The Horsehead Nebula in Infrared
The Wide Field Camera 3 (WFC3) is a fourth-generation UVIS/IR imager aboard the Hubble Space Telescope (HST). WFC3 was installed in May 2009 during HST servicing mission 4, and replaces the Wide Field Planetary Camera 2 (WFPC2).
The UVIS and IR Channels are operating nominally.
Late Breaking News from the Last 45 Days
Please note that the default aperture radius for WFC3/UVIS is 0.4 arcsec (90% of encircled energy). For 80% of encircled energy, use an aperture with radius 0.2 arcsec, comparable to the ACS default.
Quick-Start Advice to Run Reverse Correction for CTE now available here: CTE Tools
WFC3 Throughput are now available as text files: Throughput Tables
Documents added in the last 45 days
WFC3 STAN Issue 23, June 2016
1. Cycle 24 Phase II Deadline Reminder and Updates to APT
2. Changes to ETC Calculations
3. Improvements to Zodiacal Light Computations in the ETC
4. Planning "Drift and Shift" Observations
5. New Documentation
C.Martlin 10 Jun 2016
ISR 2016-10: WFC3/UVIS EPER CTE Cycles Aug 2009 - Apr 2016
This report summarizes the changes in Charge Transfer Efficiency (CTE) as determined by the Extended Pixel Edge Response (EPER) method. The results are derived from data acquired during Cycle 17 through Cycle 22 (August 2009-present). The EPER method uses large overscan regions obtained via a non-standard readout mode to measure CTE trails as a function of distance from the last row of illuminated science pixels. The CTE decline is steepest at the lowest signal values (160 e- signal level) and more shallow at the highest signal levels (5000 e-). We measure the evolution of CTE since the installation of WFC3; over 7 years the CTE has degraded by 0.07% for the lowest illumination level.
Harish Khandrika, Sylvia Baggett, Ariel Bowers 23 May 2016 (pdf)
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