- 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
Requirements to create a catalog of sources to ingest in the MSA Planning Tool within APT are discussed in detail. Candidate sets are also introduced.
In order to use the MSA Planning Tool (MPT) the user must create a catalog of objects of interest in the field to be observed. Optimal MOS spectral calibration for aperture flux loss will require catalog measurements with high-precision relative astrometry from an existing image. This is highly recommended but not a requirement. The MOS mode observations can be planned using astrometry with accuracies from 5-50mas. High precision spectral calibration needs relative positional accuracy of 15 milli-arcsec or less, which most likely requires space-based observations. Images obtained using HST/ACS or HST/WFC3 UVIS within the past ten years should have this level of accuracy. In some cases, the planning of the NIRSpec spectroscopy will require NIRCam observations, a process that is called NIRCam pre-imaging.
This page describes the process of uploading and filtering catalogs, and defining the appropriate parameters in the Catalogs tab in the MPT:
NIRSpec MPT: Catalogs, Video 1: Ingesting your Catalog
Creating and ingesting a source Catalog
Parent source Catalogs can have as many objects as needed. It is recommended that parent catalogs include all known sources in the field in order to locate contaminants and prevent the MPT from placing them into failed open shutters. The type of catalog (e.g., white space or tab delineated) that is ingested must be selected in the pull-down menu in order to automatically recognize the Target ID, RA and Dec columns.
Parent source Catalogs are ASCII files that must be created with these simple rules in mind:
- Two columns are required for the equatorial celestial coordinates (J2000) RA and Dec for each source. These can be expressed in units of degrees or in hexadecimal format.
- It is useful for at least one column to have the source fluxes or magnitudes (optional field).
- The catalog may optionally contain a line at the top of the file indicating column headers separated by whitespace. The line must begin with a "#".
- Other columns can be included and used by the tool for creating candidate sets if properly identified during ingest (e.g. an optional column of target weights.)
The MPT Catalogs - Examples article presents several examples to guide the user.
There are some checks that should be done before ingesting your source Catalog into MPT. These are key to avoiding problems with MPT planning and downstream data processing.These problems are expected to be fixed in APT 26.2:
- Commas should not be present in the source Catalog. They are not handled correctly when ingesting the Catalog to MPT.
- Make sure that there are no duplicate entries in your source IDs. Different source positions should have a unique ID.
- Make sure there are no NULL entries in the columnar data in the Catalog. MPT may read the Catalog and assign a value of zero to numerical columnar data. This would be particularly problematic for a magnitude column and could result in incorrect results in the derived candidate sets made from the Catalog, for instance. Instead, choose value (real or integer) that can be easily filtered out.
To start, make sure you are in the Catalogs pane of the MSA Planning Tool area of APT as shown in Figure 1. If you have trouble finding this view, you can navigate here by following the steps outlined in the article on the MPT Guide. To upload a catalog, click Import Catalog.
A pop-up window will appear for loading the Catalog. Several formats are allowed for the Catalogs: comma-separated, tab-separated, white-space separated or Virtual Observatory (VO) Table format as shown in Figure 2. Select the appropriate format under File Format. Use the Catalog Name space to give an appropriate name for this Catalog.
During catalog ingest, MPT will attempt to auto-identify the columns if the catalog format has been selected properly. Users should check and correct the auto-assignment, and continue to assign a column type to remaining columns using the pull-down menu located below each column, as shown in Figure 3. Several useful options are available such as Magnitude, Redshift and Source ID number. Other available options are FWHM, R50, Weight, Reference, FluxUncertainty, Number, Stellarity, and Label. Only those columns that have been identified in this way can be used during planning. After ingest, sources can be grouped into sets for potential observation based on filters placed on these catalog columns. Use the pull down menus to select or change the heading type for each column that will be used during planning.
Note: Use the column type Number to label a column you would like to work with in MPT that does not correspond to any other recognizable type listed.
An optional field is the Column for Flux. This is a pull down menu that will list all the columns that were assigned a type of Magnitude. Select the column that will be used for filtering a set a sources. Similarly, the optional field Column for Flux Uncertainty is also a pull down menu that will list columns with the type FluxUncertainty. Select the appropriate column here if you plan to use it for filtering. In the field Flux Units enter the units used; for example ABmag, Vegamag, etc.
Once the Catalog is ingested, selecting or highlighting it will display the data as shown in Figure 4. Note that additional columns are generated (Size, Redshift, Reference, Stellarity, and Weight), even though they may not be in the original Catalog. These columns are not used if not in the original catalog, though they are auto-populated with default values (usually zeros, -1 for Stellarity or 1 for Weight). For the example shown, a total of 794 sources are listed in the catalog.
Scrollbars are present to help navigate the catalog. The Catalog may be sorted (in display mode only) by clicking on any column name. Columns may be reordered by dragging an dropping. The catalog will maintain its initial ordering for making an observation plan.
Weights may optionally be used by the MPT algorithms to create the final plans. In the absence of target weights, MPT will prioritize targets based on the ordering of the sources in the Primary candidate set (which is derived from their order in the Catalog), described below. If some sources in your catalog have a higher priority than others, then it is advisable to create an additional column in the catalog with weights and assign higher values to those sources. When this Catalog is ingested, assign the weight column as a Weight type. If the use of target weights is enabled in the Planner, targets with larger weights are more likely to be observed. In the example presented in Figure 4, the catalog does not have a weight column so MPT assigns the weight 1 to all sources.
Note that if weights are assigned to sources, MPT will use these weights in a linear way when activating the use of weights in the Planner. A source with a weight of 100 will count as much as 100 sources with a weight of 1 when the tool is attempting to optimize the MSA configuration. To further improve planning of weighted targets, it is useful to pre-order your Catalog by weight before ingest. In the future, MPT will do this automatically when planning with weights.
An Astrometric Accuracy in units of milli-arcsec must be specified. If a Catalog comes from, for example, an HST/WFC3/UVIS observation, it is safe to assign the value 10 milli-arcsec. This value is used to estimate the final accuracy of the target acquisition when using the standard TA method. (Note that NIRSpec standard TA parameters do not need to be included in proposals).
The Reference Position Type allows the user to select a fiducial reference point for their observations. All pointings derived by the Planner in the final plan and used to create an observation will be referenced as offsets from this pointing. This information is used to determine appropriate observational plan windows. Three options are available: Catalog Median (default), Fixed Target, or Manual Override. They are described in Table 1. Note that this reference position can be altered or changed during the proposal planning process, but the submitted RA and Dec reference value must be the same between the proposal and the "Flight Ready Update" for accepted MOS programs.
Table 1. Description of the reference position type options
|Reference Position Type||Description|
A median value for both RA and DEC are calculated based on source position in the catalog.
This option is shown as the default Reference Position.
Selecting this option allows the user to select from the list of Fixed Targets in the Targets folder.
|Manual Override||This option allows the user to define any preferred position as their observation reference pointing.|
NIRSpec MSA observations will require the most accurate relative astrometry in order to place sources in the micro shutters. For this reason, the MPT asks for the Pre-image Availability which has the options listed in Table 2. This information is important for pipeline processing and archiving. The reference image will be stored in the archive for later archival observers, or for more detailed program specification after an Aperture Position Angle has been assigned. Also, there could be an associated imaging observation in this spectroscopic program.
Table 2. Description of the pre-imaging availability options
|Is already obtained|
The image was already obtained using a NIRCam observation.
|Will be obtained external to this program|
The image will not be part of this proposal. For example with a new HST proposal, or an upcoming NIRCam observation
in another program.
|Will be done in this program||The user will propose to observe the same field with the JWST instrument NIRCam. In this case, two options are offered: selecting a NIRCam pre-imaging observation from the same proposal, or selecting a NIRCam coordinated parallel image attached to the program.|
For some science programs, an image may not be available and/or isn't required. For example, precise pointing may not be needed for observing extended sources.
Use this option if you just want to experiment with MPT without getting warnings.
Use this option if there exists imaging from an HST program from the past.
Candidate sets are extracted from the supplied source Catalog after the catalog is loaded into MPT. Filters are applied to choose a subset of the target list based on a magnitude range, a type of source (extended vs point-like), or a redshift range, among other possibilities. Several candidate sets can be defined from the parent source Catalog.
Observers should be aware that they need to have all sources of interest in a single parent catalog for a given observation or a set of observations. The candidate lists (Primary Candidate List and Filler Candidate List) are derived from this single catalog. APT will prevent the creation of an observation from plans that were made with different ingested catalogs in the MPT.
NIRSpec MPT: Catalogs, Video 2: Creating Candidate Sets 1
|Creating candidate sets in MPT (old version)|
NIRSpec MPT: Catalogs, Video 3: Creating Candidate Sets 2
By clicking on New Candidate Set (see Figure 4) a new window (Figure 5) is displayed. First insert a Candidate Set Name and begin source filtering by clicking on Add Filter. This button will present you with several options for filtering: Magnitude, Size, Redshift, Weight, Number Column, and Script. Define the appropriate restrictions for the candidate set, and click OK to close this window. Note that the ranges are always inclusive of the numbers entered. Finally, click Make Candidate Set.
MPT's calculations are complex and involve multiple iterations. Large source lists can result in long runtimes. The computations have been parallelized to increase efficiency, but the runtime will depend on your computer. It is advisable to experiment with smaller candidate sets to see how long it takes and then add to them as needed.
Figure 5 demonstrates how to create a candidate set of bright sources from a given catalog. In the example shown, sources with magnitude F814W between 14 mag and 15 mag are selected as members of the candidate set. By clicking on the Make Candidate Set button, the new candidate set is created. As many candidate sets as needed may be created using this procedure.
Source catalogs and candidate sets may be deleted using the Delete button seen in Figure 4.
Do not delete a Catalog if you have Plans in APT that were made with the Catalog. APT will emit a warning to remind you of this. If the warning is ignored and the Catalog is deleted without first deleting the affected Plans, you will not be able to save your APT file.
The Send to Aladdin button helps the user to visualize the spatial distribution of sources. Figure 6 shows an Aladin view of the spatial distribution of sources from two candidate sets. All the Aladin features are available and we refer the user to the Aladin documentation for further information.
Having many planes in the Aladin stack can cause APT to run slowly, even after the popup is closed. To clear out all the layers, users should click Edit > Delete All.
Once the parent source Catalog has been uploaded and the candidate sets have been created, the Planner can be used to specify a plan, as explained in the article NIRSpec MPT - Planner.
Karakla, D. et al. 2014, Proc. SPIE 9149
The NIRSpec MSA Planning Tool for multi-object spectroscopy with JWST
This page has no comments.