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The James Webb Space Telescope the First Light Machine Dr

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The James Webb Space Telescope the First Light Machine Dr the James Webb SPACE TELESCOPE THE FIRST LIGHT MACHINE Dr. H. Philip Stahl is the James Webb Space Presentation by Telescope Optical Telescope Element Mirror Optics Lead, Dr. H. Philip Stahl responsible for its primary, secondary and tertiary mirrors. Tuesday, March 12th He is a Senior Optical 8:00 pm Physicist at NASA Marshall Space Flight Center. 1200 EECS Bldg, U of M, North Campus Scheduled to begin its 10 year mission after 2018, the James Webb Space Telescope (JWST) will search for the first luminous objects of the Universe to help answer fun- damental questions about how the Universe came to look like it does today. At 6.5 meters in diameter, JWST will be the world’s largest space telescope. This talk reviews science objectives for JWST and how they drive the JWST architecture, e.g. aperture, wavelength range and operating temperature. Additionally, the talk provides an over- view of the JWST primary mirror technology development and fabrication status. 2/13/2013 James Webb Space Telescope (JWST) JWST Summary • Mission Objective – Study origin & evolution of galaxies, stars & planetary systems – Optimized for near infrared wavelength (0.6 –28 µm) – 5 year Mission Life (10 year Goal) • Organization – Mission Lead: Goddard Space Flight Center – International collaboration with ESA & CSA – Prime Contractor: Northrop Grumman Space Technology – Instruments: – Near Infrared Camera (NIRCam) – Univ. of Arizona – Near Infrared Spectrometer (NIRSpec) – ESA – Mid-Infrared Instrument (MIRI) – JPL/ESA – Fine Guidance Sensor (FGS) – CSA – Operations: Space Telescope Science Institute Today 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 Concept Development Design, Fabrication, Assembly and Test science operations Phase A Phase B Phase C/D Launch Phase E The First Light Machine Formulation ICR T-NAR PDR/NAR Authorization [i.e., PNAR] (Program Commitment) Formulation Implementation … Origins Theme’s Two Fundamental Questions JWST Science Themes First Light and Re-Ionization • How Did We Get Here? Big Bang • Are We Alone? Observe the birth and early development Identify the first bright of stars and the formation of planets. objects that formed in the early Universe,Study and the physical and chemical Proto-PlanetaryHH-30 follow the ionizationproperties of solar systems for the building blocks of …. history. M-16Star Formation Galaxies Life Determine how galaxies form Determine how galaxies and dark matter, including gas, stars, metals, overall morphology and active nuclei Galaxies Evolve evolved to the present day. Three Key Facts Why go to Space There are 3 key facts about JWST that enables it to Atmospheric Transmission drives the need to go to space. perform is Science Mission: Infrared (mid and far/sub-mm) Telescopes (also uv, x-ray, and gamma-ray) cannot see through the Atmosphere It is a Space Telescope 1 NGST 32m class JWST It is an Infrared Telescope DiscoveryDiscovery SpaceSpace 100 It has a Large Aperture HST 1 year 104 10 year Time to make an imaging survey (hr) an imaging survey Time to make 8m class Grnd-based SIRTF 106 1 10 Wavelength (µm) 1 2/13/2013 Infrared Light Why Infrared ? COLD Why do we need Large Apertures? Sensitivity Matters Aperture = Sensitivity 10 10 Photographic & electronic detection Telescopes alone JWST 8 10 HST CCDs Sensitivity 10 6 Improvement Photography over the Eye 10 4 GOODS CDFS – 13 orbits HUDF – 400 orbits 10 2 Short’s 21.5” Short’s eyepiece Huygens f ratios Slow Galileo Wilson100” Mount 200” Palomar Mount 6-m Soviet Rosse’s 72” Rosse’s Adapted from Cosmic 48” Herschell’s Discovery , M. Harwit 1600 1700 1800 1900 2000 JWST will be more Sensitive than Hubble or Spitzer How big is JWST? HUBBLE JWST SPITZER 0.8-meter 2.4-meter T ~ 5.5 K T ~ 270 K 6.5-meter 123” x 136” T ~ 40 K λ/D 1.6μm ~ 0.14” 312” x 312” 324” x 324” λ/D 5.6μm ~ 2.22” λ/D 24μm ~ 6.2” JWST 6X more sensitive 132” x 164” 114” x 84” with similar resolution λ/D 2μm ~ 0.06” λ/D 20μm ~ 0.64” JWST 44X more sensitive Wavelength Coverage 1 μm 10 μm 100 μm HST JWST Spitzer 2 2/13/2013 Full Scale JWST Mockup How JWST Works Integrated Science Cold Side: ~40K Instrument Module (ISIM) Primary Mirror JWST is folded and stowed for launch 5 Layer Sunshield Observatory is Secondary deployed after launch Solar Array Mirror Spacecraft Bus Sun Hot Side JWST Orbits the 2 nd Lagrange Point (L2) 239,000 miles (384,000km) 930,000 miles (1.5 million km) 21 st National Space Symposium, Colorado Springs, The Space Foundation Earth Moon L2 JWST Science Instruments JWST Requirements enable imagery and spectroscopy over the 0.6 – 29 micron spectrum Optical Telescope Element 25 sq meter Collecting Area 2 micrometer Diffraction Limit < 50K (~35K) Operating Temp Primary Mirror 6.6 meter diameter (tip to tip) < 25 kg/m 2 Areal Density 2 FGS < $6 M/m Areal Cost 18 Hex Segments in 2 Rings Low (0-5 cycles/aper) 4 nm rms Drop Leaf Wing Deployment CSF (5-35 cycles/aper) 18 nm rms Mid (35-65K Segments cycles/aper) 7 nm rms 1.315 meter Flat to Flat Diameter Micro-roughness <4 nm rms < 20 nm rms Surface Figure Error Fun Fact ––MirrorMirror Surface Tolerance Technology Development of Large Optical Systems MSFC isJWST the JWST Primary Mirror Segment Technology Development Lead for JWST Human Hair Approximate scale Diameter is 100,000 nm 6.5 M (typical) AMSD II – Be, technology selected for JWST PMSA Surface Figure Error < 20 nm (rms) PMSA The 18 Primary Mirror segments 3 2/13/2013 JWST Mirror Technology History Advantages of Beryllium ) 2 300 240 TRL-6 Testing Very High Specific Stiffness – Modulus/Mass Ratio 200 Saves Mass – Saves Money 100 Goodrich Mirror Ball Beryllium Areal Density(Kg/m Areal 30 Kodak ULE Mirror Mirror 60 15 High Conductivity & Below 100K, CTE is virtually zero. 2000 1980 1990 SBMD 2010 Thermal Stability JWST Requirement ProcessMirror Material/Technology improvements\ Risk Selection, Reduction September, 2003 • •Schedule Beryllium and chosen Tinsley for technicalstaffing identifiedreasons as SBMDAMSD –Phase 1996 1 – 1999 AMSDJWST(cryogenic risksPhase CTE, 2 – thermal 2000 conductance, issues with • 0.535 Vendors m diameter selected for • glass,Process •stress3 vendorsimprovements issues (Goodrich, with Be via noted) 6-Sigma Kodak, Study and •studies20 m ROC Sphere follow-onPrimeBall)* Contractor identified Schedule potential Selectionand Tinsley schedule staffing savings • EDU addedidentified• •BerylliumBall as (Beryllium) key as mirror riskJWST mitigation andrisks ITT/Kodak demonstration• (ULE)DownCryo Null deviceproposedselect Figured to(2003) 4 as mirror to options,along 19 nm with rms AMSD Phase 3 architectures•ProcessGoodrichCoating improvements Adheasion dropped from (coupon AMSD and .5 meter demonstrations) Based on lessons learned, JWST invested early in mirror technology to address lower areal densities and cryogenic operations Figure Change: 30-55K Operational Range Mirror Manufacturing Process Blank Fabrication Machining Beryllium ULE Glass Y Surface Figure Y X With Alignment X Vertex Y Compensation X Completed Mirror Blank 1 1 5 15.0 mm 5 . 0 0 m m HIP Vessel being loading into chamber Machining of Web Structure Machining of Optical Surface m Gravity m Gravity Vertex Polishing Mirror System Integration Y Residual with Y X 36 Zernikes X Removed Vertex 15.0 mm 1 1 5 5 . 0 0 m Gravity m m m Vertex Gravity Brush Wellman Axsys Technologies Batch #1 (Pathfinder) PM Segments PMSA #1 (EDU-A / A1) PMSA #2 (3 / B1) PMSA #3 (4 / C1) Batch #2 PM Segments PMSA #4 (5 / A2) PMSA #5 (6 / B2) PMSA #6 (7 / C2) 4 2/13/2013 Fun Facts ––MirrorMirror Manufacturing Mirror Processing at Tinsley Before After Finished Be Billet Mirror Segment Be dust which is recycled 250 kgs 21 kgs Over 90% of material is removed to make each mirror segment – want a little mirror with your Be dust? Tinsley Laboratory – Final Shipment Primary Mirror Segment Assembly at BATC MSFC Cryogenic Test Facility XRCF Cryo Test Remove Guide Tube Section, Add GSE Station Cryotest #6 Timeline Cycle 1 Cycle 2 350 Gate Valve Measurement Measurement Add Forward He Extension 300 293K 293K 293K Module 1 250 200 150 New XL Shrouds sections Temperature (K) 100 45K 45K 50 25K 0 Add GSE 11-Apr-11 25-Apr-11 9-May-11 23-May-11 6-Jun-11 Support System A5 Date • Survival • Cryo Deployment A4 B6 Temperature • Nominal Measurement • Hexapod Deformation Pose A1 • RoC Actuation Test • Set RoC • Hexapod Envelope Test • Nominal Measurement 5DOF A2 C3 • Pullout Current & Redundant • Hexapod Tilt Test Table - Upgrade Test (3 of 6 PMSAs) • Pullout Current & Redundant Test (3 of 6 East End Dome PMSAs) 5 2/13/2013 Flight Mirrors in XRCF Mirror Fabrication Status at L-3 SSG-Tinsley – July 11 ALL DONE & DELIVERED Spare Mirrors Flight Mirrors EDU B8 13.5 nm-rms SM#2 (A type) 5.9 nm-rms 14.9 nm-rms C6 C1 10.4 nm-rms 10.0 nm-rms B7 A1 B2 13.0 nm-rms 15.3 nm-rms 13.1 nm-rms C7 A6 A2 238 nm-rms 18.0 nm-rms 16.5 nm-rms TM 4.3 nm-rms C5 PMS’s C2 14.9 nm-rms 15.4 nm-rms B1 A5 A3 8.0 µm-rms 15.3 nm-rms 9.6 nm-rms B6 A4 B3 FSM 15.2 nm-rms 9.5 nm-rms 8.2 nm-rms 2.3 nm-rms SM#1 C4 C3 33 nm-rms 15.4 nm-rms 14.2 nm-rms B5 8.5 nm - rms SURFACE FIGURE ERROR Total PM Composite: 13.5 nm RMS Telescope PM Target: 21.2 nm RMS Gold Coated Mirror Assemblies Primary Mirror Backplane Pathfinder backplane (central section) is complete for test procedure verification at JSC EDU Flight Backplane under construction B7 C2 C1 B4 A3 B8B A6 A5 Mirrors ≥ 98% at 2 µm C6 SM2 C4C A2 A4 B5 A1 B3 C5 C3 B6 Observatory level testing occurs at JSC Chamber A JWST Launched on Ariane 5 Heavy Verification Test Activities in JSC Chamber-A Cryo Position Primary Mirror Focus Sweep Test JWST folded and stowed for launch Metrology Stability Test (inward facing in 5 m dia x 17 m tall fairing sources) French Guiana SM PG PG Launch from Kourou Launch Center AOS (French Guiana) to L2 PG PG PM Crosscheck Tests in JSC Chamber-A Pass-and-a- Pupil Alignment Test Rogue Path Test Half Test Primary Mirror End-to-End WFSC WFE Test Demonstration Chamber A: 37m tall, 20m diameter, 12m door LN2 shroud and GHe panels 6 2/13/2013 JWST vs.
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