hubble fellows april 21, 2006peter stockman, stsci james webb space telescope © david a. hardy

Peter Stockman, STScI

Hubble Fellows April 21, 2006

James Webb Space Telescope

© David A. Hardy/www.astroart.org/PPARC


1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019

Phase A Phase B Phase C/D Phase E

Concept Development Design, Fabrication, Assembly and Test

FormulationAuthorization

NAR Launch

science operations ...

ICR(PNAR)

T-NAR

JWST Facts at a Glance

• 6.5 m primary • 0.7- 28 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%)



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

ReportJuly ‘06



Discovery Space

• JWST should maintain a significant advantage over 30 m diameter ground-based telescopes above 1.7 µm.

SATReportJuly ‘06



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 www.stsci.edu/jwst



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 Wavelength Wavelength

Lyman Forest

Absorption

Black Gunn-Peterson trough

z<zi

z~zi

z>zi

Neutral IGM

.

SpitzerGOODS20,000 s

JWSTGOODS1,000 s



Near Infrared Camera

• PI: Marcia Rieke, University of Arizona• Two 2.16’x2.16’ imaging fields. Each field is

simultaneously observed in two bands:– 0.7 - 2.3 µm (Nyquist sampled at 2 µm, 0.03” pixels)– 2.4 - 5 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



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



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



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 & planetesimals Mature planetary system

Circumstellar disk

The Eagle Nebula as seen by HST

The Eagle Nebulaas seen in the infrared



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 imageFomalhaut 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



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



How are circumstellar disks like our Solar System?

Here is anillustration ofwhat MIRI mightfind within thevery young corein Ophiuchus,VLA 1623

artist’s concept ofprotostellar diskfrom T. Greene, Am. Scientist

approximate field for NIRSpec & MIRI integral field spectroscopy



Progress

• All 18 mirror segments are being figured.• All major new technologies will be demonstrated in a

realistic environment by early 2007. 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.



Full Scale Model, GSFC 2005



1/6 Scale Telescope @ 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



Backplane Stability Test Article

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



Instrument ETU Hardware in Production

hubble fellows april 21, 2006peter stockman, stsci james webb space telescope © david a. hardy

Documents

hubble fellows

peter stockman

agn slide

stsci end

orgpparc slide

stsci breadth of science

hubble sequence form

stsci discovery space