A walk through of the JWST ETC for the NIRCam Grism Time Series Science Use Case is provided, demonstrating how to select exposure parameters for this observing program.
Exposure Time Calculator
Main article: Exposure Time Calculator Old
The ETC Scene
We use the JWST ETC to estimate the signal level of GJ 436 and determine the detector readout parameters. First we set up the source and observation into the ETC and determine the signal-to-noise (SNR) in a single integration, and then we will convert this to the SNR over the secondary eclipse observation time.
We open an ETC workbook and create a Scene that emulates GJ 436 with a M2V model Phoenix spectrum and renormalize it to K = 6.1 mag (Johnson). The observatory background is very low for these observations (~ 1 e- / s / pixel in F322W2 + grism and F444W + grism), and we pick an observing strategy that uses backgrounds in the regions 0.8″–1.6″ (13–25 pixels) above and below the target spectrum.
Main article: JWST ETC Creating a New Calculation
The ETC shows that the onset of saturation occurs in some pixels with 9 RAPID groups when using the SUBGRISM64 subarray with Noutputs = 4 and with the F322W2 filter. We chose the RAPID readout pattern with NGroup = 5 to allow significant saturation headroom, and this results in SNR = 180 per spectral pixel per 2.04 s integration at 3.5 µm (see Figure 1). This will allow 1341 integrations during each 0.76 hour (2736 s) secondary eclipse. Using this result and binning to 20 spectral pixels (R ~ 175) results in photon-limited SNR = 29,500 per secondary eclipse. This is reduced to SNR = 20,800 when subtracting the secondary eclipse from the out-of-eclipse data, yielding a photon-limited precision of 48 ppm. Dividing by the in-eclipse stellar spectrum will reduce this further (to ~70 ppm). We wish to achieve ~50 ppm or better, so we plan to observe 3 secondary eclipses.
Similarly, GJ 436 saturates in 17 RAPID groups using the SUBGRIMS64 subarray with Noutputs = 4 with the F444W filter. We chose 10 RAPID groups for some headroom in the observations. This produces SNR = 195 at 4.4 µm in the resultant 3.75 s integration time per spectral pixel (see Figure 1). This improves to SNR = 23,500 when binning 20 spectral pixels (R ~ 220) over the secondary eclipse. This is reduced to SNR = 16,660 when subtracting the secondary eclipse from the out-of-eclipse data, yielding a photon-limited precision of 60 ppm. Dividing by the in-eclipse stellar spectrum will reduce this further (to ~ 85 ppm). We wish to achieve ~50 ppm or better, so we plan to observe 3 secondary eclipses.