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Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 22 > Chapter 6: Exposure Time Calculations > 6.4 Computing Exposure Times

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• The detector background, or dark current, (Bdet) in counts/s/pix, and the read noise (RN) in counts, if using the CCD.We would like to emphasize that, while the ETC can only reflect an average of the dark current rate, the STIS FUV dark current rate in particular exhibits tremendous variations with position on the detector, due to the infamous glow region, and with the time during which the HV has been on. These effects are described in detail in Section 7.5.2, in particular in Figure 7.21 and Figure 7.22. STIS FUV MAMA users whose observations are sensitive to dark current (e.g., faint targets) are strongly encouraged to read the corresponding documentation to assess the feasibility of their observations and better constrain the exposure time needed to achieve the required accuracy.Section 6.5 provides the information you need to determine the sky-plus-detector background for your observation.The signal-to-noise ratio, StoN is given by:

• C = the signal from the astronomical source in counts/s;

• t = the integration time in seconds;

• G = the gain (always 1 for the MAMAs and 1 or 4 for the CCD, depending on your choice of CCDGAIN);

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• RN = the read noise in electrons; = 0 for MAMA observations.For all MAMA observations, and for CCD observations in the regime where read noise is not important, the integration time to reach a signal-to-noise ratio, StoN, is given by:In the optical, each photon generates a single electron (i.e., counts × the gain correspond to the total number of electrons). However, in the NUV, shortward of ~3200 Å, there is a finite probability of creating more than one electron per ultraviolet (UV) photon (see Christensen, O., 1976, J. App. Phys., 47, 689). Theoretically, the quantum yield (Q, or the mean number of electrons generated per photon) is given by the energy of the photon divided by 3.65 eV, and ranges from Q = 1.06 electrons for every UV photon at 3200 Å, to Q = 1.89 electrons for every photon at 1800 Å. The actual electron yield of the STIS CCD has not been measured in the NUV.For observations which are not in the read noise or dark current limited regime, the effective signal-to-noise you should expect to achieve is then ~1/sqrt(Q) times the signal-to-noise ratio calculated directly from the sensitivities given in Chapter 13 ignoring this effect. This effect is negligible at 3000 Å but amounts to 40% at 1800 Å.

Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 22 > Chapter 6: Exposure Time Calculations > 6.4 Computing Exposure Times