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This article provides instructions for filling out the NIRISS single object slitless spectroscopy APT template.

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Introduction 

Main article: NIRISS Single Object Slitless Spectroscopy
See also: NIRISS SOSS Recommended Strategies, NIRISS SOSS Science Use Case, NIRISS GR700XD Grism

NIRISS Single-Object Slitless Spectroscopy is one of four observing modes available with the Near Infrared Imager and Slitless Spectrograph (NIRISS). The SOSS mode uses a grism to generate 3 orders of cross-dispersed spectra of a single target in the wavelength range from 0.6 - 2.8 μm. Spectral orders 1 and 2 are the usable orders. Order 1 covers the wavelength range 0.9 to 2.8 μm at a resolving power (R) of 700. Order 2 covers the wavelength range 0.6 to 1.4 μm at R=1400, while order 3 peaks at 0.6 μm, largely outside the sensitivity range of the detector. The SOSS mode is optimized for spectroscopy of transiting exoplanet systems around nearby stars. A built-in lens provides mild defocus in the cross-dispersion direction, effectively raising the brightness limit for saturation.

A typical SOSS observation will consist of a single target acquisition (TA) followed by continuous spectroscopic exposures with the GR700XD grism. TA is required if a subarray is used in the exposure and strongly encouraged for full frame read-out. 

The observer will have control over: 1) target acquisition mode and exposure time (via number of groups), 2) choice of full frame read-out or subarray for the GR700XD grism, and 3) SOSS read-out pattern and exposure time (via number of groups and integrations). 

Step-by-Step APT Instructions

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PageWithExcerptMIRI Imaging Template APT Guide

Target Acquisition Parameters

AnchorNIRISS_SO_TARGETNIRISS_SO_TARGETTarget Acquisition

        Main Article: NIRISS Target Acquisition
        See Also: JWST ETC NIRISS Target Acquisition 

Target acquisition (TA) positions the centroid of the brightest object in the TA field of view on the location of the SOSS aperture used for science exposures. An observer can specify one of the 3 options for ACQ TARGNONE, SAME TARGET AS OBSERVATION, or any source within the target list that is within 60" of the science target. TA is performed with the F480M filter in the Filter Wheel.

TA is required if using a subarray, and strongly encouraged for full frame read-out. SOSS data will be processed properly in the JWST calibration pipeline only if a TA was performed. The option of using SOSS in full frame read-out without a TA will require self-calibration of the data, which is strongly discouraged in Cycle 1. This option is only useful in attempting to obtain spectra of a few sources at once, and users who wish to attempt this are encouraged to coordinate with the JWST helpdesk to ensure that their observations are feasible.

There are 2 options for ACQ MODE, based on the M-band magnitude of the target as specified in the SOSS Template Parameters PageSOSSBRIGHT and SOSSFAINT. 

AnchorNIRISS_SO_ACQ_TIMENIRISS_SO_ACQ_TIMEAcquisition Exposure Time

        Main Article: NIRISS Detector Readout Patterns

The only permitted ACQ READOUT PATTERN for SOSSBRIGHT is NISRAPID. Both NIS and NISRAPID are available readout patterns when the ACQ MODE is SOSSFAINT. The observer can specify the ACQ NO. OF GROUPS (3, 5, 7, 9, 11, 13, 15, 17, 19), where a group is defined by the number of frames in an integration (for NISRAPID) or by the number of frames in an integration divided by four (for NIS).

SOSS Parameters

AnchorNIRISS_SO_SUBARRAYNIRISS_SO_SUBARRAYSubarray

        Main Article: NIRISS Detector Subarrays

The SUBARRAY options are:

  • FULL: full 2048 x 2048 array is readout, achieving higher S/N for faint targets.
  • SUBSTRIP256: 256 x 2048 subarray which captures all 3 spectral orders. 
  • SUBSTRIP96: 96 x 2048 subarray which only covers the first spectral order. This option allows faster readouts and thus has shorter integration times, enabling observations of brighter targets and those for which the science requires a high time resolution.
AnchorNIRISS_SO_TIMENIRISS_SO_TIMEExposure time

        Main Article: NIRISS Detector Readout Patterns

Specify:

  • READOUT PATTERN
    • NISRAPID: all frames are read and stored. Generally this can be used if the number of frames per integration is small and the data volume is not an issue.  Only available option when using a subarray.
    • NIS: four frames are averaged.  Used for producing a lower data rate for longer integrations of faint targets. Only supported for full frame readout.
  • NO. OF GROUPSthe number of groups during an integration, equal to the number of frames read per integration (for NISRAPID), or the number of frames read out divided by 4 (for NIS).
  • NO. OF INTEGRATIONSthe number of integrations during an exposure, where an integration is the time between detector resets.

The Exposure Time Calculator (ETC) should be used to determine the combination of NO. OF GROUPS and NO. OF INTEGRATIONS necessary to achieve the required signal-to-noise.

  

Other Tabs

Special Requirements

A variety of observatory level special requirements may be chosen.

 

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Related links

Instrument

Near Infrared Imager and Slitless Spectrograph, NIRISS
NIRISS Overview
NIRISS Single Object Slitless Spectroscopy
NIRISS GR700XD Grism

NIRISS Operations

NIRISS Target Acquisition

NIRISS Detector

JWST Detector MULTIACCUM Integration
NIRISS Detector Readout Patterns
NIRISS Detector Subarrays

NIRISS Performance 

NIRISS Bright Limits
NIRISS Sensitivity

Recommended Strategies

NIRISS SOSS Recommended Strategies

NIRISS SOSS Science Use Case

NIRISS SOSS Time-Series Observations of HAT-P-1

Observing Methods

JWST Time-Series Observations
NIRISS-Specific Time-Series Observations

Astronomer's Proposal Tool

JWST Astronomer's Proposal Tool Overview
NIRISS SOSS Template Parameters

Exposure Time Calculator

JWST Exposure Time Calculator Overview
JWST ETC SOSS Spectral Extraction Strategy
JWST ETC NIRISS Target Acquisition
Residual Flat Field Errors in the ETC

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References

JWST technical documents

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Last updated

Published May 1, 2017

 

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Updated April 5, 2017

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Published March 2, 2017

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