Isolated pixels with anomalously-low signal in otherwise normal Hubble Space Telescope Wide-Field Channel 3 (HST/WFC3) CCD data have been dubbed 'sink pixels' or SPs. The SPs appear to contain an exceptionally large number of charge traps and thus, they capture a commensurate amount of charge during readout. The effects of the sinks on science data depend on a number of factors including the image background, SP distance from the amplifier, and data epoch. In images with high backgrounds, the sinks act as essentially negative delta-functions, impacting a relatively small number of pixels. In contrast, in images with low backgrounds, the sinks can remove charge from a significant number of trailing pixels generating trough-like profiles. In this paper, we characterize the sink pixels, evaluate their effect on science data, and summarize how the sinks are flagged in the calibration pipeline.
At the heart of the Hubble Space Telescope Wide Field Camera 3 (HST/WFC3) UVIS channel is a 4096x4096 pixel e2v
CCD array. While these detectors continue to perform extremely well after more than 7 years in low-earth orbit, the
cumulative effects of radiation damage are becoming increasingly evident. The result is a continual increase of the hotpixel
population and the progressive loss in charge-transfer efficiency (CTE) over time. The decline in CTE has two
effects: (1) it reduces the detected source flux as the defects trap charge during readout and (2) it systematically shifts
source centroids as the trapped charge is later released. The flux losses can be significant, particularly for faint sources in
low background images. In this report, we summarize the radiation damage effects seen in WFC3/UVIS and the
evolution of the CTE losses as a function of time, source brightness, and image-background level. In addition, we
discuss the available mitigation options, including target placement within the field of view, empirical stellar
photometric corrections, post-flash mode and an empirical pixel-based CTE correction. The application of a post-flash
has been remarkably effective in WFC3 at reducing CTE losses in low-background images for a relatively small noise
penalty. Currently, all WFC3 observers are encouraged to consider post-flash for images with low backgrounds. Finally,
a pixel-based CTE correction is available for use after the images have been acquired. Similar to the software in use in
the HST Advanced Camera for Surveys (ACS) pipeline, the algorithm employs an observationally-defined model of how
much charge is captured and released in order to reconstruct the image. As of Feb 2016, the pixel-based CTE correction
is part of the automated WFC3 calibration pipeline. Observers with pre-existing data may request their images from
MAST (Mikulski Archive for Space Telescopes) to obtain the improved products.
Wide Field Camera 3 (WFC3) is the most used instrument on board the Hubble Space Telescope. Providing a broad range of high quality imaging capabilities from 200 to 1700mn using Silicon CCD and HgCdTe IR detectors, WFC3 is fulfilling both our expectations and its formal requirements. With the re-establishment of the observatory level "spatial scan" capability, we have extended the scientific potential ofWFC3 in multiple directions. These controlled scans, often in combination with low resolution slit-less spectroscopy, enable extremely high precision differential photometric measurements of transiting exo-planets and direct measurement of sources considerably brighter than originally anticipated. In addition, long scans permit the measurement of the separation of star images to accuracies approaching 25 micro-arc seconds (a factor of 10 better than prior FGS or imaging measurements) enables direct parallax observations out to 4 kilo-parsecs. In addition, we have employed this spatial scan capability to both assess and improve the mid spatial frequency flat field calibrations.
WFC3 uses a Teledyne HgCdTe 1014xl014 pixel Hawaii-lR infrared detector array developed for this mission. One aspect of this detector with implications for many types of science observations is the localized trapping of charge. This manifests itself as both image persistence lasting several hours and as an apparent response variation with photon arrival rate over a large dynamic range. Beyond a generally adopted observing strategy of obtaining multiple observations with small spatial offsets, we have developed a multi-parameter model that accounts for source flux, accumulated signal level, and decay time to predict image persistence at the pixel level. Using a running window through the entirety of the acquired data, we now provide observers with predictions for each individual exposure within several days of its acquisition.
Ongoing characterization of the sources on infrared background and the causes of its temporal and spatial variation has led to the appreciation of the impact of He I 1.083 micron emission from the earth's atmosphere. This adds a significant and variable background to the two filters and two grisms which include this spectral feature when the HST spacecraft is outside of the earth's shadow.
After nearly five years in orbit, long term trending of the scientific and engineering behavior of WFC3 demonstrates excellent stability other than the expected decline in CCD charge transfer efficiency. Addition of post-flash signal to images is shown to markedly improve the transfer efficiency for low level signals. Combined with a pixel based correction algorithm developed at STScl, CCD performance is stabilized at levels only slightly degraded from its initial values.
Devices in low Earth orbit are particularly susceptible to the cumulative effects of radiation damage and the Hubble
Space Telescope Wide Field Camera 3 (HST/WFC3) UVIS detectors, installed on HST in May 2009, are no exception.
Such damage not only generates new hot pixels but also generates charge traps which degrade the charge transfer
efficiency (CTE), causing a loss in source flux as well as a systematic shift in the object centroid as the trapped charge is
slowly released during readout. Based on an analysis of internal and external monitoring data, we provide an overview
of the consequences of the ~3 years of radiation damage to the WFC3 CCD cameras. The advantages and disadvantages
of available mitigation options are discussed, including use of the WFC3 post-flash and charge injection modes now
available to observers, and the status of an empirical pixel-based correction similar to the one adopted for the HST
Advanced Camera for Surveys (ACS).
Like essentially all IR arrays, the IR detector in the Wide Field Camera 3 (WFC3) instrument on-board Hubble Space
Telescope (HST) exhibits afterimages, known as persistence, following exposures to light levels that approach or
exceed saturation of individual pixels of the detector. The nature of the persistence in the HgCdTe WFC3/IR detector is
distinctly non-linear in that the amount of persistence is not simply proportional to the exposure level. Instead, the
amount of persistence is small until the exposure reaches about half saturation at which point it rises fairly rapidly until
the exposure reaches about twice saturation and then it increases gradually with increasing saturation. The persistence
shows typical power law decay with time over the periods of time that are relevant to HST observations. Given the
frequent usage of the WFC3/IR detector on HST, it is not possible to completely avoid the effects of persistence in
observations obtained with HST by introducing time gaps between IR observations. Therefore, we have developed a
parameterized persistence model that we are using to estimate the amount of persistence in all WRC3/IR images. These
estimates are available for all existing WFC3/IR images through the Mikulski Archive at STScI (MAST) to help HST
users remove persistence from their images. Here we discuss the characterization of persistence in the WFC3 detector in
orbit, the fraction of observations that are affected by persistence, and the effectiveness of the tools we have developed
to reduce the effects of persistence in WFC3 images.
Installed in the Hubble Space Telescope (HST) in May 2009, the Wide Field Camera 3 (WFC3) is performing extremely
well on-orbit. Designed to complement the other instruments on-board the Hubble Space Telescope (HST) and enhance
the overall science performance of the observatory, WFC3 is effectively two instruments in one. The UVIS channel,
with its pair of e2v 4Kx2K CCD chips provides coverage from 200 to 1000 nm while the IR channel, with a Teledyne
HgCdTe focal plane array (FPA) on a Hawaii-1R multiplexer, covers the 800-1700 nm range. This report summarizes
the performance of the WFC3 detectors, including primary characteristics such as quantum efficiency, read noise, dark
current levels, and cosmetics, as well as hysteresis prevention and the impact of radiation damage in the CCDs. In
addition, we discuss effects in the IR detector such as persistence, count rate non-linearity, 'snowballs', and 'negative'
cosmic rays.
We now know that the flux of a source measured with HgCdTe arrays is not a simple, linear function, but depends on the
count-rate as well as the total number of counts. In addition to the count-rate non-linearity (and probably related to the
same physical mechanism), HgCdTe detectors are also susceptible to image persistence. Most of the persistence image
fades in a few minutes, but there is a longer-term component that can result in faint afterimages in the next orbit,
approximately 45 minutes later. For sources saturated at ~100 times full-well, the afterimages can persist for hours
afterwards. This report describes results from ground and on-orbit tests to characterize the persistence and the count-rate
non-linearity in the WFC3 IR detector during its first year of operation.
In ground testing of the Hubble Space Telescope Wide Field Camera 3 (HST/WFC3), the CCDs of its UV/visible channel exhibited an unanticipated quantum efficiency hysteresis (QEH) behavior. The QEH first manifested itself as an occasionally observed contrast in response across the format of the CCDs, with an amplitude of typically 0.1-0.2% or less at the nominal -83°C operating temperature, but with contrasts of up to 3-5% observed at warmer temperatures. The behavior has been replicated in the laboratory using flight spare detectors and has been found to be related to an initial response deficiency of ~5% amplitude when the CCDs
are cooled with no illumination. A visible light flat-field (540nm) with a several times full-well signal level is found to pin the detector response at both optical (600nm) and near-UV (230nm) wavelengths, suppressing the QEH behavior. We have characterized the timescale for the detectors to become unpinned (days for significant
response loss at -83°C and have developed a protocol to stabilize the response in flight by flashing the WFC3 CCDs with the instrument's internal calibration system.
The Wide-field Camera 3 (WFC3) is a fourth-generation instrument planned for installation in Hubble Space Telescope
(HST). Designed as a panchromatic camera, WFC3's UVIS and IR channels will complement the other instruments onboard
HST and enhance the observatory's scientific performance. UVIS images are obtained via two 4096×2051 pixel
e2v CCDs while the IR images are taken with a 1024×1024 pixel HgCdTe focal plane array from Teledyne Imaging
Sensors. Based upon characterization tests performed at NASA/GSFC, the final flight detectors have been chosen and
installed in the instrument. This paper summarizes the performance characteristics of the WFC3 flight detectors based
upon component and instrument-level testing in ambient and thermal vacuum environments.
Wide Field Camera 3 (WFC3), a panchromatic imager developed for the Hubble Space Telescope (HST), is fully
integrated with its flight detectors and has undergone several rounds of ground testing and calibration at Goddard Space
Flight Center (GSFC). The testing processes are highly automated, with WFC3 and the optical stimulus, which is used to
provide external targets and illumination, being commanded by coordinated computer scripts. All test data are captured
and stored in the long-term Hubble Data Archive. A full suite of instrument characterization and calibration tests has
been performed, including the measurement of key detector properties such as dark current, read noise, flat field
response, gain, linearity, and persistence, as well as instrument-level properties like total system throughput, imaging
quality and encircled energy, grism dispersions, IR thermal background, and image stability. Nearly all instrument
characteristics have been shown to meet or exceed expectations and requirements.
Wide-Field Camera 3 (WFC3) has been built for installation on the Hubble Space Telescope (HST) during the next servicing mission. The WFC3 instrument consists of both a UVIS and an IR channel, each with its own complement of filters. On the UVIS side, a selectable optical filter assembly (SOFA) contains a set of 12 wheels that house 48 elements (42 full-frame filters, 5 quadrant filters, and 1 UV grism). The IR channel has one filter wheel which houses 17 elements (15 filters and 2 grisms). While the majority of UVIS filters exhibited excellent performance during ground testing, a subset of filters showed filter ghosting; improved replacements for these filters have been procured and installed. No filter ghosting was found in any of the IR filters; however, the new IR detector for WFC3 will have significantly more response blueward of 800 nm than the original detector, requiring that two filters originally constructed on a fused silica substrate be remade to block any visible light transmission. This paper summarizes the characterization of the final complement of the WFC3 UVIS and IR filters, highlighting improvements in the replacement filters and the projected benefit to science observations.
The Wide Field Camera 3 (WFC3) is a panchromatic imager that will be deployed in the Hubble Space Telescope
(HST). The mission of the WFC3 is to enhance the imaging capability of HST in the ultraviolet, visible and
near-infrared spectral regions. Together with a wavelength coverage spanning 2000 Angstrom to 1.7 μm, the WFC3
high sensitivity, high spatial resolution, and large field-of-view provide the astronomer with an unprecedented
set of tools for exploring all types of exciting astrophysical terrain and for addressing many key questions in
astronomy today. The filter complement, which includes broad, medium, and narrow band filters, naturally
reflects the diversity of astronomical programs to be targeted with WFC3. The WFC3 holds 61 UVIS filter
elements, 15 IR filters, and 3 dispersive elements. During ground testing, the majority of the UVIS filters were
found to exhibit excellent performance consistent with or exceeding expectations; however, a subset of filters
showed considerable ghost images; some with relative intensity as high as 10-15%. Replacement filters with
band-defining coatings that substantially reduce these ghost images were designed and procured. A state-of-the-art
characterization setup was developed to measure the intensity of ghost images, focal shift, wedge direction,
transmitted uniformity and surface features of filters that could affect uniformity in flat-field images. We will
report on these filter characterization methods, as well as the spectral performance measurements of the in-band
transmittance and out-of-band blocking.
Wide Field Camera 3 (WFC3), a panchromatic imager being developed for the Hubble Space Telescope (HST), is now
fully integrated and has undergone extensive ground testing at Goddard Space Flight Center, in both ambient and
thermal-vacuum test environments. The thermal-vacuum testing marks the first time that both of the WFC3 UV/Visible
and IR channels have been operated and characterized in flight-like conditions. The testing processes are completely
automated, with WFC3 and the optical stimulus that is used to provide external targets and sources being commanded
by coordinated computer scripts. All test data are captured and stored in the long-term Hubble Data Archive. A full suite
of instrument calibration tests have been performed, including measurements of detector properties such as dark current,
read noise, flat field response, gain, linearity, and persistence, as well as total system throughput, encircled energy,
grism dispersions, IR thermal background, and image stability tests. Nearly all instrument characteristics have been
shown to meet or exceed expectations and requirements. Solutions to all issues discovered during testing are in the
process of being implemented and will be verified during future ground tests.
We present the performance of the IR detectors developed for the WFC3 project. These are HgCdTe 1Kx1K devices with cutoff wavelength at 1.7 μm and 150K operating temperature. The two selected flight parts, FPA#64 (prime) and FPA#59 (spare) show quantum efficiency higher than 80% at λ=1.6 μm and greater than 40% at λ>1.1μm, readout noise of ~25 e- rms with double correlated sampling, and mean dark current of ~0.04 e/s/pix at 150K. We also report the results obtained at NASA GSFC/DCL on these and other similar devices in what concerns the QE long-term stability, intra-pixel response, and dark current variation following illumination or reset.
Wide Field Camera 3 is a fourth generation instrument for the
Hubble Space Telescope (HST), to be installed during the next HST Servicing Mission 4. For its infrared channel Rockwell Scientific Company has developed a new type of HgCdTe 1Kx1K detector, called WFC3-1R, with cutoff wavelength at 1.7μm and 150K operating temperature. The WFC3-IR detectors are based on HgCdTe MBE grown on a CdZnTe substrate and use a new type of multiplexer, the Hawaii-1R
MUX. Two flight detectors, a prime and a spare, have been recently selected on the basis of the measures performed at NASA Goddard Research Center - Detector Characterization Laboratory. These parts show quantum efficiency higher than 80% at λ=1.6μm and greater than 40% at λ>1.1μm, readout noise of ~25 e- rms with double correlated sampling, and mean dark current of ~0.04 e/s/pix at 150K. We show that the IR channel of WFC3, equipped with one of these flight detectors, beats the instrument requirements in all configurations and promises to have a discovery efficiency
significantly higher than NICMOS. In particular, a two-band
wide-area, deep survey made with WFC3 exceeds the discovery
efficiency of NICMOS before and after the installation of NCS
by a factor of 15 and 10, respectively.
Rockwell Scientific Company is developing a new type of HgCdTe 1K 1K detector, called WFC3-1R, with cutoff
wavelength at 1.7 m and 150K operating temperature. The detector will be installed on the Wide Field Camera 3, the
fourth generation panchromatic instrument for the Hubble Space Telescope (HST) to be installed during HST Servicing
Mission 4, currently scheduled for 2004. The detector uses HgCdTe MBE grown on a CdZnTe substrate and a new type
of multiplexer, the Hawaii-1R MUX. Six lots of detectors have been produced so far, and have demonstrated the
capability to meet or exceed the project requirements. In particular, detectors show quantum efficiency as high as ~90%
at =1.4-1.6 m and greater than 50% at >1.0 m, readout noise of 30 e- rms with double correlated sampling, and dark
current <0.2 e/s/pix at 150K. We illustrate the behavior of the reference pixels, showing that they allow the
compensation of drifts in the dc output level. A number of detectors show a peculiar instability related to the variations
of diode polarization, still under investigation. We also report on the environmental testing needed to qualify the WFC3-
1R detectors as suitable for flight on the HST. We finally provide an update of the project status.
The wide field planetary camera was launched onboard the Hubble Space Telescope in April 1990 and returned to earth during the HST first servicing mission in December 1993. We report on the ongoing examination of the returned hardware. In particular, a significant decline in performance at UV wavelengths in the exterior optics has been found and studied. This appears to be the result of polymerization of molecular contamination on the external optics by UV light reflected off the Earth's atmosphere. Some conlusions from a partial disassembly of the instrument and an examination of its filter elements are presented. We also discuss the effects of radiation on the CCD detectors during their stay in orbit. Radiation damage increased the numbers of hot pixels over time but had no other discernible effects on the performance of the CCDs.
The Wide Field Planetary Camera (WF/PC) onboard the Hubble Space Telescope contains contaminants which condense on the windows in front of each CCD detector. These contaminants are UV opaque and increase with time to the extent that after several months they block 50% of the flux at 300 nm. Also, when the contaminants are warmed above -40 degree(s)C and then returned to the normal CCD operating temperature of -87 degree(s)C, particles form and severely degrade the image quality. The windows may be temporarily cleaned by raising their temperature to 0 degree(s)C. However, this results in a change in the structure of the flat field due to the partial removal of the UV flood which was applied after launch to suppress Quantum Efficiency Hysteresis in the CCDs. Repeated decontaminations will reintroduce the QEH and necessitate another time consuming UV flood and recalibration of the instrument. After 22 months of on-orbit operation, the contaminants could no longer be fully removed by the decontamination procedure. This paper describes the current state of the contaminants, what has been deduced concerning their properties and sources, the results of our efforts to remove them, and some lessons for future space-based instruments using cryogenic UV sensitive detectors.
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