ACS Instrument Handbook for Cycle 25
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Advanced Camera for Surveys Instrument Handbook for Cycle 25 > Chapter 10: Imaging Reference Material > 10.2 Using the Information in this Chapter

10.2 Using the Information in this Chapter
10.2.1 Sensitivity Units and Conversions
This chapter contains plots of throughputs for each imaging mode in Section 10.3.1. Section 9.2 explains how to use these throughputs to calculate expected count rates from your source.
The first figure for each imaging mode gives the integrated system throughput, which is the combination of the efficiencies of the detector and of the optical elements in the light path. The throughputs in this handbook are based in part on ground test data, although at the time of writing the handbook, the overall detector efficiency curve and most filter throughputs have been adjusted based on in-flight data. The total system unitless quantum efficiency, i.e. throughput, at any wavelength is defined as the probability that a monochromatic photon incident on the primary mirror produces a detected photo-electron. For the CCD, “counts” is the number of electrons detected. For the MAMA, “counts” is the number of valid photo-electron events processed by the detector electronics after passing through the various pulse-shape and anti-coincidence filters. In both cases, the detected counts obey Poisson statistics. The throughput includes all reflections and transmissions in the optical train (e.g., due to the HST secondary).
To recalculate the throughput with the most recent CCD QE tables in pysynphot, you can create total-system-throughput tables (instrument plus OTA) using the pysynphot. ObsBandpass class.
A bandpass object is created by providing any valid obsmode command string as an argument to pysynphot.ObsBandpass. For example, to evaluate the throughput of the F475W filter and the WFC detector, chip 1, you would use the command:
>>import pysynphot
> bp_F475W = pysynphot.ObsBandpass ("acs, wfc1, f475w")
The resulting throughput table is stored as an attribute of the bp_F475W bandpass object, it is accessed by the command:.
>>throughput_table = bp_F475W.throughput
The ramp filters are not included in this chapter because the passband will change depending on the chosen central wavelength. The width of the passband and available range of central wavelengths for each ramp segment are listed in Table 5.2. The passbands for ramp filters can also be obtained using the pysynphot tools.
10.2.2 Signal-to-Noise
For each imaging mode, plots are provided to estimate the signal-to-noise ratio (S/N) for a representative source, see Section 10.3.1. The first figure shows S/N for point sources (GAIN=1). The second figure shows S/N for uniform extended sources of area 1 arcsecond2.
The different line styles in the S/N figures delineate regions where different sources of noise dominate. A particular source of noise (read noise for example) is presumed to dominate if it contributes more than half the total noise in the observations.
The point- and extended-source S/N figures are shown for average and low sky levels. For point sources, an aperture size of 5 x 5 pixels is used for the WFC, 9 x 9 pixels for HRC, and 15 x 15 pixels for the SBC S/N evaluation. For extended sources, a 1 arcsecond2 aperture is used. For the CCD the read noise is computed assuming a number of readouts NREAD= integer (t / 1000 seconds), where t is the exposure time, with a minimum NREAD=2. That is, each exposure has a minimum CR-SPLIT=2. Different line styles in the figures are used to indicate which source of noise dominates.
To the left of the vertical line in the SBC S/N plots, the count rate from the source exceeds the 50 counts/second/pixel local count rate limit. This is computed from the model PSF, which gives 14% to 22% of the flux in the central pixel.
In situations requiring more detailed calculations (non-stellar spectra, extended sources, other sky background levels, unknown target V magnitude, etc.), the ACS ETC should be used.
Follow these steps to use the signal-to-noise plots:
1.
-
Examine Table 10.1, 10.2, or 10.3 and find ABν for the desired spectral type and filter. Sum the V magnitude of the target and ABν derived from the table.
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Alternatively, compute ABMAG (=V+ABν) from the source flux, using the relation ,
or .
2.
Find the appropriate plot for the filter in question, and locate V+ABν on the horizontal axis. Then read off the signal-to-noise ratio for the desired exposure time, or vice-versa.
The “x” characters at the top of each plot indicate the onset of saturation, in the case of the CCD. For the MAMA detector, the “x” shows where the total number of counts exceeds the 16 bit buffer size of 65,535.
Note that the plots show the S/N as a function of source magnitude for exposure times as short as 0.1 seconds, although the minimum exposure time for the WFC CCD channel is 0.5 seconds.
10.2.3 Point Spread Functions
All information about the PSF are based on the modeled encircled energy data presented in ACS Point Spread Functions in Section 5.6

Advanced Camera for Surveys Instrument Handbook for Cycle 25 > Chapter 10: Imaging Reference Material > 10.2 Using the Information in this Chapter

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