This example science program provides a walkthrough of creating a JWST deep extragalactic survey program of multi-object spectroscopy (MOS) using NIRSpec MOS.

Example Science Program #25

Dated material

This example program was constructed pre-launch, and details may be out of date with actual observatory performance. However, it still provides a useful example for training purposes.

Please refer to JWST Example Science Programs for more information.

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This article walks users through a science use case to plan deep NIRSpec Micro-Shutter Assembly (MSA) observations of faint high-redshift galaxies in a pencil-beam survey field. The goal is to obtain medium resolution spectroscopy for a sample of ~200 galaxies with redshift (z) in the range 2 < z < 6. The full suite of optical emission lines, from [O II] to Hα will be observed, along with the ultraviolet [CIII], CIII] 1907, 1909 Å doublet for a sub-sample of galaxies at 5 < z < 6. NIRCam parallel imaging will also be obtained to help select targets for future follow-up spectroscopy at these same redshifts.

Galaxies are selected which have a spectroscopic or photometric redshift which places their Hα and/or [CIII], CIII] emission in the NIRSpec medium resolution gratings. Figure 1 shows an example galaxy field from a Hubble image with slits placed over three galaxies of interest to illustrate this science use case.

A zoom-in Hubble image of a deep pencil beam field is shown. Target galaxies have slits placed over them (red boxes). The three-shutter slitlet pattern used in this use case is shown.

The science goals of this program are to obtain measurements of star-formation rates, dust content, ionization state, and spectroscopic redshifts for a sample of ~200 galaxies at 2 < z < 6. This will help us understand the physical states of galaxies in the very high redshift universe. It will significantly improve our understanding of how galaxies evolve in their early turbulent phases, and will place constrains on models for galaxy formation and evolution. Specifically, for galaxies at redshifts 2 < z < 5, you will use the Hα emission line in the optical at 6563 Å and additional optical lines that fall into the wavelength ranges of the observed spectra. At redshift 5 < z < 6 you have access to both Hα and the coveted [CIII], CIII] doublet. This diagnostic will allow for a better determination of the galaxies’ metallicities and ionization states. You do not need for the doublet to be resolved for the science goals. Note that you are only observing the brightest sources at 5 < z < 6, where the relatively low equivalent CIII] emission is most likely to be detected.

The aim is to design observations for an extragalactic multi-object spectroscopy (MOS) survey to meet the science goals by surveying emission lines from a statistical sample of galaxies. Choose the GOODS-S field for these observations, using the catalog from Momcheva et al. (2016). An overview of the capabilities and performance of NIRSpec MOS mode are presented by Ferruit et al (2022).

Step 1 - Determine the range of feasible MOS Aperture Position Angles (APA) for the area of interest

Use the JWST General Target Visibility Tool (GTVT) to find reasonable APAs. For the GOODS-S field which has a central pointing of RA = 03:32:33.00, DEC = -27:48:47.0, you'll find that APAs between 30° and 210° will be available from August 2021 to February 2022. For the case shown here, test an APA of 60°.

STScI recommends that users test several angles using the steps that follow, to determine whether multiplexing (science) results depend on the assigned orientation. In general, specifying a tightly constrained orientation is discouraged, as it may decrease scheduling efficiency.

Step 2 - Obtain or create a source catalog of sufficient astrometric accuracy

Existing Hubble Space Telescope (HST) imaging within the GOODS-S field has relative astrometric accuracy better than 20 mas, allowing precise target acquisition and placement of objects in the 0.20" x 0.46" MSA shutters.

Step 3 - Decide on a target acquisition strategy

Choose the MSA Target Acquisition (MSATA) strategy for this program since this is the only way to reliably place the targets in the MSA shutters.

Step 4 - Optional NIRCam Pre-Imaging

This step can be skipped since the field has existing HST imaging which achieves the required relative astrometric accuracy.

Step 5 - Pick desired wavelength setting(s) for MOS observations

You wish to observe the Hα emission line in galaxies at redshift 2 < z < 5, requiring grating/filter combinations of G140M/F100LP, G235M/F170LP, G395M/F290LP. For the higher redshift galaxies at 5 < z < 6 where you hope to detect [CIII] and CIII], you require the G140M/F100LP disperser/filter combination.

Step 6 - Determine which dither strategy to use

You will choose to nod, taking an exposure in each shutter of the 3-shutter slitlet. Since nod positions can serve as dithers, choose not to add any additional dithers. This choice increases efficiency in two ways:

You do not have to reconfigure the MSA, saving 90 s of overhead.
You do not suffer multiplexing losses, due to the requirement that the sources be observable in two configurations, rather than one.

The down-side to this choice is that the spectra will have a wavelength gap, due to NIRSpec’s chip gap, a compromise you'll have to accept. Note that adding a 20” fixed dither to cover the chip gap would still result in half the exposure time, and a non-uniform signal to noise, over certain wavelengths. For users concerned about wavelength coverage, the MSA Target Info export file contains the wavelength coverage for each slitlet in the MSA field of view.

Step 7 - Learn about recommended practices for dithering, background subtraction, MSA leakage and general MOS recommendations

Step 8 - Determine the required exposure and detector parameters for your MOS observations

Words in bold are GUI menus/
panels or data software packages;
bold italics are buttons in GUI
tools or package parameters.

Choose the NIRSpec IRS² Detector Readout Mode, which reduces correlated noise and is recommended for long exposures. The IRS² readout mode has two patterns: NRSIRS2 and NRSIRS2RAPID. The former reduces data volume by averaging 5 frames, whereas the latter does not average any frames. The NIRSpec Detector Recommended Strategies article provides more guidance on choosing a readout mode and pattern. Choose NRSIRS2, as data volume from the added NIRCam parallels can be large. Since the exposures are long, you should anticipate that frame-averaging will have an insignificant impact on the measurements.

To determine the exposure parameters (the number of groups and integrations) for this program using the Exposure Time Calculator (ETC), please see the article MOS Deep Extragalactic Survey ETC Guide.

Step 9 - Create NIRSpec MOS Observations in the MSA Planning Tool (MPT) and Astronomers' Proposal Tool (APT)

For instructions on how to fill out the MSA Planning Tool (MPT) and Astronomers' Proposal Tool (APT) for this program, please see the article MOS Deep Extragalactic Survey APT Guide.

References

Curtis-Lake, E., et al. 2016, MNRAS, 457, 440
Non-parameteric analysis of rest-frame UV sizes and morphological disturbance amongst L* galaxies at 4 < z < 8

Ferruit, P., et al. 2022, A&A, 661, A81
The Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope. II. Multi-object spectroscopy (MOS)

Grogin, N., et al. 2011, ApJS, 197, 2
CANDELS: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey

Momcheva, I. G., et al. 2016, ApJS, 225, 2
The 3D-HST Survey: Hubble Space Telescope WFC3/G141 Grism Spectra, Redshifts, and Emission Line Measurements for ~100,000 Galaxies

Rigby, J. R., et al. 2015, ApJL, 814, 1
C III] Emission in Star-forming Galaxies Near and Far

Tremonti, C. A., et al. 2004, ApJ, 613, 2
The Origin of the Mass-Metallicity Relation: Insights from 53,000 Star-forming Galaxies in the Sloan Digital Sky Survey

Notable updates
Originally published	28 Nov 2017

JWST User Documentation

NIRSpec MOS Deep Extragalactic Survey