The James Webb Space Telescope

1. The JamesWebb Space Telescope Peter Stockman STScI

2. JWST • Introduction • Architecture overview • Project Status • Science Capabilities • Optical Performance • Science Instruments • JWST Science • 4 Science Themes • Ices in YSO disks • Lab Astro needs • Summary

3. JWST Observatory : Overview • 6-m diameter, deployable primary • Provides needed sensitivity • Diffraction-limited at 2m ~ HST resolution • 0.6-28 µm wavelength range, near-infrared optimized • Diffraction-limited imaging and spectroscopy • L2 orbit • Passive cooling to < 50K • High observing efficiency • 5 year mission life (10 year goal) • Cryocooler for MIR instrument • Station-keeping fuel for 10+ yr JWST in Ariane 5

4. Telescope with Labels

5. L2 Orbit

6. JWST Status • Prime contractor (Northrop Grumman Space Technology) • Mirror manufacture underway • Next major review -- PDR & NAR in 2006 • 4 Instruments selected and funded • Long lead time items being fabricated • Most in the process of completing preliminary design review • Detectors in fabrication • STScI supporting this effort in preparation for operating the observatory

7. JWST Full Scale Model

8. Berylium Mirror Segment

9. Mirror Manufacture • Brush Wellman uses a Hot Isostatic Press (HIP) process to form the Beryllium mirror billets • Axsys Technologies machines and etches the beryllium blanks. Beryllium billet following HIP Two blanks ready for machining • Tinsley Laboratories grinds and polishes the mirror segments, at room temperature and after cryo-testing. Back side light-weighting

10. JWST Science CapabilitiesOptical Performance (1µm) • Optical Drivers: • Segment Quality (impacts < 2 µm & coronagraphy) • Backplane & collimation stability (impacts photometry & coronagraphy)

11. Background-limited Sensitivity • Cameras and R ~ 100 spectroscopy background limited at all wavelengths • 6.5 m mirror >> HST, Spitzer  big gains • Background • Zodi light dominates at shorter wavelengths • Thermal emission dominates at l > 12 µm • Other sources • stray light from Galaxy on dusty mirror, • Earth or Moon shining past shield onto mirrors • NIRSpec sensitivity detector limited at R ~ 1000

12. Instruments NIRCam FGS NIRSpec MIRI Replaced by cryo-cooler

13. NIRCam (U. Arizona & Lockheed Martin)40 Megapixel Camera • Multiplexing • 2 fields simultaneously • 2’x2’ & 2’x2’ • 2 colors simultaneously • l < 2.35 mm : 4 x 2048 x 2048 • l > 2.35 mm: 1 x 2048 x 2048 • 3 functions • Science • Wide-field imaging • Coronagraphy • Calibration • Wavefront Sensing (WFS)

14. NIRCam Filter Set

15. Key Component: Detector • HgCdTe IR detectors • Substrate removed to enable response to 0.6 mm • Long wavelength response at 2.6 mm on short wavelength camera, 5 mm on long wavelength camera 4 2Kx2K Mosaic in test chamber Rockwell Scientific, Camarillo, CA

16. NIRSpec: ESA &Astrium & NASA • > 100 Objects Simultaneously • 9 square arcminute FOV • Implementation: • 3.5’ Large FOV Imaging Spectrograph • 4 x 175 x 384 element Micro-Shutter Array • 2 x 2k x 2k Detector Array • Fixed slits and IFU for backup, contrast • SiC optical bench & optics

17. Sensitivity AB 26.2 in R100 at 3 microns in 10000 seconds 5.2e-19 ergs/cm**2/s in 10**5 sec at R1000 Spectral Resolutions (Multi-Shutter Array, Long Slit (0.2” x 4”)Integral Field Unit (3”x3”) Prism (R~100) 0.6-5 µm 6 Gratings (R ~ 1000, 3000) 1.0-5.0 µm Focal Plane Layout – NIRSpec • 750x350 individually addressable shutters GSFC/NASA

18. MIRI (European Consortium & NASA) • Cryostat --> Cryocooler (2005) • 2 Si:As BIB 1K x 2K detectors • Imaging (1k x 1k Si:As array) • 1.9 x 4 arcmin • 5-28 mm • R=5 filter set • Coronagraph ( R~10, 25”x25”) • 10.65, 11.3, 16, and 24 μm • Spectroscopy • slit spectroscopy • 5”x0.2” slit • R=100 • 5-11 mm • Integral field spectroscopy • R=3000  1000 • 3.5x3.5”  7 x 7” • 5-27.5 mm

19. Fine Guidance Sensor (CSA) • FGS is bore sight guider • Two 2kx2k HgCd detectors • Acquires pre-planned guide stars • Centroids guide stars at 20 Hz rate to provide error signals to fast steering mirror • Tunable Filter Imager • R~100 • 1-2µm & 2-4µm

20. JWST is driven by 4 Science ThemesScience with the James Webb Space Telescope, Gardner et al (SWG), PASP in preparation (~ late fall publication) • JWST General Observer Program (>80% of time) • Annual international peer reviews (like Hubble) • International MOUs (>15% for ESA, 5% for Canadian scientists) • Requirements determined from 4 science themes • The End of the Dark Age: First Light and Reionization • The Assembly of Galaxies • The Birth of Stars and Proto-Planetary Systems • Planetary Systems and the Origins of Life • Science Program Demographics (similar to Hubble) • 1000-2000 different targets per year • Equal numbers of galactic and extragalactic targets • Exposure times per target will likely range from 1000 s to 1,000,000 s (quick Spitzer followups to ultra-deep fields and SNe surveys)

21. Redshift Neutral IGM z~zi z>zi . z<zi Wavelength Wavelength Wavelength Lyman Forest Absorption Patchy Absorption Black Gunn-Peterson trough 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? • Ultra-Deep NIR survey (1nJy), spectroscopic & Mid-IR confirmation. • QSO spectra: Ly-a forest

22. Reionization White et al 2004 • When the IGM is neutral, it is black beyond the Lyman limit at 912 A due to photoelectric absorption • It is nearly opaque beyond Lyman a due to line absorption • Exiting data suggests reionization complete around z=6.5 • The reionization epoch is unclear • WMAP suggests z~10-20 • Most distant QSOs have significant metals • Ionization history may be complex • Wide area photometric surveys for rare high redshift objects with JWST • SN e Type 1a visible to z~10 SN II

23. 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

24. Deeply embedded protostar Circumstellar disk The Eagle Nebulaas seen in the infrared The Eagle Nebula as seen by HST Agglomeration & planetesimals Mature planetary system Birth of stars and protoplanetary systems • How do clouds collapse? • What is the low-mass IMF? • Imaging of molecular clouds • Survey “elephant trunks” • Survey star-forming clusters

25. High Mass SF – Nature vs. Nurture? • Low mass star formation thought to be understood • Many rotating cores in MC • Disks forms around central concentrations • Most of mass is accreted through disk • High mass systems may be hard to form this way • Intense light destroys disk and disrupts system • Alternative – Nurture • low mass “companions” in gravitational well of GMC collide to form high mass stars • MIRI imaging of GMCs should reveal actual populations of young stars t: 0.66  1.3 1  10  25 many M 4-8 Bonnell et al. 2004

26. Planetary systems and the origins of life • How do planets form? • How are circumstellar disks like our Solar System? • How are habitable zones established? Spitzer image Malfait et al 1998 • Extra-solar giant planets • Coronagraphy • Spectra of circumstellar disks, comets and KBOs • Spectra of icy bodies in outer Solar System Simulated JWST imageFomalhaut at 24 microns Titan

27. Jovian Exoplanet detection with MIRI • Most Exo-planets to date have been detected by measuring the Doppler wobble of primary star • JWST/MIRI will attempt to image and in some cases obtain spectra of these directly •  atmospheric structure and composition Spectra – Sudarsky et al 2003

28. Direct Observations of Ices in Circumstellar Disks Interstellar IcesAdwin Boogert, California Inst. of Technology, STScI Colloquium, Feb 2005 • Protostellar disks provide crucial link between evolution of ices from molecular clouds to planetary systems (comets). • Major difficulty: does line of sight pass through disk and which part of disk? Disk needs to be edge-on. (Pontoppidan et al. 2005, ApJ, in press) see also www.spitzer.caltech.edu

29. Gas phase CO: ro-vibrational transitions allow J=1, v=1; characteristic P and R branch spectrum. Solid CO: vibrations only giving broader absorption whose width, position and shape is determined by solid state (dipole) interactions. High resolution required to separate gas and solid bands. At R=3000 JWST NIRSpec and and MIRI can do this. Solid H2O and CO Vibrational Modes [ISO satellite observation of Elias 29 in r Oph cloud; Boogert, Tielens, Ceccarelli et al. A&A 360, 683, 2000] Adwin Boogert

30. background star! Infrared Spectra of Highly Obscured (Proto)Stars Ice and dust absorption bands observed against continuum of a star or protostar Study of important species (CO2, CH4, C-H/C-O bending modes in 5-8 m region) severely hindered by atmosphere; use satellites: • ISO (1995-1998) • Spitzer (2003-now)

31. Spitzer Spectroscopy of Ices toward Protostars /SVS 4-5 Spectra from Spitzer Legacy program “From Molecular Cores to Planet-forming Disks” (c2d) Adwin Boogert

32. Ices in Disks • Direct observations of ices in disks only possible for edge-on disks (obviously). • Difficult, rarely done, and exact ice location often disputed. • Few claims were made (Kastner et al. 1995; Shuping et al. 2000; Boogert et al. 2002; Thi et al. 2002). • Understanding of ices in disks requires knowledge of disk properties (e.g. inclination) through mm-wave observations.

33. Ices in Disk L1489 IRS (Boogert, Hogerheijde & Blake, ApJ 568,761, 2002) • Prominent band of solid CO detected toward L1489, originating in large, flaring disk. • CO band consists of 3 components, explained by laboratory simulations as originating from CO in 3 distinct mixtures:

34. Ices in Disk L1489 IRS (Boogert, Hogerheijde & Blake, ApJ 568,761, 2002) • Prominent band of solid CO detected toward L1489, originating in large, flaring disk. • CO band consists of 3 components, explained by laboratory simulations as originating from CO in 3 distinct mixtures: • 'polar' H2O:CO

35. Ices in Disk L1489 IRS (Boogert, Hogerheijde & Blake, ApJ 568,761, 2002) • Prominent band of solid CO detected toward L1489, originating in large, flaring disk. • CO band consists of 3 components, explained by laboratory simulations as originating from CO in 3 distinct mixtures: • 'polar' H2O:CO • 'apolar' CO2:CO or pure CO phase [NEW!]

36. Ices in Disk L1489 IRS (Boogert, Hogerheijde & Blake, ApJ 568,761, 2002) • Prominent band of solid CO detected toward L1489, originating in large, flaring disk. • CO band consists of 3 components, explained by laboratory simulations as originating from CO in 3 distinct mixtures: • 'polar' H2O:CO • 'apolar' CO2:CO or pure CO phase [NEW!] • 'apolar' pure CO

37. Ice Processing in Disk • Are ices in L1489 IRS disk processed?

38. Ice Processing in Disk (Boogert, Blake & Tielens, ApJ 577, 271 (2002)) • Are ices in L1489 IRS disk processed? • Empirical answer by comparing CO ice band with established unprocessed line of sight, NGC 7538 : IRS9:

39. Ice Processing in Disk (Boogert, Blake & Tielens, ApJ 577, 271 (2002)) • Are ices in L1489 IRS disk processed? • Empirical answer by comparing CO ice band with established unprocessed line of sight, NGC 7538 : IRS9: • apolar CO-rich ices appear to have been evaporated in L1489 IRS disk • JWST NIRSpec resolution, at R~3000, will be capable of similar studies on many more distant YSOs, simultaneously.

40. Methane Chemistry Broad “3.47 mm” band still unidentified. Tentatively CH/OH stretch vibrations of many species, but so-far only CH3OH, and now CH4 identified. JWST can improve much • (Boogert et al. 2004)

41. Suggested areas for Lab Astrophysics for JWST (2003) from Ewine van Dishoeck (pre-Phase A SWG member, MIRI science team • Gas-phase transitions • Lowest vibrational transitions: long carbon chains seen toward post-AGBs • Higher vibrational transitions needed for modeling Exo-Solar Planetss • Ices • Higher resolution studies (R~1500-3000) to match JWST resolution • Better understanding of photoprocessing & ion-bombardment effects • PAHs • Spectroscopy of large (>30 C atoms) gas-phase PAHs • Reactions and photoprocesses involving PAHs • Silicates, oxides • Large current effort at measuring spectra and optical constants

42. Summary • JWST development is underway • It will be > 100 times more powerful than Spitzer in the NIR and MIR (5-28µm). • JWST spectral resolution is now capable of addressing astrophysically important gas and solid phase studies. • It will join the next generation of observatories (ALMA, Herschel, and SOFIA) in studying the origins of galaxies, stars, and planets. • Keep tuned to www.stsci.edu/jwst and www.jwst.nasa.gov for news.

43. Science Working Group • Marcia Rieke (U. Ariz.,NIRCam PI) • Peter Jakobsen (ESA, NIRSpec PI), Hans Walter Rix (NIRSpec Rep.) • George Rieke & Gillian Wright (MIRI PI s) • John Hutchings (CSA, FGS PI) • Matt Mountain (soon STScI, Telescope Scientist) • J. Lunine, Massimo Stiavelli, Heidi Hammel, Mark McCaughrean, Rogier Windhorst (Interdisciplinary Scientists) • John Mather, Matt Greenhouse, Jon Gardner (JWST Project Scientists) • Peter Stockman (STScI)