WFPC2 Instrument Handbook for Cycle 10

Dark Backgrounds

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Low dark noise is one of the benefits of MPP, since inverted phase operation suppresses the dominant source of CCD dark noise production (Si-SiO₂ surface states). The remaining source of dark noise, thermal generation in the silicon bulk, is determined by the quality of the silicon used in chip fabrication. The intrinsic dark rate of WFPC2 CCDs is <0.01 e^- pixel^-1 s^-1 at temperatures below -80°C.

Figure 4.5: Average Dark Rates vs. CCD Row.
 

The temperature set-points for the WFPC2 TEC coolers are: -88, -83, -77, -70, -50, -40, -30 and -20 °C. The corresponding approximate median dark rates are given in Table 4.2. For instrument health and safety reasons, GOs cannot command temperature changes.

Sources of Dark Current

The dark current appears to have two components: one from electronic sources in the CCD, and a second component whose strength correlates with the cosmic ray flux. The electronic dark current is ~0.001 e^- s^-1, consistent with the Thermal Vacuum Test data.

The second component of dark current appears only on-orbit, its strength drops towards the edges of each CCD, and it is both chip- and time-dependent. At the current operating temperature, this non-electronic component constitutes up to 80% of the total signal measured in the PC. The fraction and overall level are lower in the other chips, and lowest in WF2. This second component ranges from 0.001 e^- s^-1 (WF2) to 0.005 e^- s^-1 (PC). The edge drop off is shown in Figure 4.5, where the average of lines 200-600 for each chip (with hot pixels rejected) is plotted in e^- s^-1 as a function of column number. The drop near the edge is consistent with luminescence from the CCD windows, shadowed by a field stop mask just in front of the CCD.

Table 4.2: Dark Count Rates.

CCD Temperature (°C)	Dark count rate (e- s-1 pixel-1)
-20	10.0
-30	3.0
-40	1.0
-50	0.3
-70	0.03
-77	0.016
-83	0.008
-88	0.0045

A further indication of the possible origin of this second component is the correlation between its amplitude and the cosmic ray activity in the same exposure, as shown in Figure 4.6. For example, the cosmic ray flux in the PC varies from 7x10⁵ to 13x10⁵ DN per 1000s, while the total dark signal in the PC varies concurrently between 0.0007 and 0.0010 DN s^-1. Similar, though slightly smaller effects are seen in the WFC CCDs. These clues point to cosmic-ray induced scintillation of the MgF₂ field-flattening windows as a likely source of the second dark current component. This might be caused by impurities in the MgF₂ windows; if so, the window of WF2 must contain substantially less impurities. However, other explanations cannot be completely ruled out at this point.

Figure 4.6: Dark Signal vs. Cosmic Ray Flux. Slopes and intercepts ("int") are given on plots. Units are DN/1000s; 1 DN ~ 7 e-.
 

For the great majority of WFPC2 observations, this effect is negligible. In fact, it is noticeable mainly because the true dark rate is very low at the -88°C operating temperature. However, observations for which the dark current is an important limiting factor, either due to noise or background flatness, will require special handling to remove the signature of the dark current properly, as its amplitude depends on the time-variable cosmic ray flux.

Darktime

As of this writing, the "DARKTIME" keyword in the WFPC2 image headers does not reflect correctly the actual time during which the CCD collects dark current. Instead, DARKTIME is merely set equal to EXPTIME (the exposure time) in the data headers, and this value is used for calibration. The error is small, and usually unimportant, but could be significant for programs aimed at measuring the absolute level of the sky background. The actual darktime in seconds is given by

where t is the requested exposure time in seconds, and n is the number of the CCD (PC1=1, WF2=2, etc.), and int() indicates the next lower integer. A duration of 16.4s is required to clear the CCDs before the exposure begins, and 13.6s is needed to read each CCD after the exposure. External exposures of 180s or longer made with the serial clocks off (CLOCKS=NO; the default setting) suffer an additional 60s of darktime (restart=1). This delay is associated with restarting the serial clocks for readout in exposures where the spacecraft AP-17 processor provides shutter control with loss-of-lock checking. Exposures made with the serial clocks on (CLOCKS=YES) avoid this extra 60s (restart=0).

We note that bias frames contain approximately seconds of dark current. No attempt is made to subtract this from the bias images when creating calibration files for use in the calibration pipeline. This effect is unimportant for most observations, but could be significant if one averaged many undithered deep exposures of the same field, or if one is interested in measuring the absolute level of the sky background. If the dark current were constant in time, this could be corrected by merely changing the value of DARKTIME used during calibration. However, the hotpixels vary on monthly timescales, so this simple correction is only partially successful.

The timing of dark calibration frames is slightly different from that of external science exposures. Dark calibration frames always have restart=0 in Equation 4.1.

The dark calibration reference file in the pipeline is revised weekly to track variations in the hot pixels. The current method of generating these files is to combine the bright hot pixels from typically five on-orbit dark frames taken over the space of about one week, with the low-level dark current from the average of 120 on-orbit dark frames spanning a much longer time period. This method gives an optimal combination of low noise and accurate tracking of hot pixels. Care is also taken that the same super-bias reference files is used for both science data and generation of the dark reference file, as this tends to reduce the noise in long exposures. (Early dark reference files used a much simpler method, and were typically combinations of about ten dark frames taken over two weeks.)

Dark Current Evolution

Recent measurements of the dark current in the WFPC2 detectors indicate that the average level of dark current has been slowly increasing over the instrument's lifetime. Baggett et al. (1998) have re-analyzed dark current measurements taken at regular intervals from 1994 to 1998. Over this five-year period, the dark current has increased by a factor of about 2.2 in the WFC CCDs and by a factor of 1.3 in the PC. Figure 4.7 shows values for the central 400 x 400 pixels of each CCD at gain 7. A small increase in the cold junction temperatures over this time period was detected as well; however, the temperature change accounts for only a very small portion of the increase in dark current. The dark current increase is smaller in the optically vignetted regions near the CCD edges, suggesting that some of the effect may be caused by increased fluorescence or scintillation in the CCD windows, rather than by the CCDs themselves.

Since the dark current is generally a minor contributor to the total noise in WFPC2 images, its increase is unlikely to impact adversely the quality of WFPC2 observations, except perhaps in special cases (faint sources observed in AREA mode through narrow-band or UV filters).

We note that the increase in dark signal reported here affects all pixels, and thus is distinct from the cyclic increase in the number of hot pixels. The latter are highly localized, and are almost certainly due to radiation-damaged sites on the CCD detectors. The number and intensity of these hot pixels increases continuously, but are significantly reduced during monthly warmings (decontaminations) of the CCDs. Apparently the decontaminations anneal defects in the CCDswhich produce hot pixels (see section Radiation Damage and Hot Pixels).

Figure 4.7: Dark Evolution from 1994 to 2000.