1. NIRCam at a Glance

2. The JWST Observatory Coffee 5/02/2013 2/24, Diameter: 6.5 m

3. Observatory Performance Primary mirror is 18 hexagonal segments, 6.5 m in diameter.  Strehl ratio > 0.80 at 2 micrometers  (Encircled energy > 0.74 within 0.15 arc sec at 1 micrometer)  Gold coating  good response at wavelengths > 0.6 micrometers Field of regard  Sun angles of 85°–135° are permitted, with roll of ±5°.   >35% sky coverage at any instant  Continuous Viewing Zone (CVZ) is 5° about the ecliptic poles.  Targets will be visible for >60 days SUN Exclusion < 45° from Anti-Sun Exclusion < 85° from Sun Anti-Sun LOS Coffee 5/02/2013 3/24

4. NIRCam has Two Imagers in Two Modules Coffee 5/02/2013 4/24 Two adjacent fields of view (2.2 arcminute) 2 Both fields in SW and LW bands Two back-to-back modules

5. Fields of View of JWST Instruments Coffee 5/02/2013 5/24 0 -2 -4 2 4 0-2-4-6-82468 Horizontal Field Position (arcmin) Vertical Field Position (arcmin) NIRSpec NIRCam MIRI NIRISS FGS

6. The Near Infrared Camera Coffee 5/02/2013 6/24 Coronagraphic masks: 2 channels in each module: Short Wavelength (0.6-2.3  m) Long Wavelength (2.4-5.0  m) HgCdTe FPA Format (2  2)  (2040  2040) HgCdTe FPA Format 1  (2040  2040) 0.032 arcsec/pixel0.065 arcsec/pixel FOV= 2.21  2.21 arcmin 2 Sensitivity (10 , R=4, 10 4 s): 1.1  m: 10.4 nJy 2.0  m: 12.1 nJy 4.4  m: 24.5 nJy 2 functionally identical (mirror image) modules Filters provide (W  R=4, M  R=10, N  R=100) LW Grisms provide R~300 5” gap between SW SCAs 40” gap between A & B

7. NIRCam Optical Layout Coffee 5/02/2013 7/24

8. Assembled Modules Coffee 5/02/2013 8/24

9. NIRCam Filter Wheel Coffee 5/02/2013 9/24

10. NIRCam Optical Elements Coffee 5/02/2013 10/24

11. NIRCam Focal Plane Arrays Coffee 5/02/2013 11/24

12. MULTIACCUM Readout Mode (“ramp”) Coffee 5/02/2013 12/24

13. Detector Performance Coffee 5/02/2013 13/24

14. 5-sigma, 50,000 secs NIRCam Sensitivity Comparison microns Galaxy models: HST SST Ground JWST NIRCam TIPS 4/18/2013 14/24

15. NIRCam Coronagraph - 1 Coffee 5/02/2013 15/24

16. NIRCam Coronagraph - 2 Coffee 5/02/2013 16/24

17. 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? Key JWST Observations: Ultra-Deep NIR survey (1.4 nJy) (NIRCam, NIRISS) Spectroscopic NIR & Mid-IR confirmation. (NIRCam & NIRISS Grisms, NIRSpec, MIRI) Coffee 5/02/2013 17/24

18. 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? Coffee 5/02/2013 18/24

19. 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 Coffee 5/02/2013 19/24

20. Planetary systems and the origins of life How do planets form? How are circumstellar disks like our Solar System? How are habitable zones established? Key JWST Observations: Coronagraphy of Extra-solar giant planets Photometry & spectroscopy of transiting exoplanets Spectra of circumstellar disks, comets and KBOs Spectra of icy bodies in outer Solar System (Seager 2010) Coffee 5/02/2013 20/24

21. NIRCam’s Wavefront Sensing Role NIRCam provides the imaging data needed for wavefront sensing. Dispersed Hartmann Sensors at 0° and 60° orientations permit phasing of adjacent mirror elements. Two grisms on the long wavelength channel provide an alternative to the Dispersed Hartmann Sensor (DHS). Coarse phasing w/DHS After coarse phasing Fully aligned Fine phasing First Light After segment capture DHS at pupil Spectra recorded by NIRCam TIPS 4/18/2013 21/24

22. NIRCam Status Cryovac 3 successfully finished April 11. Rebuilding the Instrument Control Electronics (ICE) is underway. Testing for Electromagnetic Interference and Compatibility (EMI/EMC) is next. Shipment to GSFC expected at end of May. Acoustic and vibe testing (at APL) in June. ICE boxes arrive late August. Focal Plane Electronics (FPE) delivered in September. Acceptance review at GSFC in October. New SW FPAs are in house at UofA, and they look beautiful. Expect to prepare these and place in NIRCam before ISIM CV2. New LW FPAs ready at Teledyne. Hope to prepare these too. Coffee 5/02/2013 22/24

23. On-line Resources STScI JWST Home Page http://www.stsci.edu/jwst/ JWST Primer http://www.stsci.edu/jwst/doc- archive/handbooks/JWST_Primer_v20.pdf STScI NIRCam Page http://www.stsci.edu/jwst/instruments/nircam Dithering with NIRCam http://www.stsci.edu/~INS/2010CalWorkshop/anderson-dither.pdf‎ NIRCAM IR Imaging ETC http://jwstetc.stsci.edu/etc/input/nircam/imaging/ University of Arizona NIRCam Page http://ircamera.as.arizona.edu/nircam/ NASA NIRCam Page http://www.jwst.nasa.gov/nircam.html Coffee 5/02/2013 23/24

24. Coffee 5/02/2013 24/24 INS NIRCam Team Members Elizabeth Barker Deputy Lead ETC WG Lead Andrew Colson RIA Massimo Robberto Technical Lead Calibration WG Jennifer Lotz Operations WG Efficiency WG Armin Rest Pipeline WG Jerry Kriss Team Lead Backgrounds WG John Stansberry TBD in June David Golimowski I&T Lead Coronagraphs WG

25. Coronagraphic masks: 2 channels in each module: Short Wavelength (0.6-2.3  m) Long Wavelength (2.4-5.0  m) HgCdTe FPA Format (2  2)  (2040  2040) HgCdTe FPA Format 1  (2040  2040) 0.032 arcsec/pixel0.065 arcsec/pixel FOV= 2.21  2.21 arcmin 2 Sensitivity (10 , R=4, 10 4 s): 1.1  m: 12.4 nJy 2.0  m: 9.0 nJy 4.4  m: 20.5 nJy 2 functionally identical (mirror image) modules Filters provide (W  R=4, M  R=10, N  R=100)