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Hubble Space Telescope
Wide Field Camera 3

The Horsehead Nebula in Infrared


Source: Hubblesite.org

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).

WFC3 Status

Jan 16 2019: Hubble's Wide Field Camera 3 to Resume Operations
http://hubblesite.org/news_release/news/2019-10

WFC3 STAN Archive
All Telescopes documents of interest to WFC3 users

Late Breaking News from the Last 45 Days

Workaround for aXe issues on astroconda: Click Here

On June 15, 2017, 18 bias files, 4 post-flash files, and 1 image photometry table for WFC3/UVIS were delivered to the Calibration Reference Data System (CRDS) and went live in the 2017.2 release of the MAST processing pipeline for WFC3. These files will be used for processing all WFC3/UVIS data. Please check the [WFC3 reference file pages] and the [WFC3 Photometry website] for more information.

News Archive

Documents added in the last 45 days

WFC3 STAN Issue 28, January 2019
Contents:
1. Ultra-Violet Color Term Transformations
2. Update on Jitter
3. New DrizzlePac Tutorials Available
4. Improved UVIS Drizzled Products from MAST
5. Updates on 2018 UVIS Darks
6. Reclaiming WFC3/UVIS Hot Pixels
7. New Documentation

C. Martlin 01 Jan 2019

ISR 2018-15: Using Dark Images to Characterize Pixel Stability in the WFC3/UVIS Detector
Intrinsic excess thermal energy trapped in the silicon lattice of the Wide Field Camera 3 (WFC3) ultraviolet-visible (UVIS) detector, known as dark current, is typically removed from science observations using UVIS dark calibration reference files. However, this dark current can be used as a means to characterize a pixel's behavior and determine whether the pixel varies excessively over time compared to its expected noise. We use a novel data structure known as a 'pixel history' image to efficiently evaluate each WFC3/UVIS pixel over time. We find that the vast majority of hot pixels (~8% of the detector in 2018) are in fact quite stable and as such, can be calibrated. A small portion of pixels (<1%) are genuinely unstable and should not be used. To encode this distinction in the UVIS bad pixel reference files, we employ a data quality flag (32) to mark the 'unstable' pixels identified in this study. Hot pixels continue to be assigned the usual data quality flag (16). With the additional data quality flag, WFC3/UVIS users will have enhanced control over which pixels to include, and which to exclude, in their analyses. The new bad pixel tables have been installed in the automated calibration pipeline and are available via MAST.
M. Bourque, D. Borncamp, S. Baggett, T. Desjardins, N. Grogin 20 Dec 2018 (pdf)

Document Archive

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