Note: this module is still in the beta testing phase and is not yet demonstrated to be suitable for science.

Known Limitations

• On-orbit gain, and on-orbit readout noise have not yet been incorporated.
• A current limitation to the PSF models is that the cruciform structure has not yet been incorporated into the optical model.
• Stage 2 Data Quality (DQ) arrays have not been thoroughly tested for reliability. In the current release, (a) pixels flagged as saturated by the pipeline (DQ array value of 2) are considered saturated, (b) other pixels masked out by the pipeline (Science array value is exactly zero) are considered bad pixels, and (c) all other pixels are assumed good.
• DOLPHOT currently uses the file data in the FITS headers, rather than what is provided in the ASDF extension.
• DOLPHOT does not yet support MIRI subarray observing modes.

Possible Limitations (Testing in Progress)

• Limited testing to date has been performed only on data obtained by program JWST-GO-02128
• Comparison of observational CMDs to isochrones and/or synthetic CMDs (e.g., as a check on zero points and calibrations) not yet performed
• Impacts from time variability of the PSFs not yet assessed

Longer Term Enhancements

• Identification of optimal DOLPHOT parameters for both short and long modes
• Incorporation and testing of additional empirical PSF libraries
• Testing combined photometry with MIRI and other instruments

Please provide feedback if you use this code, as it will be greatly appreciated whether or not there were issues.

If you make use of the JWST MIRI module in your work, please cite Peltonen et al prep in addition to the DOLPHOT references (Dolphin 2000 and Dolphin 2016).

DOLPHOT 2.0 MIRI module sources (updated 6 Apr 2023)
DOLPHOT 2.0 MIRI module manual (also included in sources)