James Webb telescope introduction presentation
 

James Webb telescope introduction presentation

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

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

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  • Please correct the time given in slide 55 for the JWST. The correct time should be 300 million years since the big bang or 13.4 billion years ago.
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James Webb telescope introduction presentation James Webb telescope introduction presentation Presentation Transcript

  • THE JAMES WEBB SPACE TELESCOPE A BRIEF INTRODUCTION
  • JAMES WEBB Webb was formerly known as the “Next Generation SpaceTelescope” (NGST); it was renamed in Sept 2002 after a former NASA administrator, James Webb.
  • WEBB IS AN INTERNATIONAL COLLABORATION National Aeronautics and Space Administration
  • WEBB IS AN INTERNATIONAL COLLABORATION + National Aeronautics and European Space Space Administration Agency
  • WEBB IS AN INTERNATIONAL COLLABORATION + + National Aeronautics and European Space Canadian Space Space Administration Agency Agency
  • WEBB IS AN INTERNATIONAL COLLABORATION + + National Aeronautics and European Space Canadian Space Space Administration Agency Agency Managing The Main Industrial Operates Webb Development Effort Partner After Launch
  • THE JAMES WEBB SPACE TELESCOPE
  • THE JAMES WEBB SPACE TELESCOPE Infrared
  • THE JAMES WEBB SPACE TELESCOPE Infrared 6.5 meter primary mirror
  • THE JAMES WEBB SPACE TELESCOPE Infrared Hubble’s primary mirror 6.5 meter primary mirror
  • THE JAMES WEBB SPACE TELESCOPE Infrared Hubble’s primary mirror 6.5 meter primary mirror 2018 launch date
  • HOW BIG IS WEBB? HUBBLE
  • HOW BIG IS WEBB? HUBBLE TRACTOR- TRAILER
  • HOW BIG IS WEBB? HUBBLE WEBB TRACTOR- TRAILER
  • HOW BIG IS WEBB? HUBBLE WEBB TRACTOR- BOEING 737 TRAILER
  • INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror
  • INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror Ultra-lightweight beryllium optics
  • INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror Ultra-lightweight beryllium optics Detection of extremely weak signals
  • INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror Ultra-lightweight beryllium optics Detection of extremely weak signals Microshutters
  • INNOVATIVE TECHNOLOGIES Folding, segmented primary mirror Ultra-lightweight beryllium optics Detection of extremely weak signals Microshutters Cryocooler
  • FOUR MAIN SCIENCE INSTRUMENTS ON WEBB 1 Near InfraRed Camera (NIRCam)
  • FOUR MAIN SCIENCE INSTRUMENTS ON WEBB 1 2 Near InfraRed Camera Near InfraRed Spectrograph (NIRCam) (NIRSpec)
  • FOUR MAIN SCIENCE INSTRUMENTS ON WEBB 1 2 3 Near InfraRed Camera Near InfraRed Spectrograph Mid-InfraRed Instrument (NIRCam) (NIRSpec) (MIRI)
  • FOUR MAIN SCIENCE INSTRUMENTS ON WEBB 1 2 3 4 Near InfraRed Camera Near InfraRed Spectrograph Mid-InfraRed Instrument Fine Guidance Sensor/ (NIRCam) (NIRSpec) (MIRI) Near InfraRed Imager & Slitless Spectrograph (FGS-NIRISS)
  • INTEGRATED SCIENCE INSTRUMENT MODULE (ISM)
  • INTEGRATED SCIENCE INSTRUMENT MODULE (ISM) The ISM contains the four instruments
  • INTEGRATED SCIENCE INSTRUMENT MODULE (ISM) The ISM contains the four instruments
  • INFRARED RANGE Webbs 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.
  • INFRARED RANGE Webbs 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 10-5 0.2 0.4 0.75 1,000 microns (µm)
  • INFRARED RANGE Webbs 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 10-5 0.2 0.4 0.75 1,000 microns (µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in 0.6 0.75 1.5 4 1,000 microns (µm)
  • INFRARED RANGE Webbs 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 10-5 0.2 0.4 0.75 1,000 microns (µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in 0.6 0.75 1.5 4 1,000 microns (µm) Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm
  • INFRARED RANGE FGS/NIRISS (0.8 to 5.0 µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in 0.6 0.75 1.5 4 1,000 microns (µm) Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm
  • 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 0.6 0.75 1.5 4 1,000 microns (µm) Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm
  • INFRARED RANGE NIRSpec & NIRCam (0.6 to 5 µm) FGS/NIRISS MIRI (0.8 to 5.0 µm) (5 to 28 µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in 0.6 0.75 1.5 4 1,000 microns (µm) Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm
  • INFRARED RANGENear IRReveals: • cooler red stars NIRSpec & NIRCam (dust is transparent) (0.6 to 5 µm) FGS/NIRISS MIRI (0.8 to 5.0 µm) (5 to 28 µm) Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in 0.6 0.75 1.5 4 1,000 microns (µm) Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm
  • INFRARED RANGENear IRReveals: • cooler red stars NIRSpec & NIRCam (dust is transparent) (0.6 to 5 µm)Mid IRReveals: FGS/NIRISS MIRI • planets, comets, and asteroids (0.8 to 5.0 µm) (5 to 28 µm) • dust warmed by starlight • protoplanetary disks Visible Light Near Infrared Mid Infrared Far Infrared Rays Wavelength in 0.6 0.75 1.5 4 1,000 microns (µm) Infrared Sensitivity of Webb’s Instruments 0.6 µm 28 µm
  • FOUR MAIN SCIENCE THEMES1 THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION
  • FOUR MAIN SCIENCE THEMES1 THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION 2 THE ASSEMBLY OF GALAXIES
  • FOUR MAIN SCIENCE THEMES1 THE END OF THE DARK AGES: FIRST LIGHT AND REIONIZATION 2 THE ASSEMBLY OF GALAXIES 3 THE BIRTH OF STARS AND PROTOPLANETARY SYSTEMS
  • FOUR MAIN SCIENCE THEMES1 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
  • THE LAUNCH
  • THE LAUNCH Arianespaces ELA-3 launch complex near Kourou, French Guiana
  • THE LAUNCH Arianespaces ELA-3 launch complex near Kourou, French Guiana
  • THE LAUNCH Arianespaces ELA-3 launch complex near Kourou, French Guiana
  • THE LAUNCH Arianespaces ELA-3 launch complex near Kourou, French Guiana
  • THE LAUNCH Arianespaces ELA-3 launch complex near Kourou, French Guiana
  • 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
  • WEBB’S ORBIT L4 • Webb must be very cold • Shielded from the heat of the Sun AND the Earth • Solution: L2 (Lagrange point) L2 L1L3 THE L2 LAGRANGE POINT 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
  • HOW FAR BACK IN TIME WILL WEBB SEE? BIG BANG 0 AGE OF THE UNIVERSE (billions of years)
  • 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)
  • HOW FAR BACK IN TIME WILL WEBB SEE? DARK AGES BIG BANG COSMIC MICROWAVE BACKGROUND FIRST STARS 0 .0004 .3 (~400,000 yrs) AGE OF THE UNIVERSE (billions of years)
  • HOW FAR BACK IN TIME WILL WEBB SEE? DARK AGES BIG BANG COSMIC MICROWAVE BACKGROUND FIRST STARS FIRST GALAXIES 0 .0004 .3 1 (~400,000 yrs) AGE OF THE UNIVERSE (billions of years)
  • HOW FAR BACK IN TIME WILL WEBB SEE? DARK AGES BIG BANG COSMIC MICROWAVE BACKGROUND FIRST STARS FIRST GALAXIES MODERN UNIVERSE 0 .0004 .3 1 13.7 (~400,000 yrs) AGE OF THE UNIVERSE (billions of years)
  • HOW FAR BACK IN TIME WILL WEBB SEE? HST GOODS / DARK AGES CHANDRA DEPP FIELD BIG BANG COSMIC MICROWAVE BACKGROUND FIRST STARS FIRST GALAXIES MODERN UNIVERSE 0 .0004 .3 1 13.7 (~400,000 yrs) AGE OF THE UNIVERSE (billions of years)
  • HOW FAR BACK IN TIME WILL WEBB SEE? HST GOODS / DARK AGES CHANDRA DEPP FIELD BIG BANG JWST (300,000,000 billion yrs) COSMIC MICROWAVE BACKGROUND FIRST STARS FIRST GALAXIES MODERN UNIVERSE 0 .0004 .3 1 13.7 (~400,000 yrs) AGE OF THE UNIVERSE (billions of years)
  • FOR MORE INFORMATION ABOUT THE JAMES WEBB SPACE TELESCOPE HTTP://WWW.JWST.NASA.GOV/INDEX.HTML
  • www.stinsondesign.com@stinsondesign1.888.960.9851info@stinsondesign.com