# Step-by-Step ETC Guide for NIRISS SOSS Time-Series Observations of HAT-P-1

**Example Science Program #31 ETC Guide**

A 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.

**On this page**

*Main article: NIRISS Single Object Slitless Spectroscopy, JWST Exposure Time Calculator Overview*

*See also: Video Tutorials*

The JWST Exposure Time Calculator performs signal-to-noise (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 Time-Series Observations of HAT-P-1" Example Science Program, we focus on selecting exposure parameters to detect the exoplanet transit at the desired signal-to-noise 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.

The ETC workbook associated with this Example Science Program is called "#31: NIRISS SOSS Time-Series Observations of HAT-P-1 and can be selected from the **Get a Copy of an Example Science Program** dropdown on the ETC **Workbooks** page. The nomenclature and reported SNR values in this article are based on ETC v. 1.4. There may be subtle differences if using a different version of ETC.

# Define Source and Scene in the ETC

*Main article: JWST ETC Scenes and Sources Overview*

*See also: JWST ETC Defining a New Source, JWST ETC Defining a New Scene, JWST ETC Source Spectral Energy Distribution*

## Define source for "HAT-P-1" Scene

We first defined a source in ETC that emulates the HAT-P-1 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:

"ID" tab - we updated "Source Identity Information" to "HAT-P-1"

"Continuum" tab - we selected the "Phoenix Stellar Models" in the Continuum pull-down menu, and chose a star with spectral type G0V.

"Renorm" tab - we chose the "normalize in bandpass" option, renormalizing the source to a Vega magnitude of K = 8.858 in the Johnson filter.

"Lines" tab - we left this tab empty since we do not add any emission or absorption lines to the spectrum.

"Shape" tab - we kept the default option of point source .

"Offset" tab - we left this tab empty so the source will be at the center of the scene.

## Assign source to "HAT-P-1" Scene

# Select NIRISS SOSS Calculation

*Main article: JWST ETC Creating a New CalculationSee also: JWST Time-Series Observations, NIRISS-Specific Time Series Observations, Noise Sources for Time-Series Observations*

After selecting "SOSS" from the NIRISS pull-down 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 HAT-P-1 (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. Note that the background for a specific date can be entered, so based on the exoplanet's transit period and when these windows are visible by JWST, these dates can be entered into ETC to assess the effects the background would have on the transit precision depth.

# Select Instrument Parameters

*Main Article*: *NIRISS SOSS Recommended StrategiesSee Also: NIRISS Detector Subarrays, NIRISS Detector Readout Patterns, Understanding Exposure Times*

We specify JWST exposures by number of groups and number of integrations. We want to observe a balanced number of groups per integration to maximize both temporal resolution and spectral precision. Previous experience has led the community to sample up the ramp until we reach half the saturation limit. In the context of number of groups for JWST, we will derive the number of groups corresponding to the onset of saturation (NGroups_{sat}) from the Exposure Time Calculator, and choose the number of groups per integration to be NGroups_{sat}/2 (rounding up). We will then choose the number of integrations that fully covers the full transit window.

Calculation #1 represents our initial calculation to determine NGroups_{sat}, where we set the following parameters:

- "Instrument Setup" tab - there is only one option in the pull-down menu in the "Instrument Setup" tab, which is the
(cross-dispersed) grism.**GR700XD** - "Detector Setup" tab -
- subarray is set to
;**SUBSTRIP256** - we chose the
readout pattern.**NISRAPID** - number of "Groups per integration" was set to 2, the minimum value permitted by the ETC, and the number of "Integrations per exposure" and number of "Exposures per specification" were kept at the default values of 1.

- subarray is set to
- "Strategy" tab - we kept the order for spectral extraction at its default value of 1 and left the wavelength of interest to its default value of 1.575 μm.

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 Signal-to-Noise Ratio

Main 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 per integration ramp (NGroups_{sat}/2, rounding up) is 3. We create a calculation with this number of groups, and find that the SNR per pixel of ~413 (Calculation #2). From inputting 3 * Groups *into the Astronomer's Proposal Tool, with the

*and*

*NISRAPID Readout Pattern**, we find that 1 integration corresponds to 21.996 seconds.*

*SUBSTRIP256 Subarray*## Determining Number of Integrations

We plan to observe HAT-P-1 for enough time to allow for sufficient detector settling time (currently estimated to be ~30 minutes; see Noise Sources for Time-Series Observations). We also allow for some margin if the observations do not start exactly when expected or if the eclipse occurs at a slightly different time than predicted. We use the dwell time (T_{dwell}) to calculate this exposure time: T_{dwell} ~ 0.75 hr + MAX(1 hr, T_{14}/2)(before transit) + T_{14 }(eclipse) + MAX(1 hr, T_{14}/2)(after transit) + 1 hr (timing window), where T_{14} is the transit duration.For HAT-P-1, T_{14 }is 2.784 hours, giving us a total exposure time of 6.534 hours. Since each integration ramp for our set-up is 21.996 seconds, we thus need 1069 integrations to cover T_{dwell}.

## Interpreting SNR results

*Main article: JWST ETC Residual Flat Field Errors*

The scientific measurement for an exoplanet transit is the "transit depth", which is a temporal measurement. The spectroscopic result is therefore a relative comparison between a contiguous sequence of time-series measurements – i.e. transit depth over wavelength. It is equivalent to measuring variations in the stellar spectrum over time.

Our goal in this example is to achieve a relative precision of <50 parts per million (ppm) on the transit depth per "spectral bin" or "channel," after subtracting the primary transit from the out-of-transit data. Atmospheric models predict that this should provide a useful signal-to-noise on the exoplanet atmospheric spectroscopic signal (~100-250 ppm). A "spectral bin" or "channel" is a set of pixels across the spectrum that we will combine ("bin") to maximize the temporal precision per spectroscopic channel, without losing the spectral features in which we are interested in measuring. For the case of HAT-P-1, in particular, a spectral bin of 10 pixels (which decreases the NIRISS SOSS resolution from ~700 to ~70), would be enough to resolve the predicted spectral features in the atmosphere of this planet.

If we assume a box-shaped transit, the transit depth precision (*Precision _{depth}*) can be

*approximated*by:

Precision_{depth} \sim Precision_{point} \times \sqrt{1/N_{out} + 1/N_{in}} = \sqrt{1/N_{out} + 1/N_{in}}/SNR_{point} |

where *Precision _{point}* is the photometric precision per data point,

*N*is the number of datapoints (integrations) out-of-transit,

_{out}*N*is the number of datapoints (integrations) in-transit, and

_{in}*SNR*is the SNR in one integration.

_{point}*readout, and*

**NISRAPID***subarray), these times correspond to*

**SUBSTRIP256***N*=614 integrations and

_{out}*N*= 455 integrations. From the ETC, we found

_{in}*SNR*

_{point}= 413 , such that

*Precision*is ~ 0.000150 = 150 ppm, prior to binning. When binning by a factor of 10, our

_{depth}*Precision*lowers by a factor of √10, such that we achieve a precision of 47 ppm.

_{depth}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.

**Note also that the ETC does not fully account for systematic errors that affect the real spectrophotometric precision.**

# Target acquisition

*Main 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 signal-to-noise 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 pull-down menu, shows our initial calculation to determine which parameters to specify for TA:

- "Backgrounds" tab - we entered the coordinates for HAT-P-1 (22:57:46.84 +38:40:30.33) and selected "Medium" for "Background configuration";
- "Instrument Setup" tab - we kept the default selection of "SOSS or AMI Faint" for "Acq Mode" since the target is fainter than M > 6.1 (Vega);
- "Detector Setup" tab - there are no options for the "Subarray", "Integrations" and "Exposures" parameters other than the default values. We left the number of groups to the starting value of 3 and the "Readout Pattern" to
;*NISRAPID* - "Strategy" - the only permissible option for target acquisition is "Aperture centered on source", which for our case is the science target HAT-P-1.

We see that with this set up, we achieve a SNR ~120, which ensures the TA will succeed.

See the Step-by-Step APT guide to complete the proposal preparation for this example science program, where we will input the exposure parameters we derived here.