Parent article: NIRSpec MOS Operations
See also: NIRSpec MOS Operations - Slit Losses
One of the main observing modes of NIRSpec is the multi-object spectroscopy (MOS) with the micro-shutter assembly (MSA), which consists of roughly a quarter million configurable shutters that are 0.20" × 0.46" in size. The NIRSpec MSA shutters can be opened in adjacent rows to create customizable and positionable spectroscopy slits (slitlets) on prime science targets of interest. Because of the very small shutter size, the NIRSpec MSA spectral data quality will benefit significantly from accurate astrometric knowledge of the positions of planned science sources.
Images acquired with the Hubble Space Telescope (HST) usually have an the internal relative astrometric accuracy of 5–10 mas that is optimal for planning NIRSpec observations. Tiled mosaics of multiple HST image fields may have slightly decreased accuracy compared to the 5 mas level, but are an improvement over the typical in-field relative accuracy of lower resolution space based images (i.e., Spitzer Space Telescope) or ground-based cameras. Images from the HST ACS or WFC3 can provide the necessary in-field accuracy for NIRSpec spectroscopy planning. However there are reasons why other sources of imaging may be necessary: some fields of interest have no or insufficient HST imaging, galactic fields have moderate proper motions that would preclude using HST imaging from earlier epochs, and extragalactic regions observed with HST may lack source detections required for planning NIRSpec observations at wavelengths beyond 2 μm.
Moreover, the Wide Field Camera 3 (WFC3) infrared (IR) camera spans a smaller footprint than the NIRSpec MSA; a single WFC3 IR image may not provide the best catalog source for NIRSpec MOS spectroscopy across the full field of view. Images acquired with the Spitzer Space Telescope cameras or most ground-based imagers do not have adequate astrometric accuracy or field coverage for optimal NIRSpec MOS spectroscopy planning. Thus, optimal NIRSpec MOS planning and data calibration may require pre-imaging observations with the Near-Infrared Camera (NIRCam) on JWST to accurately establish source positions for alignment and configuration of the NIRSpec MSAs and target acquisition (MSATA) for IFU and FS science.
Pre-imaging observations for NIRSpec MOS science or MSA-based target acquisition are optional and not required if they can be planned with existing images and catalogs.
To aid in understanding planning constraints and field coverage, a NIRSpec Observation Visualization Tool was created to simultaneously view both the NIRCam imaging footprints and NIRSpec MOS field of view.
What is pre-imaging and when is it needed?
grid of micro-shutters, hence science sources of interest cannot all be perfectly centered within their configured shutters or slits. These centering offsets and the very small NIRSpec MSA shutter size result in moderate flux that can be lost outside of the slit. The slit throughput loss sources within the MSA shutters. Very high quality planning astrometry will limit calibration errors that result from uncertain spectral source positioning after target acquisition. In-field relative astrometry of 5–10 mas or better is needed to limit the excess flux calibration error for point source observations.
NIRCam is the workhorse imaging camera at 1–5 μm wavelengths for JWST. It is the preferred camera for high quality images for same-cycle JWST NIRSpec spectroscopy and target acquisition planning. NIRCam will provide imaging for high precision source catalogs that can be used to plan follow-up spectroscopy with NIRSpec. For this reason, same-cycle imaging with NIRCam (referred to as "NIRCam pre-imaging") is available to support and plan programs that use the NIRSpec MSA for spectroscopy or target acquisition.
In JWST observing cycle 2 and beyond, NIRCam images acquired in previous cycles will be excellent resources for NIRSpec observation planning. These images are not acquired using the same process as the NIRCam pre-imaging defined here. The NIRCam pre-imaging process we discuss here refers primarily to planning images acquired in the same observing cycle as the NIRSpec spectroscopy.
Observing process for NIRSpec spectroscopy with NIRCam pre-imaging
JWST NIRSpec MSA-based observations (MOS or MSATA) require a fixed orient assignment in order to plan the spectroscopy or MSA target acquisition. Across the 3.4' × 3.6' field of view of NIRSpec, very small deviations away from a planned orient can cause science sources to move out of their MSA shutters, as well as cause problems with the target acquisition reference star placement locations. As a result, NIRSpec programs that use the MSA must have a follow-up planning process after the proposal submission and program acceptance.
After projects are accepted by the TAC, planning teams at the Space Telescope Science Institute (STScI) will assign a fixed aperture position angle and execution window in the long range plan (LRP) for all NIRSpec MSA-based observations. After NIRCam pre-images and catalogs are available, the NIRSpec spectroscopy will be planned at the assigned fixed orient. NIRSpec spectroscopy observation requests will be submitted as place-holders at the proposal time, and updated for “flight-ready” status once pre-imaging observations are obtained and a fixed aperture position angle and observation execution window is assigned.
Figure 1 shows the timeline for a sample NIRSpec science program that uses the MSA and requests JWST NIRCam pre-imaging. At the time of proposal submission, the observing program must include: (1) the requested NIRCam pre-imaging observations specified using the NIRCam imaging template, (2) placeholder visits for NIRSpec spectroscopy that request the appropriate amount of time for the science, and (3) any observation links or special requirement constraints requested on the final program visits.
Figure 1. The JWST observing cycle timeline for NIRSpec MSA-based observations that request NIRCam pre-imaging
The during a JWST observing cycle for a science program that requests NIRCam pre-imaging in support of the NIRSpec MSA planning process for MOS science or MSATA.
- After the TAC meets and programs are approved, the long range planning team at STScI will incorporate accepted programs into a schedule for the cycle, place NIRCam pre-imaging visits at appropriate target visibility windows, and assign fixed Aperture Position Angles to NIRSpec programs that use the MSA.
- After the NIRCam visits execute and the pre-imaging is acquired, the pipeline-generated mosaics and catalogs will be uploaded to the MAST archive. The plan is to optionally have STScI team members available for review assistance, in an approximately 2- to 3-day time frame following the pre-imaging, to help verify NIRCam mosaic astrometric image accuracy and the quality of science target catalogs.
- The planning process for the NIRSpec spectroscopic science and target acquisition can commence once the images and catalogs are ready. The recommendation is that observing teams have at minimum 4 weeks to plan the spectroscopy using the NIRCam imaging products. Later in the observing cycle, the NIRSpec MSA science or TA visits will be scheduled at the prescribed fixed Aperture Position Angle used to plan the observation.
- The fully defined and executable NIRSpec MSA program submission due date will be
At the present time, there is a recommended minimum of 60 days between the JWST NIRCam pre-imaging observations and the JWST NIRSpec spectroscopy observations (both shown in red in ); one month for s, and one month for instrument scientist and program coordinator verification and scheduling.
Table 1 outlines the time frame of activities at STScI prior to NIRSpec spectroscopy execution (also described in detail in the MOS Observation Process article). The absolute minimum allowed time frame between JWST NIRCam pre-imaging observations and the JWST NIRSpec spectroscopy observations is 42 days: STScI staff need 4 weeks for internal review, leaving just 2 weeks for teams to plan the spectroscopy after NIRCam images are acquired. The flow presented in Figure 1 will be reviewed and updated as operational experience is gained with the NIRCam pre-imaging process during Cycle 1.
The absolute minimum allowed time frame between JWST NIRCam pre-imaging observations and the JWST NIRSpec spectroscopy observations is 42 days: 4 weeks for internal STScI review and processing, leaving just 2 weeks for teams to plan the spectroscopy after NIRCam images are acquired. The flow presented in Figure 1 will be reviewed and updated as operational experience is gained with the NIRCam pre-imaging process during Cycle 1.
Proposals that request NIRCam pre-imaging to plan NIRSpec MSA observations (MOS science or MSATA) should also be submitted with an observation TIMING special requirement (specifically, an "AFTER Observation Link") on the NIRSpec observation linking the NIRCam imaging observation(s) and the NIRSpec spectroscopy observation (e.g., "AFTER <Obs 1 (NIRCam observation)> BY 60 days to 100 days"). The absolute minimum separation between the NIRCam pre-imaging and NIRSpec observation is 42 days, but 60 days is the recommended minimum, as described above. APT does not currently sufficiently enforce these separations, so please use caution.
Additionally, an ON HOLD special requirement on the NIRSpec MOS science observation should be present with the note: "ON HOLD for Aperture Position Angle assignment" (also described in detail in the MOS Observation Process). also be reviewed during instrument scientist checks of accepted programs.
DK moved this to internal comment, recommended by Alaina to shorten article.
Table 1. STScI internal review of flight-executable MOS or MSATA observations
|Time frame before science observation window||STScI NIRSpec flight-executable program review activity|
|28 to 21 days||Instrument scientist review of MOS or MSATA observations|
|21 to 14 days||Program coordinator checks of MOS or MSATA observations|
|14 to 0 days||Short term scheduling of executable visits|
Observing with NIRCam for NIRSpec spectroscopy planning
NIRCam and NIRSpec fields of view
Figure 2. Sky projection of the relative sizes of the JWST/NIRSpec MSA (left) and JWST/NIRCam fields (right) fields of view for both wavelength channels
Sky projection of the relative sizes of the JWST/NIRSpec MSA field of view (left) and JWST/NIRCam fields (right) for both wavelength channels (not at the same spacecraft orient). Size of the apertures are given in arcseconds. The NIRCam SWC and LWC simultaneously observe the same imaging field, they are presented offset here to highlight the areas sampled by the 10 detectors (8 in SWC, 2 in LWC).
Figure 2 shows the four NIRSpec MSA quadrants as projected onto the sky and, for comparison, we also show the fields of view of the NIRCam imager in its two modes: long and short wavelength channels. The NIRCam detectors will image the same field of view but for illustration we separated them. It is evident that the NIRSpec field of view is large in comparison to that of NIRCam. For this reason, creating a finder image with NIRCam in order to cover the NIRSpec MOS field
of interest will require some planning, including dither patterns and mosaicking
NIRCam options for pre-imaging: filters, dithers and mosaics
The Near Infrared Camera (NIRCam) is the 1–5 μm imager on the JWST and will provide excellent sensitivity imaging for precision source catalogs that can be used to plan follow-up spectroscopy with NIRSpec. NIRCam acquires simultaneous images in 2 channels—the short wavelength channel (SWC) and long wavelength channel (LWC)—using 10 detectors. The 2 channels have a wide range of filter options available including wide, medium and narrow width filters matched to emission features. The NIRCam F115W filter available in the SWC is very well matched in profile to the NIRSpec F110W filter, which is used primarily for MSA target acquisition with NIRSpec.
The NIRCam instrument has a footprint that spans an extent of 5.1' × 2.2' on the sky. There is a gap of ~40′′ between the two NIRCam modules. The field of the SWC is sampled by 8 detectors with 32 mas/pixel and 5′′ gaps in between individual module detectors, and the LWC uses two detectors with 65 mas/pixel. See Figure 2.
NIRCam SWC and LWC data can be acquired with dithers and mosaics to create images that cover the more complete observing footprint of the NIRSpec field of view. There are a few available options that can achieve the full field coverage of the NIRSpec MSA footprint. Table 1 shows three recommended dither patterns that can be used to provide near continuous (>95%) field coverage of the NIRCam footprint (covering detector gaps) in both the SWC and LWC channels. All of these dither patterns come from the FULL dither option for NIRCam, which provides the patterns designed to span the detectors and cover the full field of the instrument. At present, an additional FULLBOX dither pattern suitable for tiling an area for NIRSpec follow-up observations has been defined, called 8NIRSPEC. Further details on this and other NIRCam tiling patterns can be found at NIRCam Primary Dithers.
The 3-Point TIGHT pattern consists of three offset positions that are optimally designed to cover the gaps in the SWC and provide good coverage and depth in the central area of the dithered image. The 3-Point TILE pattern is similar to 3-Point TIGHT, but the offsets in the vertical direction are larger which provides wider overall field coverage, but more extended detector gaps toward the edges. The 6-Point TILE pattern provides deep field coverage in the central regions of the field and over a more extended footprint than either of the 3-point patterns can provide. The fixed offsets defined for each dither pattern are listed in Table 1. Figure 3 shows two examples of these dither patterns; the 3-point TIGHT and 6-Point TILE dither coverage, overplotted with the NIRSpec MSA footprint (at the same observatory orient angle). In order to completely cover the NIRSpec MSA field of view, one of the below dither patterns plus a mosaic tile position may be necessary.
The FULLBOX 8NIRSPEC dither pattern covers a large area: 6' × 5' to serve as pre-imaging for NIRSpec MSA spectroscopy. It consists of eight pointings with offsets listed in Table 1. Note that 5th dither and the return to the start are very large and will result in visit splitting for any target.
Table 1. Recommended NIRCam dither patterns for pre-imaging
Dither pattern name
FULL 3-Point TIGHT
-58′′ 0′′ +58′′
-7.5" 0" +7.5"
FULL 3-Point TILE
-58" 0" +58"
-23.5" 0" +23.5"
|FULL 6-Point TILE||-72" -43" -14" +15" +44" +73"||-30" -18" -6" +6" +18" +30"|
|FULLBOX 8NIRSPEC||-24.6" -24.4" 24.6" 24.4" 24.6" 24.4" -24.6" -24.4"||-64.1" -89.0" -88.8" -63.9" 64.1" 89.0" 88.8" 63.9"|
NIRCam imaging acquired with the described FULL dither options from Table 1 may be insufficient for planning spectroscopy over the full NIRSpec field of view. However, NIRCam observations can also be mosaicked or tiled to create a wider image, beyond the size of the main NIRCam footprint. The 8NIRSPEC dither pattern is large enough to accommodate the MSA footprint.
A selection of one of the dither options presented in Table 1 combined with a 2 × 1 mosaic pattern with NIRCam can be used to provide full coverage of the NIRSpec field of view at any observing position angle (See Figure 4).
The NIRSpec Observation Visualization Tool was created to investigate field coverage between the NIRCam and NIRSpec MSA footprints in support of the pre-imaging process.
Figure 3. The NIRCam 3-point TIGHT and 6-point TILE Dither Patterns with NIRCam
The HST image of the Tarantula Nebula (PI: E. Sabbi) with a NIRCam 3-point TIGHT dither pattern and the SWC over plotted (a) and a NIRCam 6-point TILE dither pattern with the LWC shown (b). NIRSpec MSA quadrant views are over plotted in both cases.
Figure 4. Coverage of a NIRCam image with 6-point TILE dither and a 2 × 1 mosaic
The Tarantula Nebula image with a two tile NIRCam LWC mosaic shown. Overplotted in green and yellow is the NIRSpec MSA quadrant field of view at two possible spectroscopy execution orients. The 6-point TILE pattern with a 2 × 1 mosaic covers a wider extent field than the MSA quadrant footprint.