Cycle 1 Calibration - Absolute Flux Calibration

The absolute flux calibration of the James Webb Space Telescope follows a cross-instrument plan, with each science instrument observing stars from the same list of absolute flux standards.  To improve the efficiency of the observations, they are grouped into separate programs for each class of flux standard:  A dwarfs, Solar analogs (G dwarfs), and white dwarfs.  A fourth calibration program will repeat observations of the same standards on an approximately monthly cadence through Cycle 1 to serve multiple monitoring purposes.  The details of this plan should be considered provisional and may change in response to system developments and the final science program.

The text for each calibration activity below includes a title, program ID number, and the abstract also included with the APT file.  The program ID number links directly  to the STScI webpage for that program.  Users interested in obtaining APT files can either follow that link or retrieve the file by running the APT and retrieving it by its program ID.

Program 1536 - CAL-FLUX-001 - Absolute Flux Calibration (A Dwarfs)

Program 1537 - CAL-FLUX-002 - Absolute Flux Calibration (White Dwarfs)

Program 1538 - CAL-FLUX-003 - Absolute Flux Calibration (G Dwarfs)

Program 1539 - CAL-FLUX-004 - Absolute Flux Calibration (Repeatability)

Program 1536 - CAL-FLUX-001 - Absolute Flux Calibration (A Dwarfs)

This program obtains observations of A dwarf stars as part of the JWST absolute flux calibration effort. This effort uses all JWST instruments to provide absolute flux calibration for all JWST modes (filters, gratings, etc). The combined nature of this effort is to ensure the highest quality flux calibration internal to and between instruments and to carry out the observations efficiently. This program provides observations of A dwarf stars and companion programs provide observations of white and G dwarf observations. The absolute flux observations will be compared to model predictions of the stars flux densities to calculate the appropriate calibration factors per instrument mode

Program 1537 - CAL-FLUX-002 - Absolute Flux Calibration (White Dwarfs)

This program obtains observations of white dwarf stars as part of the JWST absolute flux calibration effort. This effort uses all JWST instruments to provide absolute flux calibration for all JWST modes (filters, gratings, etc). The combined nature of this effort is to ensure the highest quality flux calibration internal to and between instruments and to carry out the observations efficiently. This program provides observations of white dwarf stars and companion programs provide observations of A and G dwarf observations. The absolute flux observations will be compared to model predictions of the stars flux densities to calculate the appropriate calibration factors per instrument mode.

Program 1538 - CAL-FLUX-003 - Absolute Flux Calibration (G Dwarfs)

This program obtains observations of G dwarf stars as part of the JWST absolute flux calibration effort. This effort uses all JWST instruments to provide absolute flux calibration for all JWST modes (filters, gratings, etc). The combined nature of this effort is to ensure the highest quality flux calibration internal to and between instruments and to carry out the observations efficiently. This program provides observations of G dwarf stars and companion programs provide observations of white and A dwarf observations. The absolute flux observations will be compared to model predictions of the stars flux densities to calculate the appropriate calibration factors per instrument mode.

Program 1539 - CAL-FLUX-004 - Absolute Flux Calibration (Repeatability)

This program obtains repeated observations of two stars as part of the JWST absolute flux calibration effort. This effort uses all JWST instruments to provide absolute flux calibration for all JWST modes (filters, gratings, etc). The combined nature of this effort is to ensure the highest quality flux calibration internal to and between instruments and to carry out the observations efficiently. This program provides observations of two stars spread throughout the year to measure the repeatability of JWST observations. The aim is to observe in one filter/grating/etc per detector to measure how repeatable an observation is in instrument units. The expectation is that the repeatability is set at the detector level.




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