Hubble Fellows April 21, 2006Peter Stockman, STScI James Webb Space Telescope © David A. Hardy/

Hubble Fellows April 21, 2006 Phase A Phase B Phase C/DPhase E Concept DevelopmentDesign, Fabrication, Assembly and Test Formulation Authorization NARLaunch science operations... ICR (PNAR) T-NAR JWST Facts at a Glance 6.5 m primary µm (zodi limited to 10 µm) Launch ~ June 2013 L2 Operations General Observer/Legacy/GTO Programs (70%/10%(TBD)/20%) 5 year lifetime, 10 year goal (expendables) NASA/ESA/CSA collaboration (80%/15%/5%)

Hubble Fellows April 21, 2006Peter Stockman, STScI Science Philosophy Larger & colder primary to observe “first light” objects to z ~ 15 (1 nJy sensitivity) Take advantage of passive cooling to reduce telescope and instrument backgrounds to zodi or below (below 10µm) Maximize discovery space by extending into the MIR in imaging and spectroscopy but do not drive the mission by MIR requirements. SAT Report July ‘06

Hubble Fellows April 21, 2006Peter Stockman, STScI Discovery Space JWST should maintain a significant advantage over 30 m diameter ground-based telescopes above 1.7 µm. SAT Report July ‘06

Hubble Fellows April 21, 2006Peter Stockman, STScI Breadth of Science Four major themes –End of the “Dark Ages” & observing “First Light” objects –Assembly of Galaxies (1 < z < 7) –Birth of Stars and Protoplanetary Systems –Planetary Systems and the Origins of Life Studies in these areas are described in the Science Requirements Document as examples -- this science is not locked up by the GTOs. There are many other areas that JWST can make unique contributions -- see the SAR report on

Hubble Fellows April 21, 2006Peter Stockman, STScI End of the dark ages: first light and reionization What are the first galaxies? When did reionization occur? –Once or twice? What sources caused reionization? Patchy Absorption Redshift Wavelength Lyman Forest Absorption Black Gunn- Peterson trough z<z i z~z i z>z i Neutral IGM. Spitzer GOODS 20,000 s JWST GOODS 1,000 s

Hubble Fellows April 21, 2006Peter Stockman, STScI Near Infrared Camera PI: Marcia Rieke, University of Arizona Two 2.16’x2.16’ imaging fields. Each field is simultaneously observed in two bands: – µm (Nyquist sampled at 2 µm, 0.03” pixels) – µm (Nyquist sampled at 4 µm) 8 intermediate and 8 broad bands: photo z’s to 4% Coronagraphs at 2 and 4 µm Wavefront sensing optics

Hubble Fellows April 21, 2006Peter Stockman, STScI The Assembly of Galaxies Where and when did the Hubble Sequence form? How did the heavy elements form? Can we test hierarchical formation and global scaling relations? What about ULIRGs and AGN? Galaxies in GOODS Field Wide-area imaging survey R=1000 spectra of 1000s of galaxies at 1 < z < 6 Targeted observations of ULIRGs and AGN

Hubble Fellows April 21, 2006Peter Stockman, STScI Near Infrared Spectrograph (NIRSpec) ESA Contribution: PI: Peter Jakobsen Multi-Shutter Array (developed by GSFC) –3.4’ x 3.4’ field with 0.22” x 0.4” addressable apertures –R ~ 100, 1000, 3000 –Integral Field Unit (0.1” slits, 3” x 3”) –Fixed slits in center for high contrast

Hubble Fellows April 21, 2006Peter Stockman, STScI Birth of stars and protoplanetary systems How do clouds collapse? How does environment affect star-formation? –Vice-versa? What is the low-mass IMF? Imaging of molecular clouds Survey “elephant trunks” Survey star-forming clusters Deeply embedded protostar Agglomeration & planetesimalsMature planetary system Circumstellar disk The Eagle Nebula as seen by HST The Eagle Nebula as seen in the infrared

Hubble Fellows April 21, 2006Peter Stockman, STScI Planetary systems and the origins of life How do planets form? How are circumstellar disks like our Solar System? How are habitable zones established? Simulated JWST image Fomalhaut at 24 microns Extra-solar giant planets –Coronagraphy Spectra of circumstellar disks, comets and KBOs Spectra of icy bodies in outer Solar System Titan Malfait et al 1998 Spitzer image

Hubble Fellows April 21, 2006Peter Stockman, STScI Mid Infrared Instrument (MIRI) European/NASA collaboration –Gillian Wright (European Lead Scientist) –George Rieke (US Lead Scientist) 5-27 µm (1K x 1K Si:As) –Nyquist sampled imaging at 7 µm, 1.4’ x 1.2’ field –Integral Field Spectroscopy (4 bands simultaneously, 3.7” - 7.7” fields, R~ 3000 –Low resolution spectroscopy, R~100, 5-10µm –Simple and phase-shifted coronagraphy MIRI

Hubble Fellows April 21, 2006Peter Stockman, STScI How are circumstellar disks like our Solar System? Here is an illustration of what MIRI might find within the very young core in Ophiuchus, VLA 1623 artist’s concept of protostellar disk from T. Greene, Am. Scientist approximate field for NIRSpec & MIRI integral field spectroscopy

Hubble Fellows April 21, 2006Peter Stockman, STScI Progress All 18 mirror segments are being figured. All major new technologies will be demonstrated in a realistic environment by early Examples: –Backplane stability at cryo -- this summer –HgCdTe and Si:As detectors -- done –6 K cryocooler for MIRI -- this winter –Mirror segment production process -- this spring –Sunshield -- done All science instruments are currently under construction.

Hubble Fellows April 21, 2006Peter Stockman, STScI Full Scale Model, GSFC 2005

Hubble Fellows April 21, 2006Peter Stockman, STScI 1/6 Scale Ball Segments & Secondary have flight-like degrees of commanded motions Testbed will be used to demonstrate Wavefront sensing and control algorithms Piston adjustment algorithm already demonstrated on Keck with JWST-like optics

Hubble Fellows April 21, 2006Peter Stockman, STScI Backplane Stability Test Article - Picture shows the composite Backplane Stability Test Article (BSTA) Being Built at ATK - 3-meter structure is 1/6 th of the primary mirror backplane (3 mirror segments) - Plan is to perform cryogenic thermal distortion testing on it

Hubble Fellows April 21, 2006Peter Stockman, STScI Instrument ETU Hardware in Production