JWST Parallel Observations

Some capabilities to use more than one science instrument simultaneously (in parallel) will be available for JWST Cycle 4. Additional instrument combinations may be offered in future cycles.

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See also: JWST Coordinated Parallels RoadmapJWST Coordinated Parallels Custom Dithers

Parallel observing refers to simultaneously operating more than a single science instrument, each viewing a different area of the JWST focal plane.  For JWST, there will be 2 basic modes of parallel operations: coordinated parallels and pure parallels

Coordinated parallel observations are planned as part of a primary program, and are intended to amplify or supplement the primary science proposed in a given proposal. That is, the primary and parallel observations are planned together in a single program to accomplish the science goals, and hence are under the purview of a given proposal PI and science team. 

Pure parallel observations are from programs that make use of parallel observing slots derived from other accepted proposals. Hence, pure parallel programs are separate proposals, have separate PIs, and are selected independently from any primary programs they may be attached to. Several pure parallel slots have to be used for calibration observations, but there typically are several openings for pure parallel science observations as well.

There are a number of subtleties related to each of these modes of operation. For example, pure parallel observations are not permitted to impact or change the primary observations to which they are attached (with one exception described below), whereas coordinated parallel observations can be tailored to accommodate both the primary and parallel datasets since they are specified within a given proposal. (For example, dither patterns that work well with both instruments can be selected.) These subtleties are described below. 

The goal of enabling parallel observing is to enhance the efficiency and science return of the JWST mission.  However, users need to be aware that there are tradeoffs that need to be balanced. Not every potential parallel observing slot can be used for science.  One example is the limited data downlink capability available to the observatory.  For example, running NIRCam by itself in certain readout modes for several hours can use the entire data volume downlink capacity for a single contact period, leaving no room for storing parallel data taken during that period. Another consideration (for pure parallels) is that many calibration activities need to use pure parallel observing slots, and parallel calibration activities may take precedence over pure parallel science.  

Only certain modes and combinations of instruments will be allowed for cycle 4 proposals (see below).  Additional combinations may be made available in future observing cycles.



Principles in the use of parallel observing with JWST

See also: JWST Science Parallel Observation Policies and Guidelines

A detailed description of the policies related to JWST parallel observing is available. In summary, there are 3 principles that govern the policies for proposing and planning parallel observations:

  1. For coordinated parallels, the science goals of the parallel observations must be tightly linked to the science goals of the overall program. In other words, accomplishing the main goals of the proposal must require parallel observations. Coordinated parallels whose goal is to address ancillary topics will generally not be approved.

  2. Pure parallel observations may not impact the primary observations they are attached to. This means pure parallel exposures must fit under the resource footprint (exposure plus overheads) of the primary exposure to which they are attached.

  3. The needs of the JWST calibration program, a large fraction of which takes place in parallel mode, take precedence over pure parallel science programs.


 As a practical matter, adding pure parallels will add a small additional overhead for setting up the instruments. This will be handled by the scheduling system and will not be assessed post-facto as an overhead on the primary observations. Further discussion of policies can be found in the Call for Proposals.



Coordinated parallels 

See also: APT Coordinated Parallel ObservationsJWST Position Angles, Ranges, and Offsets, JWST Background ModelJWST Data Volume and Data ExcessJWST General Target Visibility Tool Help

Coordinated parallel observations are crafted within the APT template used for the primary instrument mode. Eight template combinations are supported for Cycle 4, as shown in Table 1.


Table 1. Template combinations supported for cycle 2 coordinated parallel observations

Ref. no.First (Primary) templateSecond (Parallel) templateComments
1

NIRCam imaging1

MIRI imaging1

Either template can be selected as primary, with the other as parallel.
2NIRCam imaging1NIRISS WFSSEither template can be selected as primary, with the other as parallel.
3MIRI imagingNIRISS WFSSEither template can be selected as primary, with the other as parallel.
4NIRCam imaging1NIRISS imagingNIRCam must be primary. Use to increase areal coverage, but note NIRISS differences in pixel size and available filters.
5NIRSpec MOSNIRCam imagingNIRSpec MOS must be primary.
6NIRCam WFSSMIRI ImagingNIRCam WFSS must be primary.
7NIRCam WFSSNIRISS ImagingNIRCam WFSS must be primary.
8NIRSpec MOSMIRI ImagingNIRSpec MOS must be primary.


Only direct imaging with standard narrow-, medium-, or broadband filters is allowed for NIRCam and MIRI observations in these coordinated parallel modes. 

Instrument teams have worked with developers to provide several ways of scheduling joint observations in parallel, for instance, to designate one instrument as the primary, as shown in options 1–3 in Table 1. 

One anticipated use case is to use both instruments at one epoch to observe adjacent areas of the sky, and to return at a second epoch when the instrument fields of view have rotated 180° on the sky. Users should obviously investigate the availability of the relevant position angles using the JWST target visibility tools since not all positions on the sky have the needed flexibility in available position angles to accommodate this strategy. Users should also be aware that background levels due to zodiacal emission and thermal emission from the telescope will change between two observations at different position angles. However, other science cases may not require such a "180° strategy" and can simply obtain observations (e.g., with NIRISS WFSS) of a nearby areal region to accompany NIRCam or MIRI primary imaging observations.

All dither patterns available for a given instrument template will also be available when it is selected as the primary instrument in coordinated parallel mode. However, you also have the option to select from sets of customized dither patterns that have been specifically designed to produce good results for both instruments simultaneously. The number and type(s) of customized dither patterns that are available depend on the specific prime+parallel instrument mode combination. When a parallel instrument is selected, these additional dither patterns will become available in the dither pull-down menu in the relevant APT template.

Issues regarding data volume per downlink period should also be considered, especially for options involving NIRCam. Since NIRCam observations involve up to 10 detectors (8 short wavelength and 2 long wavelength), proposers of coordinated parallel programs may need to consider selecting readout patterns that are less data intensive than they might otherwise choose. (Some of the most data intensive readout patterns for NIRCam are disallowed by APT in parallel mode.) Alternatively, depending on the science use case, a user may decide that areal coverage is less important than the parallel coverage and may opt to use only one of the two NIRCam Fields of View. APT will compute and display the data volume and data rate for each exposure, and you can adjust the detector readout pattern and/or the number of modules being read out as needed to stay within the allowed limits.

A number of additional coordinated parallel options are being considered for future cycles, including the possibility of using up to 3 instruments simultaneously. 



Pure parallels

See also: APT Pure Parallel Observations

Unlike coordinated parallels, pure parallel observations are proposed as entirely separate programs of investigation. Pure parallels use parallel observing "slots" created by exposures from other accepted programs that do not already have parallel observations specified. Pure parallel observations will not be allowed to influence the dither patterns or other aspects of the observing strategy of the primary observations to which they are attached, since the primary observations will belong to different science proposals.

In Cycle 4, the following 5 observing modes can be requested for pure parallel observations:

  1. MIRI imaging
  2. NIRCam imaging
  3. NIRCam wide field slitless spectroscopy (WFSS)
  4. NIRISS imaging
  5. NIRISS WFSS

Not all observing templates will be allowed to have pure parallel observations attached. This is for a variety of technical reasons or concerns about how a pure parallel could potentially impact the data quality of the primary observation. Any of these 5 pure parallel instrument modes can be used in combination with any of the 10 models listed next.

Templates that are allowed to have pure parallels attached are the following:

  1. MIRI imaging
  2. MIRI LRS (only if Subarray = FULL)
  3. MIRI MRS
  4. NIRCam imaging
  5. NIRCam WFSS
  6. NIRISS imaging
  7. NIRISS WFSS
  8. NIRSpec fixed slits
  9. NIRSpec IFU
  10. NIRSpec MOS

Templates that are not allowed to have pure parallels attached are the following:

  1. NIRCam time series
  2. NIRCam grism time series
  3. NIRCam coronagraphy
  4. NIRSpec bright object time series
  5. NIRISS AMI
  6. NIRISS SOSS
  7. MIRI coronagraphy
  8. MIRI LRS (if Subarray = SLITLESSPRISM)

The NIRCam WFSS and NIRISS WFSS modes require direct imaging exposures before and/or after the dispersed grism spectral exposure to obtain images of the undispersed field. Hence, to obtain such a set of exposures in a pure parallel mode, appropriate double or triple slots will need to be identified to attach these observations. An example of such double or triple slots created by a primary visit is MIRI (or NIRCam or NIRISS) imaging of a given target field using multiple filters (or multiple sets of filters in the case of NIRCam).

Pure parallels FAQ 

  1. What is a pure parallel observing "slot?" 
    A parallel slot corresponds to a single exposure of a prime program (i.e., single dither position). A slot includes instrumental overheads, however mechanism moves are not included in the parallel slot, and the slot is not constrained by them. 

  2. Can a pure parallel slot be assigned to more than one program?
    No; based on the specifications listed in the proposal, STScI will assign the pure parallel program to a prime slot. This is a one-to-one assignment, with no additional program being attached.

  3. How are visits from prime programs used in pure parallel programs?
    The main "scheduling units" of the prime program are visits. Within a visit, each slot corresponds to a single exposure, i.e., a single dither position. If a pure parallel program selects 3-slots, thus creating a slot group, made up of a 3-point dither in one visit prime observation, APT will automatically create a 3-exposure one visit pure parallel observation. 

  4. How do instrument configuration changes (i.e., filters/grisms) work for pure parallels? 
    Pure parallel observations are constrained by the number of mechanisms reconfigurations performed by the primary program. Parallel programs may not affect prime observations. Parallel programs may change mechanisms only if those changes are synchronized with mechanism moves in the primary program. In particular, it is currently not possible to change the mechanisms of the parallel instrument while the observatory is slewing between dithers. STScI is exploring whether it is possible to modify JWST's operating system to enable more flexibility.

  5. Could you give a practical example of how mechanisms changes work?
    If a prime program has a visit with the following characteristics: 3 filters, each of them using a 4-point dither pattern on the same target, with a 500 s exposure per dither, for a pure parallel program, this will translate to:
    1. Twelve parallel slots of about 500 s duration each. Three of these slots correspond to the first dither position per filter.
    2. A pure parallel program could therefore use 3 different optical element setups following the same 4-point dither pattern used by the prime. 
    3. In this example, the pure parallel program could not use 4 or more optical elements setups.

  6. Will the prime instrument "wait" for the pure parallel instrument to change filter/grating?
    Yes, the prime instrument will wait but the additional time will be charged to the parallel program. 

  7. What if a pure parallel program wants to use X filters/gratings, but the available slots only allow for (X-1) or less number of filters/gratings?
    Because redu
    cing the number of filters would be a change with respect to what the TAC approved, PIs are currently required to submit a change request to the Telescope Time Review Board (TTRB) in order to modify the number of spectral configurations. Pure parallels investigator teams are strongly encouraged to include in their proposals contingency plans for such cases, specifying which spectral configuration could be dropped if needed, and what the science impact would be. Approved programs that include contingency plans could fall back to those plans and would not need to submit a TTRB request. 

  8. Overall, how many pure parallel slots were available in Cycles 1 and 2? And how many of them were assigned? 
    Table 2 gives details on the available and assigned pure parallel slots.

    Table 2. Cycles 1 and 2 available and assigned science pure parallel slots

    CycleAvailable pure parallel slotsAssigned pure parallel slots

    Number of slotsTotal duration
    (hours)
    Number of slotsTotal duration
    (hours)
    115,8342103.06771.01282.0
    212,2911641.06461.01198.0


  9. How does the pool of slots for pure parallel science observations looks like?
    For each Cycle the slots look different, as they are driven by the prime programs selected by the TAC. As a reference for proposal planning, the plots below summarize Cycle 2 available slots for pure parallel science observations. Mechanism changes per visit are not reflected. To aid pure parallel observers, the file used to generate this plot is included here. Each row in the file corresponds to a prime visit. The "Number of Ext. Slots" is the total number of slots, where each slot is a single exposure for that prime visit. The rest of the columns have self-explanatory headers.

    Figure 1. Cycle 2 available pure parallel slots 

    Click on the figure for a larger view.

    The Y-axis indicates the number of slots (i.e., individual exposures) available per prime visit. X-axis indicates the maximum (left) and minimum (right) slot duration per visit. All parallel slots in a dither group must have the same exposure time. There are, however, visits with slots that don't belong to the same dither group, and therefore slots may have different durations. Science slots have no mechanism moves, but generally have mechanisms changes before and after. This is not a hard rule and there may be consecutive slots in a visit with the same spectral configuration.

  10. Can you say anything about over-subscription on parallel slots?
    Cycle 2 approved parallel programs did see a degree of over-subscription: both accepted pure parallel programs competed for the same slots, in terms of galactic latitude and number of slots per prime visit. In such cases, STScI works with the PIs to accommodate, as best as possible, both programs. Addition information on slots currently used per pure parallel program is provided on Table 3.

    Table 3. Slots currently used in Cycle 1 and Cycle 2 pure parallel programs

    CyclePure parallel programSlots currently used
    1PID1571272
    1PID221143
    1PID2514249
    2PID3383372
    2PID399038

      As of September 20th 2023, there is a plan to increase the number of slots available to program 3990.




Notable updates
  •  
    Added a file containing data used to generate Figure 1 in item 9 of the "Pure Parallels FAQ" section


  • Added a pure parallel FAQ section. The section includes information on slots availability in Cycles 1 and 2, and number of minimum and maximum slots duration per visit in Cycle 2.

  •    
    Added new coordinated parallel modes for Cycle 1


  • Added allowed pure parallel modes for Cycle 1.

  •   
    Made changes for consistency with current parallel capabilities being offered in Cycle 1.
    Removed Table 2 and streamlined listing in the text.

Originally published