[90.03] Status of the HST Wide Field Camera 3

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1 [90.03] Status of the HST Wide Field Camera 3 J.W. MacKenty (STScI), R.A. Kimble (NASA/GSFC), WFC3 Team The Wide Field Camera 3 is under construction for a planned deployment in the Hubble Space Telescope during Servicing Mission 4. In early 2005, WFC3 will replace the aging WFPC2 instrument in the HST radial bay. WFC3 provides two imaging channels. The UVIS channel features a 4096 x 4096 pixel CCD focal plane with sensitivity from 200 to 1000 nm. Equipped with 47 filters and an ultraviolet grism, the UVIS channel provides unprecedented sensitivity and field of view in the near ultraviolet for HST. The IR channel features a 1014 x 1014 pixel HgCdTe focal plane covering 850 to 1700 nm. With 17 filters and 2 grisms, this provides HST with a powerful near infrared capability.

2 Science Oversight Committee SOC Member Bruce Balick Howard Bond Daniela Calzetti Marcella Carollo Michael Disney Michael Dopita Jay Frogel* Donald Hall Jon Holtzman Gerard Luppino Patrick McCarthy Robert O Connell (Chair) Francesco Paresce Abhijit Saha Joseph Silk John Trauger Alistair Walker Brad Whitmore Rogier Windhorst Erick Young Affiliation University of Washington Space Telescope Science Institute Space Telescope Science Institute Columbia University University of Wales At Cardiff Institute of Advanced Studies Mt. Stromlo & Siding Spring Observatory Ohio State University (now NASA HQ) University of Hawaii New Mexico State University University Of Hawaii Carnegie Observatories University of Virginia European Southern Observatory National Optical Astronomy Observatory University of California, Berkeley Jet Propulsion Laboratory NOAO CTIO Space Telescope Science Institute Arizona State University University of Arizona

3 WFC3 is a facility instrument being developed on behalf of HST user community Will replace WFPC2 in Hubble during SM4 (February 2005) Assures excellent HST imaging science to end of mission International Scientific Oversight Committee (SOC) Integrated Product Team: GSFC, STScI, Ball Aerospace, Randy Kimble (GSFC) Instrument Scientist [replaced Ed Cheng 9/02] John MacKenty (STScI) Deputy Instrument Scientist WFC3 a panchromatic camera for HST Two channels cover Near-UV to Near-IR UVIS CCD channel backs up ACS from 200 to 1000 nm Provides powerful new wide field imaging from 200 to 400 nm NIR HgCdTe channel extends NICMOS Infrared capabilities detector offers 7x NICMOS FOV from 850 to 1700 nm

4 WFC3 UVIS WFC3 IR

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6 Calibration Subsystem UVM2 IR Fold Mirror SOFA UVIS Shutter UVIS Detector UVM1 & Corrector Mechanism IRM1 IR Cold Enclosure/ RCP/Filters/ Detector Pickoff Mirror Channel Select Mechanism IRM2 & Corrector Mechanism

7 Not Shown - WFC3 will reuse the EVA Radiator Handhold, Stowage Fixture and POM cover. LVPS Electronics Radiator Main (Detector) Radiator w/ Light Baffle Detector Heat Pipes Radiator Truss Assembly MEB #2 DEB (under MEB) Blind Mate Connector Optical Bench MEB #1 WF/PC I H/W reuse HST Heritage New H/W CEB C-Latch Enclosure A-Latch Mechanism Cover Pick-Off Mirror

8 Re-flight of WF/PC-1 Hardware UVIS Filter Assembly External Enclosure Thermal Radiator

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10 WFC3 Wide UV Filters 0.7 Transmission F218W UVIS 03 (F275W) UVIS 15 (F300X) F225W F275W F300X Wavelength (A)

11 Flight IR Filter Wheel Optical Alignment and Characterization Complete Meets or Exceed Requirements F167N F126N F164N Blank F160W F125W G141 F110W F132N F105W F130N F098W F128N G102 F127M F139M F153M F093M

12 STATUS WFC3 in Integration and Test Phase at GSFC Optical Assembly delivered by Ball Aerospace Dec 02 w/ Electronics and Software Optical Alignment complete UVIS Detectors in testing IR Detectors in fabrication On schedule for Fall 03 final System Level tests Optical Bench IR Cold enclosure With Filter Wheel Main Computer under Test at Ball Aerospace

13 UVIS Channel Focal Plane Array: Two 2K x 4K E2V (Marconi) CCDs FOV: 162 x 160 arcsec (39 mas pixels) Wavelength Range: nm Spectral Components: 42 filters, 5 quad filters, and 1 UV grism

14 Flight Build 1 CCDs QE Quantum Efficiency Wavelength (nm) CCD Detectors have 2.1 to 2.5 e- readnoise (3-3.5 e- w/ electronics) Excellent initial Charge Transfer Efficiency Provision for low noise (10-15 e- rms) Charge Injection mitigates nearly all radiation induced charge transfer loss

15 IR Channel Focal Plane Array: 1K x 1K Rockwell HgCdTe Hawaii-1R FOV: 123 x 139 arcsec (120 x 130 mas pixels) Wavelength Range: nm Spectral Components: 15 filters and 2 grisms Mounted on 6 stage TEC Similar to CCD operation Does not require cryogen MUX has 5 rows of reference pixels on each edge to provide zero level tracking

16 IR Detector #64 Quantum Efficiency Wavelength (nm) 1300 nm flat field IR Detector Status Tuned long wavelength cutoff at 1.73 microns (150K operation) Dark Current better than specification (0.1 to 0.2 e-/s/pix) Past difficulties with stability appear fixed in most recent lot Readnoise of e- (correlated double sample) Exceeds specification of 15 e- but much improved Operability and uniformity excellent