NIRSpec IFU Spectroscopy APT Template
Detailed step-by-step instructions are available for filling out the JWST NIRSpec IFU Spectroscopy APT template.
Main article: NIRSpec IFU Spectroscopy
See also: IFU Roadmap, NIRSpec Bright Spoilers and the IFU Recommended Strategies, NIRSpec IFU and MIRI MRS Observations of Cassiopeia A, NIRSpec IFU and MIRI MRS Observations of SN1987A, NIRSpec IFU and Fixed Slit Observations of Near-Earth Asteroids
The NIRSpec integral field unit (IFU) can obtain spatially resolved imaging spectroscopy of a contiguous, extended 3" × 3" area on the sky. To achieve this, the IFU uses specialized optics to reformat the spatial region and direct light to the spectrograph optics, which it shares with the multi-object spectroscopy (MOS) and fixed slit (FS) observing modes. Additional information is available on the IFU hardware and the IFU observing mode pages.
This article describes the preparation of a NIRSpec IFU observation using the Astronomer's Proposal Tool NIRSpec IFU template.
Step-by-step APT instructions
We assume the observer has already a defined target(s) to be observed, created an observation folder, and loaded the NIRSpec IFU observation template. Instructions for doing this are presented in the JWST Astronomers Proposal Tool.
The IFU template can be divided into four sections, as shown in Figure 1.
- Section 1: This section shows that the NIRSpec IFU spectroscopy template has been selected, along with a target that was previously defined by the user.
- Section 2: The area contains parameters that are for the proposer's information. The observer cannot edit this section.
- Section 3: In this section the observer enters the target acquisition parameters.
- Section 4: In this section the user defines the science paramerers that determine the specifics of the observation.
Section 3 and 4 are part of the 'NIRSpec IFU Spectroscopy' tab. There are three additional tabs: "Mosaic Properties", "Special Requirements", and "Comments", which are discussed at the end of this article.
IFU template section 1: Generic
IFU template section 2: Observation information
The following is included for information only and is generic to all templates. The article APT Observations contains more detailed information on the topics Visit Splitting
*, Duration (secs), and Data volume.
*Bold italics style indicates words that are also parameters or buttons in software tools (like the APT and ETC). Similarly, a bold style represents menu items and panels.
IFU template section 3: Target Acquisition Parameters
For NIRSpec IFU observations there are four options for TA Method, MSA target acquisition (called MSATA), the Wide Aperture Target Acquisition (WATA), VERIFY_ONLY, and NONE. The default option for this template is WATA.
Two of the options, MSATA and WATA, perform a target acquisition sequence of imaging and centroiding to make pointing corrections which will result in the science source centered in the science aperture. WATA centers the TA target in the wide aperture to determine a pointing correction to place the science target in the science aperture. MSATA uses reference stars in the MSA to determine the pointing correction. The remaining two TA Method options, NONE and VERIFY_ONLY, forego target acquisition altogether and rely on the pointing accuracy delivered by the guide star acquisition.
A complete description of the target acquisition procedures used to point the telescope with different JWST NIRSpec observing modes are addressed in the NIRSpec Target Acquisition article.
Main article: NIRSpec Wide Aperture Target Acquisition
Basically, the current implemented TA procedure starts with placing the science target in the S1600A1 aperture, centering it with onboard software. This method requires less planning effort on the part of the observer but is appropriate only for targets that are point sources or close to point sources. Typical suggested coordinate accuracies for the target are in the order of 100 milli-arcsec. Observers can define four TA parameters in the IFU APT template: the Acquisition Target, Subarray type, the Filter, and the Readout Pattern. The options for Subarray are SUB32, SUB2048, and FULL. The options for TA filter are F110W, F140X, and CLEAR. Detailed information on these filters can be found in the article NIRSpec Dispersers and Filters. The available readout patterns are NRSRAPIDD6, and NRSRAPID which define the TA exposure time. Further information on these options can be found in the article NIRSpec Detector Readout Patterns.
Main article: NIRSpec MSA Target Acquisition
When selecting the MSATA option, the target acquisition parameters will be specified at the visit level. MSATA uses reference stars to accurately correct the pointing.
Observers do not need to define reference stars in order to propose for NIRSpec IFU science. That can be deferred until the final program update. The planning parameters will be specified for accepted programs after the MSA-based Target Acquisition is assigned an aperture position angle by the long range planning system. A detailed description of this TA mode is available in the NIRSpec Target Acquisition - MSATA article.
Main article: NIRSpec Verify Only Target Position
The NIRSpec VERIFY_ONLY method relies only on guide star acquisition performed by the Fine Guidance Sensor (FGS) to derive a telescope pointing. This method is suitable for placing extended objects in the field for IFU observations or for very extended targets with the NIRSpec MOS spectroscopy mode. The precision of this method is limited by the JWST observatory pointing accuracy.
When selecting VERIFY_ONLY as the TA Method, Section 3 looks like Figure 3.
VERIFY_ONLY will obtain an image to verify the pointing during post-analysis. The image, obtained with NIRSpec’s imaging mirror, will provide knowledge of the exact pointing so that it can be aligned with other images and/or data of the field. Under the TA Method VERIFY_ONLY, the proposer needs to define a Filter for the Pointing Verification Image. The options are NIRSpec filters F140X, F110W, and CLEAR, as shown in Figure 4. The Readout Pattern options for this verification image are NRS, NRSRAPID, NRSIRS2, and NRSIRS2RAPID, which are described in further detail in the NIRSpec Detector Readout Modes and Patterns article. When selected, the Pointing Verification Image is taken at the end of the visit, after all science spectroscopy exposures are completed.
The number of groups for the Pointing Verification Image should be determined using the NIRSpec ETC in single object target acquisition mode with estimates of the brightnesses of sources within the field.
Like VERIFY_ONLY, selecting NONE as the TA Method relies only on guide star acquisition performed by the Fine Guidance Sensor (FGS) to derive a telescope pointing. Unlike VERIFY_ONLY though, no pointing verification images are taken.
IFU template section 4: Science Parameters
The Science Parameters are defined in section 4 of the IFU Template, as shown in Figure 5. The Science Parameters include the IFU dithering options, and the science exposure specification(s): the spectral configuration used for science, and the detector and exposure configuration options to specify the exposure time.
Dither Parameters and Dither Type
The user needs to define the Dither Type for the IFU observation. Dithering is always recommended for JWST observations. The dither patterns are pre-determined and the available options in the IFU Spectroscopy Template are: NONE, 2-POINT-NOD, 4-POINT-NOD, 2-POINT-DITHER, CYCLING, and SPARSE-CYCLING. These options are in a pull down menu under Dither Type as shown in Figure 6 (Left).
Gratings/Filters and Exposure Configuration
The Exposure Time Calculator (ETC) should be used to determine the best exposure configuration to optimize the SNR of your observation. An exposure is configured by setting the Grating/Filter combination, Readout Pattern, Groups per Integration, and Integrations per exposure.
Users should ultimately use the Exposure Time Calculator for all sensitivity calculations.
Recommendations about exposure parameter selection are given in NIRSpec Detector Recommended Strategies.
An exposure specification is created by using the "Add" button located at the bottom of section 4 of the IFU Template as shown in Figure 5. Each line in this field represents a set of exposures acquired with the defined dither option (e.g., a dither option of NONE will result in one exposure, a 4-POINT dither will result in four exposures). The required exposure parameters are listed in Table 1.
Table 1. Description of Science Parameters for a given exposure specification.
Select a Grating/Filter combination from the pull down menu. The article NIRSpec Dispersers and Filters describes all the available combinations for NIRSpec.
|Readout Pattern||The default value is NRS, but the available values are NRS, NRSRAPID, NRSIRS2, and NRSIRS2RAPID. These patterns are described in full detail in NIRSpec Detector Readout Patterns. Select the pattern that best suits your observation.|
|Groups/Int||The number of groups during an integration, where a group is the product of reading the detectors with a specific readout pattern.|
|Integrations/Exp||This represents the number of Integrations during an exposure, where integration is defined as the time between resets.|
|Leakcal||These IFU leakage calibrations can be acquired to mitigate the effects of excess MSA flux from open shutters or leakage.|
This option is available to automatically add calibration exposures to a science exposure. For the IFU template the only options are NONE or WAVECAL. NONE is the default and is recommended because Autocals can add significant overhead to an observation.
NIRSpec's IFU may be used to obtain data for a region larger than its 3 × 3 arcsec size by creating a mosaic pattern. The use of APT's mosaic tool is described in the article NIRSpec FS and IFU Mosaic APT Guide.
A variety of observatory level special requirements may additionally be specified.
The comments field should be used only to record observing notes. They will become part of the APT file and therefore of the submitted proposal.