UVIS
- Anneal History
- Bowtie
- Contamination
- Charge Transfer Efficiency/Extended Pixel Edge Response (CTE-EPER)
- Darks
- Gain
Disclaimer: This page will be updated as resources allow.
UVIS
Anneal History
Complete Anneal History
A complete history of all on-orbit WFC3/UVIS detector anneals.
Bowtie
1 to 3 plot
Median flatfield (image1/image3) ratio levels as a function of day since June 11th, 2009; crosses are for chip 1 and circles are for chip 2.
1 to constant plot
Median flatfield (image1/image1) ratio levels as a function of day since June 11th, 2009; crosses are for chip 1 and circles are for chip 2.
3 to constant plot
Median flatfield (image3/image3) ratio levels as a function of day since June 11th, 2009; crosses are for chip 1 and circles are for chip 2.
References:
WFC3 ISR 2009-24: WFC3 SMOV Proposal 11808: UVIS Bowtie Monitor.
Baggett and Borders 26 Jan 2010
WFC3 ISR 2013-09: WFC3/UVIS Bowtie Monitor
M. Bourque and S. Baggett 25 Jun 2013
WFC3 ISR 2014-13: No Evidence Found for WFC3/UVIS QE ‘Overshoot’
M. Bourque, S. Baggett, & L. Dressel 29 May 2014
Contamination
HST spectrophotometric standards are routinely observed to monitor throughput stability. Analysis of the high signal-to-noise photometry in W and M bands indicates that the instrument is photometrically stable, with measured variations that are <0.4%.
References:
WFC3 ISR 2010-14:The Photometric Performance of WFC3/UVIS:Temporal Stability Through Year 1.
Kalirai et al. 14 Oct 2010
Charge Transfer Efficiency/Extended Pixel Edge Response (CTE-EPER)
For information on how CTE losses affect science data as well as options for mitigating those losses, please see http://www.stsci.edu/hst/wfc3/ins_performance/CTE/.
The EPER (Extended Pixel Edge Response) method can be used to measure CCD detector Charge Transfer Inefficiency (CTI)-induced losses via internal exposures. EPER data consist of short tungsten lamp flat field exposures in several filters in order to obtain a large range of illumination levels (from ~100e- to 4000e-). By measuring the signal profiles as they extend into the trailing overscan region, an assessment can be made of the CTE level. Please see the most recent report for current plots.
Tabulated data of EPER CTE levels as a function of signal and time
Columns are filename (date encoded as
ddmmyy), Modified Juilan Date, average signal across all four amps at
five different levels (cols 3-7), CTE for those average signals
(cols 8-12), and the error bars for the EPER CTE measurements (cols 13-17).
References:
WFC3 ISR 2013-03: WFC3/UVIS EPER CTE Measurement: Cycles 19 & 20
M. Bourque & V. Kozhurina-Platais 15 Feb 2013
WFC3 ISR 2011-17: WFC3/UVIS CTE-EPER Measurement: Cycle 17 & 18.
Khozurina-Platais et al. 27 Sept 2011
2010 HST Calibration Workshop Proceedings: Internal Monitoring of WFC3/UVIS Charge Transfer Efficiency.(see page 573)
Khozurina-Platais et al. 2010
WFC3 ISR 2009-10: WFC3/UVIS CTE-EPER Measurement.
Khozurina-Platais et al. 21 Jun 2009
WFC3 ISR 2007-13: UVIS CCD EPER CTE measurements performed during the April 2007 Ambient Calibration campaign (SMS UV02S01).
M. Robberto 2007
Darks
UVIS Hot Pixels
WFC3/UVIS (Chip 2, Amps C & D)
This plot shows the hot pixel growth between anneals for WFC3/UVIS. The number of hot pixels are plotted as a function of time since the installation of WFC3 on HST, where red lines represent SIC&DH failures, when WFC3 was safed, and the grey/white
regions represent anneal cycles. Note that the implementation of post-flash occurred on day 1246.
Dark Current
WFC3/UVIS (Chip 2, Amps C & D)
Shows the dark current vs. time for WFC3/UVIS. The red lines represent SIC&DH failures, when WFC3 was safed, and the grey/white regions represent anneal cycles. Note that the implementation of post-flash occurred on day 1246.
Dark Current with linear fit to Cy 17 data
Shows the dark current vs. time for WFC3/UVIS. A linear fit to the Cy 17 data is show in magenta, the yellow lines represent the SIC&DH
failures, when WFC3 was safed, the red lines represent the anneals, and the brown vertical line is the switch between SMOV dark (1800 sec)
and Cy 17 darks (900 sec).
References:
WFC3 ISR 2009-16: WFC3 SMOV Proposals 11419, 11426, 11431, and 11446: On-Orbit Darks.
Borders and Baggett 16 Nov 2009
WFC3 ISR 2014-04: WFC3 Cycle 19 & 20 Dark Calibration: Part I
J. Biretta and M. Bourque 10 April 2014
Gain
Cycle 17 Gain Plot
Cy 17 mean-variance plot for Quad A, B, C, and D.
SMOV Gain Plot
SMOV mean-variance plot for Quad A, B, C, and D.
TV3 Gain Plot
TV3 mean-variance plot for Quad A, B, C, and D.
References:
ISR 2013-02: WFC3 Cycle 19 Proposal 12690: UVIS Gain
H. Gunning, C. Pavlovsky, S. Baggett 29 Jan 2013
WFC3 ISR 2011-13: WFC3 Cycle 17 Proposal 11906: UVIS Gain
Borders, Pavlovsky, and Baggett 23 June 2011