- JWST Cycle 1 Proposal Opportunities
- JWST Cycle 1 Guaranteed Time Observations Call for Proposals
- • JWST Director's Discretionary Early Release Science Call for Proposals
- • JWST Call for Proposals for Cycle 1
- James Webb Space Telescope Call for Proposals for Cycle 1
- •JWST Cycle 1 Proposal Checklist and Resources
- •JWST Cycle 1 Proposal Policies and Funding Support
- JWST Cycle 1 Proposal Categories
- •JWST Cycle 1 Observation Types and Restrictions
- •JWST Cycle 1 Proposal Preparation
- •JWST Cycle 1 Single-Stream Proposal Process
- •JWST Cycle 1 Special Submission Requirements
- •JWST Cycle 1 Observation Mode Restrictions
- •JWST Cycle 1 Proposal Selection Process
- •JWST Cycle 1 Awarded Program Implementation
- •JWST Cycle 1 Proposal Science Categories and Keywords
- JWST General Science Policies
- • JWST Observing Overheads and Time Accounting Policy
- • JWST Duplicate Observations Policy
- • JWST Science Parallel Observation Policies and Guidelines
- • JWST Observing Program Modification Policy
- • Policies for the Telescope Time Review Board
- • JWST Target of Opportunity Program Activation
- NASA-SMD Policies and Guidelines for the Operations of JWST at STScI
- •Policy 1 - Limitations on the Use of Funds for the Research of General Observers and Archival Research
- •Policy 2 - Data Rights and Data Dissemination
- •Policy 3 - Data Requests and Facilities
- •Policy 4 - Post-Launch Commissioning of JWST
- •Policy 5 - Clarification of Extensions of Exclusive Access Data to Public Affairs Activities
- •Policy 6 - Distribution of JWST Science Data Obtained from Investigations Other Than Those Selected Through the Peer-review Process
- •Policy 7 - NASA Needs for Support for Other Missions
- •Policy 8 - Definition of Observing Time
- •Policy 9 - Allocation of Guaranteed Observing Time to Scientists Selected Under AO 01-OSS-05 and Through NASA-ESA-CSA Agreements
- •Policy 10 - Redistribution of Guaranteed Observing Time Among Observers
- •Policy 11 - Protection of Science Programs Associated With Guaranteed Time
- •Policy 12 - Education and Public Outreach
- Methods and Roadmaps
- JWST Imaging
- • JWST Slit Spectroscopy
- • JWST Slitless Spectroscopy
- JWST High-Contrast Imaging
- •Contrast Considerations for JWST High-Contrast Imaging
- •JWST Coronagraphic Observation Planning
- •JWST Coronagraphic Sequences
- •JWST Coronagraphy in ETC
- •JWST High-Contrast Imaging in APT
- •JWST High-Contrast Imaging Inner Working Angle
- •JWST High-Contrast Imaging Optics
- •JWST Small Grid Dither Technique
- •MIRI-Specific Treatment of Limiting Contrast
- •NIRCam-Specific Treatment of Limiting Contrast
- •NIRISS AMI-Specific Treatment of Limiting Contrast
- •Selecting Suitable PSF Reference Stars for JWST High-Contrast Imaging
- JWST Integral Field Spectroscopy
- JWST MOS Spectroscopy
- JWST Time-Series Observations
- •Overview of Time-Series Observation (TSO) Modes
- •Noise Sources for Time-Series Observations
- •Sensitivity of Time-Series Observation Modes
- •Bright limits of Time-Series Observation Modes
- •Preparing Time-Series Observations with JWST
- •Target Acquisition for Time-Series Observations
- •NIRCam-Specific Time-Series Observations
- •NIRISS-Specific Time-Series Observations
- •MIRI-Specific Time-Series Observations
- JWST Moving Target Observations
- •Moving Target Roadmap
- •Field of Regard Considerations for Moving Targets
- •Instrument-Specific Considerations for Moving Targets
- •Moving Target Recommended Strategies
- •JWST Moving Target Observing Procedures
- •JWST Moving Target Calibration and Processing
- •JWST Moving Target Ephemerides
- JWST Moving Targets in APT
- •JWST Moving Targets in ETC
- •JWST Moving Target Useful References and Links
- •Overheads for Moving Targets
- •JWST Moving Target Policies
- NIRSpec IFU and Fixed Slit Observations of Near-Earth Asteroids
- JWST Parallel Observations
- JWST Target of Opportunity Observations
- Observatory Functionality
- • JWST Position Angles, Ranges, and Offsets
- • JWST Instrument Ideal Coordinate Systems
- JWST Background Model
- • JWST Guide Stars
- • JWST Mosaic Overview
- • JWST Dithering Overview
- JWST Duplication Checking
- JWST Observing Overheads and Time Accounting Overview
- •JWST Observing Overheads Summary
- •JWST Slew Times and Overheads
- JWST Instrument Overheads
- Observing Overheads for NIRCam Imaging
- • JWST Data Rate and Data Volume Limits
- Observatory Hardware
- • JWST Observatory Overview
- • JWST Observatory Coordinate System and Field of Regard
- • JWST Field of View
- • JWST Orbit
- JWST Spacecraft Bus
- • JWST Pointing Performance
- • JWST Telescope
- • JWST Wavefront Sensing and Control
- • JWST Momentum Management
- • JWST Integrated Science Instrument Module
- • JWST Solid State Recorder
- • JWST Target Viewing Constraints
- • Fine Guidance Sensor, FGS
- JWST Exposure Time Calculator Overview
- • JWST ETC New User Guide
- JWST ETC Calculations Page Overview
- •JWST ETC Creating a New Calculation
- •JWST ETC Backgrounds
- •JWST ETC Wavelength of Interest/Slice
- •JWST ETC Batch Expansions
- JWST ETC Strategies
- JWST ETC Target Acquisition
- JWST ETC Outputs Overview
- JWST ETC Workbooks Overview
- JWST ETC Pandeia Engine Tutorial
- • JWST ETC Point Spread Functions
- • JWST ETC Instrument Throughputs
- • JWST ETC Residual Flat Field Errors
- • JWST ETC NIRCam Imaging
- Astronomers Proposal Tool
- • JWST Astronomers Proposal Tool Overview
- APT Workflow
- Additional APT Functionality
- Getting Help with APT
- Other Tools
- Mid Infrared Instrument
- • MIRI Overview
- MIRI Observing Modes
- MIRI Instrumentation
- MIRI Operations
- MIRI Target Acquisitions
- MIRI Dithering
- MIRI Mosaics
- •MIRI MRS Simultaneous Imaging
- MIRI Time Series Observations
- MIRI Predicted Performance
- MIRI APT Templates
- MIRI Observing Strategies
- MIRI Example Programs
- •MIRI Coronagraphy of GJ 758 b
- MIRI Imaging, MIRI MRS, and NIRSpec IFU Observations of SN1987A
- •MIRI and NIRCam Coronagraphy of the Beta Pictoris Debris Disk
- •MIRI IFU and NIRSpec Observations of Cas A
- MIRI MRS Spectroscopy of a Late M Star
- MIRI MRS and NIRSpec IFU Observations of Cassiopeia A
- Near Infrared Camera
- • NIRCam Overview
- NIRCam Observing Modes
- NIRCam Instrumentation
- •NIRCam Field of View
- •NIRCam Modules
- •NIRCam Optics
- •NIRCam Dichroics
- •NIRCam Pupil and Filter Wheels
- •NIRCam Filters
- •NIRCam Coronagraphic Occulting Masks and Lyot Stops
- •NIRCam Filters for Coronagraphy
- •NIRCam Grisms
- •NIRCam Weak Lenses
- NIRCam Detectors
- NIRCam Operations
- NIRCam Dithers and Mosaics
- •NIRCam Coronagraphic PSF Estimation
- •NIRCam Coronagraph Astrometric Confirmation Images
- •NIRCam Apertures
- NIRCam Target Acquisition Overview
- NIRCam Predicted Performance
- NIRCam APT Templates
- NIRCam Observing Strategies
- NIRCam Example Programs
- NIRCam Deep Field Imaging with MIRI Imaging Parallels
- NIRCam Imaging and NIRISS WFSS of Galaxies Within Lensing Clusters
- •NIRCam WFSS Deep Galaxy Observations
- •NIRCam and MIRI Coronagraphy of the Beta Pictoris Debris Disk
- •NIRCam Coronagraphy of HR8799 b
- NIRCam Grism Time-Series Observations of GJ 436b
- NIRCam Time-Series Imaging of HAT-P-18 b
- Near Infrared Imager and Slitless Spectrograph
- • NIRISS Overview
- NIRISS Observing Modes
- NIRISS Instrumentation
- NIRISS Operations
- NIRISS Predicted Performance
- NIRISS APT Templates
- NIRISS Observing Strategies
- NIRISS Example Programs
- NIRISS AMI Observations of Extrasolar Planets Around a Host Star
- NIRISS SOSS Time-Series Observations of HAT-P-1
- NIRISS WFSS with NIRCam Parallel Imaging of Galaxies in Lensing Clusters
- Near Infrared Spectrograph
- NIRSpec Overview
- NIRSpec Observing Modes
- NIRSpec Instrumentation
- •NIRSpec Optics
- •NIRSpec Dispersers and Filters
- NIRSpec Detectors
- •NIRSpec Micro-Shutter Assembly
- •NIRSpec Integral Field Unit
- •NIRSpec Fixed Slits
- NIRSpec Operations
- NIRSpec Dithers and Nods
- NIRSpec MOS Operations
- NIRSpec IFU Operations
- •NIRSpec FS Operations
- •NIRSpec BOTS Operations
- NIRSpec Target Acquisition
- NIRSpec Predicted Performance
- NIRSpec APT Templates
- NIRSpec Multi-Object Spectroscopy APT Template
- •NIRSpec MOS Proposal Checklist
- •NIRSpec MSA Planning Tool, MPT
- NIRSpec MPT - Catalogs
- •NIRSpec MPT - Planner
- NIRSpec MPT - Manual Planner
- •NIRSpec MPT - Plans
- •NIRSpec MPT - Parameter Space
- •NIRSpec MSA Spectral Visualization Tool Help
- •NIRSpec Observation Visualization Tool Help
- •NIRSpec IFU Spectroscopy APT Template
- •NIRSpec Fixed Slit Spectroscopy APT Template
- •NIRSpec Bright Object Time-Series APT Template
- •NIRSpec FS and IFU Mosaic APT Guide
- NIRSpec Multi-Object Spectroscopy APT Template
- NIRSpec Observing Strategies
- •NIRSpec Background Recommended Strategies
- •NIRSpec Bright Spoilers and the IFU Recommended Strategies
- •NIRSpec Detector Recommended Strategies
- •NIRSpec Dithering Recommended Strategies
- •NIRSpec MOS Recommended Strategies
- •NIRSpec MSA Leakage Subtraction Recommended Strategies
- •NIRSpec Target Acquisition Recommended Strategies
- NIRSpec Example Programs
- NIRSpec IFU and MIRI MRS Observations of Cassiopeia A
- NIRSpec BOTS Observations of GJ 1214b
- NIRSpec IFU, MIRI Imaging, and MIRI MRS Observations of SN1987A
- NIRSpec IFU and Fixed Slit Observations of Near-Earth Asteroids
- NIRSpec MOS Deep Extragalactic Survey
- •NIRSpec MOS Observations of NGC 346
- •NIRSpec and MIRI IFU Observations of Cas A
- Understanding Data Files
- Obtaining Data
- Data Processing and Calibration Files
- JWST Data Reduction Pipeline
- • Primer and Tutorials
- • Pipeline User's Guide
- • Software Reference Documentation
- Algorithm Documentation
- • Obtaining and Installing Software
The recommended strategies for the JWST NIRSpec MOS mode depend largely on science use case and goals. The emphasis here is on universal tips and tricks to improve observation efficiency, and how to avoid common problems.
Using the MSA Planning Tool (MPT) and the Manual Planner effectively requires some background. The NIRSpec multi-object spectroscopy (MOS) mode is arguably the most complex instrument mode to plan observations for in APT. This article shares hints for specifying MOS observations for the NIRSpec MSA. The strategies are not limited to the MSA Planning Tool, but include the use of the Manual Planner to define observations directly (without the use of MPT). Ultimately, the best strategies to adopt depend to a large extent on the science goals. Some of the more common pitfalls are discussed as well. In addition to these JDox articles, there are training videos, science use case examples, and sample programs for this mode that are provided in APT from the menu item File → JWST Demonstration Proposals. Finally, the JWST Helpdesk is a good resource for problems or questions that are not answered by the documentation.
For step-by-step instructions see NIRSpec MOS Proposal Checklist.
General notes about how MPT operates, and what it produces
MOS planning with the automatic planning tool (MPT) is recommended for most MOS science. The tool makes use of the instrument model to find accurate source positions at the MSA, and it uses the shutter status information to avoid inoperable shutters, to name a few of the issues that affect planning. Using the tool to define your MOS observations is recommended for all but some specialized science cases. MPT can plan observations at a single pointing, or at multiple dithered pointings. With a proper catalog and sufficient source coverage, MPT will derive favorable pointings and matched MSA configurations at those pointings for the user. In this case, the observed sources are also not precisely defined by the user - MPT selects them for the user at the selected pointings. MPT can also be used to create an MSA configuration at a fixed pointing that the user chooses.
There are convenient tools for providing the feasible Aperture Position Angles (APAs) for a given target or pointing for JWST observations. They are the General Target Visibility Tool (GTVT) and the NIRSpec Observation Visibility Tool (NOVT).
Catalogs and candidate lists
All MOS observation planning with MPT must be done using a single parent Catalog. 'Primary' or 'Filler' candidate lists must be derived from the parent Catalog. Planning MOS spectroscopy with MPT is terminology-rich.
Catalog size and field of view
When observing in the MSA and using the MSATA methodology for target acquisition, the Catalog area should minimally cover the MSA footprint at a single pointing. This area is approximately 3' × 3'. Particularly for detailed program updates, the coverage should be large enough to provide the flexibility of planning at any Aperture Position Angle (APA). This is especially true given that the APA will be assigned to most MOS programs. The extra catalog coverage will provide some flexibility to MPT to find preferred pointings where a greater number of sources can be observed at a given APA in a single pointing or over a set of defined dithers. Additionally, it will serve to provide reference stars for the MSATA over the 4 MSA quadrants at different orientations. Reference stars must be defined in the program update, but are not needed at proposal submission.
If you have a Catalog of candidate sources that is smaller than the MSA footprint, and plan to use the high resolution gratings, try to design your plans so that the majority of the sources are in Quad 3 and Quad 4. This helps to ensure that the target spectra will not be cut off by the edge of the detector. You can do this by manipulating the position of the center and the size of the search grid in the MPT Planner.
Weights and their use
If some Catalog sources are preferred over others, put them at the top of the Catalog. Both Primaries and Fillers are added into an MSA configuration in the order they appear in the Catalog, starting from the top. Source weights can also be added to the Catalog and used during planning. The weights should be integer values, and should reflect the relative preference for observing them.
When a user chooses to use target Weights in planning, only the weights of the Primaries are used. The Filler weights are not used.
Maximizing the number of exposures that contain the same sources over a set of dithered positions
Even with preferential ordering in the Fillers list, you may find that few Fillers are repeated at all dithers. Fillers are not tracked during dithering in the way that the Primary sources are. Fillers are added to each MSA configuration independently: they are considered in order starting from the top of the Fillers list and inserted into the MSA configuration whenever possible. (Nods are treated differently for Fillers - Fillers will be present in all nods of a given configuration when they are observed.)
If there are sources that you want to observe through a set of dithers, it is recommended to include them in the Primary candidate list and assign weights according to preference.
We suspect most observers will be interested in maximizing the number of Primary sources in an observation, hence we recommend the Fixed Dithers strategy. That strategy is much more efficient at maximizing the number of Primary sources observed at all dithers. Though the MSA multiplexing (the ability to fill the MSA with targets in one shot) is better using the Flexible dithers strategy, it cannot produce the same success as the Fixed Dither strategy in observing multiple primary targets through a set of dithers.
However, since the Fixed Dither strategy currently does not save partially observed Primary sources (i.e.Primaries that could be observed at some, but not all, dither points) the resulting MSA configurations it produces may not fill the MSA, even with moderate to high source density. When using Fixed Dithers, the multiplexing efficiency in each MSA configuration can be improved by specifying a Filler candidate list. Including the Primary sources near the top of the Fillers list will provide additional observations of Primary sources, but at reduced exposure depth.
If you prefer to keep your Primary and Filler candidate lists separate, add a column to the parent Catalog with a '1' for Primaries and a '0' for Fillers. Upload the Catalog, and then create the Primary and Filler candidate sets by filtering using the added column.
Checking for contamination by other sources in the slit
The Catalog should include not only your candidate targets, but all other sources in the field, so that contamination from unplanned sources can be checked. Contamination checking must be done after a plan has been created in MPT. You can check a planned exposure (in the Plans tab of MPT) by bringing up the MSA Shutter View, and loading the parent Catalog. This will display all additional sources on top of the observed sources with different symbols. Look for slits that have more than one source within the (dark orange) planned slit. These unplanned sources are shown as black dots and plusses. If you find some affected slits, either re-plan after lowering the weight of the target source in the Catalog, or if weights are not used, move these affected sources lower in the Catalog. Alternatively, you can use the MPT's Manual Planner to select alternate targets in the MSA configuration, but that approach is tedious when there are multiple configurations in a plan.
Planning observations using the PRISM and other gratings
When planning to observe with more than one disperser, it is usually best to plan them together in the same MPT Plan to ensure the the same sources are observed with each. A primary reason why one may prefer to create separate plans is to maximize the multiplexing for PRISM observations. PRISM spectra are much shorter and it is possible to observe up to 4 to 5 times more of them at a single pointing (for high catalog density). There are no proven strategies to get a large number of the same sources in independent plans. One way to attempt this is to design the grating plan first, then export the list of targets. Increase the weights of the successful sources in the Catalog, then re-import it, and make two new plans, one for the PRISM (which will use PRISM multiplexing) and one for the grating or gratings you want to observe. The altered imported Catalog must become the new parent Catalog from which all derived plans are generated. This approach will allow for the merging of the final plans in to a single plan. Merge them, then make an Observation from them.
There are few choices for planning high- or medium-resolution grating spectroscopy in conjunction with PRISM spectroscopy:
- Plan the PRISM and grating observations separately to make the most of MSA multiplexing for each. This will likely result in many fewer sources in common in both plans (i.e. fewer sources in BOTH dispersers). The user then has the option of altering the Catalog weights during planning as described above.
- Plan them together so that more of the SAME sources are observed in all dispersers. Add all exposure specifications before generating the plan. Then, you have two choices:
a. Checking the box "multiple sources per row" will result in the use of the PRISM multiplexing and will cause overlapping spectra for the grating exposures.
b. Not checking the box will result in the appropriate GRATING multiplexing that will keep enough separation between the grating spectra, but will generate PRISM exposures with fewer sources.
Follow the prescribed recommendations in NIRSpec Detector Recommended Strategies to determine exposure parameters (Readout Pattern, Groups/Int, Integrations/Exp) that balance exposure overheads and cosmic ray hits. For deep observations - multiple duplicate exposure specifications can be specified in the same plan to obtain the total exposure time needed on sources.
Planning at a fixed pointing
To make a plan at a fixed pointing, make the search grid size 0" by 0" in the automatic MPT Planner.
Dither and Nod options for MOS spectroscopy are described in NIRSpec MOS Dither and Nod Patterns.
Dithering is highly recommended for observing with the MSA. In the automatic MPT, canned dither patterns are NOT offered as they are for other APT templates. Instead, the user specifies a set of fixed dither separations, or constraints on a set of dither separations, and the specific pointings are derived for the user by the MPT. Multiple dithers can be specified, and each will result in a new exposure. Both 'Fixed' and 'Flexible' dither methods are provided in the automatic planner in MPT and can be used for long or short dithers. Fixed dithers requires an integer number of shutters to be specified. Bear in mind that optical distortions cause individual sources to be offset by slightly differing amounts, especially when dithering over large distances (>~ 10 arcseconds). MPT will calculate the individual positions of the sources after a specified dither, and will create a new MSA configuration in order to observe all the primary sources at the new offset position.
A dither of ~ 20" or larger in dispersion (two or more exposures) will provide enough separation to bridge the detector gap, so that combining spectra from the two positions will fill in their respective wavelength gaps.
Short in-slit 'nods' are appropriate for point-like sources, but are not recommended when MSA targets are extended (e.g., when they fill the shutter). Nods are generated by MPT when the user clicks the button of the same name in the Planner. This practice will obtain independent measurements of point-like sources in spectral bands I or II that can be combined to increase S/N. The number of exposures that result will be a multiple (e.g., 3, for 3 nod positions) of the number of specified dithers for each exposure specification (i.e., each grating-filter combination that is specified in the plan). For band III, the PSF is broader than one shutter, so in this case, if nodding is desired, the longer 5-shutter slitlet can be used with nodding at 3 positions in the slitlet. Further, constraining the source centering using the MPT slit margin parameter should help to keep source flux from leaking into nearby shutters.
Dithers and search grid parameter selection
In the MPT Planner, specified dither separations must be smaller than your search grid X (dispersion) extent, or Y (cross-dispersion) extent. Using Flexible Dithers, the specified dithers should be larger than your search grid step size as well. The Fixed Dither methodology will work with dithers smaller than the search grid step size.
Fixed Dithers are recommended for most use cases, especially when the goal is to observe more primary candidates per pointing. In Fixed Dithers, only those primary sources that are observable at all dither positions become members of the observed target set. When using Fixed dithers, consider adding a Filler candidate set to fill in otherwise poorly-utilized areas of the MSA. Ordering the parent Catalog with the most desirable sources at the top will cause the Fillers to have the same ordering. Adding a column of target weights and sorting the catalog by it before uploading it to MPT is a good way to do this. Sources will be considered in that order for each MSA configuration that is generated from the Catalog.
Strategies for examining MPT Plan results
Highlighting targets in the Plans pane will also highlight them in other views ('MSA shutter view' and 'Collapsed shutter view') just as clicking on targets in those views will highlight them in other views.
Adding NIRCam parallels
When adding NIRCam parallels to NIRSpec observations, the NIRSpec observations will typically drive the pointing selection. Dither patterns can be added for the NIRCam parallels to improve sampling in the images. The patterns are described in the article Coordinated Parallel Dither Tables. Some considerations concerning exposure time matching of the parallels and the primary observations are described below.
It is important not to specify any AUTOCALs for the NIRSpec observations as these are incompatible with the parallels that will be added after the NIRSpec planning is completed. AUTOCALs are not recommended for most science programs, with or without parallels.
An example use case, NIRSpec MOS Deep Extragalactic Survey, describes planning NIRSpec MOS from an existing catalog and adding NIRCam parallels for nearby imaging.
Compromise dithers and exposure time matching
There are a few optional dithering choices offered with the addition of the NIRCam coordinated parallels. Two- or three-point "compromise" dither patterns, in three different possible separations each, may be selected via the "Dither Type" parameter in the "Science Parameters" section of the template AFTER the NIRSpec observations are defined. Adding these dithers will double or triple the NIRSpec exposures. Therefor, NIRSpec planning should be done with this in mind. Divide the total exposure time you need by this factor BEFORE planning the NIRSpec observations.
Note that there needs to be an exact match between the number of NIRSpec exposures generated by the plan, and the number of NIRCam parallel exposures.
If you are planning to add NIRCam parallels and wish them to become pre-imaging for follow-up NIRSpec observations, be aware that there are special requirements that should be added to the NIRSpec observations. These are outlined in NIRSpec MOS Operations - Pre-Imaging Using NIRCam.
Crowded fields MOS observing strategies
Note in the Call for Proposals the observing restriction for crowded fields needing MSATA:
NIRSpec observations that require the MSA-based Target Acquisition in fields with a high density of targets (>~1 star per sq. arcsec) or with many bright targets (<ABMag 19.1 at higher density than 1 star per 10 sq. arcsec) are not permitted.
These restrictions are in place because crowded fields beyond these limits have a either: 1) (>~1 star per sq. arcsec) - greater likelihood of failure in the complex MSATA process that uses reference stars to align the pointing, or 2) (<ABMag 19.1 at higher density than 1 star per 10 sq. arcsec), will not work with the MSATA process at all because of too many saturated stars. If feasible in the science use case, observations of crowded fields may be carried out using blind pointing (TA_Method=NONE), which results in greater pointing uncertainty. The restriction limits on executing MSATA in crowded fields will be revisited once experience and characterization of the TA on-sky is gained.
In crowded fields, it may be difficult to have clear, uncontaminated shutters adjacent to the target, as normally used for local background measurements in the 'nod' options. Users may instead find that selecting a single target shutter is preferable, and creating a Master background spectrum for application in the data reduction pipeline will be sufficient. It is possible to select master background shutters in the Manual Planner for each planned exposure or pointing.
Extended source MOS observing strategies
Spatially extended targets of tens of arc seconds to an arc minute or more can be observed using the NIRSpec MOS mode. These observations are accomplished by positioning sources in the left side (quadrant 3 and/or 4 (Q3, Q4)) of the MSA field of view. Positioning these extended targets in Q3 or Q4 affords the best chance of getting complete spectra unaffected by the long wavelength detector cutoff. The MSA planning Field Points in Q4 are offered with TA_Method = NONE, Verify_Only, or the Wide Aperture Target Acquisition (WATA) strategy as an alternative to automatically generating planned observations using the MPT. The process of specifying such an observation directly in the MOS template (without using the MPT) is described in the article MOS Custom Configuration Process. In this example case, a column of NIRSpec MSA shutters can be open in a "longslit" configuration, for example, providing users with a way to acquire spectra across the full cross-dispersion direction on these extended sources in the MOS mode. Two canned longslit configurations are offered in the pull-down for the MSA configuration in the exposure specification. The two canned long slits, or a custom-designed MSA configuration made using the Manual Planner can be used with the corresponding two Q4 Field Points in the Science Aperture selection.
Moving targets MOS observing strategies
Moving targets can pose a challenge for NIRSpec MOS, but they are feasible to observe with special constraints. Particularly, the standard target acquisition process - MSATA - using nearby reference stars will not work, because the reference stars will be moving with respect to the stationary moving target tracking. Instead, moving targets with the NIRSpec MOS may use blind pointing (TA_Method=NONE) or the Wide Aperture Target Acquisition (WATA) strategy if the source is compact with a measurable centroid. The process of planning an observation directly in the MOS template (without using the MPT) can be used for moving targets; this is described in the article MOS Custom Configuration Process.
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