NIRISS Aperture Masking Interferometry APT Template
Instructions for filling out the JWST NIRISS aperture masking interferometry APT template, using the Astronomers' Proposal Tool (APT), are provided in this article.
Aperture masking interferometry (AMI) is one of the 4 observing modes for the Near Infrared Imager and Slitless Spectrograph (NIRISS). The AMI mode uses a non-redundant mask (NRM) in the pupil wheel of NIRISS. It has 7 "holes" (apertures) that produce an interferogram in the image plane, and samples 21 unique ("non-redundant") baselines. AMI provides the highest effective angular resolution of any instrument mode on JWST, enabling the detection of planetary or stellar companions at a distance of ~70–400 mas from their host stars. This mode also enables high resolution mapping of extended sources through near-infrared aperture synthesis.
The NRM is used in conjunction with one of 3 medium band filters (F380M, F430M, F480M) or a wide band filter (F277W) in the filter wheel (FW). A typical observation with AMI will include a target acquisition (TA) image, which is required if the science exposures use a subarray, followed by several exposures with the NRM in the PW with one of the 4 allowed filters in the FW, and possibly a direct image to help associate features in the NRM images with morphological features of the target. Direct images may help constrain or stabilize image reconstruction methods applied to extended object NRM data. Direct images can also be used on fainter multiple point source targets, especially when recently-developed “kernel phase” data analyses are used.
NRM data analysis of a target observation requires one or more PSF reference stars. The PSF reference is used to calibrate out the instrumental contribution to closure phases and visibility amplitudes. To minimize the impact of detector effects, the PSF reference star should be observed with the same dither pattern, especially for more demanding observations. It is likely that lower contrast targets may not need dedicated PSF reference stars, but could be calibrated with PSF reference data taken by other programs. Ideally, for higher contrast needs, target and reference observations should be scheduled close in time, so that the telescope is in a similar state, thermal or otherwise, for all the observations. In this case, the science target(s) and PSF reference star(s) should be observed using the same telescope optical configuration, so no wavefront correction should occur between any of the observations. We recommend specifiying "GROUP NON-INTERRUPTIBLE" or "SEQUENCE NON-INTERRUPTIBLE" in the timing special requirements window in APT. The APT requires justification if an observer does not request any reference star observation.
Step-by-step APT instructions are provided below.
Words in bold are GUI menus/
panels or data software packages;
bold italics are buttons in GUI
tools or package parameters.
NIRISS Aperture Masking Interferometry tab
Target acquisition parameters
Target acquisition (TA) places the centroid of the brightest object in the TA field of view on the location of the AMI aperture used for the science exposure. An observer can specify one of the 3 options for Acq Target: NONE, Same Target as Observation, or any source in the target list whose position is within 30"–80" of the science target (where the maximum distance depends on Galactic latitude). If a subarray is chosen for the science observation, a TA must be performed. TA is performed with the F480M filter in the filter wheel.
There are 2 options for Acq Mode, based on the M-band magnitude of the target which is specified in the AMI Template Parameters article: AMIBRIGHT and AMIFAINT.
Acq Exposure Time
See also: NIRISS Detector Readout Patterns
The only permitted Acq Readout Pattern for AMIBRIGHT is NISRAPID. Both NIS and NISRAPID are available readout patterns when the Acq Mode is AMIFAINT. The observer can specify the Acq Groups/Int (3, 5, 7, 9, 11, 13, 15, 17, 19), where Acq Groups/Int is defined by the number of frames in an integration (for NISRAPID) or by the number of frames in an integration divided by 4 (for NIS).
The ETC workbook identification number used to determine the exposure parameters for the TA can be entered in the ETC Wkbk. Calc ID field. Though this input is optional, it is strongly recommended to provide this information so the TA can be assessed during technical reviews to ensure the observation can be executed correctly.
Specify numer of dithers:
Primary Dithers: NONE, 2, 3, 4
Subpixel Positions: NONE, 5, 9, 25
See also: NIRISS Detector Subarrays
Allowed options for Subarray are FULL and SUB80. Observations of bright and compact targets can make use of an 80 × 80 subarray (SUB80). Target acquisition is required if observing with a subarray. See the NIRISS AMI article for the limiting Vega magnitudes accessible with the SUB80 and FULL subarrays for the various filters.
To set up a science observation or PSF reference star observation, Add an observation to include it in the Filters dialog box. Select the Filter for the observation, where allowed options are F277W, F380M, F430M, F480M.
The only supported Readout Pattern for the SUB80 array is NISRAPID. For the FULL array both NIS and NISRAPID readout patterns are supported. Specify:
Groups/Int: the number of groups during an integration, equal to the number of frames read per integration (for the SUB80 array that uses the NISRAPID readout pattern). Up to 800 groups are supported for this mode.
Integrations/Exp: the number of integrations during an exposure, where an integration is the time between detector resets.
- ETC Wkbk. Calc ID: the accompanying ETC workbook ID number for the calculation (optional).
Exposures can be Added, Duplicated, Inserted Above existing exposures, and Removed.
Direct Imaging Parameters
Specify True or False depending on whether a direct image is to be taken in the observation.
If True is selected, then specify:
Image Dithers: refers to primary image dithers. Options are NONE, 2, 3, 4
ETC Wkbk. Calc ID
The direct image will be performed with the same filter as the corresponding NRM image specified in AMI Parameters.
Note: the Exposure Time Calculator mode for AMI does not include calculations for direct imaging. To run calculations for direct imaging to determine Groups/Int and Integrations/Exp, use the NIRISS imaging mode in ETC.
PSF Reference Observations
This is a PSF Reference Observation
If this observation is the PSF reference star, then the This is a PSF Reference Observation box must be checked, in the PSF Reference Observations panel at the bottom of the page. Note that PSF reference star observations have a 0 month exclusive access period.
PSF reference observations
If PSF reference observations have already been specified, then one or more of those observation(s) can be selected in the PSF Reference Observations dialog box. The PSF reference observations must be observed with the same Filter and Subarray as the science target to show up in this dialog box.
If a PSF reference observation is not deemed to be required for the current observation, then the Additional Justification box must be checked. In that case, the absence of PSF Reference Observations must be scientifically justified in the PDF attachment of the proposal.
Verify your observation set-up
Create Target Confirmation Charts to verify that the input target coordinates will position the telescope in the correct place.
Run APT Visit Planner to check schedulability of observations, check constraints, and see whether guide stars are available to support the observation. Then run APT Smart Accounting to update time accounting and to remove excess overhead charges. APT can generate various reports through the "Reports" option in the Visit Planner view. Observers can access additional reports through the File → Export option in the top menu bar. For example the ".times" file provides a breakdown of individual exposures and associated exposure times, including overhead. These reports may help observers to tweak their observations to increase efficiency.
Observers can also visualize their observations on the celestial sphere using the APT Aladin Viewer.
See also: APT Special Requirements
Target and reference star observations can be temporally grouped by using the Timing → Group/Sequence Observations Link option in the Special Requirements dialog box under the Special Requirements tab. We recommend specifying parameters for "Group non-interruptible" or "Sequence non-interruptible" in the dialog box.
Extended object imaging may need observations at more than one position angle in order to fill in gaps in uv-plane coverage, which can be achieved by invoking the Position Angle option in the Special Requirements dialog box under the Special Requirement tab.