WEBB HUBBLE TRACTOR- TRAILER BOEING 737

    16. INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror

    17. INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror Ultra-lightweight beryllium optics

    18. INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror Ultra-lightweight beryllium optics Detection of extremely weak signals

    19. INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror Ultra-lightweight beryllium optics Detection of extremely weak signals Microshutters

    20. INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror Ultra-lightweight beryllium optics Detection of extremely weak signals Microshutters Cryocooler

    21. FOUR MAIN SCIENCE INSTRUMENTS ON WEBB 1 Near InfraRed Camera (NIRCam)

    22. FOUR MAIN SCIENCE INSTRUMENTS ON WEBB 2 1 Near InfraRed Camera Near InfraRed Spectrograph (NIRCam) (NIRSpec)

    23. FOUR MAIN SCIENCE INSTRUMENTS ON WEBB 2 1 3 Near InfraRed Camera Near InfraRed Spectrograph Mid-InfraRed Instrument (NIRCam) (NIRSpec) (MIRI)

    24. FOUR MAIN SCIENCE INSTRUMENTS ON WEBB 2 4 1 3 Near InfraRed Camera Near InfraRed Spectrograph Mid-InfraRed Instrument Fine Guidance Sensor/ (NIRCam) (NIRSpec) (MIRI) Near InfraRed Imager & Slitless Spectrograph (FGS-NIRISS)

    25. INTEGRATED SCIENCE INSTRUMENT MODULE (ISM)

    26. INTEGRATED SCIENCE INSTRUMENT MODULE (ISM) The ISM contains the four instruments

    27. INTEGRATED SCIENCE INSTRUMENT MODULE (ISM) The ISM contains the four instruments

    28. INFRARED RANGE Webb's instruments will be designed to work primarily in the infrared range of the electromagnetic spectrum, with some capability in the visible range. It will be sensitive to light from 0.6 (orange) to 28 micrometers (µm) in wavelength.

    29. INFRARED RANGE Webb's instruments will be designed to work primarily in the infrared range of the electromagnetic spectrum, with some capability in the visible range. It will be sensitive to light from 0.6 (orange) to 28 micrometers (µm) in wavelength. Gamma Rays X-Rays UV Rays Visible Light Infrared Microwave Radio waves Wavelength in microns (µm) 10-5 0.2 0.4 0.75 1,000

    30. INFRARED RANGE Webb's instruments will be designed to work primarily in the infrared range of the electromagnetic spectrum, with some capability in the visible range. It will be sensitive to light from 0.6 (orange) to 28 micrometers (µm) in wavelength. Gamma Rays X-Rays UV Rays Visible Light Infrared Microwave Radio waves Wavelength in microns (µm) 10-5 0.2 0.4 0.75 1,000 Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in microns (µm) 0.6 0.75 1.5 4 1,000

    31. INFRARED RANGE Webb's instruments will be designed to work primarily in the infrared range of the electromagnetic spectrum, with some capability in the visible range. It will be sensitive to light from 0.6 (orange) to 28 micrometers (µm) in wavelength. Gamma Rays X-Rays UV Rays Visible Light Infrared Microwave Radio waves Wavelength in microns (µm) 10-5 0.2 0.4 0.75 1,000 Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in microns (µm) 0.6 0.75 1.5 4 1,000 Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm

    32. INFRARED RANGE FGS/NIRISS (0.8 to 5.0 µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in microns (µm) 0.6 0.75 1.5 4 1,000 Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm

    33. INFRARED RANGE NIRSpec & NIRCam (0.6 to 5 µm) FGS/NIRISS (0.8 to 5.0 µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in microns (µm) 0.6 0.75 1.5 4 1,000 Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm

    34. INFRARED RANGE NIRSpec & NIRCam (0.6 to 5 µm) FGS/NIRISS (0.8 to 5.0 µm) MIRI (5 to 28 µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in microns (µm) 0.6 0.75 1.5 4 1,000 Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm

    35. INFRARED RANGE Near IR Reveals: •cooler red stars (dust is transparent) NIRSpec & NIRCam (0.6 to 5 µm) FGS/NIRISS (0.8 to 5.0 µm) MIRI (5 to 28 µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in microns (µm) 0.6 0.75 1.5 4 1,000 Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm

    36. INFRARED RANGE Near IR Reveals: •cooler red stars (dust is transparent) NIRSpec & NIRCam (0.6 to 5 µm) Mid IR FGS/NIRISS (0.8 to 5.0 µm) MIRI (5 to 28 µm) Reveals: •planets, comets, and asteroids •dust warmed by starlight •protoplanetary disks Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in microns (µm) 0.6 0.75 1.5 4 1,000 Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm

    37. FOUR MAIN SCIENCE THEMES THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION 1

    38. FOUR MAIN SCIENCE THEMES THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION THE ASSEMBLY OF GALAXIES 1 2

    39. FOUR MAIN SCIENCE THEMES THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION THE ASSEMBLY OF GALAXIES THE BIRTH OF STARS AND PROTOPLANETARY SYSTEMS 1 2 3

    40. FOUR MAIN SCIENCE THEMES THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION THE ASSEMBLY OF GALAXIES THE BIRTH OF STARS AND PROTOPLANETARY SYSTEMS PLANETARY SYSTEMS AND THE ORIGINS OF LIFE 1 2 3 4

    41. THE LAUNCH

    42. THE LAUNCH Arianespace's ELA-3 launch complex near Kourou, French Guiana

    43. THE LAUNCH Arianespace's ELA-3 launch complex near Kourou, French Guiana

    44. THE LAUNCH Arianespace's ELA-3 launch complex near Kourou, French Guiana

    45. THE LAUNCH Arianespace's ELA-3 launch complex near Kourou, French Guiana

    46. THE LAUNCH Arianespace's ELA-3 launch complex near Kourou, French Guiana

    47. WEBB’S ORBIT • Webb must be very cold • Shielded from the heat of the Sun AND the Earth • Solution: L2 (Lagrange point) L2 150 million km 1.5 million km

    48. WEBB’S ORBIT L4 • Webb must be very cold • Shielded from the heat of the Sun AND the Earth • Solution: L2 (Lagrange point) L2 L1 THE L2 LAGRANGE POINT L3 150 million km 1.5 million km Lagrange Points provide a stable configuration in which three bodies can orbit each other yet stay in the same position relative to each other. L5

    49. HOW FAR BACK IN TIME WILL WEBB SEE? BIG BANG 0 AGE OF THE UNIVERSE (billions of years)

    50. HOW FAR BACK IN TIME WILL WEBB SEE? BIG BANG COSMIC MICROWAVE BACKGROUND 0 .0004 (~400,000 yrs) AGE OF THE UNIVERSE (billions of years)