- 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
- •Field of Regard Considerations for Moving Targets
- •Instrument-Specific Considerations for Moving Targets
- •JWST Moving Target Calibration and Processing
- •JWST Moving Target Ephemerides
- •JWST Moving Target Observing Procedures
- •JWST Moving Target Policies
- JWST Moving Targets in APT
- •JWST Moving Targets in ETC
- •JWST Moving Target Useful References and Links
- •Overheads for Moving Targets
- •Moving Target Recommended Strategies
- JWST Parallel Observations
- • JWST Target of Opportunity Observations
- • General Proposal Planning Workflow
- 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
- Astronomers Proposal Tool
- • JWST Astronomers Proposal Tool Overview
- • APT Proposal Information
- APT Targets
- • APT Observations
- • APT Visit Splitting
- JWST APT Coordinated Parallel Observations
- • JWST APT Pure Parallel Observations
- • APT Target Acquisition
- JWST APT Mosaic Planning
- • APT Special Requirements
- • APT Visit Planner
- • JWST APT Aladin Viewer
- • APT Smart Accounting
- • JWST APT Target Confirmation Charts
- • APT Submitting Your JWST Proposal
- JWST APT Functionality Examples
- • JWST APT Help Features
- • JWST APT Training Examples and Video Tutorials
- 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 and NIRSpec Observations of SN1987A
- •MIRI and NIRCam Coronagraphy of the Debris Disk Archetype around Beta Pictoris
- •MIRI IFU and NIRSpec Observations of Cas 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 Imaging and NIRISS WFSS of Galaxies Within Lensing Clusters
- •NIRCam Coronagraphy of HR8799 b
- •NIRCam Deep Field Imaging
- NIRCam Grism Time-Series Observations of GJ 436b
- NIRCam Time-Series Imaging of HAT-P-18 b
- •NIRCam WFSS Deep Galaxy Observations
- •NIRCam and MIRI Coronagraphy of the Debris Disk Archetype around Beta Pictoris
- 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 WFSS and NIRCam Imaging of Galaxies Within Lensing Clusters
- NIRISS AMI Observations of Extrasolar Planets Around a Host Star
- NIRISS SOSS Time-Series Observations of HAT-P-1
- 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 and MIRI Observations of SN1987A
- •NIRSpec and MIRI IFU Observations of Cas A
- NIRSpec Bright Object Time Series Observations of GJ 1214b
- NIRSpec MOS Deep Extragalactic Survey
- •NIRSpec MOS Observations of NGC 346
- 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
JWST multi-object spectroscopy (MOS) is used for simultaneous spectroscopy of multiple sources in a single exposure. It is offered using the NIRSpec micro-shutter assembly (MSA) with the MOS spectroscopy template in APT.
Main article: NIRSpec Multi-Object Spectroscopy
This article provides a general background on the multi-object spectroscopic (MOS) observing technique as well as JWST-specific MOS information.
About MOS spectroscopy
What is MOS?
MOS is an efficient way to observe the spectra of an aggregate of sources that are within the FoV of an instrument at a single pointing. Most MOS instruments are wide field instruments with fields of view covering several square arcminutes up to a square degree. Typically, the source light exiting the telescope optics is focused onto the aperture plane of an instrument where the light passes through narrow slits or fiber optics and becomes dispersed by a refractive element like a prism or grating. The spectra are then imaged onto a detector. The data undergo rectification, registration, extraction, wavelength and flux calibration, typically using software designed specifically to handle multiplexed spectra.
Over the past 15 years, the demand for astronomical MOS capabilities has expanded significantly. Today, most large 8–10 meter class ground-based observatories offer at least one MOS instrument option. Some employ configurable masks on sources in the FoV. Often, they are fiber-fed to get the light from the sources at different positions in the mask to the dispersive elements of the instrument. Observation planning with these instruments typically involves the preparation of slitmasks which are often milled out on-site about 1 month prior to the observations. Most ground-based MOS instruments operate primarily at optical wavelengths shortward of J Band, except MOSFIRE on Keck, which is the closest ground-based comparison to the JWST NIRSpec Micro-Shutter Assembly (MSA). Additionally, there are large area IFU spectrographs (e.g., MUSE on the VLT), discussed in Introduction to IFU Spectroscopy. In this article, we will limit our discussion to the general properties of more standard MOS instruments.
NIR spectroscopy is particularly well-suited to the study of high-redshift galaxies whose important rest-frame optical diagnostic emission lines are redshifted to the NIR. In galactic investigations, vibrational and rotational molecular lines in the NIR are indicative of the chemical-dynamical structure stars of the Milky Way and can be used to study the stellar radial velocities and abundances. The NIR spectra of young stars provide a means to enhance our understanding of star formation. However, the NIR wavelength regime also presents some challenges. NIR MOS spectroscopy from the ground, particularly from 3 to 5 μm, must contend with the high background from the Earth’s atmosphere. Atmospheric seeing from the ground can vary on the same timescale as the observation.
Ground-based MOS compared with JWST MOS using the NIRSpec MSA
Main article: NIRSpec Micro-Shutter Assembly
The operating range of the JWST NIRSpec MSA is from 0.6 to 5.3 μm. From the ground, NIR spectroscopy is usually limited by the atmospheric absorption and OH (hydroxyl) emission. The MOSFIRE on Keck is the closest ground-based equivalent. It can operate over an extended range from 0.97 to 2.45 μm (into K band) compared to other ground-based MOS instruments (which mostly stop before J band, around 1 μm).
Ground-based instruments have apertures that are either slit masks or use fibers arranged into patterns on the sources in the field. At Keck, the MOSFIRE instrument uses a precisely positionable slit mask that can be configured shortly before observations begin. Fiber-fed spectrographs have fibers that can be configured on source positions automatically at the telescope. The NIRSpec MSA on JWST uses a planning tool to create MSA configurations which are the equivalent of these slit masks.
Below are discussed the differences between ground and space-based MOS spectroscopy related to aperture considerations and angular resolution.
- The angular resolution of ground-based observations depends upon the seeing, which can vary during the exposures. In space, the seeing is not an issue; the angular resolution remains stable and is primarily determined by the instrument optics.
- In ground-based MOS spectroscopy, the slits are precisely positionable. Conversely, the MSA is a fixed grid - MSA sources will not all be well-centered. Theresultisthat slit losses are in general greater than for ground-based MOS spectroscopy. Accurate astrometry and pointing will allow for precise slit-loss correction for point sources.
- A small percentage of MSA shutters have impediments. There are stuck shutters (open and closed type), and shorted rows and columns. The MSA Planning Tool will help to plan around these problematic shutters. The tool uses an MSA shutter operability map that is expected to be monitored and updated frequently (~every 1 to 2 months).
- The MSA suffers from light leakage between the shutter doors and the bars that support the doors. NIRSpec Micro-Shutter Assembly discusses the origin of these leaks in detail. Typically this will not greatly affect target spectra unless there is broad-scale nebular emission in the MSA field of view.
- The MSA shutters are very small - each shutter has an open area of approximately 0.20" × 0.46", surrounded by bars of width ~0.075" on all sides. Slits on ground-based instruments are typically larger, ~1", matched to the seeing conditions. The narrower slit widths in the MSA are afforded by the higher sensitivity of the NIRSpec detectors. These tiny tolerances highlight the need for greater astrometric accuracy for MSA observing, but especially relative astrometric accuracy. Target acquisition will remove the absolute astrometric uncertainty.
- Absolute astrometric correction for space-based operations will require target acquisition, which for NIRSpec MOS is done using reference stars across the MSA field of view at the start of a Visit. Mask alignment strategies are similarly performed for ground-based MOS spectroscopy, but the accuracy requirement is less stringent because the slits are typically larger and the PSF wider.
See Also: NIRSpec MOS Recommended Strategies
Multiplexing is the ability to observe a large number of targets in one exposure, at a given pointing. The multiplexing efficiency varies for MOS instruments, largely because the size of the field of view varies. The FOV of the NIRSpec MSA is smaller than for ground-based instruments, but JWST has high spatial resolution compared to seeing-limited ground-based MOS spectrographs. Since the JWST PSF is smaller, more spectra can be packed into a smaller distance in the cross-dispersion direction. In crowded fields, this provides an advantage over ground-based instruments.
Sensitivity and background
- At 3 to 5 μm, JWST will have a much lower background than ground-based spectrographs, as the thermal background is greatly reduced in space.
- Ground-based instruments are subjected to atmospheric variability. The "seeing" from the ground limits the spatial and spectral resolution that can be achieved. Furthermore, seeing can vary on the same timescale as the observation itself. One component of background is the OH airglow spectrum, which is composed of many atmospheric emission lines in the NIR. Other skylines are present as well. The continuum background is usually measured between these skylines. Space-based spectroscopy in the NIR is not affected by these atmospheric lines. Other types of the background are predominant in space, including zodiacal light and thermal emission from the telescope itself. But these are at a much lower level. The zodiacal emission will vary, but on much larger (seasonal) time scales with the orbital position of the telescope. A description of the background signal components at NIRSpec MOS wavelengths can be found at Components of the JWST Background.
- For JWST, the dark current of the state-of-the-art detectors is low. Except for the PRISM, NIRSpec MSA observations are detector noise limited in low background environments and have high sensitivity in the NIR.
- The ETC can be used to estimate the background and to obtain a good estimate of the expected Signal-to-Noise in the presence of the various background components. The background signal for JWST can reasonably be considered to be fixed for the duration of most observations.
Main article: JWST Position Angles, Ranges, and Offsets
See Also: NIRSpec MOS Observing Process
A number of observing process differences exist between ground-based and JWST MOS observing, including position angle assignment, observation planning iterations, target acquisition and pre-imaging.
- For ground-based MOS observing, the telescope orientation is usually not restricted during the cycle and the observer ultimately chooses a desired aperture position angle (APA), which is fixed only when the slit mask is completed. Because of the orbit of JWST, only certain ranges of telescope orientation and APA are available on any given date. Depending on the ecliptic latitude of a target, there may either be one long period when the target can be observed at a given position angle or two shorter periods during the cycle. Orientation angles are assigned operationally for MSA observations to provide scheduling flexibility on JWST.
- Observers are expected to use the MSA Planning tool to design place-holder visits for proposal submission at a feasible user-selected APA. After APA assignment, detailed planning for program updates occur about 2 months before observations are executed, again using the MSA Planning Tool, but at the assigned aperture position angle. This is also when the most current knowledge of the evolving MSA shutter operability will be available to observers. The NIRSpec MOS Observing Process article describes this process in detail.
- As mentioned above, the most common target acquisition for this mode is done with reference stars, which must be in the correct brightness ranges (19.5–25.7 ABmag in the NIRSpec TA filters). Finding suitable point sources in these ranges may be challenging, and may require prior imaging.
- Pre-imaging will commonly be needed to support the increased astrometric accuracy of both the reference stars and the MSA targets. If pre-imaging is desired, the NIRCam pre-imaging observations must be specified completely at proposal submission. But the complete specification of the follow-up NIRSpec MOS observations, including reference stars, must wait for angle assignment, so there will be a second planning iteration that must happen. Other options for target acquisition in the MOS science template exist, and these are outlined in detail in NIRSpec Target Acquisition.
Main article: NIRSpec MOS Dither and Nod Patterns
Dithering and nodding along with the long (cross-dispersion) axis of the slit during an observation are useful in MOS spectroscopy to place the spectrum of each source onto different areas of the detector for better estimation of source and background signal and removal of detector artifacts. This strategy is particularly useful in ground-based infrared MOS observing, where it helps to obtain accurate source fluxes in the presence of high background. In instruments that have a marginal sampling, this strategy can improve the spatial sampling and can lead to more reliable estimates of the source flux. The terminology of dithers and nods for JWST observations departs a little from the meaning of those terms in ground-based observing, where they can mean the same thing. For JWST, 'dithering' means the telescope is moved to place sources in a different location on the MSA, requiring a reconfiguration of the MSA to observe the same targets. 'Nodding', or movement from one shutter to the next along the slilet in the MSA, does not require a new MSA configuration.
- Nodding is a common practice for all NIR instruments to measure and remove variable sky background.
- Nodding is used for background subtraction, dithering is used for improved wavelength coverage (e.g., to provide measurements across a detector gap).
- Both nodding and dithering can be used to mitigate detector effects and improve data quality.
- Nodding in JWST "slitlets" moves the telescope over small separations (<1") from shutter to shutter; sources remain within the small slitlets. This is shown in Figure 1.
- Nodding distances for ground-based spectroscopy is specified by the user.
- The ground-based seeing-limited PSF requires larger nod offsets for sky background subtraction. Larger nod separations along the slit (>~2" typically) require longer slits and can impact the multiplexing efficiency. Since the slits are often customized to the targets, to perform nodding, the nods can be no larger than the smallest slit length.
In general, MOS spectroscopy planning begins with a catalog of sources whose positions are known with enough accuracy to be able to place sources into slits. Typically, these positions are derived from imaging of the area of interest. When suitably accurate images are not available, the observer will need to obtain one from imaging instruments on the same or other telescopes.
JWST requires high astrometric accuracy catalogs (5–15 mas relative astrometry) to position the very small 0."2 wide shutters accurately onto science sources. Pre-imaging with NIRCam can provide this level of accuracy. Though pre-imaging is not required, t is desirable in many cases. Without this level of accuracy in the Catalog, slit losses, and slit loss errors will result in increased data calibration uncertainties. Users may wish to propose for NIRCam pre-images in the same program as their NIRSpec MOS observations. For more details on pre-imaging with NIRCam, please read NIRSpec MOS Operations - Pre-Imaging Using NIRCam. JWST NIRSpec Observation Visualization Tool describes a tool to help with the planning of NIRCam pre-imaging.
NIRCam parallels can be added to NIRSpec MOS observations. There is a one-to-one mapping between exposures of NIRspec and NIRCam, and there are extra overheads associated with the parallels because the instrument setups happen in series, not in parallel. Read JWST Parallel Observations for more details.
Data calibration considerations
Calibration of space-based and ground-based MOS spectroscopy pose different challenges, particularly in the robust estimation of the background, which is considerably higher and more variable for ground-based observing, and in slit loss correction, which must be done carefully for space-based MOS.
- 3 to 5 μm thermal IR spectroscopy is very difficult from the ground. The background is very high and photometric conditions can vary during the observation, making the slit loss correction more difficult. Conversely, assuming good positional astrometry, and since the PSF is stable (i.e., there is no atmospheric 'seeing'), space-based photometry is more stable and more accurate.
- The background in ground-based instruments is measured between skylines in J and H bands, from measurements made by nodding the target in the slit.
- Background estimation and subtraction in JWST: For point-like sources, the local background is estimated from background shutters in the slitlets, or from a combination of background shutters in nodded exposures. Alternatively, master background regions may be designated with the Manual Planner. Master background shutter spectra are co-added before subtraction from the source spectra. Background removal is described in CALWEBB_SPEC2.
- Aperture flux loss correction (i.e., slit loss correction) is less complicated from the ground for sources that may be moderately resolved in JWST, but are unresolved from the ground. In cases where the structure is resolved, source structure should be modeled for proper removal.
- The accuracy of wavelength calibration (and velocity measurements) depends on slit size, source centering, and the errors involved in calibrating the centering which depends on the pointing accuracy and slit losses. The wavelength calibration for NIRSpec is model-based. The data reduction pipeline wavelength assignment is expected to improve with on-orbit calibration. Wavecals are possible, but not recommended for most observations since they may cause persistence in subsequent spectroscopic observations. Off-centered sources will require a zero-point correction in the data reduction pipeline.
JWST Proposing Considerations
Science Use Cases
Astronomer's Proposal Tool
Exposure Time Calculator
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