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Example Science Program #31 ETC GuideA walk through of the JWST ETC for the NIRISS SOSS Example Science Program is provided, demonstrating how to select exposure parameters for this observing program. 
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Exposure Time Calculator Main article: NIRISS Single Object Slitless Spectroscopy, JWST Exposure Time Calculator Overview The JWST Exposure Time Calculator performs signaltonoise (SNR) calculations for the JWST observing modes. Sources of interest are defined by the user and assigned to scenes which are used by the ETC to run calculations for the requested observing mode. For the "NIRISS SOSS TimeSeries Observations of HATP1" Example Science Program, we focus on selecting exposure parameters to detect the exoplanet transit at the desired signaltonoise ratio (SNR). An accompanying ETC workbook on which this tutorial is based can be downloaded as a sample workbook from the ETC user interface. The optimal exposure specifications (e.g., numbers of groups and integrations) are the input needed for the Astronomer's Proposal Tool (APT) observation template, which is used to specify an observing program and submit proposals.
Define Source and Scene in the ETCMain article: JWST ETC Scenes and Sources Overview Define source for "HATP1" SceneWe first defined a source in ETC that emulates the HATP1 system. After selecting the source, we opened the Sources and Scenes tab and then updated the default source parameters in the "Source Editor" pane as follows:
Assign source to "HATP1" SceneWe highlighted "Scene 1" in the "Select a Scene" pane and then renamed the "Scene Identity Information" entry in the "ID" tab of the "Source Editor" to "HATP1". Since we updated the default source which was assigned to the default scene, we did not need to define a new ETC scene. Select NIRISS SOSS CalculationMain article: JWST ETC Creating a New Calculation After selecting "SOSS" from the NIRISS pulldown menu in the "Calculation" tab (Calculation #1), we specified the background parameters. Since the JWST Background is position dependent, fully specifying background parameters are important. We entered the coordinates for HATP1 (22:57:46.84 +38:40:30.33) in the "Background" tab, and selected "Medium" for "Background configuration," which corresponds to the 50th percentile of the sky background. Select Instrument ParametersMain Article: NIRISS SOSS Recommended Strategies
Calculation 1 represents our initial calculation to determine NGroups_{sat}, where we set the following parameters:
After selecting the "calculate" button to perform the calculation with these parameters, we see that the observation does not suffer from saturation, i.e., there is a green checkmark next to Calculation 1 in the "Calculations" tab and no warnings or errors are reported in the "Reports" pane. This pane also reports that the number of groups prior to saturation (NGroups_{sat}  1) as 4. The reported SNR per pixel is ~290. Adjust Exposure Parameters to Obtain Desired SignaltoNoise RatioMain Articles: JWST ETC Batch Expansions, JWST ETC Reports As noted above, the Reports pane tells us that the onset of saturation thus occurs at NGroups_{sat} = 5. Our optimal number of groups (NGroups_{sat}/2, rounding up) is 3. We create a calculation with this number of groups, and find that the exposure time is 22.0s, for a SNR per pixel of ~413 (Calculation #2). To fully cover the transit window of 9.352 hours (33667.199 s), we thus need 1530 integrations. Interpreting SNR resultsMain article: JWST ETC Residual Flat Field Errors To estimate the SNR for the desired exposure setup that covers the transit window, we use the Poissonian approximation: we multiply the SNR results above for Number of Groups = 3 and Number of Integrations = 1 by the square root of the increase in exposure time. In NISRAPID mode, there is 1 frame per group, so the exposure time for 1530 integrations increases by a factor of 1530, and the SNR increases by √1530. The SNR for the full transit window is thus 413 × √1530 ≈ 16000. Because we are making a relative measurement, we are comparing the "before/after" window with the window during the transit. The accuracy of the transit depth is defined as SNR_{transit} = SNR_{total} / √2 = 16000 / √2 ≈ 11300. This result implies a relative precision on the transit depth of 1/11300 = 89 ppm. Because the spectroscopic features are nominally between 100–250ppm, we want to increase the precision on the time series by binning pixels. We will bin the spectrum by 10 pixels, which increases the temporal precision by √10, which results in a precision of 28 ppm. This precision is high enough to measure the average exoplanetary atmosphere beyond the 3σ level. Note that the ETC includes an error term for residual flat field errors which affects long exposures. For exposures longer than ~10,000s, ETC calculations have a "noise floor" above which an increase in exposure time no longer results in an increase in SNR that scales with the square root of the exposure time. Since we are making relative measurements on the same pixels for exoplanet transit spectroscopy, our precision is not affected by the "noise floor" imposed by the residual flat field errors. Thus, using the Poissonian approximation above provides a better estimate of the SNR using the ETC reported results for 1530 integrations 3 groups. Target acquisitionMain articles: NIRISS Target Acquisition, JWST ETC NIRISS Target Acquisition A target acquisition (TA) must be performed when using a SOSS subarray so that the target is precisely positioned on the detector. A signaltonoise ratio (SNR) ≥ 30 is recommended to achieve a successful TA, which achieves a centroid accuracy of ≤ 0.15 pixel. Increasing the SNR to 100 improves the centroiding accuracy up to ≤ 0.05 pixel. If the TA fails, the observation will not be performed. Only one integration and one exposure is allowed for a TA. The acquisition mode is either SOSSFAINT (for objects between 6.1 < M < 14.5, Vega mag) or SOSSBRIGHT (for objects between 3 < M < 6.1, Vega mag). Calculation #3, where we selected "Target Acquisition" under the NIRISS pulldown menu, shows our initial calculation to determine which parameters to specify for TA:
We see that with this set up, we achieve a SNR ~120, which ensures the TA will succeed.

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