7.3 CCD Operation and Feasibility Considerations
7.3.1 CCD Dark Current
At launch in 1997, the median dark rate (excluding hot pixels) for the STIS CCD was about 0.0015 e−/s. The on-orbit environment causes radiation damage which, over time, increases both the dark current and the number of hot pixels. The CCD is annealed once every four weeks by turning off the thermo-electric cooler (TEC) which allows the CCD to warm from its usual operating temperature near −83° C to approximately +5° C. While this slows the effects of radiation damage it does not eliminate it. By the time that the STIS Side-1 electronics failed in May 2001, the median dark rate had increased to about 0.004 e−/s.
As the Side-2 electronics lack a working temperature sensor at the detector itself, the CCD can no longer be maintained at a fixed temperature, and this causes both the temperature of the CCD chip and the dark current to vary as the temperature of the HST aft-shroud environment into which the STIS CCD TEC radiates heat changes. This leads to fluctuations of the CCD dark current on short time scales as HST changes its orientation with respect to the Sun and Earth and moves in and out of the Earth’s shadow, as well as on longer time scales where the heat input can vary due to the annual changes of the Earth’s distance from the Sun, the degradation of HST’s thermal insulation, and the heat inputs from other HST instruments. While the CCD detector temperature can no longer be directly measured, it has been shown that the temperature of the CCD housing (available in the telemetry value
OCCDHTAV) can be used as a surrogate for the detector temperature. The dark current scales are observed to increase by between 5% and 10% for each degree increase in housing temperature, depending upon the individual pixel and when the exposure was taken in the lifetime of STIS. This is approximated by a 7%/° C correction, (see STIS ISR 2001-03 for additional details).
The combination of radiation damage and the resulting loss of charge transfer efficiency (Section 7.3.7), also results in a dark current that is no longer distributed uniformly over the detector. The effective dark current is much lower near the top of the detector, close to the readout register. This provides another reason to utilize the E1 aperture positions when observing faint objects (see Section 7.3.8). The trend for the dark current both at the center of the detector and near the top of the chip at the E1 aperture positions is shown in Figure 7.8. In this figure, all measured dark values have been scaled to a CCD housing temperature of 18° C, which is typical of values observed during September 2009. We expect that the CCD dark current will continue to increase with time and note that the scatter in the dark current values has increased when compared to the scatter in dark current values for darks taken prior to SM4. See STIS ISR 2012-02 for detailed information on the behavior of the CCD dark current after SM4. For use in the STIS ETC for Cycle 29, we have adopted dark current values of 0.023, 0.028, and 0.033 e−/s; these values are the expected values at the detector bottom, middle, and top (near the E1 position) during April 2022.
7.3.2 CCD Saturation
There are no hard bright object limits to worry about for CCD observations, because the CCD cannot be damaged by observations of bright sources. However, the CCD pixels do saturate at high accumulated count levels, due to the finite depth of the CCD full well. The level at which the behavior of individual pixels deviates from linearity varies over the surface of the chip. Near the center of the detector, (row 515), this may occur after collecting about 130,000 e–/pixel, while some regions saturate at levels as low as 120,000 e–/pixel. The variation of the CCD full well over the chip occurs because of nonuniformity in the process of boron implantation, which creates the potential wells in this type of CCD. Accumulations up to the full well limit can be observed only in the CCDGAIN=4 setting, as the gain amplifier already saturates at ~33,000 e–/pix in the CCDGAIN=1 setting (see Section 7.2.10).
Saturation imposes a limit on the product of the count rate and the integration time. Keep the total counts in the pixels of interest below the saturation level, either by keeping the exposure time short enough that the limit is not violated in any single integration or by choosing a more appropriate configuration. You can allow saturation to occur in regions of the image over which you do not wish to extract information (e.g., you can allow a star or single emission line to saturate if you are interested in other features). Remember, however, that once the CCD well is over full, charge will bleed along the columns of the CCD so that neighboring pixels (along the slit for spectroscopic observations) will also be affected. Saturation cannot be corrected in post-observation data processing.
An interesting workaround for this is described in Gilliland, Goudfrooij & Kimble, 1999, PASP 111, 1009. For
CCDGAIN=4 the response remains linear up to, and even far beyond saturation if one integrates over the pixels receiving the charge bleed. Because the bleeding is perpendicular to the dispersion direction, for point sources such saturation does not compromise spectral purity. Signal to noise values of ~10,000 have been demonstrated for saturated data (see STIS ISR 1999-05 for a time series application and Bohlin & Gilliland, 2004, AJ 127, 3508 for a measurement of Vega’s absolute flux). This technique is, however, best applied near the center of the detector. Near the top of the detector, (e.g., at the E1 aperture position near row 900), the full well depth of the detector is larger, and this can lead to serial transfer artifacts when too many electrons are read out of a single pixel. For more information see STIS ISR 2015-06.
In Section 6.2, we explained how to determine the peak counts/s/pix expected for your observation. In Chapter 13 for each spectroscopic mode and in Chapter 14 for each imaging mode, we provide plots of exposure time to fill the CCD well versus source flux for each STIS configuration. Lastly, STIS ETCs are available on the STScI STIS website. Use one of these sources to ensure that your observations will not saturate sources of interest.
The minimum CCD exposure time is 0.1 seconds, providing a true limit to the brightest source that can be observed without saturating.
For standard applications keep the accumulated e–/pix per exposure below 120,000 at
CCDGAIN=4 (determined by the CCD full well), and below 30,000 at
CCDGAIN=1 (determined by gain amplifier saturation).
7.3.3 CCD Shutter Effects
The STIS CCD camera features a high-speed shutter that eliminates the need for a shutter illumination correction, even at the shortest commandable exposure time of 0.1 seconds. The only two minor drawbacks of using this shortest exposure time are the following: (i) a non-reproducible large-scale variation in intensity of a very low amplitude (~0.2%) which is due to a slight non-uniformity of the shutter speed, and (ii) a mean count rate which is ~3% lower than those of longer exposures, which is due to an inaccuracy of the shutter timing at this setting. These minor effects occur only for the shortest exposure times, and disappear completely for exposure times of 0.3 seconds and longer.
7.3.4 Cosmic Rays
All CCD exposures are affected by cosmic rays. The rate of cosmic ray hits in orbit is very high compared to ground-based observations. The current rate at which pixels are affected by cosmic ray hits is 30.0 (±3.7) pixels per second for the STIS CCD. To allow removal of cosmic rays in post-observation data processing we recommend that whenever possible, given signal-to-noise constraints, you take two or more exposures in any given CCD configuration (see also Section 11.2.2). The greater the number of independent exposures, the more robust is the removal of cosmic rays and for very long integrations it is convenient to split the exposure into more than two separate images to avoid coincident cosmic ray hits. As an example, for two 1200 second exposures, about 1250 CCD pixels will be hit in both images and will therefore be unrecoverable. Moreover, since cosmic ray hits typically affect ~5 pixels per event, these pixels will not be independently placed, but rather will frequently be adjacent to other unrecoverable pixels. In general, we recommend that individual exposures should not exceed ~1000 seconds duration to avoid excessive amounts of uncorrectable cosmic rays in the images. However, observers must balance the benefit of removing cosmic rays against the loss in signal-to-noise that results from the splitting of exposures when in the read noise-limited regime.
In observations of faint sources, particularly for dispersed light exposures, the intrinsic count rates can be very low. The exposure time needed to reach a break-even between the read-out noise and the Poisson noise per pixel associated with the minimal sky background is ~15 minutes for imaging in
50CCD mode, and ~36 minutes for slitless spectroscopy with G750L. With a dark current of 0.009 e–/s it takes 35 minutes of integration for the Poisson statistics on the detector background to equal the read noise. Therefore, repeated short exposures of faint sources can significantly increase the total noise from added readouts. Selecting the correct number and length of repeated integrations requires a consideration of the trade-off between increased read noise and more robust cosmic ray elimination. The STIS Exposure Time Calculators (ETC), or the S/N plots in Chapter 13 and Chapter 14, can help you determine whether your observations are in the read noise dominated regime.
Be sure to take at least two identical CCD exposures in each configuration to allow removal of cosmic rays in post-observation data processing.
7.3.5 Hot Pixels
Hot pixels, caused by radiation damage, occur in the STIS CCD. Dark frames are routinely obtained twice a day in order to maintain a master list of hot pixels and to update the pipeline superdark reference files on a weekly basis. On a monthly time scale, the CCD is raised to ambient temperature, from its normal operating temperature of ~ –83° C, in order to permit annealing of hot pixels.
Analysis of on-orbit data has shown that the annealing process is successful in slowing the growth rate of transient hot pixels (hotter than 0.1 e–/s/pix) each month. Apart from the transient hot pixels, there is a substantial number of hot pixels that stay persistently hot after anneals. In early 2014, ~5% of the pixels of the STIS CCD were persistently hot, and the total number of hot (>0.1 e–/s/pix) pixels immediately after an anneal was ~53,000.
Figure 7.9 illustrates the long-term increase in hot pixel numbers with time. The different symbols indicate numbers of pixels with dark current above each listed threshold immediately after an anneal. The break in the trend near year 2001 reflects the switch to the STIS Side-2 electronics. In this figure, Side-2 darks were scaled to a housing temperature of 18° C, which corresponds to a detector temperature lower than the −83° C set point that was used when the Side-1 electronics were functional. The large scatter seen in data points just before the start of 2010 is due to the fact that STIS had been turned off and on several times during SMOV4. A detailed description of the variation in hot pixel numbers since launch and the differences between the anneal rates while running under Sides 1 and 2 can be found in STIS ISR 2009-01.
While post-pipeline calibration using appropriate STIS reference superdarks allows one to subtract most hot pixels correctly (to within the accuracy set by Poisson statistics), the best way to eliminate all hot pixels is by dithering (making pixel-scale positional offsets between individual exposures). Dithering as a method of data taking is described in detail in Section 11.3. An HST handbook on dither strategies and advantages, together with example data is available on-line at:
7.3.6 CCD Bias Subtraction and Amplifier Non-Linearity
Analysis of CCD images taken during ground calibration and in Cycle 7 has revealed low-level changes in the bias pattern (at the tenths of a DN level) and a low-level amplifier nonlinearity. This non-linearity ("amplifier ringing") was uncovered during the analysis of the overscan region on flat-field images (reported in STIS ISR 1997-09). The bias value of a given row in the serial overscan region of flat-field images is depressed with respect to the nominal bias value by an amount proportional to the mean signal in that row. However, the small proportionality factors and low DN levels at which the nonlinearity occurs render the problem negligible for most STIS scientific applications. Instances of data that may be slightly affected by this problem (at the <1% level) are aperture photometry of faint sources (in imaging mode), especially in the case of a crowded region with nearby bright sources that would cause a local depression of the bias value, and photometry of diffuse extended objects that cover a large number of pixels. The brightest hot pixels (see Section 7.3.5) also cause a measurable local depression in the bias value, but their effect is corrected by using the appropriate superdark reference file (or daily dark file) during CCD calibration.
Observers taking full-frame CCD images obtain both physical overscan (i.e., actual CCD pixels; columns 1–19 and 1016–1062 on the raw image) and virtual overscan (i.e., added electronically to the image; rows 1–20 on the raw image) on their frames; the virtual overscan is not subject to the amplifier nonlinearity problem and can be used to estimate the importance of this effect in the images. Observers using subarrays (e.g., to reduce the time interval between reads and limit the data volume when performing variability observations in the optical; see also Chapter 11) will obtain only the physical overscan.
7.3.7 Charge Transfer Efficiency
Radiation damage at the altitude of the HST orbit causes the charge transfer efficiency (CTE) of the STIS CCD to degrade with time. The effect of imperfect CTE is the loss of signal when charge is transferred through the CCD chip during the readout process. As the nominal read-out amplifier (Amp D) is situated at the top right corner of the STIS CCD, the CTE problem has two possible observational consequences: (1) making objects at lower row numbers (more pixel-to-pixel charge transfers) appear fainter than they would if they were at high row numbers (since this loss is suffered along the parallel clocking direction, it is referred to as parallel CTE loss); and (2) making objects on the left side of the chip appear fainter than on the right side (referred to as serial CTE loss). In the case of the STIS CCD, the serial CTE loss has been found to be negligible for practical purposes. Hence we will only address parallel CTE loss for the STIS CCD in this Handbook.
The current lack of a comprehensive theoretical understanding of CTE effects introduces an uncertainty for STIS photometry. The CTE problems are caused by electron traps in the CCD that are filled as charge passes through the pixels. However, not all traps are accessible to all electrons passing through. Some traps are only accessible if there is significant charge involved. This model suggests that there will not be significant CTE losses in the presence of background, particularly for faint stars, because background electrons fill the traps before the charge associated with such stars passes through. There will still be some loss for brighter stars with background, because their charge may access traps that are unaffected by the background that previously clocked through. Faint stars in areas with little background may suffer from larger losses.
In general, the amount of (parallel) CTE loss depends on the elapsed time on orbit, the distance (i.e., the number of CCD rows) from the source location on the CCD chip to the readout amplifier, the source signal, and the background level.
It should be noted at the outset that the effect of CTE loss has not, as yet, been incorporated into the STIS ETCs. Thus, should you believe the CTE losses described herein may impact your spectroscopic or imaging observing program, you will need to provide longer exposure times in your Cycle 28 Phase
II proposal to compensate for the anticipated losses. In particular, Cycle 28 observers using the STIS CCD to observe faint targets (especially in spectroscopic mode) producing less than a few hundred electrons above a low background, are advised to adjust their exposure times appropriately (within the restrictions of their allocated number of HST orbits).
Analysis of a comprehensive calibration program has allowed us to derive a formula to correct spectroscopic observations of point sources for the parallel-register Charge Transfer Inefficiency (CTI = 1-CTE). This correction has been implemented in the standard calibration pipeline. For spectra at the standard reference position at the CCD center, CTE losses as big as 20% are corrected to within 1% at high signal levels, and to within ~1.5% at low signal levels of ~100 electrons. Further information on CTE loss in spectroscopic mode, including the CTI correction formula, can be found in STIS ISR 2006-03. The correlation of fractional signal loss and the shift of the centroid of the spectrum is demonstrated in STIS ISR 2006-01. For the CCD imaging mode, no correction is available at present in the pipeline, and we refer the reader to Goudfrooij and Kimble’s 2002 HST Calibration Workshop article for the parametrization of the CTE loss, and Goudfrooij et al., PASP, 118, 1455, 2006.
Figure 7.10 depicts the amount of CTE loss suffered as a function of source signal and background level, for spectra taken at epoch 2011.25 with the target at the center of the detector (solid lines) and at the E1 aperture position (dashed lines). Note that the CTE loss can be significant. A typical spectrum with a signal of about 150 e–/pix along the dispersion direction (extracted over the spatial extent of the PSF) and a background level of 5 e–/pix (appropriate for a 1000 second exposure in
G430L mode) is expected to experience a CTE loss of ~34% at epoch 2011.25 when located in the center of the CCD, and a loss of ~10% when placed at the E1 aperture position (discussed below), which is much closer to the readout amplifier. For a background of 1 e–/pix (e.g., a 200 second exposure), a spectrum with the same source signal level would suffer a CTE loss of ~36% if placed at the center of the detector, and ~11% at the E1 aperture position. This emphasizes the need to take CTE losses into account when estimating exposure times needed to accomplish your science goals.
Our discussion thus far has focused on the loss of flux due to charge-transfer inefficiencies, but another effect is also important: trails from cosmic rays and hot pixels that lie between the target and the read-out amplifier (down-stream trails) add noise to the target's spectrum or image. To explore the effects of CTE trails on faint spectra, consider the spectrum plotted in Figure 7.11. It was observed in late 2012 with grating
G430M for a total of 540 seconds using
CR-SPLIT=1. The cosmic rays just above the extraction region produce down-stream CTE trails that get included in the 1D extracted spectrum. For comparison, the same data are processed with the STIS pixel-based CTE-correction and extracted, showing a reduction in the trail contamination. These faint CTE trails represent an important source of noise that is not included in the ETC. For more information on this effect, see STIS ISR 2011-02.
52X*E1apertures; see Section 7.3.8).
The STIS team created a stand-alone pixel-based CTI correction script. As of right now, it can only process non-binned, full-frame data read out with amplifier D and from after SM4. More information and links to installing the script may be found at the Pixel Based CTI page.
7.3.8 Mitigation of CTE Loss for Long-Slit Spectroscopy
Decreasing charge transfer efficiency in the STIS CCD has a detrimental effect on faint spectra acquired at the default location at the center of the chip. For sources with fluxes less than ~1 × 10–16 erg/cm2/s/Å, less than ~100 electrons are accumulated per pixel in exposure times of 1000 seconds or less. (This is the longest integration time we recommend due to the deleterious impact of multiple cosmic rays in a
CR-SPLIT at longer integration times.) At signal levels of 50–100 electrons, 25% or more of the charge can be lost during readout due to charge-transfer inefficiencies. Many STIS science programs have fluxes in this range. For spectra of point sources and compact objects such as galactic nuclei, the full length of the slit is not needed. A target location closer to the read-out amplifier near the end of the slit can decrease the charge lost during parallel transfers by a factor of ~4. One could achieve this offset through the use of offset targets or appropriate
POS-TARG entries on the Phase
II proposal, but these methods are a bit cumbersome and can be prone to error.
Therefore, for first-order spectra we have defined a set of E1 pseudo-apertures that use the same physical long slits available for STIS CCD observations, but have their default target placement near row 900, ~5 arcseconds from the top of the STIS CCD. This is schematically illustrated in Figure 7.12. Observers can use these aperture names to place their targets at this location in a rather transparent fashion.
POS-TARG. These apertures are also recognized by the calibration pipeline software, so spectra are extracted from the correct location using appropriate wavelength solutions, spectral traces, and background regions. For optimum throughput when using these apertures, we recommend using an
ACQ/PEAKexposure to center the target in the aperture when using aperture
52X0.05E1. While use of these apertures will ameliorate CTE losses, we caution observers to carefully assess the potential impact on their science programs due to the decreased spatial coverage and the relative locations of the bars on the slit.
Table 7.5: E1 Aperture Names and Approximate Y Location of the Resulting Spectra.
7.3.9 Pixel-Based CTI Corrections for the STIS CCD
The STIS team at STScI has created stand-alone automated software to apply Charge Transfer Inefficiency (CTI) corrections to STIS CCD data. This software will remove trails and other artifacts caused by CTI effects in the CCD detector, and will help correct target fluxes and positions to their proper values. The software script, called stis_cti, uses a pixel-based correction algorithm, and will correct both images and spectra. The script automatically generates CTI corrected dark reference files, applies CTI corrections to the science data, and outputs the usual CALSTIS products with CTI corrections applied. Currently only the most common observation modes are supported—full-frame, non-binned data, taken with the default CCD amplifier. The script will not correct the signal-to-noise ratio degradation which results from CTI, and hence it is still important for observers to mitigate CTI effects as much as possible during observation. It is available to the community for download and use. Further information can be found at the STIS website under Software Tools.
7.3.10 Ultraviolet Light and the STIS CCD
In the optical, each photon generates a single electron. However, in the NUV, shortward of ~3200 Å there is a finite probability of creating more than one electron per UV photon (see Christensen, O., J. App. Phys. 47, 689, 1976). Users will need to take this into account when calculating signal-to-noise ratios and exposure times for the
G230MB gratings, as described in Section Special Case: Spectroscopic CCD Observations at λ < 2500 Å.
Initial laboratory testing of STIS CCDs showed that excessive illumination by UV light can cause an elevation in residual dark current, due to a surface chemistry effect. However, the actual STIS flight CCD was tested for this effect during ground calibration by the STIS IDT and the effect was found to be much less than previously suspected; this effect is now a concern only for clear (
50CCD) imaging of extremely UV-bright targets. Observations of fields with UV-bright objects should be dithered (i.e., positional offsets applied between readouts) to ensure that the UV tail from bright sources does not cause a residual elevation of the dark current for subsequent science observations. It is also recommended to use the longpass-filtered aperture,
F28X50LP, rather than the
50CCD clear aperture, during target acquisitions (see also Section 8.2.3) when possible. The specific results of the ground testing on the effect of UV overillumination are summarized in Table 7.6. Note that at launch in 1997 the median STIS CCD dark current was about 0.0015 counts/pix/s.
Table 7.6: Effect of CCD UV Overillumination on Elevation of Dark Current.
Initial Dark Current Elevation
Time to Return to Nominal
STIS Instrument Handbook
- • Acknowledgments
- Chapter 1: Introduction
Chapter 2: Special Considerations for Cycle 29
- • 2.1 STIS Repair and Return to Operations
- • 2.2 Summary of STIS Performance Changes Since 2004
- • 2.3 New Capabilities for Cycle 29
- • 2.4 Use of Available-but-Unsupported Capabilities
- • 2.5 Choosing Between COS and STIS
- • 2.6 Scheduling Efficiency and Visit Orbit Limits
- • 2.7 MAMA Scheduling Policies
- • 2.8 Prime and Parallel Observing: MAMA Bright-Object Constraints
- • 2.9 STIS Snapshot Program Policies
- Chapter 3: STIS Capabilities, Design, Operations, and Observations
- Chapter 4: Spectroscopy
- Chapter 5: Imaging
- Chapter 6: Exposure Time Calculations
- Chapter 7: Feasibility and Detector Performance
Chapter 8: Target Acquisition
- • 8.1 Introduction
- • 8.2 STIS Onboard CCD Target Acquisitions - ACQ
- • 8.3 Onboard Target Acquisition Peakups - ACQ PEAK
- • 8.4 Determining Coordinates in the International Celestial Reference System (ICRS) Reference Frame
- • 8.5 Acquisition Examples
- • 8.6 STIS Post-Observation Target Acquisition Analysis
- Chapter 9: Overheads and Orbit-Time Determination
- Chapter 10: Summary and Checklist
- Chapter 11: Data Taking
Chapter 12: Special Uses of STIS
- • 12.1 Slitless First-Order Spectroscopy
- • 12.2 Long-Slit Echelle Spectroscopy
- • 12.3 Time-Resolved Observations
- • 12.4 Observing Too-Bright Objects with STIS
- • 12.5 High Signal-to-Noise Ratio Observations
- • 12.6 Improving the Sampling of the Line Spread Function
- • 12.7 Considerations for Observing Planetary Targets
- • 12.8 Special Considerations for Extended Targets
- • 12.9 Parallel Observing with STIS
- • 12.10 Coronagraphic Spectroscopy
- • 12.11 Coronagraphic Imaging - 50CORON
- • 12.12 Spatial Scans with the STIS CCD
Chapter 13: Spectroscopic Reference Material
- • 13.1 Introduction
- • 13.2 Using the Information in this Chapter
- • First-Order Grating G750L
- • First-Order Grating G750M
- • First-Order Grating G430L
- • First-Order Grating G430M
- • First-Order Grating G230LB
- • Comparison of G230LB and G230L
- • First-Order Grating G230MB
- • Comparison of G230MB and G230M
- • First-Order Grating G230L
- • First-Order Grating G230M
- • First-Order Grating G140L
- • First-Order Grating G140M
- • Echelle Grating E230M
- • Echelle Grating E230H
- • Echelle Grating E140M
- • Echelle Grating E140H
- • PRISM
- • PRISM Wavelength Relationship
- • 52X0.05 Aperture
- • 52X0.05E1 and 52X0.05D1 Pseudo-Apertures
- • 52X0.1 Aperture
- • 52X0.1E1 and 52X0.1D1 Pseudo-Apertures
- • 52X0.2 Aperture
- • 52X0.2E1, 52X0.2E2, and 52X0.2D1 Pseudo-Apertures
- • 52X0.5 Aperture
- • 52X0.5E1, 52X0.5E2, and 52X0.5D1 Pseudo-Apertures
- • 52X2 Aperture
- • 52X2E1, 52X2E2, and 52X2D1 Pseudo-Apertures
- • 52X0.2F1 Aperture
- • 0.2X0.06 Aperture
- • 0.2X0.2 Aperture
- • 0.2X0.09 Aperture
- • 6X0.2 Aperture
- • 0.1X0.03 Aperture
- • FP-SPLIT Slits 0.2X0.06FP(A-E) Apertures
- • FP-SPLIT Slits 0.2X0.2FP(A-E) Apertures
- • 31X0.05ND(A-C) Apertures
- • 0.2X0.05ND Aperture
- • 0.3X0.05ND Aperture
- • F25NDQ Aperture
- 13.5 Spatial Profiles
- 13.6 Line Spread Functions
- • 13.7 Spectral Purity, Order Confusion, and Peculiarities
- • 13.8 MAMA Spectroscopic Bright Object Limits
Chapter 14: Imaging Reference Material
- • 14.1 Introduction
- • 14.2 Using the Information in this Chapter
- 14.3 CCD
- 14.4 NUV-MAMA
- • 25MAMA - FUV-MAMA, Clear
- • 25MAMAD1 - FUV-MAMA Pseudo-Aperture
- • F25ND3 - FUV-MAMA
- • F25ND5 - FUV-MAMA
- • F25NDQ - FUV-MAMA
- • F25QTZ - FUV-MAMA, Longpass
- • F25QTZD1 - FUV-MAMA, Longpass Pseudo-Aperture
- • F25SRF2 - FUV-MAMA, Longpass
- • F25SRF2D1 - FUV-MAMA, Longpass Pseudo-Aperture
- • F25LYA - FUV-MAMA, Lyman-alpha
- • 14.6 Image Mode Geometric Distortion
- • 14.7 Spatial Dependence of the STIS PSF
- • 14.8 MAMA Imaging Bright Object Limits
- Chapter 15: Overview of Pipeline Calibration
- Chapter 16: Accuracies
Chapter 17: Calibration Status and Plans
- • 17.1 Introduction
- • 17.2 Ground Testing and Calibration
- • 17.3 STIS Installation and Verification (SMOV2)
- • 17.4 Cycle 7 Calibration
- • 17.5 Cycle 8 Calibration
- • 17.6 Cycle 9 Calibration
- • 17.7 Cycle 10 Calibration
- • 17.8 Cycle 11 Calibration
- • 17.9 Cycle 12 Calibration
- • 17.10 SM4 and SMOV4 Calibration
- • 17.11 Cycle 17 Calibration Plan
- • 17.12 Cycle 18 Calibration Plan
- • 17.13 Cycle 19 Calibration Plan
- • 17.14 Cycle 20 Calibration Plan
- • 17.15 Cycle 21 Calibration Plan
- • 17.16 Cycle 22 Calibration Plan
- • 17.17 Cycle 23 Calibration Plan
- • 17.18 Cycle 24 Calibration Plan
- • 17.19 Cycle 25 Calibration Plan
- • 17.20 Cycle 26 Calibration Plan
- • 17.21 Cycle 27 Calibration Plan
- • 17.22 Cycle 28 Calibration Plan
- Appendix A: Available-But-Unsupported Spectroscopic Capabilities
- • Glossary