Step-by-Step APT Guide for NIRCam WFSS Deep Galaxy Observations
Instructions are providing for filling out the JWST APT observing template for the NIRCam WFSS Deep Galaxy Observations example science program, consisting of NIRCam WFSS observations. The steps below roughly follow those given in NIRCam Wide Field Slitless Spectroscopy APT Template.
Fill Out Proposal Information
Main article: JWST Astronomers Proposal Tool overview
After opening APT, we selected New JWST Proposal under the New Document pull-down menu. On the Proposal Information page, we entered Title, Abstract, and Category of proposal and kept Cycle number at its default value.
Enter proposed target
Main article: APT Targets
This program is targeting SDSS J0100+2802, a z > 6 quasar at RA = 01 00 13.02, Dec = 28 02 25. In Targets, create a new Fixed Target with those coordinates and provide a name J0100+2802 (abbreviated as spaces are not allowed in APT target names).
Main article: APT Observations
In Observations, create a new Observation Folder. Observation 1 will be created automatically. Select NIRCam Wide Field Slitless Spectroscopy as the Template and select the Target defined above.
- Instrument: NIRCAM
- Template: NIRCam Wide Field Slitless Spectroscopy
- Target: J0100+2802
Complete APT Observation Template for NIRCam WFSS observations
Main articles: NIRCam Wide Field Slitless Spectroscopy APT Template
See also: NIRCam WFSS Recommended Strategies
Proceed to the NIRCam Wide Field Slitless Spectroscopy tab (leftmost tab on the lower half of the APT screen). Since a wide observing area is desired (saturation is not a concern for these faint targets), choose Module = ALL and Subarray = FULL to cover a larger field of view. For the Grism (long wavelength), select GRISMR as discussed in the introduction.
- Module: ALL
- Subarray: FULL
- Grism (Long Wavelength): GRISMR
- Primary Dither Type: INTRAMODULEX
- Primary Dithers: 3
- Subpixel Positions: 4-Point
Science (Grism) Exposures
Enter the WFSS exposure parameters determined in our ETC Calculations (Calculation #1). Again note the full WFSS F356W exposure time is divided in 2: the first half with simultaneous F115W imaging and the second with F200W imaging.
|Direct Image||Long Filter||Short Filter||Readout Pattern||Groups||Integrations||ETC Wkbk.Calc ID|
The first column indicates that a single direct image will be obtained after the final WFSS exposure, as required. This program forgoes the option of obtaining an additional direct image after the first set of exposures (F356W GRISMR and F115W imaging).
Direct Image Exposures
Next, enter the direct image exposure parameters determined in our ETC Calculation #2.
|Long Filter||Short Filter||Readout Pattern||Groups||Integrations||ETC Wkbk.Calc ID|
Exposure Sequence Display
Given the inputs above, the display below will automatically populate showing the sequence of exposures. Note that after the direct image, 2 out-of-field images are obtained with the same exposure specifications.
|Sequence||Exposure Type||Long Wavelength||Short Wavelength||Readout Pattern||Groups||Dithers||Total Exposure Time|
|1||Grism & Imaging||GRISMR + F356W||F115W imaging||SHALLOW4||6||12||3736 s|
|2||Grism & Imaging||GRISMR + F356W||F200W imaging||SHALLOW4||6||12||3736 s|
|2||Direct Image||F356W imaging||F200W imaging||SHALLOW4||10||1||526 s|
|2||Out of Field||F356W imaging||F200W imaging||SHALLOW4||10||2||1052 s|
Define mosaic strategy
The above observation sequence will be repeated 4 times in a 2 × 2 mosaic, as described in the introduction. The mosaic tiles will be spread to cover more area and capture more high redshift galaxies surrounding the primary target quasar. But the mosaic tiles will also overlap such that every observation will include the quasar. The desired mosaic coverage is implemented as follows in APT and shown below in Figure 1.
Under the Mosaic Properties tab:
- Rows: 2
- Columns: 2
- Row Overlap %: 45
- Column Overlap %: 72
- Row shift: 0
- Column shift: -1.2° (rotation)
The overlap and shift values can be determined by trial and error after inspecting the results in APT Aladin. The final entry (column shift) makes the final mosaic a bit more symmetric (rectangular) as there are slight asymmetries in the NIRCam Field of View.
Define special requirements
To recenter the target within the mosaicked observations, a small offset of (4", -3.5") in (X, Y) is added via the Special Requirements tab (again determined by trial and error inspecting the output in APT Aladin).
Finally, the Aperture PA Range was restricted to include other targets of interest. Two options are provided: 60–65 degrees and 230–240 degrees.
Run Visit Planner
Main article: APT Visit Planner
To determine the visibility window of our proposed observation and ensure that guide stars can be found, we run the Visit Planner Tool, by clicking the Visit Planner icon in the top toolbar, selecting the observation, and clicking Update Display. The Visit Planner confirms observable windows totaling over 2 months per year.
Note after updating the display, there is no need to run Smart Accounting (the option is grayed out).
View Observations in Aladin
Main article: APT Aladin Viewer
In the top toolbar, click View in Aladin to see the observations oriented on the sky in a new window. Then in that window, click DSS in the top toolbar to see the observations overlaid on images from the Digital Sky Survey.
Note the orientation (rotation) is 62.5 degrees, the middle of the first range of position angles input as an option.